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1. N mee LU U e H X e VE TR WE LP rhe Sya L mise x A AS TA Nc ta owe REG a ah N L Kr vf ns oR i w E gt r iU figure shows a browse view of some of the data imported into a workstation in a single frame More information about the data can be obtained by using other McIDAS tools by clicking on each of the thumbnail images in the overview frame McIDAS eXplorer user interface At its core McIDAS and McIDAS eXplorer are command driven and not menu driven A certain familiarity with the command syntax is thus necessary until users become proficient To eliminate the need to learn the syntax of different commands a graphical user interface GUI has been developed for McIDAS eXplorer so that both text or command line and a GUI are available The command line and the GUI are supple mented by function keys and single letter key strokes to communicate with McIDAS eXplorer The function keys are user programmable to fit oe ee CH S 4 lt aire EE we ee a tr E N E La H k y HZ a N soe ka F 1 AAA EA AAA A APE ARA TT PISE vara nra N epn cA e T A De ty 1 79 L A 1 ADA Terit Y eaa RNT ThA menu sows you to choose the planet Mortis Chosen you are to sederl whet m The nera ap unns are set up in such a way HS 3 KP YOU cho34 and they prompt you ts anage finding it ether on a CD or ma fe Once the unage n loaded you have the opt the vous ba IDAS
2. A negative darea signifies that the destination area should be overwritten if it already exists This command allows one build a visual index of the images imported or processed into McIDAS areas The output should be displayed using the DF key in at full resolution so that my using the mouse each image can be queried using the SCANE command APPENDIX I 88 SCNCPP Scan the file containing a Pioneer Venus Orbiter Cloud Photopolarimeter OCPP image of Venus in the NSSDC tape format to determine the average spin period look angle roll angle changes and log the information to a file SCNCPP area filename LOG logfilename KEYWORDS HELP print the TEXT file containing the explanation of the CPP data REMARKS This command is useful for diagnostic purposes if after importing the image into eXplorer using GETCPP some discrepencies are found in the data or navigation APPENDIX I 89 SCANE This command allows one to query the contents of the index frame created and displayed from the output of the SCANA command A command string relating to that area can be specified containing an as a replaceable character for the area number corresponding to the image selected by positioning the cursor with the mouse and clicking on the right button The command will stay resident for 30 minutes or unti ALT G key stroke is entered while in the command window Command should be entered when an area created using SCANA is bei
3. DSN NAIF Code Time Year Time Day Month Time hh mm ss Size in scan direction Size in cross scan direction 182 Eccentricity of Orbit 183 inclination of Orbit to Ecliptic 184 Ecliptic Longitude of Ascending Node 185 Argument of Periapsis 186 Orbital Period 187 Semi Major Axis of Orbit 188 Ecliptic Latitude of Periapsis 189 Ecliptic Longitude of Periapsis 190 Altitude from Target Center at Periapsis 191 192 Image Compression Algorithm LEFT RIGHT OTHER Central amp Picture Body 193 195 Central Body Name 196 Central Body NAIF Code 197 199 Picture Body Name 200 Picture Body NAIF Code hrs km SORT e2 p2 p 201 Picture Body Rotational Period 202 Picture Body Pole Right Ascension 203 Picture Body Pole Declination 204 Nominal Picture Body Eq Radius 205 Nominal Picture Body Pol Radius km 206 Nominal Picture Body Cross Eq Radius km 207 209 Spare 210 Picture Body Eccentricity 211 256 Spare WORD ITEM Imaging or Map Projection Geometry 257 Map Projection Type 258 Original Map Scale 259 Sampling Factor 5 18 TYPE COMMENTS C 8 1 4 1 4 C 6 C 4 C2 MIDR C 8 LLNLLL I 4 I 4 I 4 1 4 1 4 I 4 C s I 4 1 4 C s R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 cs NONE HUFFMAN LZW etc TYPE COMMENTS Crd I 4 EE Lg R 4 R 4 R 4 R 4 R 4 R 4 R 4 TYPE COMMENTS c 4 generally SIN R 4 1 4 260 Image Scale Factor km pixel 2
4. 1 Creating an output area to store the result So that the output can be readily identified it is best to attach the same directory information for the output as is available for the source image There are two ways to accomplish this one is to use the AA command to copy the directory and create an output area of appropriate size the DDB and the processing history records AA source_area output_area frame_ coord_type x_coor y_coor 1 _lines _elements The second method eliminates the need to copy the entire data by using the MAKOUT command to create the output area directory based on the source area MAKOUT source_area output_area SIZE _lines _elements _bytes pixel pe Attaching the required navigation for the output area The second task is to attach the proper navigation information for the output image corresponding to the projection desired This is accomplished using the MAKNAV command for the rectilinear constant scale factors for latitude and longitude map and most standard cartographic projections polar stereographic sinusoidal equal area transverse Mercator Lambert Conformal and Mollweide equal area projection For perspective views of a planet or a moon the navigation for the output area is created with the PLANAV command MAKNAV output area 4 RECT ine lat ele lon degplin degpele PLANET MAKNAV output area SIN n at ele lon degplin degpele PLANET MAKNAV output area PS lin ele lat fon pixsiz hemisphe
5. COMMENTS EEE 22 l1 or 1 COMMENTS e O r a ee ee dt mage MEXP FIT 309 397 358 399 360 377 3138 399 396 413 414 431 432 433 434 435 MEXP FIT McIDAS eXp Flexible Image MEXP VO McIDAS eXp Viking Orbiter specifies user dependent block format Spare Computed North Angle from Limb fit Computed Transform Matrix Inst gt PicBod Computed Transform Matrix Inst gt Planet Computed C Matrix Inertial gt instrument Computed Rot Matrix Inertial gt PicBody Computed Optic Axis RA Computed Optic Axis Decl 436 Minnaert Fit Constant Max DN Used 437 Minnaert Fit Constant Cale Slope 438 Minnaert Fit Constant Calc Intercept 439 Minnaert Fit Constant Mean Abs Dev 440 441 442 443 444 445 446 447 448 449 450 451 452 460 461 462 Picture Body Center Line Picture Body Center Element Pixel Diameter of Picture Body Navigation Status Navigation System Type Image Navigation Processing Status Spare ITEM Supplementary Information o am a y y n ee e A s ie mr r e A r e k A A e AAPP A ee Supplementary Block Type 463 465 Data Source Laboratory Scientist 465 512 Spare 5 23 Transport System R 8 R 8 R 8 R 8 R 8 R 8 R 8 I 4 R 4 R 4 R 4 R 8 R 8 R 8 66 CY D C 6 TIPE C 8 CIZ Not used for Nav 11 If avaiable and necessary needed for Pul TS COMMENTS SUPD ELE r e n m p cor m ia e e e r m r ar re mer ee mm m r wrar v s mes ee ee s
6. May be used to convert 2 dimensional data in standard FITS format to a McIDAS area This may handle some Faint Object Camera FOC data Different sources use different header formats and keyword spellings which are mapped in a text file named SOURCE EIT where SOURCE is input here as a keyword value If the SOURCE keyword is not used the data file must have a standard FITS header and all standard keyword spellings as defined by NOST 100 0 3b LABEL List the header label only Default DATA Create an area HIST List the plotted 256 bin histogram values while creating the area may be useful for setting the RANGE keyword values frame_number magnification Frame number on which to display w magnification Target Object name The program will complain if it cannot find a target identification in the header information or if the header and user specified target are not the same The user will then have to make a runtime decision Minimum DN value for bright limb in unconstrained fit to locate the planet center Defaults to mode DN 6 PIXSIZ PIXSIZ which is 4 6 histogram bins above the dark noise peak This is crucial to good limb points and conic fit Failure to specify SKY may cause center finding to fail with poor or hyperbolic fit to ellipse or program may locate limb inside or outside the correct location Image cannot be properly navigated if that occurs APPENDIX 36 NORTH S AMP TIMEZONE SWAPB
7. TIRO for Polar Orbiter Nadir Scanners or binary 0 GODO or binary 80808080 for no navigation If the type is PLAN the succeeding words are the same as the 128 word McIDAS MVS planetary navigation codicil format This navigation format provides geometry parameter and a matrix for conversion from a framing camera image to planet lat lon coordinates and contains some redundant information from the Supplementary Experimenter Data Records SEDR for Manner 10 and Voyagers l amp 2 Other map projections are usually just sets of a few map parameters and scale factors and fill just a few of the first 128 words The first 128 word block must be loaded by a call to subroutine NVPREP prior to doing anything with a McIDAS navigation module This is normally handled by each applications keyin 5 4 DATA DESCRIPTION BLOCK The last 512 words in the navigation block are part of the Data Description Block DDB The words fall into five groups 1 Spacecraft Image amp Instrument Specific 129 192 Describes orbit parameters instrument and image types 2 Central amp Picture Body Specific 193 352 Describes target body physical constants and positional parameters WRT the central body 3 User Computed Quantities 353 460 Ancillary information used in data analysis by the scientist Fixed block size amp format 4 Supplementary Information 461 512 User definable block 5 13 5 User Defined Navigation 513 640 D
8. photometrically calibrate the data and to navigate it The calibration in general requires the following steps 1 Interpolate the data for image compression gaps primarily Voyager 2 Uranus and Neptune system data 11 Determination of the image geometric distortion by locating the reseau marks in the image ili Photometric calibration of the image output is a new area using the shading file for the appropriate camera and filter and a dark current file appropriate for the exposure and data rate Ideally the dark current file should be created from appropriate dark frames acquired as close in time to the image in question as possible Typically four or more dark frames should be averaged and or smoothed spatially iv Geometric rectification of the photometrically corrected image new output area These four steps can be accomplished by a single macro command provided appropriate dark noise area is available Unlike VICAR eXplorer does not do internal geometry correction in the navigation of the data and hence the geometric distortion must be removed by remapping the data into object space prior to making any position measurements Refer to How to Navigate Planetary Images to navigate the Voyager images Images with FITS headers Use GETFITS to import images with FITS headers If the headers contain enough information about the imaging geometry and calibration then the images can be navigated and calibrated If the exact k
9. a with INV OHO SORO 1 du gt o vD AAA 4 stk A vi ED KAD 747 OA p Fx tae woen Lo stack zeua sal Coen ROMP mre Po ee ar SR AS nS 0 Wi act K La Prior Conter o OL OPO a Er NOAA EOD EE EEE RA AADA ARAARA A A A g A AAA AA i haoa a i a i Y REEERE A EEE EE EE EEE PEPP PEPP AJA IIA Jr fa ett stg OCG AEE AAN P kale e a e AA Kaea ee Nae AN PONE ANI es wee EAARARA RARA PLOLLEPL PEL Figure 1 2 An illustration of the Graphical User Interface that cascades menus from which tasks can be chosen with mouse button clicks utes PLP PLLA LE LL SLL IAAL PEL AR ED A y lt EE 22 7 ORARE RERA RARER AARAA IR Nee E L C I T L 9 y eo aaa ee III SAA nn AAA AL AAA AAA RARA RARA RARA RARA SARA AR ARA RARA ARA RRA RR RAR AR RRAR RA ARA ARTIC RAR ELA tie ts oe Y SA ARA RARA AA AAA AAA LIEBE IL A IICA IIA a e RARA AAA RARA ARAARARAARRARRA ARA RA EBIDPIGIDA IIA CA IICA COC AAA IIA AAA EA ASS E R RRA RRA RRA AAA ddd RARA RAR RARA RA RARA RA EP ddd ddd CEE PD DTE PP E PPE DAA AAA AI AA ACA ICALI ee ee Hisplay an Image from an Hres Enbarce Frame B W Res stor e Enhane CENT Tabla ARSE ATA TRE Ree eee eee eee ee eee ee eee ee eee ee eRe Ne K KA A i Y G R an Enhancement Table a See ata De scription Black NNN N Na LG S CD ROM directory S RIN Press ESC key to Exit Henu A 1 3 An ion of E Function a Key based User interface This one invoked from a tent file containing the menu script
10. s database displayed in different frames and this information is available to the application programs and the user McIDAS 1s designed as a dynamic environ ment so that new applications can be developed and released for use even in operational situations e g mission support McIDAS uses a unified approach to data calibration navigation and display with a common interface both to the user and to the software applications for different data and different solar system objects The approach it takes and the capabilitics enabled are summanzed below McIDAS eXplorer enables use of the SPICE kernels for image navigation and also provides tools to determine the navigation transforms when the kernels are not available but the basic image geomctry information namely the trajectory and pointing information are available In this case full or partial disk images containing at least some portion of the bnght limb can be navigated by finding the limb points the image center and the navigation transform from the supplementary data Images from the older missions such as Viking Orbiter and the bulk of Voyager imagery fall in this category Most spacecraft data undergo several specific processing steps some are mandatory such as radiometric or geometric calibration and many others are optional such as creating a map projection or multispectral classification For post processing analysis it is useful to maintain a processing histor
11. 183 Inclination of Orbit to Ecliptic R 4 184 Ecliptic Longitude of Ascending Node R 4 185 Argument of Periapsis R 4 186 Orbital Period R 4 187 Semi Major Axis of Orbit R 4 188 Ecliptic Latitude of Periapsis R 4 189 Ecliptic Longitude of Periapsis R 4 190 Altitude from Target Center at Periapsis R 4 191 192 Image Compression Algorithm c 8 NONE HUFFMAN LZW etc WORD ITEM Central amp Picture Body TYPE COMMENTS 193 195 Central Body Name C 12 Mars 196 Central Body NAIF Code I 4 499 197 199 Picture Body Name c 12 5 24 200 Picture Body NAIF Code 201 Picture Body Rotational Period hrs 202 Picture Body Pole Right Ascension 203 Picture Body Pole Declination 204 Nominal Picture Body Eq Radius km 205 Nominal Picture Body Pol Radius km 206 Nominal Picture Body Cross Eq Radius km 207 Color Dep Picture Body Eq Radius km 208 Color Dep Picture Body Pol Radius km 209 Color Dep Picture Body Cross Eq Rad km 210 Picture Body Eccentricity SQRT e2 p2 p 211 217 Spare 218 219 Reference System 220 225 S C Frame x y z of Picture Body 226 231 Central Body EME x y z of S C Position 232 237 Central Body EME relative S C Velocity 238 Scan Platform Clock Angie 239 Scan Platform Cone Angle 240 245 Earth Direction Unit x y z Vector 246 251 Sun Direction Unit x y z Vector 252 256 Spare WORD ITEM Imaging or Map Projection Geometry 257 PG Intersect Latitude of S C x y z at Sfc 258 PC Intersect Latitude
12. 4 R 4 R 4 R 4 Crs TYPE CF 12 1 4 SE I 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 TYPE c 8 1 4 1 4 1 4 1 4 1 4 R 4 R 4 R 4 R 4 R 4 TYPE COMMENTS id NONE HUFFMAN LZW ete COMMENTS COMMENTS YYDDD HHMMSS YYDDD HHMMSS Degrees Degrees Default from file 269 Commanded Look Angle R 4 270 True Look Angle R 4 271 272 Roll Index Pulse Time R 8 273 Roll Angle Code 1 Position at Beginning 1 4 274 275 Contact Time 1 sec R 8 276 Roll Angle Code 2 I 4 277 278 Roll Shift Time 2 at sec R 8 279 Roll Angle Code 3 I 4 280 281 Roll Shift Time 3 at sec R 8 282 Roll Angle Code 4 I 4 283 284 Roll Shift Time 4 at sec R 8 285 Roll Angle Code 5 1 4 286 287 Roll Shift Time 5 at sec R 8 288 Roll Angle Code 6 I 4 289 290 Roll Shift Time 6 at sec R 8 291 Contact Code First or Last I 4 292 Contact Sector I 4 293 Roll Contact Code I 4 294 High Low Mode Code I 4 295 Gain State HIGH or LOW I 4 296 297 One Way Light Time Venus to PVO R 8 298 Roll Pixel Correction ISA 299 Old Spin Period R 4 300 Old Orbital Period R 4 301 Average Spin Period Scan Length Lines R 4 302 Mean of the Line by Line Spin Periods R 4 303 Phase Angle R 4 304 Time since Periapsis from Scan Start R 4 Hours 305 Alternate Roll Code Flag is Present 1 4 l if Present 306 352 Spare WORD ITEM User Computed Quantities TYPE COMMENTS 353 354 User Block Type Cra MEAP Gre MEXP VGR McIDAS exXp Voyager MEXP MGN
13. 4 9 4 10 4 11 4 12 4 13 4 14 4 15 5 0 5 1 5 2 5 3 5 4 5 5 5 6 HOW TO OBTAIN INFORMATION ABOUT AN IMAGE AREA HOW TO MAP PROJECT IMAGES HOW TO GENERATE A THREE COLOR COMPOSITE IMAGE HOW TO CLASSIFY A MULTISPECTRAL IMAGE HOW TO MEASURE CLOUD MOTIONS HOW TO EXPORT DIGITAL IMAGES FROM MCIDAS eXplorer HOW TO CREATE A FUNCTION KEY MENU MCIDAS EXPLORER DATA STRUCTURES EXPLORER AREA STRUCTURE AREA DIRECTORY COORDINATE SYSTEMS FOR THE IMAGE BLOCK DATA DESCRIPTION BLOCK CALIBRATION BLOCK AUDIT TRAIL APPENDIX I McIDAS EXPLORER COMMAND FORMATS APPENDIX II McIDAS EXPLORER SYSTEM DATA FILES APPENDIX II SUMMARY OF EXPLORER COMMANDS GLOSSARY 4 19 4 20 4 24 4 26 4 27 4 27 4 28 A a eee T Iae a Te 1 0 INTRODUCTION This document describes McIDAS eXplorer a set of planetary analysis tools designed for the McIDAS environment McIDAS is Man Computer Interactive Data Access System developed by the Space Science amp Engineering Center SSEC of the University of Wisconsin Madison Suomi et al 1983 Somewhat earlier in late 1960 s a similar facility was being born at the Jet Propulsion Laboratory JPL called Video Information Communication and Retrieval VICAR for analysis of the data being returned from the space probes such as the Mariner 6 mission to Mars Castleman 1979 McIDAS originated as a tool for providing interactive access to the earth weather satel
14. A utility to access the navigation parameters contained in the DDB for an area Also activate or change the navigation type or cordinate system attached to the area when multiple coordinate frames are possible e g native body fixed system to celestial Right Ascension Declination or swtiching from RING to central body system for ringed planets RING navigation type has yet to be implemented Brightness normalize a planetary image i e remove the brightness variation due to scattering geometry Minnaert or a modified Minanert are the only functions used for the normalization others can be introduced later The image is produced as a deviation from a bias brightness rather than by multiplicative scaling Determine the first available free area or a block of areas between a specified range of valid area numbers Total number of areas containing digital data in the specified range is also returned Determine the sky view for specified surface loations to see if an orbiting spacecraft is visible from the surface Program to obtain the Physical constants of an object Either the NAIF ID preferred or its name capitalized can be entered Radii and length of day are currently listed Determine a limited number of limb points within the cursor positioned on the limb in a displayed planetary image for the purpose of navigation Create a general perspective view navigation codicil for a given area for any object APPENDIX Ill 7 P
15. DF s and grid both images with MAP LALO for analysis MAP LALO will show a lat lon grid even on a completely black image unless the planet surface lies completely outside the image boundaries EARTH is a Special Case aa One must remap images using the right handed transformations generated by PLANAV we don t spatially invert clouds in the real world but the lat lon grid being left handed must be inverted This is accomplished post REMAP by using keyin PLAREV to interchange east and west longitudes PLANAV area EARTH ANGLE 0 0 REPLACE AREA REMAP source_area area PLAREV area DF area frame MAP LALO Always DF and MAP after navigation mods to check results APPENDIX 81 PLAREV Flip the longitude system east positive to west positive or vice versa for an area with PLANAV created navigation Useful for mapping earth data in the generalized perspective projection PLAREV area_ Remarks McIDAS uses a 0 180 longitude system for navigation and for earth the longitudes west of Greenwich meridian are considered positive and negative to the east This convention is contrary to general usage and can create a reversed map than one intended if using PLANAV to attach navigation PLAREV will reverse the convention This should normally be started by PLANAV if the TARGET is specified as EARTH APPENDIX I 82 POLEN Program to convert Image Co ordinates to RA DEC Vogager Images POLEN FDS LINE ELE OPT TOEM
16. GEOM or i PHOT or i etc NONE HUFFMAN LZW etc COMMENTS e s rek eee eee ee eee ee ee ee 200 Picture Body NAIF Code I 4 201 Picture Body Rotational Period hrs R 4 202 Picture Body Pole Right Ascension R 4 S C EME 203 Picture Body Pole Declination R 4 S C EME 204 Nominal Picture Body Eq Radius km R 4 205 Nominal Picture Body Pol Radius km R 4 206 Nominal Picture Body Cross Eq Radius km R 4 207 Color Dep Picture Body Eq Radius km R 4 208 Color Dep Picture Body Pcl Radius km R 4 209 Color Dep Picture Body Crsss Eq Rad km R 4 210 Picture Body Eccentricity SQRT e2 p2 p R 4 211 217 Spare 218 219 Reference System Crs 220 339 Spare 340 345 S C Position Vector WRT Central Body R 8 S C EME 346 351 S C Velocity Vector WRT Central Body R 8 S C EME KM S 392 West Convention for longitude 1 4 L lt T WORD ITEM User Computed Quantities TYPE COMMENTS 465 512 333 334 User Block Type Crs MEXP VGR MEXP VGR McIDAS eXp Voyager MEXP MGN McIDAS eXp Magellan MEXP CPP McIDAS eXp Pioneer Venus MEXP FIT McIDAS eXp Flexible Image Transport System MEXP VO McIDAS eXp Viking Orbiter specifies user dependent block format 355 357 Spare 358 359 Computed North Angle from Limb fit R 8 Not used for Nav 360 377 Computed Transform Matrix Inst gt PicBod R 8 g 378 395 Computed Transform Matrix Inst gt Planet R 8 396 413 Computed C Matrix Inertial gt Instrument R 8 414 431 C
17. Jupiter 599 Mimas 601 Enceladus 602 Tethys 603 Dione 604 Rhea 605 Titan 606 Titan 6060 Hyperion 607 Iapetus 608 Phoebe 609 Janus 198051 610 Epimetheus 198053 611 Helene 198056 612 Telesto 1980513 613 Calypso 1980525 614 Atlas 1980528 615 Prometheus 1980527 616 Pandora 1980526 617 Saturn 699 MERCURY VENUS SFC VENUS CLD MOON EARTH SFC EARTH ATM PHOBOS DIEMOS MARS SEC MARS ATM IO EUROPA GANYMEDE CALLISTO AMALTHEA HIMALIA ELARA PAS IPHAE SINOPE LYSITHEA CARME ANANKE LEDA THEBE ADRASTA METIS JUPITER MIMAS ENCELADUS TETHYS DIONE RHEA TITAN SFC TITAN ATM HYPERION IAPETUS PHOEBE JANUS EPIMETHEUS HELENE TELESTO CALYPSO ATLAS PROMETHEUS PANDORA SATURN Ariel 701 ARIEL Umbriel 702 UMBRIEL Titania 703 TITANIA Oberon 704 OBERON Miranda 705 MIRANDA Puck 1985U1 706 PUCK Portia 1986U1 197 PORTIA Rosalind 1986U2 798 ROSALIND Juliet 1986U3 709 JULIET Cressida 1986U4 710 CRESSIDA Belinda 1986U5 711 BELINDA Desdemona 1966U6 712 DESDEMONA Cordelia 1986U7 713 CORDELIA Ophelia 1986U8 714 OPHELIA Bianca 1986U9 LO BIANCA Uranus 799 URANUS Triton 801 TRITON Nereid 802 NERIED 1989N1 803 1989N1 1989N2 804 1989N2 1989N3 805 1989N3 1989N4 806 1989N4 1989N5 807 1989N5 1989N6 808 1989N6 Neptune 899 NEPTUNE Charon 1978P1 901 CHARON Pluto 999 PLUTO 5 3 COORDINATE SYSTEMS FOR THE IMAGE BLOCK The image block usuallv starts at byte 9040 in an area although it c
18. McIDAS eXp Magellan MEXP CPP McIDAS eXp Pioneer Venus MEXP FIT McIDAS eXp Flexible Image Transport System MEXP VO McIDAS eXp Viking Orbiter specifies user dependent block format 355 435 Spare 436 Minnaert Fit Constant Max DN Used 14 437 Minnaert Fit Constant Calc Slope R 4 438 Minnaert Fit Constant Calc Intercept R 4 439 Minnaert Fit Constant Mean Abs Dev R 4 440 460 Spare WORD ITEM Supplementary Information TYPE COMMENTS 461 462 Supplementary Block Type Crs SUPL CPP 463 465 Data Source CD ROM Volume tape name GIA 465 512 Spare 5 21 131 132 Data Type 133 Spacecraft ID 134 Instrument ID 135 136 Instrument ID TELESCOP INSTRUME 137 141 142 146 147 149 150 131 Lo2 229 194 1399 1591091 FILTER OBSERVER Spare e e a a rer vk e a e bs Ba f SN dr p f bs i er bs A Ba US r n ak a o n m e rb EA s A pe FITS b a e ia ii mp k vb n n n s vf a rn m do be r b r n n Pm ll rd UE o A A A S C Image ren mp m m m ii ee eee ee ee eee ii Telescope Image Other Data DSN NAIF Code NAIF Code Name DDB amp Instrument Name of telescope Name of Instrument Name of Filter FOV Degrees in scan direction FOV Degrees in cross scan direction Name of observer 182 Bccentricity of Orbit 183 Inclination of Orbit to Ecliptic 184 Ecliptic Longitude of Ascending Node 185 Argument of Periapsis 186 Orbital Period 187 Semi Major Axis of Orbi
19. NIIT participants are primanly motivated to enhance the competitiveness of industry specifi cally related to distributed computing and information access and use through this coopera tive effort The knowledge gained through the NIIT is expected to enhance the U S role in the rapidly developing field of information systems The NIIT distinguishes itself from other groups related to the NII by integrating existing tech nologies to deploy and study real infrastructure applications Note that by including users in the development of the NIIT infrastructure the feasibility of creating and marketing high performance networking and distributed computing resources can be evaluated The formation of the NIIT cooperation arose out of the expression of common interests in high performance distributed computing environ ments demonstrated at Supercomputing 22 The Earth Data System The first reference application identified for a demonstration by NIIT addresses the problem of global environmental change Environmental researchers must consider the interplay between various complex systems that compnise the environment which affect changes in the biosphere Earth data research is specifically founded on the location of acquisition of and analysis of large heterogencous datasets These data are stored in many different archives that are geographically distributed ranging from large government archives of satellite imagery with full data
20. The frames can be any size as desired and each one can be of a different size If the frame size is larger than the screen size then the screen provides a scrollable window into the displayed frame and can be moved with the mouse Frames can also be dynamically added to a session as allowed by available system memory but at present they can be unloaded to free up memory only by exiting the McIDAS session and re starting McIDAS with the new parameters On UNIX workstations the number of frames to configure and their sizes are specified by the user in the profile as constrained primarily by the amount of random access memory RAM available in the workstation The user controllable frame size is useful to optimize the number of display frames for the specific data being analyzed in that session Even if animation may not be a desire a large number of frames are still immensely useful in streamlining an analysis session by eliminating the need to erase and re draw graphics as well as by keeping them around for reference The planetary image data available on PDS CD ROMs range in size from 800 x 800 for Voyager and Galileo to 1024 x 1024 or larger for Magellan products a considerable difference in frame size and memory requirements The display frame contains much more information than just the visible image in McIDAS environment For each frame that contains an image McIDAS keeps track of the image source its calibration and most important the
21. Thus the lower the data rate the longer it takes to read out an image and the greater the dark current build up Dark Current Removal The dark noise begins to build up on the vidicon face plate as soon as the exposure be gins and is thus a function of the exposure time and the image readout time The image readout time is determined by the data transmission rate The rates used for transmission of data during the Voyager 1 and 2 encounters with e Saturn system typically used a 3 1 scan rate The background brightness thus increases from the top of the image to the bottom and from the left to right As may be expected the dark noise has quantization noise so that there is a slight variation from frame to frame and from pixel to pixel Usually the dark noise frame is therefore generated from average of several frames and or also low pass averaged to reduce the noise in the output image Typically the dark current is subtracted during the radiometric correction step SHADE9 command Occasionally the dark current subtraction alone is desirable for quick look analysis in which case the McIDAS MC command can be used to subtract the dark noise frame from the Voyager image of interest The reseau marks should also be generally located in an image prior to dark noise removal and or shading correction The non linear vidicon response to uniform incident light manifests itself in differing output brightness levels across the image The non linearity
22. below BRTCEN BRTCEN accomplishes two tasks First it finds a first guess object center by determining the center of brightness under the implicit assumption that the image is full disk and that the limb and terminator regions are contained in the area Second it determines the locations of the limb points by determining the points where the radial brightness gradient from the guess center is maximum between two azimuths at a given angular spacing For full disk full phase images the center of brightness is a fairly good guess for the target image center The agreement worsens as the phase angle increases or when the image contains only a partial view of the target The sky brightness is estimated from the brightness histogram and is not used for the brightness center calculations The line and element sampling and the brightness range to use for the center of brightness can be specified on the command line to override the default values EDGES The EDGES command allows the edge points for an image to be interactively determined from a displayed image and stored in a limb points file LIMBxxxx where xxxx is the area number The edge points are determined as local maximum directional derivative locations for the brightness distribution in the image in a 3 x 3 neighborhood about that point If the bright limb is located within each image then this algorithm will find the limb location In the original version of this command the points w
23. but within a block or within an array an image or a frame coordinates start with the index 1 The calibration block may arbitrarily be of length 0 6224 but all other blocks must always be present The global structure of a McIDAS eXp area for Magellan MIDR is illustrated below BYTES WORDS A ey 00 DIRECTORY 256 64 NAVIGATION 2816 7404 CALIBRATION 2816 704 IMAGE ENDIMG EOF oor The byte offsets for any McIDAS area may be seen by executing the core McIDAS command LA FORM ALL 5 2 AREA DIRECTORY Each area that is extracted from a spacecraft image has associated with it a record called the area directory The data in the directory are stored as 32 bit 4 byte two s complement binary integers or as ASCII character data The length of the directory is 256 bytes 64 words A list of the directory contents follows pp G 9 wW J dam E LM La LA N E Uy 14 Tax 16 Eba 18 19 NAME AND DESCRIPTION Contains zeros if record is valid Area Format Always 4 current core as of June 1985 OO Spacecraft Identification Number YYDDD Nominal Year and Julian day of area HHMMSS Nominal Time of image UPPERLEFTLINE Image line coordinate of area line 0 elem 0 UPPERLEFTELE Image element coordinate of area line 0 elem 0 Not used Reserved for true three dimensional data sets NL
24. initializes area storage block to zero before adding found locations NO overlays found locations on previous ones ON Tests if word GEOM appears in audit trail default RF will not modify the found reseau locations OFF Turns off GEOM test so found reseau locations can be modified default ON APPENDIX 86 SCANA Create a visual index of images contained in McIDAS ar s by writing a thumbnail image of each area into the index area As ma as 484 areas can be scanned in a grid as large as 22 x 22 The output s another area which can be displayed withe the DF key in The SCANE command allows the particulars of selected using the mouse area to be accessed A variety of options for annotating each thumbnail image are available first_area last_area output_area GRID SIZE KEYWORDS range1 range 2 rangeN outpur_area KEYWORDS PARAMETERS first_area first area number to begin scanning last area last area number to scan if only one range of ares is to be scanned range s source area range s format beg_area end_area No spaces between the area numbers default 1 9999 output_area destination area default first unused area KEYWORDS IMA frame_ image frame number for display default no display GRID _row _col set the number of rows columns of thumbnail images in darea def 5 x 5 For a display frame size of 900 x 1200 a grid of 15 x 20 is a practical limit The SIZE should corresp
25. interfaces make it unnecessary to know the syntax or even the command names and most tasks can be accomplished readily through the interface The GUI does require some familiarity with the scripting language if it needs to be modified by the user although in most cases it is unlikely and is completely independent of the commands It is a system of cascading menus that offer different tool bars which can be chosen with mouse button clicks When needed these will prompt the user for input The function key based interface is similar in operation in that it is also a set of cascading menus where the choice is made by pressing a specific function key Only minimal user input is possible with this scheme It is however much simpler to create and can be easily manipulated with a text editor The details of how to write a function key based interface can be found in the McIDAS X manual KRA Aa aaae 4 S if Coe ARA ASAP ASAP us L T Poke PA Y PE a daas E genes iloatesalec ete 04 TT AAA COSTRA RARA ARA AA as N LN e E oe s a aves a BN Y ta s S at we A L N N v a TB wees Lt VARIA A AE EE E Peper Chart RRR AAA AR AAA RA RAR RARE IA RRA li IA O EN eS gt ATT rane TRJ 13x ANE eke s a Nt 74 nt AO aa RRS TUR AUS eee eo S S es Sy OA VAARAA AI LT OLED OCR OLE LICE LE E a Fo arianna N PAPLE PP PIPAS Ri BEA a ates eis Prab aie DELILE Kn y Pons Tena Itaca Ent torito lt BT TO 2 1 HI 1 iv firk Types gt l U DI
26. length of day etc In most cases the planetary data refer to a single target object such as a planet or its satellite or ring system Occasionally however there can be multiple objects in a single frame such as the images of a planet and its ring system or a Satellite in the same frame In such cases the decision on which NAIF identification number to use within McIDAS eXplorer is made on the basis of which single object is being analyzed in that frame Another complication arises in investigating images of bodies with extended atmo spheres such as Venus or Titan The visible or infrared images of these planets do not see the surface but only the cloud top level which is about 65 70 km above the surface for Venus and nearly 300 km for Titan Thus the effective radius for such objects needs to be different for the purpose of not only image navigation the process of relating the image co ordinates to the planet s co ordinates and vice versa but also for measuring distances etc For this reason McIDAS eXplorer distinguishes between the solid surface and the cloud level Further this level can be different at different imaging wavelengths such as for Saturn therefor allowance is made for having as many as 9 separate radii for different levels for objects with atmospheres The NAIF identification code for an object is entered as a four digit number rather than as a three digit number with the rightmost digit denoting the level for which the
27. mcidas data sub directory McIDAS generally uses standard prefixes always UPPER CASE for its standard data files The convention is as follows Digital images AREAxxxx Gnidded data files GRIDxxxx Random ordered data MDxxxxxx In addition McIDAS eXplorer uses similar convention for the files used in some solar system applications programs They are LIMBxxxx Image edge points xxxx ET Enhancement tables created by USCLAS xxxx LOG A log file of the USCLAS multispectral classification program There are many data files associated with specific missions and instruments that are useful in using McIDAS eXplorer These are also in mcidas data sub directory Their names and brief description are given below file name Remarks acumdir tab Magellan Mission cumulative directory for the ARCDR data PDS CD ROM Volumes MG2001 through MG2015 This is the version from MG2015 volume attsppin pvo Pioneer Venus Orbiter Spin axis pointing log Needed for navigation of OCPP images cumindex vo Viking Orbiter cumulative index for the PDS CD ROMs dell8 bsp JPL Planetary ephemenis file NAIF de202 tsp JPL planetary ephemeris file NAIF etopo5 NGDC global topography and bathymetry file with 10 minute resolution 1bmints gazetter tab Gazetteer table for Mars from the USGS Digital Image Map CD ROM Volumes geo tab An ASCII file containing the names of the geographic features on Venus This file is found on all PDS Magellan CD ROM volumes through MG
28. then zeroes in image are filled by average of up to NUMAVG x NUMAVG non zero or DN gt MINDN pixels centered on a pixel REMARKS After the Saturn encounter the image readout for Uranus and Neptune encounters of Voyager 2 was changed to account for the lower data rate due to the increased range So that more images could be returned image data were compressed by editing out data on alternate lines altenating between the right and the left edges of the frame These gaps need to be removed before reseau s can be found near the edges and certainly before rectifying the images The gaps are filled by interpolating across the gap element by element from the immediate neighbors above and below the compressed line APPENDIX 24 FILTVGR Acommand to apply a spatial filter to an image with planetary limb This is an adaptive edge sensitive filter that shrinks its domain as it approaches the limb and therefore produces a cosmetically better looking image near the limb Will also remove noise pixels FILTVGR souce_area_ dest_area_ opt NOTE The filters are so heavily parameterized it is often impossible to predict in advance what effect will be produced We suggest trying the default values first and then selectively varying the parameters one at a time until desired results are obtained This filter keyin will work on most McIDAS X or McIDAS OS 2 images KEYWORDS INAREA area OUTAREA area default is input area number FRAM
29. DF and MAP commands to check the navigation Occasionally the roll angle or the look angle may have to be adjusted for a better fit See NAVCPP command to accomplish this The program creates an image such that each image line contains a spacecraft scan even if it is missing on the NSSDC tape so that the time and image line numbers relate to each other through the average spin period of the s c over the image duration Further the APPENDIX I 35 GETFITS GETFITS Make a McIDAS area from a FITS format data file Try to first cut Navigate using available information Only a Primary HDU with a two dimensional data array can be read by this program currently No FITS extensions no random groups FILE AREA SOURCE OPTION FRAME UNSIGNED TARGET MINDN NORTH SAMP SWAPBYTE TIMEZONE RANGE RATIO HIST DATEOBS TIMEOBS KEYWORDS FILE AREA SOURCE OPTION FRAME TARGET SKY filename extension without the period FITS file name in mcidas data case sensitive Input as FILE file ext form file ext assumed If input file is in another directory or is too long for the 12 character FILE fields put the full path and file name as trailing string i e GETFITS AREA 122 user path file ext or GETFITS AREA 353 data verylong_name img McIDAS area number reformatted image destination IRTF NSFcam Superhero Camera Hawaii WFPC HST Wide Field Planetary Camera OTHER _
30. Green or Blue Three separate calls one for each color to three different colors will produce a color composite on a display frame DFC will accomplish the same if the three images are in a single multibanded area and hence the same navigation APPENDIX III 2 DFC A three color version of DF to display a color composite of 3 bands from the same area for the 24 bit display mode bp 24 option DSTNCE Measure distances on any navigated solar system image either between a pair of points or along a trajectory to determine the cumulative distance and segment lengths EDGES Find the edge points bright limb in an image using a 3 x 3 local maximum brightness gradient method Edge points are written to a LIMBxxxx file and can be edited plotted or listed Uses a different algorithm from LIMBPT and is best used with the key in assigned to a function keys using TE KEYFnn for deleting adding limb points ELLIPS Draw signature ellipses from a USCLAS spectral assification to see the spectral class distributicn for a specific classified area EXPDOC List the User guide and command help documentation in an X Window that can be scanned using vi editor commands FILHOL Interpolate missing data in an image by two dimensional interpolation over a specified box FILLO Fill in the alternate line data compression gaps in Voyager 2 images of Uranus and Neptune by interpolation across lines for each missing element NOTE The line pr
31. Magellan mission has returned synthetic aperture radar images of the surface and high vertical resolution topography data over nadir footprints along the Magellan orbit tracks The surface imagery from Magellan is available on PDS CD ROM volumes as Mosaicked Image Data Record MIDR in a variety of different spatial resolutions in a mapped format The Pioneer Venus mission and Magellan mission have together returned a significant amount of image data Subsequently Galileo Orbiter on its way to Jupiter via a Venus Earth Earth Gravity Assist VEEGA trajectory to Jupiter also acquired a small number of images of Venus in reflected solar light through blue and near infrared filters These data can also be imported into McIDAS eXplorer and manipulated as described below 3 2 1 Pioneer Venus OCPP Images OCPP images are available in the roll by roll format on NSSDC archive tapes Other files on the tape describe the tape format as well as the orbital elements for the Pioneer Venus orbiter and other information necessary for determining the navigation transform PVORBELE PVOATTSPN GETCPP command imports data from the tape files into a McIDAS area and also attaches a preliminary navigation to the area BARAK w NN N Sert eli by donar Varis ILL c 7 EEE r ree PSE PS TL ata de 19 HEE f i 00 0 Tye Matten ct Ree Lines Ean Ean GANO Date ELITE LeS C Y Ar ormie E3436 Toth LU S caf MaR See RAT M L Wy e LS ALG Law tuio al genta Hote UU LE
32. Number of Image I 4 Needed for DDB access passed in NAV block 1 128 129 DDB Identifier Cc 4 Always DDBO 130 DDB Block Type amp Version BBBV c 4 VGR Voyager VO Viking Orbiter CPP Pioneer Venus MGN Magellan MO Mars Observer HST Hubble Space Telescope 1 GO Galileo Orbiter CLEM Clemintine Lunar Survey words 133 134 identify spacecraft and camera 131 512 MISSION SPECIFIC DATA INFORMATION SEE BELOW 513 640 Navigation information defining the position of observer pcinting of the instrument and parameters describing the image geometry This block contains mest of the data needed for the NAIF and SPCE navigation routines to function WORD ITEM Position Attitude Image Geometry TYPE COMMENTS 513 Spare 1 4 514 Smear Direction deg relative to scan dir R 4 If present 515 Smear Velocity km s relative to tgt sfc R 4 S 516 Data North Angle as read from SEDR etc R 4 517 Optic Axis RA R 4 Nav S C 518 Optic Axis Decl R 4 Nav S C 519 Sun Phase Angle at SC Planet Sun Center R 4 520 522 L Vector Az El Twist R 4 523 525 Pitch Yaw and Roll Limit Cycle Angles R 4 IOS VECTOR 526 527 Direction to sun in image coord system R 8 LSUN 528 529 Nav North Angle deg relative to scan dir R 8 Nav NORANG 530 531 Nav Ecliptic North Angle as above R 8 Nav ECLANG 532 533 Spare 536 553 3x3 Transform Matrix Inst gt Planet R 8 From data source 554 571 3x3 C Matrix Inertia
33. ORBITER CLOUD PHOTOPOLARIMETER IMAGES OF VENUS These images are available from NSSDC on computer compatible tapes McIDAS eXplorer uses a navigation model for these spin scan images that is based on the assumption that the spin axis orientation and the average spin period of the spacecraft is constant over the duration of that image Files containing orbital elements and other required information for the navigation of these images are also contained on these tapes A preliminary navigation is attached to the area containing the image when the images are first imported using the GETCPP command These files should have been copied into the default mcidas data sub directory previously The default navigation which depends on the average spin period of the spacecraft the spacecraft orbit around Venus and the CPP telescope look and roll angles can be verified by drawing a latitude longitude grid and or using the E key The navigation can be updated using the NAVCPP command if necessary by re determining the exact look and roll angles based on first last contact with Venus and the location of the bright limb Please refer to the User Guide for information on how to use the NAVCPP command GENERIC NAVIGATION RECIPE FOR FRAMING CAMERA IMAGES To attach navigation to a planetary frame the following quantities need to be known name and NAIF ID of the target object the location of the sub observer and sub solar points on the target object lat
34. PLANET JUPITER REPLACE AREA default projection of Jupiter is generated in a 500x500 size area PLANAV 23 EARTH VIEWPOINT 23 5 10 1 025 ANGLE 0 50 20 REPLACE AREA 23 5 lat 160 km above earth surface looking leftward toward limb NOTES If the remap runs too fast and gives a black image you do not have a destination location which ought to contain any source data typically you are on the back side of the planet or are using incompatible parame ters which the program resolves in a way you don t expect The trouble could be in either the source area or the destination area navigation Destinations with all data within a single spline domain may also truncate to black Try DF s and grid both images with MAP LALO for analysis MAP LALO will show a lat lon grid even on a completely black image unless the planet surface lies completely outside the image boundaries One must remap images using the right handed transformations generated by PLANAV we don t spatially invert clouds in the real world but the lat lon grid being left handed must be inverted This is accomplished post REMAP by using the keyin PLAREV to interchange east and west longitudes PLANAV area EARTH ANGLE 0 0 REPLACE AREA REMAP source_area area PLAREV area DF area frame MAP LALO Always DF and MAP after navigation mods to check results Once the navigation has been attached to the destination area its validity can be verified before actually creating the o
35. Radii above RAD N will be plotted in COL N 1 APPENDIX 33 COLORS 51126142411 93 7 default values low red magenta orchid blue average sky cyan green aqua Examples GETALT 2185 21812200 PLOT YES plots entire orbit GETALT 2067 20612080 FP 737 LIST DATA PLOT YES lists footprint 737 and plots it on displayed frame The ephemeris files used to process the ADF files are not accessed by this program REMARKS The FINDALT cammand can be used to determine the CD ROM volume corresponding to the orbit number that has a ndir pass over the region of interest Eventually it should be possible to determine both the MIDR and ARCDR volume numbers for a given geographic region directly but as yet the two have not yet been linked since the altimeter measurements are made in the nadir look while the SAR imagery is acquired at a nominal 45 degree angle with the nadir in either the left or the right side Thus the look angle for the SAR must be known to compute which orbit the altimetry could have been acquired on however that information is not present in the MIDT labels APPENDIX 1 34 GETCPP Import a Pioneer Venus Orbiter Cloud Photopolarimeter image from a file in the NSSDC tape archive format roll by roll Attaches navigation at the same time Requires files orbele cpp and contact cpp in mcidas data sub sirectory GETCPP area_ file_name REMARKS The image can be immediately displayed and gridded using
36. Spain and China and provides real time w her support to one of the most remote sites in ts world McMurdo station in the Antarctic over an Intemet link to Madison Wisc The National Science Foundation National Center for Atmo spheric Research sponsored UNIDATA project uses McIDAS for educational programs in nearly 100 atmosphenc science departments of colleges and universities in the U S McIDAS eXplorer McIDAS eXplorer is an extension of McIDAS capabilities for use with data obtained by NASA s missions to solar system targets The principal goals are to provide target specific tools to analyze planetary data and to use the SPICE library developed by the Navigation and Ancillary Information Facility NAIF team at JPL for image navigation Planetary data span a large range in terms of quantity type and global coverage The strength of McIDAS is in its ability to interact with satellite data for geophysical applications such as multispectral imagery surface network data and atmospheric soundings One of the goals of McIDAS eXplorer has been to provide a unified approach to the analysis of target dependent data by accounting for the differences in their physical charactenstics such as size and shape To this end the NAIF approach of assigning a unique identification tag to each object and spacecraft is adopted within McIDAS eXplorer with some enhan ements for atmosphere beanng bodies These enhancements allow use of different
37. Wiener are being added MA This command also has both low pass and high pass filter options that are one dimensional along the line direction and can be useful in some cases This command can also remove noise in the image that usually occurs due to telemetry errors in the transmission of the data Please refer to the command description for more information on how to use it HOW TO DETERMINE THE PLANETARY PHOTOMETRIC FUNCTION MINFIT The gross brightness variation in a full or partial disk planetary image obtained in reflected sunlight is due to the variation of the scattering geometry the incidence and viewing angles also called limb darkening This variation masks the variation in the reflectivity distribution over the planet On occasion it is desired to visualize these reflectivity variations alone devoid of the scattering geometry variation To accomplish this the contribution due to the scattering geometry can be removed if the scattering function is known There are several theoretical and empirical models of the scattering from planetary surfaces Chandrasekhar H functions Hapke function Buratti function and Minanert law are a few of the models that are generally used for this purpose The Minnaert law is an empirical model based on symmetry of incidence and reflection directions and can be used for most applications lo powB or In lo In upo where Observed intensity A constant called normal albedo cos
38. a status line Figure 1 and is the primary user interface to McIDAS There are two text windows 1 and 2 which are made active by clicking in the particular window or from the numeric keypad by pressing 1 or 2 key These two text windows contain output from McIDAS commands The fourth window is the image display which is sized according to the frame size specified in the start up procedure To close a McIDAS session simply enter EXIT in the command window which will end a session The eXplorer GUI can be started from your home directory with rs sh f topmenu term _ amp where ferm_ is a terminal number assigned by McIDAS to the session and can be found in the Title Bar for the McIDAS Text and Command windows Alternately the interface can also be started from the McIDAS session with the GUI key in from the command window Figure 2 1 The initial screen for the GUI that allows the user to chose between different actions using the mouse button clicks on the desired item N NNN SAS ENSSAASAS NNN SAS RAAS 5 SASS N b E A S gt if fe Ea C9 K E A va A 7 LN f HA gt 2 Ky SNAS McIDAS Display _ Since the prime motive behind McIDAS is the analysis of data acquired in the temporal domain animation is a key feature and thus McIDAS uses multiframe display capability The image data are displayed on a frame which can contain either image or graphic data
39. and OD commands on multi byte data as well 54 62 Internal use only 63 Byte offset to the start of the calibration block within the area file 64 Number of lines in the audit trail McIDAS assigns a unique three digit code field to spacecraft for use in the area directory This SSS spacecraft code is converted to a CHARACTER 12 name when the image is loaded to a frame by the keyin DF The name appears in a title bar at the bottom of the frame The file mcidas data SATANNOT contains the table converting SSS to a name Negative codes are used by NAIF and the SPICE routines for spacecraft The NAIF ID number which controls definition of all spacecraft identification is the one in word 133 of the Data Description Block for an area The code assigned to a particular spacecraft is the negative of the code assigned to the same spacecraft by JPL s Deep Space Network DSN Integer codes have been assigned for the following spacecraft 12 Pioneer 12 Venus Orbiter 18 Magellan Venus Orbiter 27 Viking 1 Mars Orbiter 30 Viking 2 Mars Orbiter 3 Vovager 32 Voyager 2 77 Galileo Jupiter Orbiter 94 Mars Observer Vehicle has failed The current spacecraft SSS numbers used in McIDAS eXp are shown in the table below Contents of mcidas exp SATANNOT ee ee ee ee ee re rra ee ee ee ee ee ee ee p _ ee ee re ee ee P ee ee ee k b ee ee ee a Sensor Source SSS Code Spacecraft Target Name Pioneer Venus Orbiter ae PIONEER OR
40. appropriate expander based on the compressor ID stored in the compressed file DECOMP area_to_decompress new_area KEYWORD KEYWORDS OPT STAT will display some information on the various files used during decompression REMARKS Decompression routines presently coded DISCRETE COSINE TRNSFORM ARITHMETIC ADAPTIVE HUFFMAN LZW APPENDIX I 17 a peat DDBUTIL Utility for manipulating inserting and copying DDB entries The utility may be used to build an area with a DDB from an existing area withou a DDB or to copy a DDB from one area into another DDBUTIL source_area dest_area KEYWORDS KEYWORDS DEFAULT DDBSIZE word size of the DDB block 640 OPT option describing operation INSERT INSERT COPY DDBTYPE 3 letter DDB identifier FIT FIT VGR CPP VO GO CLEM TARGET NAIF ID of target body 0 OBS ID of observer 50 Hubble EXAMPLES Take an area 122 and build a new area with a DDB 222 for a Hubble derived image of Jupiter DDBUTIL 122 222 TARGET 599 Copy the DDB from 122 and place the data in area 222 DBUTIL 122 222 OPT COPY REMARKS This command can be used to attach a DDB block so that the eXplorer specific commands can be used on that area APPENDIX I 18 DF3 Display a component of a three color composite in a specified color Red Green or Blue Basically a version of the core command DF for the 24 bit version of MciIDAS area_ frame_ opt loc_x loc_ymag BAND COLOR Para
41. available on PDS CD ROM volumes the SPICE kernels are available Voyager 2 images of Uranus and Neptune Systems and a limited number of Jupiter and Saturn System images For newer missions such as Galileo and soon Clementine SPICE kernels should be generally available In some cases the pointing implied by these kernels is not sufficiently accurate and may need to be refined before any quantitative analysis can be accomplished This refinenment requires that the C Matrix or kernel by updated based on refined knowledge of target object location in the image either by limb fits or by location of known features How to actually update the C kernel is described later NAIF Navigation Type For images without any SPICE kernels the required C matrix needs to be computed from available information about the imaging geometry For a spacecraft mission such as 4 5 Viking or Voyager these data are generally available as Supplementary Experiment Data Record SEDR The name NAIF here refers to the use of the NAIF FORTRAN subroutine package tool kit to determine the C matrix directly from the SEDR data For other data such as ground based images the SEDR information is not generally available typically only the time when the image was acquired and hopefully some knowledge of the orientation of the imaging system with respect to the target object s reference frame North Angle For the NAIF navigation type eXplorer tools can compute the planet and t
42. by a grid and the tile numbers are shown as well Currently TILES does not check the area to see if it indeed contains a browse frame APPENDIX 1 96 TLST Lists areas on a tape saved using TPUT SCSI tape drives only TLST VOLNAM DEVNUM KEYWORDS VOLNAM s DEFAULT s UNKNOWN DEVNUM i DEFAULT i 0 TLST lists the contents of an area save tape written with TPUT on either the Exabyte or the DAT drive The device number is likely to be site dependent APPENDIX 1 97 TPUT Save one or more McIDAS area files from disk to tape i e in mcidas data sub directory TPUT darea darea2 KEYWORDS darea1 beginning disk area required darea2 ending disk area DEFAULT darea1 KEYWORDS APPEND Y N DEFAULT Y APPEND should be N for Exabyte and 1 4 inch DEVNUM i DEFAULT 0 REMARKS When the areas are written onto the tape all of the navigation information related to that area that is accessible using the LA or the LISTNAV commands is also stored along with it Thus the navigation processing history etc can be restored with the TGET command at a later date This utility is similar to the PUT and GET commands available on the mainframe system except that it is currently restricted only to area format data files The other difference is that it is assumed that the user will physically interact to mount and dismount the tape cartridge from either the DAT or the Exabyte drive The data can be restored by
43. calibration units def onginal from area BRIT RAW RAD TEMP dB as applicable ylo yhi xlo xhi x and y plot limits A graph of image data is drawn on the graphics along a scan line either over the entire displayed line or within the cursor or between two points chosen with mouse clicks If Magellan radar data is displayed MIDR s or GxDRs the the proper units are automatically chosen depending on the data type dB for radar reflectivity km for topography deg km for slope and rms slope if the frame area is navigated the distance scale by default is km else pixels Draws a line plot on the graphics of the data on the line through the center of the cursor prompts you indicate the end points using cursor locations through mouse movements and button clicks APPENDIX 63 MAKESU MAKESU KEYWORDS NAME TYPE FRAME LIMITS Make a stretch table for a McIDAS area containing FITS data The table displays saturation and user can either define a percent ends in stretch or approximately define a slope gamma at the center of the transfer function for the sigmoid inverse sigmoid logarithmic or exponential curves The program pauses to let the user look at the transfer function and requires a mouse click in the graph window to resume NAME TYPE AREA FRAME LIMITS HIST stretch table name for SU keyword in DF keyin 8 characters maximum length SIGMOID gamma horiz_dn_value gamma approximates the
44. can make use of the keywords for this command to produce additional output by keying in LA 101 FORM AUDIT which queries the area to produce the audit trail for the image contained in the Area 101 and the output may look like area ss yyddd hhmmss lcor ecor lr er zr lsiz esiz z 101 48 89214 83159 1 800 proj 0 created 93048 191147 memo CDROM DECOMPRESS type VISR cal type BRIT area offsets data 9040 navigation 256 calibration 2816 doc length 36 cal length 0 lev length 0 PREFIX 36 valcod O zcor 1 band 8 NA reel Audit Trail yyddd hhmmss PICNO 0338N2 023 TARGET NEPTUNE FDS 10706 02 CAMERA NARROW ANGLE SPACECRAFT VOYAGER SHUTTER TIME 89214 83159 NAONL Y FILTER GREEN 5 EXP 15 3600SEC GAIN LOW LINES 800 ELEMENTS 800 SCAN 5 1 EDIT VCDROM Internal Parameters and Defaults SOURCE cdrom neptune c1070xxx c1070602 imq__ FDS START 1070600 FOS END 1070700 TARGET neptune CAMERA FILTER SEARCH_INDEX 0 OUTPUT AREA 101 93048 191155 VCDROM FDS 10706 00 10707 00 AREA 101 TARGET NEPTUNE 93119 175624 RF 101 93119 175657 FILLO 101 93119 175727 RF 101 93119 175813 SEDRIN 101 Some commands which require no arguments at all One example is EXIT which shuts down an active McIDAS session and closes all active McIDAS windows Then there are some single letter commands which can be alternately entered using the ALT key simultaneously with another key These commands do not require a CR if en
45. carry it to the other extreme of Venus disk At this time to acquire another full disk image the telescope is repointed A full disk image thus takes anywhere from 2 5 to 5 hours to acquire depending on the position of the Pioneer Venus orbiter in its highly inclined 105 highly eccentric 0 8453 orbit Consequently NAIF SPICE kernels are not available for these images Instead these images are navigated using the knowledge of the spacecraft orbit and imaging geometry A single McIDAS eXplorer command will import and navigate the raw roll by roll images into McIDAS areas as described below GETCPP This command will import a Pioneer Venus OCPP image into a McIDAS eXplorer area and attach the necessary navigation transform to it by retrieving the appropriate information from supplementary files stored within the mcidas data sub directory The image can then be manipulated e g remapped gridded or brightness normalized using the general McIDAS commands CAUTION If the time of observation is critical for analysis e g in measuring cloud drift winds then the nominal image start time with which McIDAS eXplorer images are tagged with should not be used for Pioneer Venus images as each image takes several hours to acquire and time difference between the same regions on Venus in two successive full disk images is not constant Use CPPTIM command to determine the observation time for a given location in a navigated OCPP image 3 2 2 OCPP P
46. comrends wtech wil D Jv fa K UE a ote ee eer pee L TT T ves context specific application needs and can be saved and restored via string tables that characterize the workstation context A specific function key menu can also be created by the end user for a Specific purpose Pipeline processing of data can be accom plished directly as well A McIDAS application program can Start the execution of another existing application either synchronously or asynchronously as desired Implementation of such an application by the end user is possible if the user is comfortable wnting a FORTRAN or C language program with the benefit of the McIDAS applications programming manual and some knowledge of McIDAS Tools A variety of tools are available to manipulate the data within McIDAS eXplorer For solar system image data these include geometric and Se p OED rr A O Ca e E aat a Ga OP DD n A iaia ia S cs 6 2 MODAS Jange Window DT A A aa cam a T oe LC Ka pig y ET 3598 310 TAER as DISHAY OPTIONS FHHAMNCF UST FRIER MODMY MAP OVTRLAY NAVIGATE MEASURE g CENTTR IMAGE S Bi HAAGI INDOX 9 2 i 4 431441111111 MM L UST DATA DESCRIPTION BLOCK FE UST AUDIT TRAR j CW FUE UTILITY LWU j 4 LOCATE aa ma DERES ea AE GON BRA E G n 2 gt E P e AS lt as pat A E RS DS KT O 1 Current Navigation Type zx 463 465 Data fource La a Vol i 153 32 Image Compress ion Al
47. consideration of the use of UNIX workstations and PC s as soft ware platforms The primary target data for this endeavor are the imaging data from NASA s solar system missions are the CD ROM volumes pubiished by the Planetary Data System PDS Another goal of the proposed effort was the facilitation of a graphical user interface for user interaction These goals have been met McIDAS eXplorer allows the user to access the full calibration and navigation data attached in the PDS labels The data can be manipulated displayed animated using the developed tools The user manual and help are accessible on line from within an eXplorer session These capabilities have been achieved in the last three years by the development of over 160 000 lines of code mostly FORTRAN and C These are based on about 150 000 lines of sore McIDAS X and McIDAS OS2 versions McIDAS eXplorer is now able to access the PDS solar system cata including the attached navigation and calibration information For images that do not have the SPICE kernels attached new image navigation tools based on the NAIF SPICE toolkit have been incorporated within the eXplorer suite To expose the planetary community to the capabilities McIDAS eXplorer has been demonstrated at Division of Planetary Sciences Meeting in Boulder October 1993 and at the 25th Lunar and Planetary Sciences Meeting in Houston in March 1994 It is also being demonstrated at the 26th Meeting of the Division of Plan
48. data etc These ingestion capabilities are of course not required for analysis of planetary data The other hardware element of McIDAS MVS and McIDAS OS2 versions is a SSEC designed workstation called the Wide Word Workstation WWW This workstation is controlled by an IBM PS 2 personal computer and is capable of storing and displaying up to 1500 image graphic frames in its video memory allowing animation at video refresh rates The interface to this workstation does not yet exist for the RISC 6000 series computers although it is technically possible For reasons of technology and price vs performance the UNIX workstations from different vendors such as Silicon Graphics IBM RISC 6000 series Sun Microsystems and Hewlett Packard McIDAS software has been ported to the X Window environment which is supported by these workstations At the moment all of the new planetary code has been developed for the McIDAS X environment however it can be easily ported to the OS2 environment Finally a general observation about McIDAS is in order By comparison with many of the commercial applications particularly in the McIntosh and Windows 3 1 domains the user interface used by McIDAS may seem dated The primary reason why the interface has not yet changed is that McIDAS is used at many operational meteorological facilities throughout the world as well as colleges and universities in the US The hardware environment McIDAS is used under ranges from IBM com
49. different data into McIDAS and specific planetary applications are described herein Thus the user also needs access to the McIDAS X User handbook to be able to utilize the standard McIDAS capabilities In the past the different missions usually provided the data in the form of Experiment Data Record EDR tapes Supplementary navigation data required to analyze these data were provided as Supplementary Experiment Data Record SEDR tapes The process of using these data for analysis required custom software for each mission and each instrument Fortunately the situation is much improved now with the advent of the CD ROMs Much of the planetary data are now being made available through the Planetary Data System on CD ROMS which allows some commonality to accessing these data However the SEDR data such as trajectory pointing etc are not yet available for all the CD ROMS although limited data are available as SPICE kernels There are many capable software products available which unfortunately can be used only with specific data particularly terrestrial data With many successful missions to the solar system targets we now have an immense amount data collected at numerous objects that are as diverse as the airless moon or Mercury to rings of Neptune as well as comets and asteroids The only thing common about these objects is that they have vastly different physical properties besides the fact that the opportunities to collect data on these targets fr
50. e g date time target etc file_name REMARKS The FITS key words that will get scanned by GETFITS as indicated by this program will get written into the file_name specified GETFITS will scan this file to search for keywords in the file A file can be created once for each non standard variant of the data format APPENDIX 31 GEOM Remap a Voyager frame to remove vidicon geometric distortion using the reseau locations found by the Key in RF source_area destination_area KEYWORDS all optional only areas have to be specified as positional parameters SPLINE Spline size default 12 limits depend on area size for remapping SCALE Area size scale Default is SCALE 1 0 for a 1000 line image SMOOTH ON OFF Smoothing option averages neighboring pixels a bit making nicer looking limbs at the cost of some resolution and line sharpness Default is ON REMARKS Shading correction and or only a dark current removal using SHADE9 must be done before using GEOM APPENDIX I 32 GETALT GETALT Read Magellan Radar Altimeter CD ROM ARCDR s Altimetry Fta Fles ADF s and plot the data along the orbit track on a displayed Magellan SAR image orbit DIR FP PLOT LIST LAT LON ALTS COLORS PARAMETERS orbit_ KEYWORDS ORBIT DIR FP PLOT SIZE LIST LAT LON ALTS ALTS COLORS orbit number for the altimetry data 4 digit Magellan Orbit Number nnnn required either as a
51. ee r A e e r S e r Be e ee n R d ee m mn ee vd mr ee am ms t WORD ITEM S C Image Instrument TYPE COMMENTS 131 132 Data Type S C Image Data Mapped c 8 RAW S C Raw Spacecraft Image 1056x1204 PROC S C Processed Spacecraft Image MAP PROJ Map Projection MOSAIC Mosaic 133 Spacecraft ID NAIF Code I 4 pS 134 Instrument 1D NAIF Code 1 4 135 136 Instrument ID c 8 137 138 Picture ID 1 FDS Crs S C Data ID 139 141 Picture ID 2 IMAGE ID u 142 Picture Time Year 1 4 143 Picture Time Day 1 4 144 Month 1 4 145 146 Picture Time hh mm ss Cra 147 Frame Size Pixels in scan direction I 4 148 Frame Size Pixels in cross scan direction I 4 149 150 FOV Degrees in scan direction R 8 151 152 FOV Degrees in cross scan direction R 8 153 Focal Length mm R 4 154 Exposure Time sec R 4 155 156 Filter ID name Cs 157 Filter ID ordinal 1 4 158 Filter ID central wavelength R 4 159 Filter Half Width at Half Maximum R 4 160 161 Units of Above nm microns C 8 Normally nm 162 163 Imaging Sequence Mnemonic E 8 164 165 Imaging Mode Mnemonic c 8 GAIN OFFSET FLOOD 166 Imaging System Camera Gain C 4 HIGH LOW 167 168 Spare 169 GEOMed or not C 4 GEOM or T 170 PHOTometrically Corrected or not c 4 PHOT or i 171 Al photometric constant ft L to I R 4 172 A2 photometric constant DN to ft L R 4 173 A3 photometric constant ft L to I F R 4 174 180 Spare 181 Orbit Number I 4 182 Eccentricity of Orbit R 4
52. file s for a Voyager image to determine which CD ROM amp sub directory it resides on The index is in mcidas data sub directory Locate a Viking Orbiter image of Mars on the PDS CD ROM volumes VO001 VO0012 This command maps the keywords contained in a pseudo FITS label to the standard FITS keywords expected by the GETFITS command Remove the geometric distortion in a Voyager image for which the reseau locations have been measured RF command and write a new area Read Magellan Radar Altimeter CD ROM ARCDR s Altimetry Data Files ADF s and plot the data along the orbit track on a displayed Magellan SAR image Import Pioneer Venus Orbiter Cloud Photopolarimeter OCPP images from NSSDC tape archive files into McIDAS areas Import an image stored in a FITS format file into a McIDAS area Useful for importing earth based telescopic images of solar system targets This program attempts a first guess image navigation by determining i the image center from limb points using the BRTCEN command ii computing the sub earth and sub solar points on the target from the observation time contained in the label if they are not contained in the label and iii attaching the navigation to the data using the PLANAV command Both the BRTCEN and the PLANAV commands are issued internally by the GETFITS program Since not all earthbased data files available conform to the FITS keyword and value standard some known variations of the form
53. finding for the purpose of image navigation of mages of objects without permanent fixed surface features Primarily intended for earth based images BRTCEN area_ linskip eleskip KEYWORDS KEYWORDS COL color_level 1 7 default 3 INC angular_increment azimuth increment degrees default 5 RADIUS hi low radial range for limb point test 1 0 estimated radius default 1 1 0 8 SCAN start stop azimuth interval for timb point test degrees default 0 0 360 0 NUMBYTE number_bytes_data_per_pixel default 1 usually picked up from area directory DN low hi dn range for limb scan default 10 255 1 byte pixel data 100 32000 for 2 byte data PLOT QUE plots the inner and outer radii for the limb test default is no plot Note that the use of a median filter on dark noisy images can improve BRTCEN s performance REMARKS Once a guess image center is determined by using the center of brightness this key in initiates a radial search for the planet s bright limb in specified azimuth range in increments of deginc from an inner radius to an outer radius and then plots the detected limb points over the image The array of limb points are written to LIMBxxxx where xxxx is the area number of the displayed frame APPENDIX 1 9 CALCMA Calculates Transform Matrix for Planetary Navigation for framing camera image navigation Currently is set up for Voyager images only CALCMA area No_Center_Find_F
54. frame Parameters function SEE to list an entry or PUT to change see below entry_type format used to store data in entry see below KEYWORDS CENTER line element pixel_diam_of_body changes the pixel location of body center and the pixel diameter of the body NAV type NAIF PLAN RADC changes the type of navigation to the indicated format NORTH angle_degrees changes the north angle Example NAVUTL NORTH 330 5 north angle value in the displayed area DDB is set to 330 5 degrees RDC right_ascension declination degrees changeopti axis right ascension and or declination entries RATIO Width_to_Height_ratio_of_image_data FILTER name_of_filter ID area_number some Mcidas or UNIX utilities that copy areas may not change the area number stored in the navigation block to the new area number correct with this keyword option COPY source_area destination_area copies the source area to the destination area while preserving all data and the audit trail but updating the user identifier and the area numbers stored in the DDB and directory Note The use of the COPY keyword superceeds any other command COPY should be used alone Example NAVUTIL COPY 9050 9060 copy area 9050 into 9060 DDB function entry_type entry_size DDB_address new_value APPENDIX I 73 entry_size DDB_address new_value SHIFT The DDB option allows the user to directly see or alter ANY DDB entry Extreme care is ad
55. frame does not contain an adequate or any bright limb to be able to determine the object center with any accuracy If a simultaneously shuttered wide angle frame is available then this command transfers the navigation from the wide angle frame to the narrow angle frame accounting for the misalignment determined from ground based measurements between the two cameras on both spacecraft Note that because the resolution of the WA cameras is 7 5 times worse than that of the NA cameras the navigation of the the NA frames navigated frames this way is no better than that of the wide angle frames APPENDIX 1 7 BROWSE Display a Magellan MIDR 8 x Browse image on a frame and overlay the 7 x 8 tiling grid with framelet or tile numbers to show the component frames Normally called by GETMGN when retrieving Browse images from MIDR CD ROM volumes BROWSE area_ frame_ PARAMETERS area_ Area containing browse image frame_ Frame to load and grid REMARKS This program is a combination of the DF keyin and a specialgridding routine specifically used for Magellan browse images Normally this keyin is called by GETMGN but you may call it separately to restore the browse image to the McIDAS Screen if the browse frame was overwritten APPENDIX I 8 BRTCEN Determine the center of brightness of a full disk at a given sampling then conduct a radial scan at a set angular interval to determine the limb of the body as the first step in center
56. further divided into two parts the Line Prefix and the actual line data image elements line prefix 1 line data 1 line prefix 2 line data 2 etc Nt 0 byte numbers increase gt The line prefix contains documentation about the image and the particular line val code documentation calibration level 0 byte numbers increase gt The size and content of the line prefix depends heavily upon the area type which in turn is determined by the data source The area type is given in word 52 of the area directory McIDAS eXp areas usually contain the area type VISR Regardless of the area type each line in the area has the same length prefix This length in bytes is given in word 15 of the area directory It may be zero and if so there is no line prefix defined for the area Images will normally default be displayed by the DF keyin from the first byte of each line in the area unless specified otherwise NAVIGATION BLOCK To navigate an image is to associate planet based coordinates usually planetocentric latitude and longitude with the pixels of the image This is done using highly complex mathematical models of the spacecraft and camera embedded in parameterized McIDAS navigation software modules Navigation parameters for a digital area when present in the McIDAS system will be supplied in the NAV block of the area file Navigation information is used with the McIDAS navigation software to convert image coo
57. image the block will be zero filled or contain the McIDAS standard hex byte string 80808080 meaning no data This block also contains the Data Descnption Block DDB subblocks described later Word 35 of the area directory contains the byte offset of the NAV block within the file For eXplorer the new navigation block length is always 5 128 640 words or 2560 bytes This is the maximum block length which core McIDAS is currently able to accomodate The next block of bytes contains a CAL entry This entry will be filled with data if the image is radiometrically calibrated or if in the case of Mariner or Voyager imagery reseaus need to be located in the image to geometrically calibrate it This CAL entry may be zero length if no calibration information is needed Like the area directory and NAV blocks each value in a CAL block ts a 4 byte 8 byte or 12 byte quantity Word 33 of the area directory is a byte offset to the CAL block s position within the file For Voyager image data the calibration block entry consists of three parts totalling 512 4096 1616 6224 bytes This is the maximum size the calibration block can be l Part one is a 128 word entry 512 bytes used to parameterize a function to display the image Two byte image data on the mainframe for example uses a three parameter linear transfer function min max scale factor to convert a range of 16 bit DN values to 63 levels on the display screen The keyins MAKESU and DF w
58. management and access services to small field datasets under the control of an individual scientist Examples include the Landsat imagery at the University of New Hampshire ocean data color and temperature na E A n a TS a am rrr L Lana m am m e ae A Laa product The position of objects relative to each other or within the frame can be edited along with the object s size and surface properties e g color shininess and transparency Components that affect the whole scene can also be edited such as lighting and viewpoint camera position In addition to the above features any of the possible adjustments to the scene can be ani mated including the parameters that generate the visualizations Animation is specified by setting what are called keyframes Keyframes specify what certain key frames of the animation should look like The tool uses interpolation methods to generate the frames in between the keyframes A keyframe is set at the beginning of an animation specifying how everything should appear initially Another keyframe is then set at some later time specifying how things should look then For example an object might be shown from the front in the first frame and then from behind in a later frame The viewing position in between keyframes is then automati cally interpolated When all the frames are played the object would appear to rotate More complex animations would involve the use of a number of keyfra
59. navigation C single letter command LF and WHERE commands allow the user to query a frame s contents LISTDDB provides more detailed information about the displayed frame Overlay graphics can be drawn which can also be dynamically saved in separate graphics files for re display later This is particularly useful in the X environment wherein peelable graphics are not possible or implemented on some workstations Thus if any changes are required in the graphic frame the entire contents have to be erased and re displayed 2 1 McIDASese Not quite a language but a syntax of its own At its core McIDAS and McIDAS eXplorer are command driven and not menu driven A certain familiarity with the command syntax is thus useful A Graphical User Interface GUI and a function key based interface are also available to execute most of commonly used McIDAS eXplorer and core McIDAS X applications The GUI is based upon the Tcl Tk scripting language The function key based interface is user programmable and allows creation of a function key based menu system and can be created using a text editor outside of McIDAS environment More than one such menu can be created and used during a single session The function key based menu is invoked with the ESC key which then prompts the user for the name of the file containing the menu script Typically a process can be performed with a command entered in the command window from the workstation key board Usual
60. of McIDAS eXplorer is running 5 1 eXplorer AREA STRUCTURE The mainframe version of the planetary McIDAS software kept navigation data in files called codicils separate from the image areas On McIDAS X and McIDAS OS 2 each eXplorer area is stored as a single binary disk file containing all the information necessary to display and navigate the image Image calibration conversion of DN values to physical values is directly available for images with a single calibration table of 10 bits or less per pixel for the entire image For composite images such as Magellan Venus mosaic data where many small tiles have different incidence angles it is necessary to have a separate keyin MAGCAL to recover such things as surface reflectivity Each eXplorer area has the same format although file lengths are variable with image size calibration data and the amount of audit trail The first 256 bytes of every file contains the area directory block for the image Each value in the block is a 4 byte word 64 words total This directory contains information about both the area and the original image it was created from The area directory is described in detail later The next entry contains the NAV or navigation block for the image Again each value in this block is a 4 byte 8 byte or 12 byte quantity holding the navigation parameters necessary to locate the projection of the image pixels on a target body surface If no navigation is available for the
61. of S C x y z at Sfc 259 Orbital Longitude of Picture Body 260 PG Sub Sun Intersect Latitude at Sfc 261 PC Sub Sun Intersect Latitude at Sfc 262 Sun Longitude 263 264 S C Range from Picture Body Center 265 266 S C Range to Earth 267 268 S C Range to Sun 269 274 S C x y z Velocity in Target Frame 275 Smear Direction deg relative to scan dir 276 Smear Velocity km s relative to tgt sfc 277 North Angle deg relative to scan dir 278 295 3x3 Transform Matrix Inst gt Planet 296 313 3x3 C Matrix Inertial gt Instrument 314 331 3x3 Rot Matrix Inertial gt PicBody Cent 332 Optic Axis RA 333 Optic Axis Dec 334 336 L Vector Az El1 Twist 337 339 Pitch Yaw and Roll Limit Cycle Angles 340 Nadir Angle of Optic Axis 341 Azimuth Angle of Optic Axis 342 352 Spare WORD ITEM User Computed Quantities jm am se ar u a ae ee eee i es ee ees ee ee ee ee es a X X ee se ee 353 354 User Block Type 335 3556 3375358 MEXP VGR McIDAS eXp Voyager MEXP MGN McIDAS eXp Magellan MEXP CPP McIDAS eXp Pioneer Venus MEXP FIT McIDAS exp MEXP VO McIDAS eXp Viking Orbiter specifies user dependent block format Navigation Status Navigation System Type 5 25 1 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 CS R 8 R 8 R 8 R 4 R 4 R 8 R 8 TYPE R 4 R 4 R 4 R 4 R 4 R 4 R 8 RES R 8 R 8 R 4 R 4 R 4 R 8 R 8 R 8 R 4 R 4 R 4 R 4 R 4 R 4 TYPE COMMENTS Cc 8 Crs Cres E
62. past McIDAS differs from most other image display and analysis environments in that it is a multitasking multiframe intelligent display environment In fact to the user McIDAS func tions as a pseudo operating system providing some of the basic functions of an operating system Further it provides the user with a pass through connection to the operating system McIDAS supports multitasking such that while one user application is being executed others can be invoked as needed and limited only by the hardware capabilities The intelligence derives from the fact that the system knows the key data attributes of the images as well as graphics displayed in different frames and this information is available to the application programs This is crucial for quantitative analysis in a multitasking environment Execution of a profile file sets the display environment flags such as number of bits displayed initial number of frames created at start up size of the display frames default font for text and graphics windows image display mode 24 bit three color mode or 8 bit false color etc For example on workstations with 24 bit graphics the session can be started as mcidas bp 24 ig y fr 24 48 imsiz 256 256 This starts a session with independent graphics W key toggles the graphics on and off the image with 3 color 256 lines x 256 elements sized display frames of which 24 are allocated initially and up to 24 more can be allocated dynamicall
63. positional parameter or as a keyword value 8 digit directory holding data Illimmmm required Ml lt nnnn lt mmmm CDPATH variable may be set in string table instead lo hi max footprint number range or max points where lo single footprint or lower limit default 2000 hi upper footprint number limit default 2000 max total number of points to plot default hi lo 1 if lo hi are defaulted the first max points will plot NO default YES plots ADF data locations on navigated frame n size of footprints on frame default SIZE 7 Sinusoidal projection is preferred to show all of Venus surface a 50 km pixel scale will just fit into a 400 x 800 pixel frame HEADER Lists Orbit Header Record LABEL Lists Altimetry Header Record DATA Lists Altimetry Data Records default is no list MINLAT MAXLAT Latitude bounds default LAT 90 90 MINLON MAXLON Longitude bounds default LON 0 360 If lat lon bounds are left unspecified all data points will be listed for orbit nnnn and those falling within the displayed frame will be plotted in the appropriate colors if PLOT YES RAD1 RAD2 RAD3 RAD4 RAD5 RAD6 RAD7 RAD8 RADY RAD10 0 6047 6048 6049 6050 6051 6052 6053 6054 9999 default COL1 COL2 COL3 COL4 COL5 COL6 COL7 COL8 COL9 COL10 COL11 Radii below RAD1 will be plotted in COL1 Radii between RAD1 and RAD2 will be plotted in COL2 Radii between RAD2 and RAD3 will be plotted in COL3
64. radii for solid surfaces and various levels in the atmosphere and are important in dealing with objects such as Venus or Titan Although McIDAS eXplorer is general enough to be utilized for most types of data its Strength lies in its ability to manipulate and analyze multispectral images or data that can be visualized as a two dimensional image Other data such as from station observations from regularly spaced sites or numerical model output can also be manipulated conveniently within McIDAS Atmospheric vertical profiles spectra and Magellan altimeter profiles are examples of different data that can be analyzed within the McIDAS environment linplementanon McIDAS differs from most other image display and analysis environments in that it is a multipro cessing multiframe intelligent display environ ment In fact to the user McIDAS functions as a pseudo operating system providing some of the basic functions of an operating system Further it provides the user with a pass through connection to the operating system to send and execute native operating system commands McIDAS allows for multiprocessing such that while one user application is being executed others can be invoked as needed it is limited only by the hardware capabilites and resources available The frame intelligence derives from the fact that the system knows the key data attributes of the data navigation calibration and physical location in the system
65. tangent of the slope at the 128DN output level 2 0 is default 10 is steep 1 2 is shallow horiz DN value offset of center of curve default is center of the dynamic range INVSIG gamma vert_dn_value gamma approximates the tangent of the slope at the 128DN input level 0 5 is default 0 9 is steep 0 1 is shallow slopes larger than 1 0 give a poor shape vert DN value offset of center of curve default is center of the dynamic range ENDSIN lo hi lodn hidn percent ends in stretch defines limits where linear transfer function saturates lo and hi are the input histogram limits where saturation begins default 10 90 lodn and hidn are the output DN values where saturation begins default 30 225 LOG gamma vert_dn_value gamma approximates the tangent of the slope at the 128DN output level for the LOG function a gamma of 2 0 is default 10 is steep 1 2 is shallow vert DN value offset of center of curve default is center of the dynamic range EXP gamma horiz_dn_value gamma approximates the tangent of the slope at the 128DN output level for the EXP function a gamma of 2 0 is default 10 is steep 1 2 is shallow horiz DN value offset of center of curve default is center of the dynamic range BRKP i1 01 12 02 i3 03 i4 04 i5 05 6 06 7 07 8 08 9 09 10 010 manually defines a set of 10 or fewer breakpoints which the keyin will insert into the SU table no offsets are used here input_area calib_t
66. the displayed frame frame_ graphic frame number on which to enter the annotation Default is current frame KEYWORDS TV line_ ele_ spacing where line_ and ele_ specify the frame coordinates where the label will begin spacing is the line spacing between the day and time strings SIZE font size in pixels APPENDIX 1 51 IMGTS compile and display Time series Data for a given geographic region from image areas filename function KEYWORDS text Parameters filename function text Keywords AREA BAND BOX CHECK COLOR ERASE FACTOR GRA LAT LON MAX MIN REMARKS H H t out filename for the time series data file default none APPEND or PLOT program function default PLOT up to 40 characters used if the LW file is new as the information for the first header line default Iwfile a1 a2 sequential range of areas default current frame band number default current frame numlin numele target box lin ele pixel size must be an odd number default cursor size YES or NO option to check LAT LON SSN BAND UNIT FACTOR parameter values against the LW file header values default YES color level of display symbols default 3 YES or NO erase graphic frame before plotting default NO internal scaling factor for calibration type default 1 0 specify graphics frame default current target box latitude location default cursor position target box longitude location default cursor p
67. the limb points for the diaplayed image from the corresponding file List the limb points file corrresponding to the displayed image TOT for total derivative actually max of gradient in the line or element direction ELE to compute derivative in the element direction dB dE LIN to compute derivative in the line direction dB dL Limb points are found along the longer dimension of the cursor This is crucial when finding limb points near the top or the botom of the image when the planet s visible bright limb is almost tangent to one of the sides of the rectangular cursor box This command is useful when there is excessive noise in the background or when there are rings present such that automatic limb determination is problematic Use IMGCTR to determine the shape size and center of the object by a general conic fit to the image frame limb co ordinates APPENDIX 54 LIMPRO LIMPRO Determine and plot the Limb Profile of a Planetary Image along a radial direction Also plots the derivative profile on the next frame option KEYWORDS Parameter option KEYWORDS AXIS COLOR PLOT MINDN BAND UNIT SCALE Remarks Example CUR a line plot using data through center of cursor SEG a line segment of the image RAD a radial plot at a given azimuth LIN or LOG for y axis scaling color def 3 plot type SLD DOT or any ASCII char def SLD data lt the specified value are set to 0 5 for the case when Y axis is
68. the width to height ratio YES NO Turns interactive histogram on or off Default is YES The area DDB will contain a small subset of standard FITS keywords or those specified by the user in the translation table file FIT which is accessed modified via the McIDAS eXplorer menu interface A listing of the current translation table file contents is obtained using keyin FITSKEY Two extra keywords DATEOBS amp TIMEOBS are available for when the program cannot extract a valid date or time from the FITS header using existing translation tables DATEOBS a single date token MM DD YY TIMEOBS a single time token HH MM SS APPENDIX I 37 GETMGXDR Import a Magellan GxDR global composite framelet from PDS CD ROM volumes MG_3001 or MG_3002 GETMGXDR area frame_ directory File_name KEYWORDS TYPE GTDR Global Topographic Data Record GSDR Global Slope Data Record GEDR Global Emissivity Data Record GREDR Global Reflectivity Data Record ERROR Radius Error Sinusoidal Proj only PROJ MERC Mercator NORTH North Pole Polar Stereographic SOUTH South Pole Polar Stereographic SINUS Sinusoidal extracts 8 browse blowdown of mosaic default FF 1 n extracts a numbered 1024 x 1024 framelet tile where n lt 56 CUR identifies framelet from displayed browse image FILE NAME any valid framelet or browse image file name REMARKS There are four ways of specifying image data on a GxDR
69. view or even a stereoscopic display In all cases looping and animation helps the user in many respects immensely Typically the atmospheric data is quite variable in the time domain so that time lapse observations are a key aspect of any analysis McIDAS provides a means of displaying such time lapse data in a sequence of user controlled animated loops with each component frame providing full access to the Original data in calibrated or uncalibrated units and navigation Users interact with McIDAS through a variety of means A Graphical User Interface GUI is available that can be customized for Specific tasks and is independent of the underlying prograr structure in the sense that the GUI can be changed without usually having to recesign the process itself Experienced users usually prefer to interact with the system directly through a command window McIDAS commands accept both positional parameters as well as keyword oriented parameters The task of entering a sequence of commands that is used repetitively can be simplified through three different methods The first method is to set up a string name with the commands to be used with the replaceable parameters identified explicitly Then a Single command can execute that sequence for the range of parameter values specified for the replaceable parameters A second and more explicit method is to record the sequence of commands to be executed in a batch text file and then issuing the comma
70. 0 returns all MG_NNNNSs for SON FINDFF 50S returns all MG_NNNNSs for 50S FINDFF LAT 50S returns all MG_NNNNSs for 50S FINDFF XS 23 returns all south latitude MG_NNNNs for longitudes 230 to 239 REMARKS This is one of the possible means of locating the image data for a region of interest on the MIDR CD ROM volumes APPENDIX I 29 FINDTM KEYWORDS Ss MIN MAX AREAS string REMARKS 182 S3 s4 DAY TIME DAY TIME MAX MIN Loate areas containing images from different spacecraft acquired within a given time window and send a string to the McIDAS Control program for execution FINDTM SS MIN MAX AREAS string command to processor List of up to four McIDAS spacecraft SSS codes lower window limit in YYDDD HHMMSS format upper window limit in YYDDD HHMMSS format area limits to perform search Default area limits are 1 9999 string command limited to 8 tokens in length This is a macro command that is useful to locate areas from multiple satel lites covering a planet for near simultaneous coverage command can be sent to the control program to execute once the areas are located On example of such a command may be to remap and mosaic those areas to make a global composite such as from earth satellite data APPENDIX I 30 FITSKEY A program to create a translation table for FITS header keywords and the FITSKEY keywords in a datafile if it contains non standard definitions for the required inoput
71. 0 workstations the core McIDAS X software has been ported to HP and Sun workstations SunOS 4 1 3 SunOS 5 3 and Solaris 2 3 and and hence the explorer portion can also be used on those workstations The port to the UNIX on a PC platform UNIXWARE from UNIVEL was a disappointment in terms of operating system peculiarities and support of graphics cards The effort required to support this particular operating system has been considerable and is now deemed to be unaffordable at least in the short run until either the operating system itself matures and more support is available from the vendor We have briefly looked into the use of an alternate UNIX implementation on a PC platform the LINUX operating system which is in the public domain Some portions of the PC McIDAS have been ported but once again the support of high end graphics cards is minimal and it is not known whether the eXplorer software could be effortless ported For lack of sufficient resources the work has on porting the software to the UNIX on Intel chip based machines ihas been at least temporarily halted pending future Support McIDAS and McIDAS eXplorer can be used under the IBM OS 2 Version 2 1 operating system except for the GUI available on X window platforms Previously running McIDAS under OS 2 required the use of a special video display card which was available only for the microchannel bus We supported the development of the Presentation Manager for the graphical display e
72. 0080 JSEDR1 Voyager 1 Jupiter encounter SEDR file JSEDR2 Voyager 2 Jupiter encounter SEDR file jup035 5 bsp P kernel file for Galilean moons of Jupiter for 1990 2010 APPENDIX II 2 Pe PAGE MANDO MOT T MX jupitertapes mcumdir tab NSEDR2 neptapes orbele pvo pck00003 tpc pvocpp img RESEAUDATA SSEDR SSEDR2 uranustapes verl_jup bsp verl_sat bsp ver2 jup bsp vgr2 sat bsp vgr2 ura bsp vgr2_nep bsp vgr1n0 through vgr1n7 vgr1w0 through vgr1w vgr2n0 through vgr2n7 A catalog of Voyager 1 and 2 Jupiter EDR tape cartridges Each cartridge contains 240 images 10 1600 bpi original EDR tapes Magellan Mission cumulative directory for the MIDR data PDS CD ROM Volumes MG0001 through MG0080 This is the version from MG0080 CD Voyager 2 Neptune encounter full SEDR file A catalog of Voyager 2 Neptune EDR tape cartridges Each cartridge contains 240 images 10 1600 bpi original EDR tapes Pioneer Venus Orbiter orbital elements file text The NAIF kernel file containing the planetary physical constants and other data used by NAIF software Other NAIF data files are also copied into this directory Catalog of Pioneer Venus Orbiter Cloud Photopolarimeter images text This is a binary file containing nominal reseau locations for Voyager 1 and 2 NA and WA cameras The structure of this file is described elsewhere Used by RF and RESEAU commands Voyager 1 Saturn encoutner SEDR file V
73. 140 141 142 143 181 Image Type Number of Scan Lines Scan Sample Rate Image number Spare 182 Eccentricity of Orbit 183 Inclination of Orbit to Ecliptic 184 Ecliptic Longitude of Ascending Node 185 Argument of Periapsis 186 Orbital Period 187 Semi Major Axis of Orbit 188 Ecliptic Latitude of Periapsis 189 Ecliptic Longitude of Periapsis 190 Altitude from Target Center at Periapsis Data DSN NAIF Code 191 192 Image Compression Algorithm ITEM Central amp Picture Body 193 195 Central Body Name 196 Central Body NAIF Code 197 199 Picture Body Name 200 Picture Body NAIF Code 201 Picture Body Rotational Period 202 Picture Body Pole Right Ascension 203 Picture Body Pole Declination 204 Nominal Picture Body Eq Radius 205 Nominal Picture Body Pol Radius km 206 Nominal Picture Body Cross Eq Radius 207 209 Spare 210 Picture Body Eccentricity 211 256 Spare WORD ITEM Imaging or Map Projection Geometry 257 258 Map Projection Type Roll by Roll Proj 259 Date Scan Begins 260 Time Scan Begins 261 Orbit Number 262 Date of Last Periapsis 263 Time of Last Periapsis 264 Ecliptic Latitude of S C Spin Axis 265 Ecliptic Longitude of S C Spin Axis 266 Navigation Spin Period 267 R M S Deviation Spin Periods 268 Length of Scan sec SORT e2 p2 p 5 20 hrs km Remapped km c 8 ra 1 4 IMAGE LIMBSCAN POLARIM C 8 crs I 4 R 8 1 4 R 4 R 4 R 4 R 4 R 4 R
74. 2 and 4 are linked as opposites if the McIDAS session has 4 active frames This is a leftover from the days when an analog disk was used to Glossary 4 display the imagery The disk had two surfaces which were recorded and read independently P Toggle command to freeze free the cursor position as controlled by the mouse OS 2 version only on the image MACRO Commands A macro command is created by using a precompiler fx name mac assuming the source file called name is in the mcidas src sub directory As far as the user is concerned there is no noticeable difference in the entering or the execution of the macro commands as compared to the regular McIDAS commands The macro commands are used to chain several McIDAS commands into a specific sequence for a particular application but if a component command terminates abnormally for some reason then the entire macro command may abort Examples of such commands are AAMAP and LODSSP Explanation of how to use a given macro command can be obtained in the same way as a regular McIDAS command by typing HELP command_name Key ins A complete list of core and eXplorer McIDAS key ins can be found in the User s Manual Batch mode Commands can be executed in the batch mode from a text file by typing RUN file_name The text file containing the commands must reside in the mcidas data sub directory Coordinate Systems McIDAS recognizes several coordinate systems for the data Typic
75. 61 PROJSAMP 262 263 Projection Longitude 264 265 Image Center Latitude 266 267 Image Center Longitude 268 269 Image LAT UL 270 271 Image LAT UL 272 273 Image LAT UL 274 275 Image LAT UL 276 277 Image LAT UL 278 279 Image LAT UL 280 281 Image LAT UL 282 352 Spare R 4 1 4 Rs R 8 R 8 R 8 R 8 R 8 R 8 R 8 R 8 R 8 WORD ITEM User Computed Quantities TYPE COMMENTS 353 354 User Block Type Cre MEXP MGN MEXP VGR McIDAS eXp Voyager MEXP MGN McIDAS eXp Magellan MEXP CPP McIDAS eXp Pioneer Venus MEXP FIT McIDAS eXp Flexible Image Transport System MEXP VO McIDAS eXp Viking Orbiter specifies user dependent block format 355 435 Spare 436 Minnaert Fit Constant Max DN Used I 4 437 Minnaert Fit Constant Calc Slope R 4 438 Minnaert Fit Constant Calc Intercept R 4 439 Minnaert Fit Constant Mean Abs Dev R 4 440 460 Spare WORD ITEM Supplementary Information 461 462 Supplementary Block Type 463 465 Data Source CD ROM Volume tape name 465 512 Spare TYPE COMMENTS _ oo mek gg r mr tial Crs SUPL MGN Cr lz m a nr e mr cere o a ee ee ee ea le a a a mr oe eww aps bak oe eee ee eee eee ee ee eee ee ee eee eee eee ee dehe ee dra m m mr m n mm rr rer res eee e re cr s es ee ee ee eee erer rha mr ee m n e e Kin eee r 131 132 Data Type Raw S C Image 133 Spacecraft ID 134 Instrument ID NAIF Code 135 136 Instrument Mode ID 13 L39 139
76. 8 Frame Size Pixels in cross scan direction I 4 149 Focal Length mm R 4 150 151 FOV Degrees in scan direction R 8 152 153 FOV Degrees in cross scan direction R 8 154 Exposure Time sec R 4 155 156 Filter ID name 8 157 Filter ID ordinal 1 4 158 Filter 1D central wavelength R 4 159 Filter Half Width at Half Maximum R 4 160 161 Units of Above nm microns Crs 162 163 Imaging Sequence Mnemonic C6 164 165 Imaging Mode Mnemonic c 8 166 Imaging System Camera Gain C 4 167 Imaging System Camera Scan Rate C 4 168 Imaging System Edit Mode C 4 169 GEOMed or not C 4 170 PHOTometrically Corrected or not C 4 171 Al photometric constant ft L to I R 4 172 A2 photometric constant DN to ft L R 4 173 A3 photometric constant ft L to I F R 4 174 182 Spare lg2 ECcentricity of OrDIit R 4 183 Inclination of Orbit to Ecliptic R 4 184 Ecliptic Longitude of Ascending Node R 4 185 Argument of Periapsis R 4 186 Orbital Period R 4 187 Semi Major Axis of Orbit R 4 188 Ecliptic Latitude of Periapsis R 4 189 Ecliptic Longitude of Periapsis R 4 190 Altitude from Target Center at Periapsis R 4 191 192 Image Compression Algorithm C B WORD ITEM Central amp Picture Body TYPE 193 195 Central Body Name C 12 196 Central Body NAIF Code I 4 197 199 Picture Body Name C 12 5 16 COMMENTS VGl 31 VG2 32 31001 31002 etc ISSNA ISSWA S C Data ID normally nm VPHOT etc BOTSIM etc HIGH LOW b R D 5 T T D 1 1 1 3 etc
77. A 005 50 50 addback of image no display FILTVGR 20 21 1 OPTION C F 22005 10 5 5 5 5 display a low variance scene using a smaller filter size FILTVGR 20 21 FRAME 3 LOCATE AC XCOORD 275 YCOORD 330 MAG 2 OPTION DFA display DFA filtered image centered at line 275 element 330 in frame 3 APPENDIX I 27 FINDALT Determine the Magellan ARCDR CD ROM volume number containing altimetry and radiometry data for a specific Magellan orbit FINDALT _orbit_ Remarks The orbit number passing over a given geographic location on Venus can be found using FINDFF which first locates the MIDR CD ROM volume containing the Magellan radar image of a region of interest The label of that image indicates the first orbit number used to create that image tile APPENDIX I 28 FINDFF Determine the MAGELLAN CD ROM MIDR volume numbers containing a given latitude longitude region FINDFF lat HEM Ion PARAMETRS lat LL two digits must be a multiple of 5 HEM NorS single letter north or south hemisphere lon LL two digits including leading 0 representing any longitude between 0 360 divided by 10 Program does a character search for records using the byte strings LLN NLL LLNLL or LLSLL assembled from keyin parameters returns CD ROM ID for each such record Blank lat lon fields are ignored but N is assumed default Examples FINDFF 30S 12 returns all MG_NNNNSs for latitude 30 and longitudes between 120 and 129 FINDFF 5
78. AL FRL bax pu Jalis i 1 Bitameort ciL O LT taneli By daa th O AHE OR Inland Cocot ml i EST K S o lt TFT ERE Hoan 3 TT T Deoiniton Soe J SRIBVSE YH Ficiuse ad Le TET B C T RE 154 333 8 Pastore toad Centar Fiw Bp tas E d TT H FT TT LA N Texty Navigation RIO a sa hen yada sk on Pres SEITE eee BE ZN de den da ROE DE E 0 R noai aT EL E L s gt S aupplesautery T bi S ST AAA ETAT E NT N P eP Wita vE e Pw w a ra soe ARI SADA Sigg ea DIR Pto i o S gt as Y Od pala for LTD Rom o as 6 099 PaaS LIER Saved lizes hada amp AERTS ntexton a stert e topa L pork A E S BABO RL Broz cbc Ruto Las mad Sica ball E LIT DELL re PA i ae MR ee a N DJe gt Optic bria tac Pry E 278 929 May North dx le hes relativi te PTA da EEE L ON D30 WEE MD RIE PLA lao Vanek cit PRL oat ay Ki cad Conte vat cae es i CULL IS ESSES ELE NS TERED 096 691 80 Sub ae Planetacantrta Latitude 0 SEE 2 95 330 92 404 Pub B C PULLAN TS LT tdo E pss 3 199 B 1 T Kia al halt TITUS T T R Ta 11T ep QEG ee ve es TES 1RSE DI GIS 14 Sub Del Plapetocanmtr a TT T S i i 619 Reds Sar Plubeluonutaio TTT Linde gt o La EE Fueron iton Gatton igor ad VEA e Dn LATING SY tHe Pins Kay 103921 DUO 9 cag Rk ea R AAA ARA VAN RI RAS rb T SEE S M NORAT E SAS Hort e Moon oT Damo SPP IELLEOAE TE AAA ELL FPP EP PPP PP ALP Figure 1 1 A view of the McIDAS X screen The Command window is at t
79. ALCMA is an associated Kevin that actually facilitates the PLAN navigation from Limb points determined using PLAEDG It is assumed that the SEDR data are available and attached to the image using either SEDRIN or GETSEDR PLAEDG options allow the limb points to be listed removed from the DDB or entered at the cursor location IMGCTR In most planetary analysis the planetary images first need to be navigated The first step in image navigation is to locate the center of the target object in the image space IMGCTR is a command that facilitates this task by determining the center from the 4 10 bright limb locations which have been previously recorded in a limb points file LIMBxxxx where xxxx is the area number The limb locations themselves can be determined from one of two distinct methods using LIMBPT to locate the limb by the method of the maximum rate of change of brightness along a line or a column of the image or by using BRTCEN to locate the limb by determining the location where the brightness gradient along a radial direction is maximum relative to the first guess center location The guess center location is found as the center of brightness and works well for full disk images For partial disk images the guess center can be specified manually or found iteratively using BRTCEN and IMGCTR commands in sequence IMGNAV Once the image center has been found from the bright limb or by other means and entered into the DDB for that im
80. AN and TITANIA EXAMPLES PHYSCON 399 to list constants for earth PHYSCON PHOBOS 10 list constants for Phobos Remarks 1 NAIFID is determined from the name by subroutine BODCON Only the first 4 characters of the object name are significant and must be in upper case 2 For bodies with massive atmospheres the radii are defined separately for solid surfaces and atmospheres at the cloud top level In such cases the NAIFID is modified by multiplying by 10 and adding 1 Thus Venus NAIF ID 299 atmosphere becomes 2991 299 10 1 In general the NAIF ID s for planets and satellites can be entered as the actual NAIF_ID multiplied by 10 without any confusion 3 The NAIF ID s for asteroids are defined differently As of May 4 1993 no asteroid data is available 4 PHYSCON also prints the acceleration due to gravity m sec 2 and the escape velocity for the object km sec along with the length of the day hours and the triaxial radii and equator pole eccentricity for the spheroid 5 If a new object is to be added to the MciDAS eXplorer environment or if any of the current parameters need to be updated the subroutine BODCON needs to be edited and recompiled Naturally all commands that call BODCON need also to be relinked This is done primarily to ensure that the change is made deliberately and not inadvertently by editing constants from a file as with the NAIF physical constants kernel file pck00003 tpc which can be edited at w
81. ARAMETER PERIOD AFTER START TO BEGIN PLOTTING DEFAULT 1 TIMET TIME PER ORBIT TICK min DEFAULT 2 CROSST DRAW EVERY NTH CROSS TRACK DEFAULT 100 IROTRAT INSTRUMENT ROT RATE rpm DEFAULT 2 FOVSTEP DRAW EVERY NTH FOV DEFAULT 1 PLOTLON LON PLOT TYPE PLA OR SUN DEFAULT PLA DATE TEXT STRING OF START DATE DEFAULT 1 JAN 2001 TIME TEXT STRING OF START TIME DEFAULT 00 00 00 0 REMARKS This command is useful for determine the coverage obtained by an orbiter around a solar system object with a given orbit from nadir pointing spacecraft A newer version will also compute the spacecraft visibility windows from a given set of surface locations APPENDIX 67 MDCLAS Spectrally classify a multi band image using mean distance statistics PARAMETERS inarea outarea sigarea KEYWORDS BANDS NULL area to be classified Output classified area with the FINAL N spectral classes AREA WITH SIG STATISTICS FILE BANDS BAND1 BANDZ BANDN Bands to classify default is all bands in the area DATA DROP OUT DECISION ANY classify as ZERO if ANY band in image O ALL classify as ZERO if ALL bands 0 APPENDIX 68 MGNORB IS AN EXPERIMENTAL PROGRAM TO PREDICT WHEN THE MAGELLAN ORBITER WILL SCAN A GIVEN SITE ON VENUS WITH EITHER NADIR LEFT OR RIGHT POINTING SENSORS THE PREDICTION IS MADE IN REFERENCE TO A GIVEN ORBIT PRESENTLY DEFAULTED AT ORBIT 2667 THE PRESENT FORM LIMITS THE ORBIT PRED
82. Appl Meteor 22 766 778 PEPE PAGE BLANK NOT FILMES 60 T rere Abstract for 25th LPSC Houston March 14 18 1994 Access Analysis and Display of Magellan Data with McIDAS eXplorer R S Saunders The compilation of radar observations of the Venus surface from tge Magellan mission data has been resulted in over 70 giga bytes of radar reflectivity and radiometry images and altimetry profiles along the spacecraft track The imagery data are available from the Planetary Data System on 80 CD ROM volumes the altimetry data on 15 CD ROM volumes and the global topography radiometry and surface slope compisites are available on a set of 2 CD ROM volumes To facilitate access analysis and display of these data a software environment McIDAS eXplorer has been developed It is based on a mature system that is used extensively for earth weather satellite observations and the extensions actually allow analysis of most solar system targets for which spacecraft and ground based telescopic data are available in recognizable formats Navigation registration and calibration of the planetary data are an integral part of the environment Designed to run on most UNIX workstations supporting X windows the environment is user extensible allowing addition of end user developed applications and includes both a Graphical User Interface and a command line interface multi frame display and animation capability and tools for most image processing applicati
83. B Magellan Venus Orbiter 1 MAGELLAN Viking Mars Orbiter 1 21 VIKING 1 ORB Viking Mars Orbiter 2 330 VIKING 2 ORB Voyager 1 Jupiter Saturn S VOYAGER 1 Voyager 2 Jup Sat Uranus Neptune 32 VOYAGER 2 Galileo Jupiter Orbiter F GALILEO ORB Mars Observer 94 MARS OBSERVR Non Image Derived Data U DERIVED DATA Miscellaneous 1 TEST IMAGE Graphics 2 GRAPHICS MDR Radar 3 MISC Meteosat Visible 4 METEOSAT VIS Meteosat Infrared 5 METEOSAT IR Meteosat Water Vapor 6 METEOSAT WV RADAR 7 RADAR Miscellaneous Aircraft Data MAMS 8 ACET 9 RMET 10 COMPOSITE 11 GMS Visible 12 GMS GMS Infrared 13 GMS IR ATS 6 Visible 14 ATS6 VIS ATS 6 Infrared 3 ATS6 IR SMS 1 Visible 16 SMS I SMS 1 Infrared 17 SMS I IR SMS 2 Visible 18 SMS II SMS 2 Infrared Lo SMS LIL ER GOES 1 Visible 20 GOES 1 GOES 1 Infrared 21 GOES 1 IR GOES 2 Visible 22 GOES 2 GOES 2 Infrared 23 GOES 2 IR GOES 3 Visible 24 GOES 3 GOES 3 Infrared 25 GOES 3 IR GOES 4 GOES 4 GOES 5 GOES 5 GOES 6 GOES 6 GOES L GOES 7 Visible VAS Infrared amp Water Vapor VAS Visible Infrared amp Water Vapor VAS Visible Infrared Visible Infrared TIROS N NOAA 6 NOAA 7 NOAA 8 NIMBUS Satellites Mariner 10 Voyager 1 Voyager 2 Galileo Hubble Space Telescope Meteosat 3 Meteosat 4 Meteosat 5 NOAA 10 NOAA 11 NOAA 12 NOAA 13 NOAA 14 GVAR GVAR Sounder Future GOES Future GOES Future GOES Future GOES Future GOES Future GOES Future GOES Future G
84. CD ROM 1 Use the keywords TYPE PROJ FF The first two specify a leaf of a directory tree while the last identifies a file in the specified directory This is the most common way to identify data 2 Load a browse image to the screen using the TILES keyword to define the McIDAS frame and overlay a tile framelet grid Then use the FF CUR option to select a tile by positioning the cursor within the tile outline on the graphic overlay 3 Identify the directory using the DIRECTORY keyword and the file using the FF keyword Note that DIRECTORY is limited to 12 characters does not include cdrom and you must use lower case characters 4 Use the FILE NAME string at the end of the command line You do not need FF or a file extension as the program will do that for you If you are working in the same directory all the time you can set the CDPATH prefix to the path e g TE CDPATH cdrom gtdr error and then erely have to set the FILE NAME string to f23 where File_name a valid file name containing GxDR data OPTIONAL Must begin with and be the last entry on input line APPENDIX 38 EXAMPLES GETMGXDR GETMGXDR GETMGXDR GETMGXDR GETMGXDR If full path is given CDPATH in string table must be the GxDR CD ROM is assumed mounted as cdrom using the UNIX commands mountcd and or umountcd in the directory bin or the McIDAS eXp command CHANGECD Use keyins FINDFF and FINDALT to locate a CD
85. CR 189382 Final Report for work performed under USRA Contract No 5555 08 JAPA y 4 R towards the development of MCIDAS EXPLORER A VERSION OF MCIDAS FOR PLANETARY APPLICATIONS Sanjav S Limaye Principai Investigator Co Investigators P R Stephen Saunders JPL SS Lawrence A Sromovsky SSEC is 4 Michael Martin JPL L m U E z gt i Q ho wd Ora e Space Science and Engineering Center a University of Wisconsin Madison T 1225 West Dayton Street vi Madison Wisconsin 53706 G Q 608 262 9541 sanjayl ssec wisc edu July 1994 A VERSION OF McIDAS FOR PLANETARY APPLICATIONS Final Report NASA CR 189382 276 p Z S Tas 0033941 G3 82 A TE T TEE tJ APPENDIX I Abstracts of presentations at the Division of Planetary Science Meetings in 1993 and 1994 at the Lunar and Planetary Science Meeting 1994 and the Planetary Data Visualization Workshop in 1993 A Ee eee ee SUMMARY This is the final report on the development of McIDAS eXplorer an extension of McIDAS for solar system applications This work has been supported under the Applied In formation Systems Research Program funded by NASA under USRA contracts 5555 08 and S C 550 08 and NASA Contract NAS5 31347 The initial goals of this effort were to bring to the planetary community the tools used by the terrestrial meteorological community for the access display and analysis of weather satellite data An additional
86. Clear Clear Clear Clear Violet Violet Violet Violet Blue Blue Blue Blue Green Green Green Green Orange Orange Orange Orange UV UV Average over the entire frame measured from reseaus Central 100 pixels only after Danielson et al 1981 The vidicon images obtained from Voyager cameras suffer from geometric and radio metric distortions Before much of the quantitative analysis can be carried out it is necessary to correct the data for these distortions The removal of the geometric distortions requires the use of the geometric distortion indicated by the known locations of the reseaus and their image locations The radiometric distortion removal requires the shading files that contain tables of the vidicon response at each pixel for a given exposure 3 1 1 Pre Processing of the Voyager 1 and 2 Images The images acquired from the Voyager vidicons suffer from two kinds of distortions a photometric and b geometric The photometric distortions correspond to the non linear response of the brightness read out across the image for a uniform incident illumination This nonlinearity actually is from two distinct sources i non linear response of the vidicon itself and ii the development of dark current on the vidicon as soon as the image is shuttered The geometric distortion arises from optical distortions due to the magnetic focusing used in the vidicon system for reading out the image brightness data and results primarily in a
87. D ROM Volumes 4 5 Hubble Space Telescope images of Saturn Uranus and Satellites Voyager 2 images on EDR tapes and PDS CD ROM Volumes 1 3 Neptune Rings and Satellites Voyager 2 images on EDR tapes and PDS CD ROM Volumes 9 12 References Castleman K R 1979 Digital Image Processing Prentice Hall Englewood Cliffs New Jersey 429 pp Suomi V E R J Fox S S Limaye and W L Smith 1983 McIDAS III a modern interactive data display system J Clim Appl Meteor 22 766 778 1 10 2 0 USING McIDAS eXplorer McIDAS eXplorer is a set of specific commands or applications programs that can be run under McIDAS X and familiarity with McIDAS X workstation environment is useful The current release of McIDAS X and eXplorer also support a Graphical User Interface GUI based on the Tcl Tk scripting language This GUI provides access to many of the commands in an intuitive manner using toolbars Help about specific commands a glossary a tutorial section on how to accomplish certain tasks is also accessible via this GUI A completely GUI based version of McIDAS X called MERLIN is also available via anonymous ftp McIDAS X capabilities installation notes can be found in the Users Guide available from SSEC For novice users a brief introduction to the McIDAS concepts 15 given here Starting and ending a McIDAS Session At the console login enter the user ID and the password to log onto the workstation The user ID and the password a
88. E frame magnification displays OUTAREA to frame default is no frame load OPTION NOI threshold gradient BAD threshold gradient DIV idrange threshold bleedbloom addback length height increment decrement DIF idrange threshold bleedbloom addback length height increment decrement DFA midrange threshold bleedbloom addback length height increment decrement LOW midrange threshold bleedbloom addback length height increment decrement NOT OPTION IS A LINE DROPOUT AND SHOT NOISE FILTER COMBINED BAD OPTION REMOVES REALLY BAD NOISE CORRELATED ALONG A LINE THRESHOLD DN DELTA ABOVE NEIGHBORING PIXELS ON A LINE BEFORE A NOISE SPIKE 15 SQUASHED GRADIENT DN DELTA TOLERATED BETWEEN PRECEEDING LINE amp SUBSEQUENT LINE BEFORE SQUASHING SPIKE NOISE REMOVAL ALGORITHM FIRST CHECKS TO SEE IF THERE IS A SMOOTHER THAN GRADIENT TRANSITION FROM THE PRECEEDING TO THE SUBSEQUENT LINE IF SO AND THE MIDDLE LINE PIXEL EXCEEDS THE AVERAGE OF ITS ABOVE AND BELOW PIXELS BY THRESHOLD THE MIDDLE PIXEL IS REPLACED BY THE AVERAGE OF ITS TWO VERTICAL NEIGHBORS THEN A SHOT NOISE FILTER IS APPLIED HORIZONTALLY TO ANY PIXEL DEVIATING BY MORE THAN THE THRESHOLD FROM ITS PRECEEDING OR SUBSEQUENT NEIGHBOR THUS GRADIENT 0 GIVES AN ORDINARY SHOT NOISE FILTER WHILE SETTING IT NON ZERO REMOVES CORRELATED NOISE BURSTS ALONG A LINE APPENDIX 1 25 DIV OPTION IS A DIVIDE FILTER ENHANCES LOCAL ALBEDO CHANGES DIE OPTION IS A DIFFERENCE FILTER ENHANCES D
89. E AREA SEDR LOC POLEN FDS RA DEC OPT TOIMG AREA SEDR LOC POLEN FDS OPT TOIMG POLE POLEN FDS OPT TOIMG POLE C OPT is one of the following TOEME conversion option for Line Ele gt RA 4 DEC default TOIMG conversion option for RA amp DEC gt Line Element TOIMG POLE Calculates picture body POLE default is TOIMG POLE C Corrects C matrix for pic body default is Required arguments FDS FDS number of the Voyager image default 0 0 LIN Star or planet center line position in image ELE Star or planet center element position in image RA Input Right ascension for conversion default 297 0 DEC Input Declination for conversion default 18 1 OPTIONAL KEYWORDS AREA Area number default is 0 which implies displayed frame SEDR SEDR file name default is VGRNSEDR LOC CURSOR next uses LIN ELE keywords Default 500 0 500 0 IMAGE RAW GEOM default is GEOM SKIP Skip lines in searching for star centroid default 1 no skip POLE Source of pol RA amp DEC default SEDR values else 42 81179327 amp 298 857487705 satellite orbit SEDR values currently default to 42 8 amp 298 9 respectively STARLOC OPNAV File containing star location SKY HIST AVG Method for subtracting background AVG is default ROT Roll angle offset default 0 91 POLRAD Polar radius of planet in image Neptune default 24414 0 STAR Star identification 12 characters RA Right asce
90. EA destructive REPLACE AREA re generates area amp nav NAV Display NAV words of current PLAN navigation only Maximum useful number and default is NAV 128 MORE 0 3 Adds additional output for detailed nav diagnosis APPENDIX I 80 NOTE AREA PLANET and NORTH angle may be specified as positional parameters Examples PLANAV Indeed the area and planet identification are required but if you misspell keywords they will be ignored and the default parameter values will apply Lists current navigation for last accessed area PLANAV 23 VENUS_CLOUDS 180 0 REPLACE AREA Venus upside down in area 23 PLANAV 23 SATURN REPLACE AREA VIEWPOINT 90 0 180 0 15 north polar perspective view at a distance of 15 planetary radii PLANAV AREA 23 500 500 PLANET JUPITER REPLACE AREA default projection of Jupiter is generated in a 500x500 size area PLANAV 23 EARTH VIEWPOINT 23 5 10 1 025 ANGLE 0 50 20 REPLACE AREA NOTES 23 5 lat 160 km above earth surface looking leftward toward limb If the remap runs too fast and gives a black image you do not have a destination location which ought to contain any source data typically you are on the back side of the planet or are using incompatible parameters which the program resolves in a way you don t expect The trouble could be in either the source area or the destination area navigation Destinations with all data within a single spline domain may also truncate to black Try
91. EA no default must be specified BEGL ENDL IMAGE LINES default uses brightness center BEGE ENDE IMAGE ELEMENTS default uses brightness center SAMPL SAMPE SAMPLING INCREMENT defaults SAMPL 1 amp SAMPE SAMPL MIN MAX LATITUDE EXTENTS defaults 90 0 90 0 MIN MAX LONGITUDE EXTENTS defaults 180 0 180 0 COLOR OF POINTS ON MINNAERT PLOT default 3 LIMITS FOR LOG MUMUO X AXIS FROM STRING TABLE ACCEPTABLE RANGE FOR LOG I MU Plot is not drawn if no limits are specified Works either with 1 or 2 byte data As currently set 2 byte raw data must be in the 0 4095 DN range Needs a change so that the calibrated data units are used such that the raw data range can be 32767 to 32766 and calibrated data in any units APPENDIX l 70 NAIFNAV Command to calculates position of an observer and the sun with respect to a target body planet or spacecraft via the SPICE SP kernels and or the body center and body pixel diameter from a limb point file These values are then written to the DDB for access by the nvxnaif dim navigation routine If the spacecraft is Voyager 2 and the target body is Uranus or Neptue the C pointing matrix is alo retrieved from the SPICE C kernel and placed in the DDB NAIFNAV area_number RATIO pixel_ratio Defaults area_number currently_displayed_image pixel_ratio ratio of width_to_height default 1 1 REMARKS This routine may not return the correct state information for narrow a
92. ER I E gt 100 HAS LITTLE NOTICEABLE EFFECT AT ALL SET TO 999 TO TURN OFF THIS CORRECTION ADDBACK PERCENTAGE 0 100 OF ORIGINAL IMAGE APPEARING IN DFA FILTERED OUTPUT 100 ADDBACK IS THE PERCENTAGE OF THE FILTERED IMAGE WHICH APPEARS IN THE OUTPUT AREA DEFAULT 30 FOR DIV DIVIDE OPTION SPECIFIES THE DN OUTPUT AS A RATIO USING THE NUMBER OF PIXELS IN THE FILTER NOMINALLY 300 VERY LOCALLY LOW CONTRAST IMAGES SUCH AS CLOUDS MIGHT REQUIRE A MULTIPLIER VALUE AS HIGH AS 900 A VERY BUSY LOCALLY HIGH CONTRAST SCENE MIGHT REQUIRE A VALUE AS LOW AS 20 CHOOSE THIS PARAMETER TO MAXIMIZE THE DYNAMIC RANGE OF THE OUTPUT IMAGE WITHOUT GOING OVER THE 255 DN LIMIT DEFAULT 300 DN WITH MIDRANGE 160 DN FOR THE DIF DIFFERENCE OPTION MULTIPLIES THE DIFFERENCES DEFAULT 3 LOCALLY LOW CONTRAST CLOUDS MIGHT REQUIRE A VALUE OF 10 TO GET UNSCALED OR REAL DIFFERENCES SET THIS PARAMETER TO 1 APPENDIX I 26 LENGTH HEIGHT HORIZONTAL amp VERTICAL FILTER DIMENSIONS DEFAULTS ARE LENGTH 30 HEIGHT 10 INCREMENT FILTER SIZE CHANGE PER PIXEL AT A THRESHOLD DECREMENT VALUES 001 099 PERMITTED DEFAULTS ARE INCREMENT 15 DECREMENT 15 DEFAULTS inarea outarea frame OPTION DFA 005 30 30101515 OPTION DIF 128 05 3 30101515 OPTION DIV 160 0 5 300 30101515 EXAMPLES FILTVGR 20 21 1 OPTION DIV 200 0 600 filter a low contrast scene FILTVGR 20 21 3 OPTION DIF 16005 1 look at the real differences FILTVGR 20 21 OPTION DF
93. ETAILS EVERYWHERE DFA OPTION IS A DIFFERENCE WITH ADDBACK DETAIL AND ALBEDO MIX LOW OPTION IS A LOW PASS FILTER REPLACES PIXEL VALUE MIDRANGE MIDDLE OF DYNAM RANGE FOR DIF 8 DFA OUTPUT NOMINALLY 128 FOR AN IMAGE OF 0 255 DN IMAGES WITH SMALLER DYNAMIC RANGE SHOULD BE CONTRAST STRETCHED PRIOR TO FILTERING FOR BEST RESULTS DFA OPTION ESPECIALLY WILL PRODUCE DARK OUTPUT IF IMAGE DOESN T HAVE FULL DYNAMIC RANGE THE DIF OPTION WILL ALSO REQUIRE A LARGER MULTIPLIER DN OFFSET FOR WINDOW ENHANCEMENT OF DIV OUTPUT SUBTRACTED FROM PIXEL VALUES WITH SLOPE DETERMINED BY ADB MUL PARAMETER DEFAULT 160 DN IF ABM UNSPECIFIED OTHERWISE DEFAULT 0 DN OFFSET THRESHOLD DN THRESHOLD AT WHICH ADAPTIVE FILTER SIZE CHANGES NOMINALLY 1 2 DN ABOVE BACKGROUND BELOW THRESHOLD THE FILTER WILL SHRINK BY DECREMENT PIXELS FOR EACH PIXEL TO A LIMIT OF 1 PIXEL IN SIZE NO FILTER ABOVE THRESHOLD THE FILTER WILL GROW BY INCREMENT PIXELS TO A LIMIT OF LENGTH BY HEIGHT IN SIZE MAXIMUM SIZE IS SPECIFIED BY THE KEYIN PARAMETERS LENGTH amp HEIGHT 1 PIXEL VALUES BELOW THRESHOLD ARE NOT INCLUDED IN THE MOVING AVERAGES 2 A THRESHOLD SET TOO HIGH MAY CAUSE VERTICAL BLEEDING BLEEDBLOOM A CONSTANT SET TO CONTROL BLEEDING FROM A THRESHOLD OR BLOOMING AT BRIGHT LIMBS THE NOMINAL VALUE SHOULD BE IN THE RANGE 5 10 DEFAULT 5 TOO SMALL AN INTEGER GIVES SEVERE CONTOURING AND MINIMIZES THE VERTICAL FILTERING EFFECT WHILE TOO LARGE AN INTEG
94. EYWORDS MANDATORY BANDS CUTOFF BANDWIDTH UNIT REMARKS BANDS area rea2 areaN Single Banded rea s to regroup Areai will be BAND1 of outarea areaz will be BAND2 outarea etc Percent of data to CUTOFF in 2 BYTE to 1 Byte compression DEFAULT 1 0 of data at upper and lower ends output range for 2 BYTE raw data from 2 to 255 DEFAULT 255 BRIT or RAW input data type DATA BRIT RAW DEFAULT RAW Combine several singel banded areas into a single multibanded area APPENDIX 1 13 COMP General data compression utility for eXplorer area data which allows a choice between several lossless and lossy compression methods The metadata i e the data directory and the DDB are NOT compressed at all only the image data The output is a compressed file with a different name than the area name DECOMP command will reverse the process exactly and in place if the compression method used was lossless else the best rendition if the method applied was lossy COMP area_to_compress KEYWORDS KEYWORDS CMP compression_algorithm LZW DCT HUF ARI default LZW QUAL quality_factor forthe DCT compressor1 50 default 3 ORDER order_of_compressor for Arithmetic compessor 1 2 or 3 default 2 OPT option to output information on the various files used during compression OPT STAT displays the information Compression routines presently coded DISCRETE COSINE TRNSFORM DCT Lossy ADAPTIVE HUF
95. FMAN HUF Lossless ARITHMETIC ARI Lossless Lempel Ziv Welch LZW Lossless REMARKS This is one way of increasing the disk space used in the data directory APPENDIX 14 DBL Query an eXplorer database file MDB extension created using DBI to list specified fieldnames or KEYS DBL database_filename KEYS sort Parameters database_filename database file MDB to list data from KEYS list of database KEYS to list values for To print list of the KEYS or fieldnames use DBU LIST KEYS data_base_file_name sort list of sort conditions REMARKS To facilitate a quick search of the contents of a CD ROM or mission specific data the respective CD ROM index for each volume or each data type can be imported into a database file within MciDAS eXplorer using the fieldnames provided in the index This is a poor man s version of a more sophistacated database but servers the desired purpose quickly APPENDIX 15 DBU Database utility program to query the fieldnames or keys constituting a database in the MDB file format DBU option database_filename PARAMETERS option LIST to list the database file configuration information KEYS to list the list of valid fieldnames for the specified database file REMARKS See also DBL Examples DBU LIST voyager1 mab to list information about the Voyager 1 index file APPENDIX 16 DEC OMP To decompress a file compressed using COMP The routine will apply the
96. ICTION TO ONE PERIOD OF VENUS AXIAL REVOLUTION 1 VENUS DAY BUT THE USER MAY INPUT THE ELEMENTS FOR A DIFFERENT ORBIT MGNORB KEYWORDS THE PROGRAM DEFAULT IS TO USE THE MOUSE TO SELECT A POINT ON THE IMAGE KEYWORDS OPT scan_option ALTIM _EFT RIGHT determines which scan path to test for the given site ALTIM is the nadir pointing sensor for altitude LEFT is the left looking SAR RIGHT is the right looking SAR EXAMPLE MGNORB OPT RIGHT asks for a prediction when the right pointing SAR will scan a location selected with the mouse default ALTIM When the ALTIM mode is used a field of view ellipse will be projected on the surface centered on the nadir location closest to the site of interest LOC lat lon degs direct input of location EXAMPLE MGNORB LOC 15 22 asks for a nadir predication at 15 deg latitude 22 deg longitude A semimajor_axis_of_orbit ECC eccentricity_of_the_orbit INC inclination degs NODES longitude_of_nodes degs ARGPER argument_of_the_periapsis deg NUMORB mission orbit number corresponding to the orbital elements PERIAP periapsis_time_J2000 not functional at this time AS STATED THE REFERENCE DEFAULT ORBIT IS 2667 APPENDIX 69 MINFIT MINFIT Determine Minnaert scattering Coefficients lo and amp for a navigated image lo pyB area_ LIN ELE SAMP KEYWORDS AREA LIN ELE SAMP LAT LON COLOR MUMU IMU REMARKS Navigated McIDAS AR
97. IGATION OF IMAGES OF PLANETARY RINGS Navigation of planetary rings for Saturn Uranus Neptune has not been implemented NAVIGATION OF IMAGES OF ASTEROIDS amp IRREGULAR MOONS The smaller moons of the outer planets e g Phobos and Deimos Amalthea 1989N12 and asteroids such as Gaspra and Ida are irregularly shaped Triaxial ellipsoid models are available for many of these irregular objects eXplorer however does not currently have the ability to implement the shape model based navigation of these objects How TO UPDATE SPICE KERNEL NAVIGATION OF PLANETARY IMAGES The SPICE kernel navigation provides the C matrix that transforms image co ordinates to the native coordinate system of the target Occasionally there may be a need to update these kernels if the navigation is deemed to require a change either in the planet center orientation or size Prior to updating the existing SPICE kernel the revised planet center in the image and the orientation of the planet in the image and any change in the size and shape used for the target object must be obtained The image center can be obtained using the bright 4 12 limb if available or using features with known coordinates either from simultaneous wide angle images or preceding or succeeding navigated images A common problem with planetary image navigation is noticeable error in the north angle which results in a slight tilt of the navigation grid with respect to the true reference frame S
98. INES Number of lines in this digital area NELES Number of elements in each line ELESIZ Number of bytes element 1 2 or 4 area file LINERES Line Resolution spacing in image lines between consecutive area lines ELERES Element Resolution spacing in image elements between consecutive area elements NCHANS Maximum number of bands line of area PRESIZ Length of line prefix in bytes Indicated by the sum of words 49 50 51 4 if validity code is present see 36 PROJ McIDAS user project number under which the area was created CREATION DATE Area creation day in YYDDD format CREATION TIME Area creation time in HHMMSS format FILTER MAP for Multi Channel Images a 32 bit vector If a bit 1 there are data for that band in the 5 5 e _ area The rightmost bit is for band 1 20 FDS COUNT Spacecraft clock ticks since last computer reset 21 24 Internal use only 25 32 Memo 32 ASCII characters available for comments 33 Number of area containing this directory 34 Byte offset to the start of the image data within the area file 35 Byte offset to the start of the navigation block within the 36 Validity Code If these bytes are non zero they represent a code which must match the first 4 bytes of the line prefix If the code and prefix bytes are not equal the line does not contain valid data and must be ignored 37 44 PDL Exists if the image was made in GOES mode AA or AAA packed
99. LAREV POLEN POPVAL QA REDISP REDONAV RENAVF RESEAU RESREM RF SCANA SCANE SCANG Flip the longitude convention for the navigation created using PLANAV This is required for earth views because of the McIDAS longitude system convention which is opposite to the general planetary longitude convention Refine the C matrix for a Voyager image by using a known star which can be located in the image Will also optionally determine the pole position for Neptune List the digital data at the cursor location continuously in a separate window Quit an area Releases up the disk space occupied by the area This is a core key in and does not delete any area associated files e g LIMBnnnn Re display a displayed frame from the original given area at the cursor co ordinates on the same or another frame using an integer blow up or blow down factor Similar to BU on the McIDAS MVS system Update the target observer ephemeris and the image center information Use this command if the time of image acquisition is changed The ephemeris is computed using NAIF P kernels Use RENAVF if only the center is to be updated Update navigation for a planetary image usually an earth based telescopic that has PLAN type navigation that requires updating the center Lists and or plots reseau data for Voyager spacecraft Remove the reseau marks in Voyager images by interpolation of brightness from their immediate neighborhood Dete
100. MESO etc S C EME Central Body EME Central Body EME S C EME S C EME COMMENTS Central Central EMESO Central Central Central MEXP VO Flexible Image Transport System 359 Computed North Angle 360 377 Computed Transform Matrix Inst gt PicBod 378 395 Computed Transform Matrix Inst gt Planet 396 413 Computed Transform Matrix Inst gt EME 414 431 Computed Transform Matrix PicBod EED gt EME 432 433 Computed Optic Axis RA 434 435 Computed Optic Axis Decl 436 Minnaert Fit Constant Max DN Used 437 Minnaert Fit Constant Calc Slope 438 Minnaert Fit Constant Calc Intercept 439 Minnaert Fit Constant Mean Abs Dev 440 PicBod Center Line 441 PicBod Center Element 442 Pixel Size on PicBod Surface 443 RMS PicBod Radius Error for Navigation 444 Sun Phase Angle at OptAxis Sfc Intersect 449 Best Fit Equatorial Radius of PicBod 446 Best Fit Polar Radius of PicBod 447 448 Image Navigation Processing Status 449 460 Spare WORD ITEM Supplementary Information 461 462 Supplementary Block Type 463 465 Data Source CD ROM Volume tape name 465 512 Satellite amp Shadow Positions Star Locations Rings 5 26 R 8 R 8 R 8 RO R 8 R 8 R 8 I 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 c 8 TYPE COMMENTS Ces SUPL VO GLZ 5 5 CALIBRATION Calibration is the process of converting the raw data stored in the eXplorer area into meaningful physical units Calibration data are specific to th
101. MIDR CD ROM into consecutive areas 3 11 FINDALT FINDALT searches the ARCDR index to locate a particular CD ROM volume on which the altimetry and radiometry data corresponding to a given orbit is stored The Magellan orbit number corresponding to a specific location on Venus is most readily determined by scanning the audit trail of an area containing a Magellan radar image F or any C MIDR by using the LA area FORM AUDIT command GETALT GETALT will retrieve the radiometry and altimetry data for that orbit and plot it on the screen over a displayed image of that region assuming the proper ARCDR volume has been mounted in the CD ROM reader ARCDR data are organized by orbit numbers MGNORB can be used to guess the orbit number for either a nadir look altimeter or the side look radar for a given location on Venus indicated by the cursor location in a displayed MIDR image COV Pee SEttetn 1 CFP TAER yer C332 Cy wa 3 12 Figure 3 6 An example of Magellan altimetry data retrieved from ARCDR s and displayed on a composite of the Ovda region created by remapping several F MIDR images The spacecraft orbit track is shown by the sign passing roughly north south while the radius at each footprint is shown as a horizontal barb MGNORB key in will retrieve a very good guess for the orbit number and display the radar and altimeter footprint for a given Venus location 3 4 GALILEO SSI IMAGES OF VENUS Galileo SSI images of Venu
102. McIDAS eXplorer The following data are planned to be fully supported for analysis in terms of navigation and data calibration In addition to the following earth based telescopic images of solar system targets can also be readily imported and analyzed using McIDAS eXplorer if the data are available in a standard format such as FITS or TIFF Earth and Moon Data from all US civilian meteorological satellites GOES POES as well as METEOSAT and GMS European and Japanese geosynchronous satellites Galileo Orbiter SSI images during Earth and Earth 2 encounters in December 1991 and December 1992 Venus Magellan Mosaicked Image Data C and F MIDR s on PDS CDs MIDRCD 01 MIDRCD 120 and Altitude and Radiometry Data CDs on Volumes ARCDRCD 001 through ARCDRCD 015 and Composite Global topography and Radiometry Data GxDR_ 3002 Pioneer Venus Orbiter Cloud Photopolarimeter OCPP images Pioneer Venus OCPP Polarimetry Maps from NSSDC archive tapes Galileo SSI images of Venus GO_0002 Mars Mapped Image Data Model USGS MDIMS volume 1 6 Viking Orbiter Images PDS Volumes VO_1001 through VO_ 1006 Jupiter and Satellites Voyager 1 and 2 images on EDR tapes and PDS CD ROM Volumes 6 8 and Volumes 13 25 Volume 17 is the last one published so far more are forthcoming Hubble Space Telescope images of Jupiter Earth based telescopic images of planets with FITS headers Saturn and Satellites Voyager and 2 images on EDR tapes and PDS C
103. OES ERBE 5 8 GOES 4 GOES 4 GOES 5 GOES 5 GOES 6 GOES 6 GOES 7 GOES 7 IR IR IR IR TIROS N NOAA 6 NOAA 7 NOAA 8 NOAA 9 MARINER 10 VOYAGER1 VOYAGER2 GALILEO ORB HUBBLE ST METEOSAT3 METEOSAT4 METEOSATS NOAA 10 NOAA 11 NOAA 12 NOAA 13 NOAA 14 GVAR GVAR SNDR GOES J GOES J GOES K GOES K GOES L GOES L GOES M GOES M ERBE Defense Dept Weather 87 DMSP F8 88 DMSP F9 89 DMSP F10 90 DMSP F11 91 DMSP F12 92 93 94 99 EY 1B 26 FY 1C 97 FY 1D 98 Codes have also been assigned for the following barycenters Solar system barycenter Mercury 9 Venus Earth m Mars Jupiter Saturn Uranus Neptune Pluto b Sun Ow 0 Jana L K KA LA The code for a satellite is normally computed by adding its LAU designation to 100 times the code for its barycenter A planet is always considered to be the 99th satellite of its own barycenter For a visible target body surface one would simply use the NAIF ID number 99 999 For planets with atmospheres we have adopted a McIDAS eXplorer protocol which requires the target body to be identified by its NAIF ID number times 10 a four digit number NNNO which is fed to a target body constants subroutine BODCON and produces three nominal atmospheric radii defined at the 1 bar level along with other IAU constants For rotating planets two or more of those radii will of course be equal One can add the digits 1 9 to this number NNN1 NNN9 to obtain spectral o
104. PLOT L 1 I e Bir o E y y H pa f EJ AE ON 0ND2 PIONEER ORB 16 FEB 82047 1827955 00001 OMAI Ton VE T Figure 3 4 Plot generated by MINFIT command depicting the linear and robust fit to the brightness data The Minnaert coefficients are stored in the DDB for the area which can be used by NRMIMG to remove the photometric shading Pioneer Venus OCPP images are normally available from NSSDC on 9 track tapes The individual files containing the images can be imported into a McIDAS eXplorer workstation via any available means local tape drive or over a network Unlike majority of the images acquired by NASA s solar system missions the OCPP images were obtained using the spin scan technique pioneered by the geosynchronous earth weather satellites and also used on Pioneer 10 and 11 spacecraft to reconnoiter Jupiter and Saturn in the 1970 s In the case of the OCPP images the spin of the spacecraft provides a swath across the disk of Venus and the orbital motion of the spacecraft translates the successive scans across the disk of Venus The CPP telescope optic axis is in a plane containing the spin axis of the Orbiter spacecraft and can be pointed between 45 and 135 with the spin axis The spacecraft spin axis nominally points towards the celestial south pole At the beginning of acquisition of a full disk image the Telescope is pointed towards the farther cusp of Venus and held there such that the orbital er h E motion will
105. POSITE IMAGE If McIDAS eXplorer is being run on a workstation with a 24 bit video capability then it is possible to display multispectral data as three color composites as opposed to using false colors In order to be able to display three color composites the mcidas session needs to be started with the bit plane option set to 24 mcidas bp 24 ig y n fr 1 n imsiz lin ele where the braces indicate optional specifications for initial and maximum number of frames allowed frame size for the initial frames allocated and whether graphics are to be embedded in the image or shown as an overlay Since each frame in the 3 color mode requires three times the memory the number of frames to be allocated should be limited so as not to exceed a reasonable fraction of the physical memory installed in the workstation Typically in a workstation with 32 mb of real memory installed four 1000 x 1000 frames will required about 12 Mb of memory and twice that if the double buffered display mode is being used If all three bands to be superposed coexist in a multibanded area then entering a single command a variation of the DF command will enable a three color composite to be displayed on the chosen frame number DFC area_ frame_ Red band_ Green band_ Blue band_ or if the three bands are in three different areas then DF3 red_area frame_ COLOR R DF3 grn_area frame_ COLOR G DF3 blu_area frame_ COLOR B where red_area grn_
106. R2U VGRNXXX TARGET JUPITER SATURN URANUS NEPTUNE TITAN_CLOUDS TITAN_SFC other moons Voyager1 Voyager 2 CAMERA NAIF_ID Wide 31002 32002 Narrow 31001 32001 Note that if the frame is not reloaded the new navigation parameters will not be available for the displayed frame Always reload a frame after navigation is completed for an area before running the MAP or PC keyins or using the E key APPENDIX 91 SEDRRD SEDRRD Load Voyager SEDR tape file records into LW file sedrfile_name LWFILE PLANET HEAD NO NO HEADER FDS beginning_fds ending_fds KEYWORDS INPUT LWFILE PLANET HEAD FDS COUNT DEBUG Remarks SEDR FILE NAME MCIDAS LW FILE NAME FOR INDEX amp DATA NEPTUNE or OTHER OTHER IS DEFAULT Neptune SEDR has a larger record size than others YES NO INDICATES PRESENCE OF HEADER RECORD IN FILE YES IS DEFAULT RANGE OF FDS COUNTS TO ENTER INTO LW FILE omit period DEFAULT IS ALL RECORDS IN TAPE FILE RANGE OF RECORDS TO ENTER INTO LW FILE DEFAULT IS ALL RECORDS IN TAPE FILE YES Display INT HEX and ASCII listing of each record This command creates an indexed LW file from the SEDR tape records As there is no on line 9 track tape drive available on the system it is assumed that SEDR file is copied onto disk first The command actually accesses this file to create the LW file The purpose of this command is to provide access to all of the SEDR words which vary depe
107. RDS ADD point add a point 1 30 DELETE point delete a point 1 30 LIN begend line bounds default beg 50 end last line 50 ELE begend element bounds def beg 50 end last ele 50 NUM n number of limb points to find default 15 maximum is 30 higher numbers interpreted as area id BLOB mindn minimum dn bound for brightness center maxdn maximum dn bound for brightness center Iskip line skip increment for sampling dn s def 5 leskip element increment for sampling dn s def 5 BOX YES finds NUM limb points within cursor defined box bounds Follow the program s instructions to define box size amp location This option is useful to exclude triggering on large gradients near reseaus terminators shadows GRAD threshold local dn gradient threshold defining the bright limb default 50 for 2 byte pixels 10 for single byte pixels APPENDIX I 78 REMARKS This command adds limb points to the older PLAN navigation block for the purpose of finding the image center by the use of constrained fits for objects of known shape and size For constrained fits such as these a small number of points is frequently sufficient lt has been modified recently to also create a limb point file LIMBnnnn in the same format as the other limb point finding programs LIMBPT EDGES BRTCEN EXAMPLES To add limb points for image navigation PLAEDG PLAEDG NUM 25 PLAEDG BOX YES PLAEDG BLOB 20 180 PLAEDG 6465
108. ROM AREA 23 FF 0 DIRECTORY gtdr merc TILES 2 23 TYPE GTDR PROJ MERC FF 0 TILES 5 AREA 24 FF CUR directory is not needed AREA 1211 FF 23 DIREC TORY gedr north no leading cdrom is required AREA 20 cdrom gtdr error f23 FF is not used APPENDIX 39 GETMDIM Import Mars Explorer USGS Processed Viking Mars Data images from CD ROM into McIDAS areas GETMDIM area file_name PARAMETERS area Area number into which to load the image from the CD ROM disk file_name A valid file name containing the image OPTIONAL Name must begin with and be the last entry on input line NOTE If full path is given CDPATH in string table must be The string table can be listed using the TL command and entries in the table can be updated using the TE command KEYWORDS AREA A valid McIDAS area number 1 9999 REQUIRED def 0 REMARKS This command is used to import USGS processed Viking Orbiter images of Mars from PDS CD ROM s APPENDIX 40 GETMGN Import a Magellan Mosaic Image Data Record MIDR rr age from CD ROM into a McIDAS area GETMGN area framelet ff directory file_name PARAMETERS area area number to import the data into framelet or ff_ frame number of the MIDR image to import 1 56 directory name of the sub directory containing the data file file_name Any valid source file name OPTIONAL Must begin with and be the last entry on input line NOTE If full path is give
109. SAR and topography data have a set of commands that are not useful to any other data Such mission specific commands are described in Section 4 The commands available to import planetary image data currently are described in Section 4 in detail These commands are supplemented by the core McIDAS commands to manipulate the image and other data The core McIDAS commands are described in a separate volume which is available upon obtaining the basic McIDAS license from UW Madison SSEC 2 11 IMPORTING DATA into McIDAS eXplorer Most of the planetary data analysis takes place from archived data as opposed to real time data which is more typical with earth meteorological satellite environments The most common format now for the archived planetary data is the CD ROM Appendix contains a list of the data available through PDS in this format One notable exception is the HST WF PC data which are so far available only on 9 track or Exabyte tapes usually in FITS format There is another medium or format of data input output from Digital Audio Tape DAT cartridges available from within McIDAS X If a DAT drive is available on the system then McIDAS areas can be saved as individual files on these cartridges and restored later This is a fairly attractive method for short long term archiving of processed data as these cartridges can hold up to 8 Gbytes compressed of data Thus as the McIDAS work space gets full the image areas can be stored and restor
110. The trouble with the EB command therefore is that it enhances the DN values of the pixels already in the BRIT screen buffer when they are mapped to the CRT screen and when the two byte brightness resolution is already lost We would like some way of putting a limited larger or smaller segment of the image s dynamic range into that screen buffer before we apply EB enhancement The MAKESU command permits this by utilizing the SU command of McIDAS in a sophisticated way The SU command is designed to generate a table of 1 60 breakpoints describing a transfer function of contiguous line segments This transfer function is stored in a file mcidas data ST under whatever stretch table name one cares to assign When the DF command loads an image to the display screen with the SU keyword set to the appropriate stretch table name that lookup table is applied to transform the image data on disk to the output data in the screen buffer and on the screen independent of how EB is applied The D key keyin will show the effect of such a stretch table by converting the BRIT screen pixel values BRIT is a linear mapping of 32K to 0 and 32K to 255 to MODB pixels which are the stretch table output It is the MODB DN values which then are placed into the screen buffer instead of the BRIT values Note that the stretch table must correspond to the McIDAS area calibration type and band number or it will not be used by DF Those values are normally correctl
111. To edit limb points PLAEDG L PLAEDG 5 PLAEDG ADD 5 PLAEDG DELETE 3 PLAEDG 3 PLAEDG 30 PLAEDG 5 LIN 230 PLAEDG 200 3 tries to find 15 limb points distributed throughout the lines of the displayed frame tries to find 25 limb points in the frame tries to find 15 limb points within a box tries to find 15 limb points between the bounds of brightness contours 20 and 180 DN tries to find 15 limb points for area 6465 lists all points in navigation block add or replace point 5 within the cursor add or replace point 5 within the cursor remove point 3 in the displayed frame remove point 3 in the displayed frame remove any normally non existent point to see the plotted points amp trial fit once again point 5 added as found on line 230 add point 3 within the cursor to area 200 PLAEDG AREA 22 DELETE 3 remove point 3 from area 22 APPENDIX 79 PLANAV Generate a new area for a perspective view of an image and attach navigation so that a given area can be remapped into it using REMAP command area Planet angle VIEWPOINT DIRECTORY REPLACE NAV Keywords AREA AREA Area to define navigation for required LINES line dimension if a new square area is to be created Default is LINES 1000 a 1000 x 1000 pixel area PLANET Name ID of a solar system object either the NAIF ID number or name is required RADIUS amp ECC will default correctly if the value of PLANET is spec
112. U LOGSE V T ILL 167 140 LILA verter 22 9278 E STE Agate ot chp EE JAS he Eea a L Bark train i Perhot te adhiak Lohsutis KIL KDG of NLA Z 20 709 L Gitatuado Jroa aiya CELL AL rta pnl PLL UY E jwn does Sages able ES whe OOK ST SSS SEAT RANA AD x P 8 Xd Ate be mon eS pet we we TaN Se an ee a th ap M Oe a N Ne Le Be wX we wae st E Picture funiy Phas Tent cal any Pawe Flori Pemtrat Edy zarn Code hs Ubetiunse Pory Now i Uant 1 EZ PLT 0 L NW ELIF soc 2500 gt pierin KY Ran LOL coria ches 3 l 100 Suk RR pictura AxEJ E ifion KOS o BRIG Ot Horna Pretoria fake Mead Rathun Rand i 572 NU E bla Pirtoro txly Corres ida Chop etzi un E S Yop DOGS enn Lane lr yg Bik sp XI9joction T T T by Bork Kiojr EL WY E Late oid laii co l C 021 HT Soati CTT i i d S BRN Debt e t are E Ben DL Of 540 H LY l CA Babs Fromm at Bank izt dao LRA 140 Extipalio wit theca at CFT Kyia Ache 9 DE ESLI hong T Mi of KIC spin Kee 1 A TE MXSLOaLZ GX son Mario pirig Tron File 1 23N E CBR Levitation of Spln Porno REEL SAS CU A E E 147 3 5 tasien land dam L HT E Dira kenak wolo 62 6435 E E RoS Aspis Cah amp 1 D H 41 Reji pern QAP gnt Tire do see lt E OO Rojal angle tudo 2 P s i E lt odc 2 Comtat Tito Lam 310 5 AR c 7 Mist Arale Soto 3 N x a PS H Trem A l 34 E O L E v META Woda first OF jast wat 2 HEH T T T Rois Contact Bui 0000 HPQ AN guia
113. U SAVE table_name and can be removed by EU and restored back on that frame by EU REST table_name A saved enhancement table can be restored either for a looped sequence of frames or any other range of frame numbers with the EU command if desired The enhancement table may or may not be suitable for the data displayed on those frames The enhancement tables for each frame can be different even when the frames are being animated in a loop EU LIST will list all the names of the enhancements saved on a given workstation and can be recognized by the ET extension to the individual file names False Color Enhancement False color enhancements are handled in a manner similar to the black and white enhancement except that instead of EB the command EU is used with the MAKE option to specify the output brightness range in red green and blue for a specified input brightness number This is the same as input image data number for one byte data or the output of the calibration table for two byte data The calibration or conversion from two byte data to a display brightness level always a 1 byte value can be changed with the SU command The syntax of the command for false color enhancement is as follows EU MAKE low input high_input low_red hi_red low_green hi_green low_blue hi_blue Note that this format allows the user to arbitrarily assign an output color combination to any of the input 256 brightness levels If a saw tooth or other multipl
114. VGR Voyager l and 2 Missions to the outer planets MGN Magellan Radar Mission to Venus GXDR Magellan Global Data Products GO Galileo Orbiter SSI Images of the Earth Moon and Venus GONIMS Galileo NIMS Observations future FITS Hubble Space Telescope and other ground based images in FITS format VO Viking and 2 Orbiter Missions to Mars MDIM Mars Digital Image Model Data derived from Viking Observations CLEM Clementine Image products future These CD ROM readers allow the user to import the corresponding data directly to the new McIDAS eXp area format with a DDB so that the eXplorer tools can be utilized Images can also be imported or input directly to McIDAS X from tapes such as Mariner 10 or Voyager EDRs and VICAR tapes Such images would have to be reformatted using Unix or OS 2 versions which as of yet do not exist of the mainframe McIDAS MVS background programs PBNEWEDR and PBVICAR2 Those programs may be rewritten for McIDAS eXp if a need arises to read tapes at the workstation level but the current trend is toward acquiring data either remotely via TCP IP and FTP in standard PDS formats or locally from CD ROM The new planetary area format is documented below The format is fully backward compatible with all existing McIDAS workstation software so the areas may be freely moved from one McIDAS workstation environment to another via FTP from Silicon Graphics to Sun to PC to RS6000 and can be used wherever a copy
115. YTE UNSIGNED RANGE RATIO REMARKS HIST North Angle optional defaults to angle from a conic fit used to adjust if conic fit is bad HEADER means use north angle from FITS header instead of user input value or conic fit Line amp element sampling interval for computing brightness center of target default lines 100 elements 100 12to 12 Positive Zones West of Greenwich Used to adjust local time in FITS header to UT Times in area directory and DDB are always in UT and TIMEZONE defaults to 0 assuming UT in FITS header if no time correction is specified YES Data is from a VAX so must flip bytes Do not flip the bytes default YES Input data is 2 byte unsigned integer format NO Signed 2 byte unsigned 1 byte defaults User may have to experiment with some data depending on how it is offset relative to zero lo hi Dynamic range of displayed data Often the DATAMIN amp DATAMAX in the ile header include background and spurious bad pixeis aS Can be seen in the image histogram This is the range of true useful data you want displayed on the screen by the DF command A default range is set at 5 and 98 cutoffs User can choose more precise limits by looking at the histogram and setting lo and hi These limits are disregarded during DF for 1 byte areas Use MAKESU instead HEIGHT to WIDTH ratio for non square pixels for the NAIFNAV and NAVUTIL keyins this keyword is inversely defined as
116. a 2 if the path is included in the FILE NAME field or 3 if the normally used FDS keyword option is chosen A PATH IS REQUIRED EVEN IF IT IS A BLANK FIELD ANY VALID SOURCE FILE NAME OPTIONAL if FDS is given Must begin with and be the last entry on input line a path may be included in FILE NAME if CDPATH is blank mmmmm mm anann nn A single FDS or a range of numbers A range specified will generate up to 50 areas consecutively starting with AREA unless AREA 0 name NAME Must be specified when FDS numbers are used TARGET is always converted to lower case internally GREEN BLUE ORANGE CLEAR VIOLET UV CH4_JS 5410A CH4_U 6180A WIDE or NARROW ANY VALID MciIDAS AREA NUMBER 1 9999 default 0 AREA 0 will allow a CD ROM search with no ingestion of data into McIDAS X Caution Searching through literally thousands of FDS numbers on a CD ROM is time consuming Choose FDS limits as narrow as possible to reduce waiting time Use the command and the pid command to kill errant searches GETVGR FDS 43975 00 43985 00 TARGET SATURN FILTER BLUE AREA 0 GETVGR FDS 43885 65 TARGET MIMAS AREA NNN APPENDIX i 44 GETVO KEYWORDS FILE NAME AREA REMARKS Import a Viking 1 or 2 Orbiter image from PDS CD ROM volumes into a McIDAS eXplorer area area_ filename to import a file or LIST filename to list the header for a specified image file ANY VALID SOURCE FILE NAME Must begin wi
117. a vad FHA 1 1 4 L XS d 7 tore U SELLE EEL TTT TTT TTT t Than pr sa RIGHT mouse button to select final point oh Press BOTH mouse buttons to end option DIETANCE OF SECHMENT km 33 89379803 MUMBER OF PIXELS RETURMED 1 3 BECNENT_ POE 0106 0070 To TA 0197 a DORE SE E AS e S e E E av d Fonts use has been turned ot E L 4 D CS T RECIN TV LOAD PROCTESTEG ron reve iti Processing completed for frama 1 cand y L CNT TT ONTT BRIT CAEr l a aE gt Press the MIDOLE mouse button to select initial point for opt tos EE HE i Then press RIGHT mouse button to select final potat ETA Press BOTH mouse buttons to end option E A 4 DISTANCE OF REONT hm 67 70345306 E MUMBER OF PIEELS 2 RETURNED 2 SUCIA PLOT 0334 0365 To 0173 0564 CAHCT Pai e GL eke uP OR xv N tot G CI TTT T TTT T TT TTT TTT TT TTT TTT T TTT A ages Magetan Mane ler imanes Cte nt are ar eel sare a worn od OO OS L AA D gO ROS PRE REC RR ER LLLE Tr LL Ps Fo LT i s y Monear Vana TT e UR N s 4 6 9a fs Currently McIDAS eXplorer is able to import process and analyze planetary images from PDS CD ROM volumes as well as images from most routinely available weather satellite images and Earth based telescopic images in the Flexible Image Transport System FITS format These include Voyager images of the giant planets and their satellites and Magellan SAR i
118. a perturbations on the Oort cloud In extreme cases star passages through the Oon cloud or encounters with GMC s can cause showers of 10 or more comets to enter the planetary system Hills J G Astron J 86 1730 1981 In order to correctly estimate the population of comets in the Oort cloud it is necessary to know whether or not the solar System is currently experiencing an enhanced cometary flux In addition cometary showers have been invoked to try and explain the enbanced cratering rate currently estimated for the Earth over the past 250 Myr which is about twice that estimated for the Moon over the past 3 Gyr Using computer based dynamical simulation models it is shown that the current distributions of long period comet orbital elements are inconsistent with a cometary shower Two different dynamical tests are empioyed First it is shown that the predicted orbit element distributions from a cometary shower are highly non random in contrast with the random distributions of the long period comets Second the 1 a distribution for the long period comets shows no evidence of a perturbation of the inner Oort cloud as would be expected for a major cometary shower Taken together these two tests allow one to set an upper limit on the magnitude of any recent major perturbations on the Oort cloud This work was INTRODUCTION This is the final report for work performed for the development of McIDAS eXplorer a version of McIDAS for
119. a or all valid areas within a range of numbers MA Modify an area MA digitally modifies the contents of an area Options include one dimensional along the scan direction low pass and high pass filters shot noise removal and histogram equalization QA Quit an area QA deletes an area from the mcidas data directory i e deletes the file AREAxxxx where xxxx is the area number to be deleted Upon quitting an area the space occupied by the area is immediately available for use NOTE The area cannot be un deleted once it is quit XPORT Copy the image contained in an area into a pseudo FTTS format file an attach an ASCII header describing the image WHERE Lists frame area limb points file contents Where lists target and mission specific details of the images in areas or displays them on a frame WHERE also lists the image indentifiers if a limb points file exists for a given area BAND Some instruments acquire image data in more than one spectral wavelength Except for interferometers and specrtrometers this number is usually small for instruments that use spectral filters the GOES VISSR has 12 spectral channels These spectral channels are sometimes referred to as bands Since areas can contain multibanded images some McIDAS commands that operate on a single channel require that the band number be specified Calibration The digital data corresponding to an image is generally stored in McIDAS areas in raw counts as returne
120. age area the navigation transform can be completed by attaching the ephemeris data to it For earth based images this essentially means that the location of the sub earth and the sub solar point on the target object and the distance to the sun and the earth be known to the navigation utility programs These quantities are computed using the NAIF SPICE library routines for the observation date and time attached to the image and stored in words 5 amp 6 of the image area directory For spacecraft images it is the spacecraft target geometry at the time of the image acquisition that is required and this information is usually provided as part of the mission s data For the new missions such as Galileo this data can be found in the PDS label on the CD ROM volume itself For the older images the SEDR data are found in SEDR files also provided by the flight project For the Voyager images all Uranus and Neptune images and a limited number of images of Jupiter and Saturn and their moons the pointing information is available as SPICE kernels For these images the IMGNAV command is not needed because other commands read the SEDR or SPICE kernels and provide the required information to the navigation programs within McIDAS eXplorer LODSSP For animation or other purposes it is desired to display a registered sequence of images in a loop For most imaging systems the pointing of the camera is such that the target image is seldom at precisely the location i
121. ally they are the instrument coordinates which usually are the same as image coordinates or there is a One to one relationship between them area coordinates which locate the data in a McIDAS area Earth or planetary coordinates which locate data in the target object s native coordinate system of latitudes and longitudes the display frame or TV coordinates which tell about where the data are displayed in the frame and finally window coordinates which locate a frame within the X window McIDAS generally does not do anything with the window coordinates and the display MUST be left with the default settings If not the mapping of the frame coordinates to planetary or area coordinates will not be correct Area Line and element units These are the same as the image coordinates if the data are not sub sampled or oversampled replicated in line or element direction Celestial Coordinates Used for stellar and planetary positions in the sky as Right Ascesion given in hours minutes and seconds and Declination given in degrees NAVUTIL command can be used to change between palnetary and celestial coordinate systems Glossary 5 Cursor Data Earth Latitude and longitude Only in the case of the Earth is the latitude system geographic rather than geocentric FRAME or TV Display line and element coordinates Image Original image line and element coordinates that have a unique relationship to the acquiring instrument s
122. an image is brought into view by displaying a new image on a particular frame The cursor coordinates and the calibrated data value are also displayed so that this process accomplishes simultaneously the same purpose as the E and the D key commands together The D key will list the raw calibrated and brightness values corresponding to the image location identified by the cursor position in a displayed image The digital area must be present The listing includes the image frame and target object s native reference frame coordinates of the cursor OD When the digital data for more than a single pixel need to be examined the OD command can be used to list the data within the cursor positioned on a displayed image in specified units BRIT RAW or calibrated As with the D key the digital data source area from which the frame was loaded must be present and unchanged LINPLT 4 16 LINPLT allows the data along a path between any two arbitrary points in the displayed image to be extracted and plotted on the displayed frame as a line plot of distance vs data value The data is plot in the respective physical units except if the image displayed is a Magellan MIDR product image For Magellan MIDR data the raw DN S are shown unless the unit is specified explicitly UNIT DB when the command is entered The reason for this exception is that the calibration of MIDR data from raw DN to calibrated radar brightness is somewhat time c
123. area and blu_area refer to the area numbers in which the data to be displayed in red green and blue color exist respectively In both the cases the syntax is identical to that of the DF command with the addition of the COLOR keyword _ Since most scientific data are not acquired through the red green and blue filters the appearance of the image data will not be in natural colors and the combination of different spectral bands among those available for the data and color in which they are displayed will usually require some experimentation For data from the AVHRR instrument on NOAA polar satellites the combination of bands 1 0 5 micron 2 0 9 micron and 4 10 7 micron displayed through red green and blue channels usually gives a pleasant looking image assuming the infrared data are shown inverted such that cold clouds low radiance values appear white and the warmer land ocean areas are dark In most cases the appearance of the image may require enhancement by using either histogram equalization in all bands or other methods The histogram equalization can be performed using the MA command on each of the bands separately Unfortunately MA can process only one band at a time thus three different output areas are produced if three bands are processed one at atime These three output areas can then be combined into a single area using the COMBIN command If this is to be done repetitively the commands can be collapsed into a single
124. arget object ephemeris using NAIF supplied P kernels PLAN Navigation Type This navigation type is provided for backward compatibility with McIDAS and is redundant It is however used in the general perspective view navigation Initially developed for Mariner 10 images of Venus it was adapted for use with the Voyager images of the outer solar system and as such used the SEDR data exclusively For synthesizing views in a general perspective projection from known data the viewing distance the relative location of the viewpoint target frame latitude and longitude the orientation of the image North Angle and the look angle view angle with respect to the vector from the viewpoint to the target object center can be specified to establish the transform RADC Navigation Type RADC navigation type enables the sky coordinates to be determined if the camera pointing is known This is useful in optical navigation of some images where the need to determine the right ascension and declination of a point in the image arises e g in locating a new target such as a planetary moon against a field of reference stars For Voyager Galileo and some ground based images the optic axis pointing information is picked up from the image headers and stored in the DDB attached to the area HOW TO NAVIGATE VOYAGER ISS IMAGES OF GIANT PLANETS AND SATELLITES WITHOUT SPICE KERNELS Voyager images of the giant planets and their satellites were among the first planetar
125. at encountered are recognized by the command Minor deviations of the keywords contained in the label can be accounted for by the FITSKEY command Import Galileo SSI images of the Earth Moon and Venus from PDS CD ROM volumes GO_002 GO_006 Import a map tile from Mars Digital Image Model MDIM CD ROMs published by USGS in PDS compatible format GETMGN can import mounted MIDR CD ROM into an area i all the browse frames contained on a as a composite browse view ii a single browse frame and display the 7 x 8 framelet grid on the frame on which the browse frame is displayed and iii a Magellan Mosaic Image Data Record MIDR image from CD ROM into a McIDAS area APPENDIX III 4 GETMGXDR GETSEDR GETVGR GETVO GRADNT GUI HELP IDMOON IMGCTR IMGDAY IMGTS LA LIMBPT LIMPRO Import Magellan Global composites of topography surface reflectivity slope and emissivity from the PDS CD ROM Volume MG_3001 and MG_3002 Attach to Voyager images the full SEDR data from Voyager SEDR files for PLAN navigation type Import compressed Voyager 1 or 2 images from CD ROM and write a McIDAS area containing that image Import Viking Orbiter 1 amp 2 Mars images from CD ROM into McIDAS areas Create an image that shows the local brightness gradient of an image Start the Graphical User Interface assumiong X window workstations have Tcl Tk installed List the help instructions for a McIDAS key in Ident
126. ata on Venus surface Magellan Global Topography Radiometry and Terrain Data GxDR s Mars Digital Image Model MDIM s Data Viking images of Mars and its moons Voyager images of the giant planets and their satellites Images with FITS headers All other images HOW TO NAVIGATE AN IMAGE OF A SOLAR SYSTEM TARGET Navigation Reference Frames Navigation Types in eXplorer Voyager ISS Images of giant planets and satellites without SPICE kernels Earth based telescopic images of planets Viking Orbiter images of Mars Spin Scan Pioneer Orbiter Cloud Photopolarimeter Images of Venus Generic Navigation Recipe for Framing Camera Images Finding the Limb Points and Image Center Specifying the Image Center Using the found center for navigation Recomputing the Sub observer and Sub solar point data How to Update SPICE Kernel Navigations of Planetary Images HOW TO MEASURE DISTANCES and AREAS WITHIN AN IMAGE OF A PLANET OR A MOON HOW TO DIGITALLY FILTER AN IMAGE HOW TO DETERMINE THE PLANETARY PHOTOMETRIC FUNCTION HOW TO REMOVE THE PHOTOMETRIC FUNCTION FROM AN IMAGE OF A PLANET OR A MOON HOW TO EXAMINE IMAGE DIGITAL DATA IN A DISPLAYED IMAGE HOW TO ENHANCE AN IMAGE Black and White Enhancement False Color Enhancement True or Three Color Display or Enhancement Digital Filtering Digital Data Modification vi 3 13 3 15 4 1 4 2 4 3 4 3 4 3 4 4 4 14 4 15 4 16 4 17 4 17 4 18 4 18 4 19 4 19
127. atabase program within McIDAS eXplorer DBL command and another is to use a mission specific command e g FINDVGR for Voyager images More in information on how to use these commands can be found in the user guide Chapter 4 and the command reference Assuming that a particular image has been located on a specific PDS CD ROM volume the user can proceed to import that image into McIDAS eXplorer as described below 2 11 Mounting and Unmounting CD s Most versions of UNIX require that a CD volume be mounted before it is recognized by the system and McIDAS X is no exception Here is how to mount and unmount the CD s physically remove the CD ROM in the drive if there is any and insert a new CD into the CD ROM reader and then click with the right mouse button in the active frame window to finish the mount process The CD drive light should go on to read the directory which indicates that the command has taken effect Note that the contents of the CD ROM can be queried using the UNIX command ls via McIDAS eXplorer by typing in the Command window At this point the data from the particular CD inserted into the reader is accessible from within McIDAS eXplorer though mission and data specific commands or via the GUI These commands have a prefix GETabc where abc refers either to the specific mission or the mission specific data type For example GETMGN GETALT and GETMGXDR all refer to different commands to import data from PDS CD ROM vol
128. aying a maximum of 256 monochrome or color A A PS a Erxsanmantixr tha data hace mare ar lacee Avnamier ranoe than that ie
129. barrel type distortion It is possible to remove both of these distortions to a large degree as described be low The systematic processing of Voyager images can be streamlined by using a macro command that daisy chains the steps described below as the processing steps need to be se quential See the macro DOVGR for example which will begin with a either Wide or Narrow angle camera images acquired with a specific filter and will sequentially process it to fill the data compression gaps determine reseau locations correct for shading including dark noise subtraction using an appropriate dark noise file perform geometric rectification and determine a preliminary set of limb points for interactive navigation all in a single command Optionally multiple images can be processed in exact same manner sequentially Within McIDAS eXplorer environment whenever the original data are being modified in some form the application program will always retain the original area and create a new version of the data in another area and will copy the accompanying directory and DDB infor mation as well as make an entry in the audit trail The original can then be deleted if no longer necessary Thus if an error is made at any step the process can be repeated as desired The individual steps are described below 3 1 2 Removal of Geometric Distortion To account for this distortion a network of 202 3x3 reseau marks is etched on the face plate of the each of the vi
130. being developed to provide access to and enable efficient analysis of geophysical data acquired about solar system objects It is an enhancement of McIDAS X a toolkit directed at the terrestrial meteorological community for analysis of real time weather satellite conventional and forecast model ourput McIDAS eXplorer provides access to and enables investigation of data from the CD ROM volumes published by the Planetary Data System from NASA s solar system missions and incorporates the SPICE subroutine library developed by the Navigation and Ancillary Information Facility NAIF at the Jet Propulsion Laboratory for the display navigation animation and analysis of planetary data on most UNIX workstations with X windows support Primarily intended for analysis of image data the user extensible environment provided by McIDAS eXplorer allows analysis of a wide variety of data with minimal effort in a multiframe with overlay graphics multitasking environment Currently tools are available for calibration navigation and analysis of Voyager images of the giant planets and their satellites Magellan radar and altimeter data Viking Orbiter Mars Mosaicked Digital Image Model data and Galileo images Tools are being added for access to and analysis of ammospheric profiles as well as spectral data such as Mariner 9 IRIS and Voyager IRIS observations This work is funded by Contract NASS 31347 from NASA s Applied Information Systems Research Prog
131. byte format 45 If image is a Mode AA DS STEP DWEL these bytes indicate the origin of Band 8 Not used for GOES mode AAA 46 Actual image start YYDDD Nominals above are set by convention 47 Actual image start HHMMSS 48 Actual starting scan line 49 Line prefix documentation section length in bytes 50 Line prefix calibration section length in bytes 51 Line prefix level map section length in bytes AR Image type VISR VIERES VAS Ty ERBE AVAR y TELIS 33 2 McIDAS eXp images default to line ele imagery of type VISR unless they are two byte photometrically corrected VICR 53 Calibration Type Physical units in which the digital data are stored The calibration type determines how the image is displayed on the screen or processed by various applications e g BRIT 8 bit DN values CAL 16 bit DN values specific units RAW 16 bit DN values undefined linear units TEMP Degrees Kelvin RAD Watts cm 2 ster scaled integer Bi 2 byte signed integers If not VISR BRIT or CAL or VICR RAW the core DF command may not work for the data in an area Also VICR RAW images have to be converted to albedo using solar distances and other con stants located in the audit trail for instance A separatee keyin must be used to convert physical units in multi byte data into an acceptable range of usable visible contrast in the displayed McIDAS X frames This restriction extends to the use of the D
132. cIDAS X system related issues Mr Ken Bywaters Mr Russel Dengel and Mr Gerry Peltzer developed several new applications Much needed other support was also provided by the Space Science and Engineering Center Planetary Data Visualization Workshop Report of a workshop sponsored by NASA s Solar System Exploration Division and held at San Juan Capistrano Research Institute Nov 15 17 1993 Watt Aaa KN lt SJI Prepared by Doug Nash San Juan Capistrano Research Institute San Juan Capistrano California April 26 1994 SJI TECH REPORT 94 1 GMGINAL PACE Y OP POOR QUALITY MCIDAS EXPLORER A SOFTWARE ENVIRONMENT FOR VISUALIZATION OF SOLAR SYSTEM DATA S S Limaye D Santek L A Sromovsky U of Wisconsin Madison and R S Saunders Jet Propulsion Laboratory McIDAS eXplorer is a software environment designed to provide a capable means of accessing analyzing displaying and visualizing the data collected by missions to solar system targets as well as the earth Built as an extension to the X windows version of McIDAS the eXplorer environment is user extensible and is implemented on many different flavors of UNIX MCIDAS has been developed by the Space Science and Engineering Center of the University Of Wisconsin Madison with primary focus on providing an integrated interactive access to the meteorological data and model output collected by the weather Satellites and corventional means as well as to numerical model ou
133. cessary For the solar System targets the first data type is the most prevalent form illustrated by nearly 60 gigabytes of solar system images contained on nearly 100 CD ROM volumes and most McIDAS eXplorer tools These data are imported into the McIDAS environment and stored in files called Digital Areas with an data block containing the particulars of the contents The second data type is illustrated by low spatial resolution topography gravity field data or numerical model output data and is stored within McIDAS in the form of Grid Files Each Grid File can contain multiple grids of different quantities and a Grid File Directory provides the access roadmap for the contents of the file Simple arithmetic or spread sheet operations are possible with the grids from within McIDAS The third and the simplest data type is illustrated on the Earth by Surface weather station observations or for solar System targets by infrared spectra acquired for a specific location These types of data are optionally stored as Meteorological Data MD files with data tagged by keywords or as a simple flat file with a directory structure The MD file format allows database search and retrieval as well as data editing functions PRM PAGE paje NOT FILMED ZAFLORER Limaye Santex Sromovsky and Saunders These different data types can generally be visualized in a variety of ways either as a two dimensional image as a pseudo 3 D image in a perspective
134. ch mode by specifiying the blemish locations image line and element numbers and the size of the box that specifies their size also in lines and elements from a text file APPENDIX 6 BOTSIM BOTSIM Transfer navigation from the navigated frame to the unnavigable frame for a pair of Simultaneously shuttered Wide Angle Narrow Angle Voyager Images To be used only for images with the PLAN navigation type navigated_area unnavigated_area SIMUL YES NO SIMUL CENTER NOTE REMARKS Uses transform matrix for simultaneous WA NA Voyager 1 or 2 image pair to link the unnav_area to a navigated navigated_area using the WA NA co ordinate transform matrix Both images must have identical shutter times and be BOTSIM shutter mode must have previously run SEDRIN to define the camera geometry for the unnavigated frame YES NO YES is default NO turns off date time check for simultaneous shutter times If times are not the same no correction for rotation of the target planet between images is made LIN ELE Planet center line element in unnavigated image default is planet center translated from the navigated image The north angle of the navigated_area is used for the unnavigated_area This permits navigated_area roll angle and spin axis corrections to be propagated to the unnavigated This command is useful for close encounter images from Voyager cameras of obbjects when the higher resolution narrow anlge
135. cks specified defaults to displayed frame EXAMPLES LISTNAV defaults to SC and displayed frame LISTNAV BOD displays picture body block for displayed frame LISTNAV USER 2335 displays user block for area 2335 If there is no displayed frame will try last accessed area KEYWORDS AREA area number whose blocks are to be listed area defaults to displayed frame image APPENDIX 59 LISZEN A command to enable conversion between planetary coordinates and image coordinates assuming image is navigated Will also provide zenith satellite sub solar zenith angles at a given image location and the location of the sub solar and sub spacecraft points LISZEN opt x coord y coord area_ Parameters opt x coord y cood area REMARKS PLA to convert image coordinates line element numbers to planetary coordinates latitude and longitude IMG to convert planetary coordinates latitude longitude into image coordinates line element ZEN to determine the spacecraft and solar zenit angles at a given image location SP to print the sub spacecraft and sub solar locations image and planetary coordinates latitude in degrees if opt IMG line number if opt PLA or opt ZEN longitude in degrees if opt IMG element number if opt PLA or opt ZEN area number corresponding to the image This is a macro command that invokes area navigation to do the transforms The area need not be displayed second area nu
136. cludes a magnification factor A frame never exists without an image but many different frames can be generated on the video screen from a single image An image must always reside in an area Thus every frame gets its coordinates and image from a source area The core McIDAS keyin C relates a displayed frame to its source area All that is known by McIDAS about a displayed image comes from information or file pointers stored in the source area for each frame All of the coordinate conversions are handled internally by McIDAS so that when a user places the cursor over a pictel on the screen McIDAS knows the exact value and location of the corresponding pixel in the image in the data file as well as all the available navigation and calibration data related to that specific byte We have defined a new McIDAS eXp area structure compatible with all versions of McIDAS A new McIDAS eXp keyin DDBUTIL accepts standard or core McIDAS area formats and converts them to the new planetary McIDAS eXp area format which contains a new entity called a Data Description Block DDB DDBUTIL will also generate a new McIDAS eXp format area for any chosen image size which the user can then read and wnte with other McIDAS X or McIDAS eXp keyins There are additional options within McIDAS eXp for reformatting imagery from other sources There exists a set of CD ROM reader commands named GETxyz where xyz is a three letter acronym for a planetary spacecraft
137. command can accept positional as well as keyword parameters The names can be one character or as long as allowed by the native system but preferably short and mnemonically representative of the process McIDAS has several single letter commands entered either as letter followed by a cr or by the ALT etrer key strokes from the keyboard Other commands can be entered in the command window using the key board with associated parameters positional or key word oriented followed by a cr Alternately the commands can be entered using the graphical user interface GUI Single letter Commands Single letter commands can be entered using the ALT efter combination and generally control the terminal display state The most often used are A Step to the next frame in the frame display loop The loop bounds are between the first and the last frame defined by default when the McIDAS session is started The begining and ending frame number bounds can be changed using the LB command or a random sequence of valid frame numbers can be set using the LS commmand The loop bounds are circular so if the A key is entered while displaying the last frame the next frame displayed is the first frame in the sequence In McIDAS X the graphics frame is part of the image frame and the graphics will also switch The graphics loop bounds can be set independently using the GRA option in LB and LS and can also be decoupled using the J key in This allow
138. coordinates for each element called the image coordinates of the element This coordinate system is defined only by the spacecraft camera combiand is independent of how the data are stored If all of the elements of a raw image were contained in 5 11 nation an area there would be no point in distinguishing between image and area coordinates What is stored in an area however is a rectangular subset or superset of an image obtained by sampling averaging repeating or editing of lines and elements or some other pixel mapping process In order to map an area to the original image the following formulas are used Image Line UpperLettiine Area Line LineRes Image Element UpperlLeftEle Area Element EleRes UpperLeftLine is the image line coordinate of the first area line UpperLeftEle is the image element coordinate of the first area element When LineRes EleRes 1 the area is said to be at Resolution 1 or Full Resolution When for example LineRes EleRes 4 only every fourth line and element of an image originally at resolution 1 are included in the area This area is said to be at Resolution 4 Each line in an area has the same total length This length in bytes 1s always multiple of four The image data in an area may be viewed as a continous stream of bytes numbered from 0 Within this stream of bytes the area data are contained line by line with the lines in order first to last Each line is
139. ction Minnaert Scattering Law is the preferred function default but the extended Minnaert and Hapke functions can also be used The Minnaert function can be fit to a given image using MINFIT INPUT source_area OUTPUT dest_area FUNC SPLINE spline_size STRETCH scale or source_area dest_area spline intcpt slope stretch Use the first format for Pioneer Venus images KEYWORDS INPUT OUTPUT SPL NE FNC MINN EXMINN HAPKE STRETCH SATMAX SUNMAX SPLINE AO A1 SCALE REMARKS Source area number Area into which the output image will be written Sptine size for the remapping usually 4 or 5 MINN intercept slope Default HAPKE abc EXMINN intcpt slope muoffset where Minnaert Intercept and Slope coefficients Extended Minanaert function for thick atmosphere bearing bodies Hapke Photometric function Linear contrast stretch factor try between 1 2 and 3 Maximum S C zenith Angle allowed for output image Maximum solar zenith angle allowed for output image SPLINE SIZE DEF 1 Minnaert Intercept for that image Minnaert Slope for that image Contrsat stretch factor linear multiplicant default is 1 5 This command removes the limb darkening by the additive method i e by adding the deviation from the limb darkening function to a constant value rather than multiplicatively which would produce a true image brightness normalization The reasons for doing so are purely cosmetic The additive method does not blow u
140. d will compute the ephemeris data and update the DDB using the time that the image in an eXplorer area is tagged with It will use the current center location to attach to the navigation Computing the North Angle for Planetary Images with Moons For images of Jupiter and Saturn taken through small telescopes particularly amateur telescopes the north angle of the target object in the image is not easily obtainable unless there is moon present in the image The IDMOON key in allows the user to identify one or more moons of Jupiter as well as use the observed image location of the moon to determine the angle the planetary axis of rotation makes with the image scan lines North Angle Finding limb points McIDAS eXplorer provides a choice of four commands to determine the limb points in a planetary image They use somewhat different algorithms and therefore the choice depends more on the image characteristics such as sharpness contrasts and noise If the noise is minimal the edge points determined by these commands are in general consistent The limb points are stored in a standard file named LIMBnnnn where nnnn corresponds to the area number in which the image is stored and is padded on the left with zeroes if the nnnn is less than a 4 digit number A complete copy of the DDB is stored within the limb points file so that the correspondence between an existing file and the digital area can be validated The limb point finding choices are described
141. d by the instrument after the telemetry decoding has been done Glossary 2 Calibration is the process that converts the raw data counts into physical units This also includes the conversion of the counts into a single byte integer number that is used to represent the brightness on the video display for a given image pixel An example is the infrared data that is stored as a digital number which with appropriate calibration information such as wavelength and conversion factors can be converted to a brightness temperature or an image brightness The name of the sub program unit that performs this conversion is stored within the area directory for an image CD ROM Compact Disk Read Only Memory the media format that is compatib with the audio Compact Disks on which the digital data is stored NASA s Planetary Data System PDS has published a large amount of digital data acquired from Data planetary missions on such disks A current list of CD ROM s containing planetary data is available from the National Space Science Data Center NSSDC located at the Goddard Space Flight Center GSFC Greenbelt MD 20771 Command A command is 2n instruction to McIDAS eXplorer to execute a process The name of the command is the name of a FORTRAN subroutine or a C procedure that is compiled and linked with the McIDAS main o and all the associated libraries In McIDAS eXplorer the command name can be as long as allowed by the native operating system A
142. d by using a second sub directory This sub directory can be thought of as workspace for McIDAS X and needs to be large enough to accept the data to be accessed as well as for any output created and typically this is the largest sub directory With each area basic information about the data contents regarding acquisition time source instrument calibration navigation and format is stored in a carried along the processing chain Standard McIDAS X file format for multidimensional spectral im ages includes a directory block 64 words as well as a 128 word block containing the naviga tion information for the data Data Description Block McIDAS eXplorer extends the data directory concept by using an additional Data De scription Block DDB in as many multiples of 64 words as needed The DDB allows access to detailed descriptors of the data about the target object the source instrument data acquisi tion geometry calibration and other ancillary information that is potentially useful The exact definition of a DDB is dependent on the instrument type that returned the data Thus the Voy ager images have a specific DDB type defined which is different from the Magellan radar im ages of the Venus surface which are available only in map format At present the DDB concept has been implemented only for the image data The PDS has adopted a standard for labels for the datasets produced on CD ROM s These PDS labels usually include information present
143. d from some standard format from a PDS CD ROM volume or from a FITS file as well as comments regarding the processing history See Data Directory and Data Description Block for the explicit format of the area layout The following list includes some general commands that pertain to areas or how to obtain information about the images contained in the areas AA Copy an area or part of it into another area AA will create an exact copy of a given area by copying the calibration navigation and processing history The destination area that is created can be smaller or larger than the original in terms of the image extents ASTAT Measure area statistics ae gE ASTAT measures the area or strictly speaking the number of pixels at specified brightness thresholds within an arbitrary outline or cursor or within the whole area CA Change area Some entries in the area directory can be changed manually through the command CA Change Area Only the satellite identification number SS day and time when the original image acquisition began YYDDD HHMMSS the area start coordinates upper left hand line and element coordinates area sampling factors LRES and IERES and the MEMO fields can be changed DF Display the contents of an area on a given frame FILTER Digitally filter an image contained in an area LA List area LA lists the area directory Several options permit varying amounts of detail to be listed for a given are
144. d sheet capability allows anthmenc operations on the gridded data to compute other derived quantities Spectral data can be displayed averaged and staged for further processing as desired for temperature retnevals or other analysis Figure 2 An Earth based telescopic image of Jupiter with an overlay latirude longirude snd and a view of available GUIs OPINAS Pase JE NE Figure 3 A line plot between two arbitrary points ina Magellan SAR frame 14 o pi S a M per e Enr R 1 L L N tert wry vean tarth Man Asterents amr yal youn Urarars wepia Hte liw cena Mow x you Lo chouse the panel or Sale le you wnh te vew Once the Oeri rt Caen you are to peter what H 18T 1 00 mages vou wan to see The ye op bans are setup UA a wey as LO veny wtach shert and whet WENN YR der ani Vey peel YN an ma Ve Lia ot bey hete ul Uw wage SAR r ins ite thee Tir sane m MA kru you hove De oplon 01 6 Oh 1 Yv De rhage ining any ef Ow vam Ha IDA G mne winch wall he ested tale L gw tint MR X the deta Mr m a erp mri nt He dr v real taap S an A Y Y mint DISPLAY OFT tott t riba 1397 fa ITA MUDITY Ma OVERI AY WAVIGATE ME ATURE HPORI i HEIP CANCE Nde o _ a poo Po C bratawi ruta sf f l Sloe OD 1 Mrs rapt Y Y aie pr LG R R b ips IMAGE DIST AHC 1 IMAG 316119 11C3 Menam n Y V d e WAGE iMIF MOI H 908 000 LLL 1 DU as HD y ER 1 T birun asn X Vda Map mrn X Vah
145. dicons and their positions on the face plate were carefully measured to a thousandth of a mm on the ground before launch Benesh and Jepsen 1977 The loca tions of these marks are first measured in the images using key in RF and their ground mea sured locations used to compute the transformation between the observed and expected object space locations The coordinates for other points in the image are then obtained by bi linear interpolation The nominal and found locations of the reseaus in the raw image and the object space locations in the geometry corrected image can be displayed on using the RESEAU key in Finally after the image has been geometrically corrected there is no need to retain the reseau marks in the image and are generally removed for cosmetic purposes by replacing their image signature with brightness values from the surrounding region This is also recommended prior to determining photometric function parameters for the image e g with MINFIT so that the reseaus themselves do not anomalously contribute to the photometric function fit In order to minimize the effect of round off or truncation error the output images size is set to 1000 x 1000 pixels 25 larger than the original size in either dimension The GEOM command accomplishes this latter task The required key ins are as follows RF source _area_ to measure and store the image locations of the reseaux marks The spacecraft and camera information as well a
146. different Frequently the colors may be muted and may require at the very least significant contrast stretches in one or more colors for a pleasing output or other selective enhancements Please see How to make a Color Composite for the tools available within McIDAS eXplorer to accomplish this Digital Filtering The appearance of Monochrome or multicolor images can also be altered by selectively enhancing or removing certain spatial frequencies in the image by digitally filtering the image using either the FILTER FILTVGR or the MA command Different filters produce different effects as may be expected FILTVGR is a spatially adaptive filter that produces least objectionable output when the image contains sharp boundaries e g the bright planetary limb MA filter options are one dimensional along each image line and are useful in only certain applications A Low Pass filter may remove high frequency noise and make the resulting image look smoother and perhaps more pleas ing while a High Pass filter applied to a full disk planetary image acquired in reflected sunlight can remove the shading due to the varying scattering geometry an effect similar to flattening or brightness normalizing Digital Data Modification Besides digital filtering the image data can be altered in other ways such as by adding a constant value to all or selected data points applying an analytic function that changes the appearance of the image e g a known p
147. display restrictions A calibration block tells McIDAS how to convert the two byte data into a 1 byte brightness value so that any specific part of the entire dynamic range of the data can be displayed as an image Normally the conversion is linear so that the entire 2 byte range is scaled into a 1 byet brightness value However other scalings are possible through the SU command so that the raw data conversion into the image brightness can be arbitrarily set Directory Directory for areas or grids refer to the descriptive elements of the respective data types See Area Directory or Grid Directory Area Directory McIDAS uses 64 4 byte integer words to describe the contents of an area The words are defined as follows Frame Directory Whenever an area is loaded or displayed onto a McIDAS frame the area directory is copied into the directory for that frame Word 17 in the frame directory contains the area number that was displayed in that frame Sub directories OS McIDAS and McIDAS eXplorer use several sub directories in the native workstation s default drive directory The binaries mx files in UNIX are stored in the mcidas bin subdirectory Directory Virtual Graphics All vector graphic output can be saved in virtual graphics a specific file format Many graphic images can be stored in a virtual graphic file A directory lists the contents of the stored vector graphics Enhancement Most video systems are capable of displ
148. dow by issuing appropriate command s Galileo SSI Images of Earth Moon and Venus Use GETGO to import images from PDS CD ROM volumes GO_0002 through GO_0006 Volume GO_001 has not been published yet GETGO will also allow the user to create a browse area that contains thumbnail versions of a range of images on the CD ROM a facility that is common to all the PDS mission specific CD ROM key ins Since the SSI images of Venus reveal only the Venus cloud deck as opposed to the surface in Magellan radar images the target name is set to Venus Cld to reflect the fact that the cloud deck is a considerable distance above the Venus surface and hence a different radius is required for image navigation Magellan Radar Images of Venus surface Use GETMGN to import radar images of Venus surface from PDS CD ROM volumes MG 0001 through MG_0123 These volumes contain the Mosaicked Image Data Record constructed from the radar returns at four different map resolutions F MIDR C1 MIDR C2 MIDR and C3 MIDR The F MIDR data has a nominal resolution of 225 meters The compressed MIDRs are successively 8x sub sampled at each step between Cl and C3 For each set a browse image containing 7 x 8 grid tiles is also contained on each volume The first problem that faces a novice Magellan data user is how to determine which CD ROM volume to look at If either the latitude and longitude of a region are known or the name of a feature then FINDFF can be used to de
149. e Rotation angle of nadir angle about optic axis lat lon dist Planetocentric latitude at s c subpoint default 0 0 Planetocentric longitude at s c subpoint default 0 0 Distance s c to planet center in RADIUS def 10 0 DIST 1 000 is at planet or cloud top surface Infinite distance yields orthographic projection Line in area to put subpoint default area LINES 2 20 Pixel in area to put subpoint default area ELES 2 sub sun lat sub sun longitude ss yyddd hhmmss McIDAS Spacecraft ID Default 50 Image day amp year default is current day amp year Image time default is current time If the area exists prior to PLANAV call HHMMSS will be used as defaults the existing SS YYDDD NAV NO AREA REPLACE NO merely generates CRT output of the navigation parameters default is REPLACE NO which with default value of 128 for the keyword NAV lists the 128 word navigation block REPLACE NAV replaces only current nav block for area destructive REPLACE AREA re generates area amp nav Display NAV words of current PLAN navigation only Maximum useful number and default is NAV 128 0 3 Adds additional output for detailed nav diagnosis PLANAV Lists current navigation for last accessed area PLANAV 23 VENUS_CLD 180 0 REPLACE AREA Venus upside down in area 23 PLANAV 23 SATURN REPLACE AREA VIEWPOINT 90 0 180 0 15 north polar perspective view at a distance of 15 planetary radii PLANAV AREA 23 500 500
150. e Files Although the CD s offer a convenient means of archival of image data the speed of access is less than desirable For this reason and for reasons of compatibility with the McIDAS environment as well as efficiency the image data is imported into the McIDAS environment as files At the same time a Data Description Block is created that provides a road map to the navigation calibration information for the image data While there is some commonality between various formats mission and science instrumentation differences result in mission specific variations These are accommodated by classifying the DDB s into specific models such as one for framing cameras one for spin scan imagery one for nadir pointing scanning instruments etc The Magellan SAR and altimetry data are exceptions in that the image products are available only as mapped products various compressions achieved through sampling while the latter is mostly available along orbit tracks The datafile structure is described in detail in Appendix III for the different models used A brief overview of the files used by McIDAS for storing the imported image data is given below McIDAS X stores image data in files called areas all of which have names of the form AREAxxxx where xxxx is a four digit number Each area contains one single image which can be multibanded As many as 9999 areas can be accessed by McIDAS from the ul mceidas data sub directory and more can be allocate
151. e Information Systems Newsletter wy paisa gt ra fe BL AA way gt A ae A 4 we phe ad Rene oN P ES toate LL T Nu FA eet SSSA L FEATURES a r a NUT Testbed Envision 3 NCSA PATHFINDER 7 McIDAS eXplorer 10 FY93 NRA Awards 15 Planetary Visualization 20 CD Media Study 32 Data Service Expands 36 Reach Out 40 DEPARTMENTS Calendar 4 Astrophysics ADS 16 Research Announcements 20 TAE 21 NAIF 22 Networking NSI 26 Accomplishments 37 a February 1994 Issue 3 NL ER open Stem RA A R On Rog Sans wes Se Ee E NL CEP eT ets Bt lt C L a ms c Ke Ka af L ee armen 0 C ja 1 A 27 se 9 US Y ead 7 al y O bi IEPS The Earth Data System and the National Information Infrastructure Testbed Carol A Christian Center for EUVE Astrophysics University of California Berkeley and Stephen S Murray Smithsonian Astrophysical Observatory and CM Science Innovations The National Information Infrastructure Testbed The National Information Infrastructure Testbed NIIT is an industry led consortium of commercial academic and government institu tions formed expressly to develop a prototype nationwide infrastructure to study and demon strate distributed computing applications NUT testbeds will address actual applications specifi cally to gain and share experience in creating and operating such infrastructure
152. e center for the purpose of image navigation Particularly useful for ground based telescopic images of the planets as no navigation data are required either for EDGES or for IMGCTR EDGES option Parameters option FIN ADD DEL PLT LIS KEYWORDS DER DER DER Remarks is one of the following Find limb points from a displayed image and create a new limb points file to store the points and display them on the graphics frame Append more limb points to an existing file Delete limb points for locations within the cursor from the limb points file and erase them from the graphics display not in McIDAS X Plot the limb points for the diaplayed image from the corresponding file List the limb points file corrresponding to the displayed image TOT for total derivative actually max of gradient in the line or element direction ELE to compute derivative in the element direction dB dE LIN to compute derivative in the line direction dB dL Limb points are found along the longer dimension of the cursor This is crucial when finding limb points near the top or the botom of the image when the planet s visible bright limb is almost tangent to one of the sides of the rectangular cursor box This command is useful when there is excessive noise in the background or when there are rings present such that automatic limb determination is problematic Use IMGCTR to determine the shape size and center of the object by a general conic
153. e combinations of ramp black and white enhancement are desired using identical red green and blue ranges for output brightness will achieve the desired enhancement As with the black and white enhancement tables the false color enhancements can also be saved removed and restored using the EU command in exactly the same manner True or Three Color Display or Enhancement If the display hardware allows it McIDAS eXplorer can be operated in the 24 bit mode which allows display of three different images through the red green and blue guns of the display device If these three images are components of a 24 bit images such as from a color scanner then the result is a true color image Spacecraft images generally are not obtained as true color images but are acquired either through different filters either singly or simultaneously such as with an imaging spectrometer If the images are acquired one at a time through different filters over a short time such as the Voyager images of giant planets and their satellites they need to be registered to 4 18 account for any camera pointing differences and or time differences which may reveal small but significant rotation of the target object in the three different filtered images Depending on the target the wavelength at which the images are obtained and which wavelength image is displayed in which of the three colors available through the display device the color composite rendered will appear
154. e component tiles Determine the center of the image of a disk by first finding the centroid of brightness of the image data in an area and then determining the limb points from radial brightness profiles The limb points are stored in LIMBxxx file where xxxx is the 4 digit left zero padded area number in the same format as used by EDGES command The file can be interactively edited using EDGES A least squares general conic fit is used to determine the center Multiple passes allow exclusion of deviant limb points and he edited points can be stored in the file as an option Calculates Transform Matrix for Planetary Navigation for framing camera image navigation Currently it is set up for Voyager images for PLAN navigation type only CHANGECD CLEAN COMBIN COMP CONFIT DBI DBL DBU DDBUTIL DECOMP DF DF3 Unload load or load unload CD ROM in the CD ROM drive from within McIDAS The disk of course has to be manually removed and replaced Clean up a Voyager raw image to remove cosmic ray noise and replace any bad lines Make a multiband area from several single band area May also be used to reduce 2 byte data to 1 byte data using the calibration constants in the area directory Useful for multispectral classification remapping of multi filter images such as Voyager or Viking Compress the image data contained in a digital area file using the Huffman coding lossless or DCT lossy coding The former is revers
155. e data are utilized as well as in their content These differences can be illustrated by the presence of clouds in the satellite data for geographic remote sensing applications the presence of clouds is a hindrance to the analysis of the underlying surface data yet the presence of the same clouds in weather applications is used for determining the atmospheric flow and radiation budget or storm development Further the information for geographic applications is concentrated in the spatial and spectral domain whereas for meteorological applications the information IS contained primarily in the time domain and in spatial and spectral domain for climate applications The spatial resolution of the data as well as coverage is also a distinguishing factor For geographic and geologic applications highest achievable spatial resolution is desirable whereas for weather and climate applications global and temporal coverage is more important than high spatial resolution Planetary data in general differ from both the geographic satellite remote sensing data and the terrestrial weather satellite data in several key aspects First of all while some data is analyzed in near real time for mission sequencing and public affairs reasons much of the scientific analysis is carried out later The data is usually acquired over a limited period of time and is often unique Thus while we have global weather satellite data for nearly two decades we have less than two days wort
156. e it is at the end of the area file this entry may grow without limit as the image continues to get processed The first six lines of the audit trail are called the image identification block and those six lines have the same format for every planetary image independent of the source Some Voyager images acquired from EDR s or VICAR tapes may have erroneous data in this block but the information acquired from CD ROM sourced images via keyins GETXXX is generally correct All McIDAS eXplorer keyins use the Image Identification Block data acquired by subroutine ITIDBLK and the Data Description Block acquired by subroutine DDBBLK to identify default keyin values for any image The user is permitted a wide latitude to change McIDAS eXplorer Kevin parameters but we try to prevent misidentification of data or its stage of processing by keeping many parameters internal to the system and requiring that the system complain if patently wrong input or output is specified by the user If information is available internally to the system the user should not be required to specify it The global structure of a McIDAS eXp area for Voyager images is illustrated below BYTES WORDS AR ee 0 DIRECTORY 256 Roo o o oo OA NAVIGATION 2816 004 CALIBRATION 90040 co 3 coe n ee GO IMAGE ENDIMG EOF Again please note that all coordinates relative to an area are zero based
157. e spacecraft the instrument and thus the calibration procedures and software also may differ Although the area format allows some room for the calibration information to be stored frequently other means are necessary to accomplish this task Often particularly for scanning type of devices the calibration is included as part of line documentation on every line and treated as a line prefix in McIDAS Sometimes the calibration data require a significant amount of data in which case these are stored separately and more than one calibration may be necessary Voyager images require both a radiometric and a geometric calibration Radiometric calibration of Voyager vidicon images are an illustration of the situation where the data files that are necessary for converting raw data numbers into radiometric units occupy about 240 Mbytes of disk space for each camera The calibration is actually a separate processing step SHADE9 keyin raw DN values to watts cm 2 ster with a separate specific dark noise file corresponding to the Voyager camera and exposure time and a 9 point transfer function for each of the filter positions The calibration produces a two byte per pixel output from single byte raw Voyager images Simple field flattening using a linear two point transfer function is often adequate for many tasks and requires far less disk space to operate It runs fast removing hot comers and improving contrast and produces a compact one byte per pixel
158. ed as desired McIDAS X stores image data in files called areas all of which have names of the form AREAxxxx where xxxx is a four digit number Each area contains one single image which can be multibanded As many as 9999 areas can be accessed by McIDAS from the ful mcidas data sub directory This sub directory can be thought of as workspace for McIDAS X and needs to be large enough to accept the data to be accessed as well as for any output created and typically this is the largest directory If another directory name is desired for the default data directory it can be specified by the core REDIRECT command Reading data from PDS CD ROM s The first challenge is to know which particular CD ROM volume to load into the CD ROM drive to read the data Some familiarity with the mission is useful to select a specific image and a CD ROM volume for a given target object This task can be accomplished in several means One is to browse through the CD ROM contents for a specific mission or a solar system target either directly outside of McIDAS eXplorer or using the browse feature included in most data importing commands for the PDS data which allows to create a visual thumbnail view of a number of images that can be viewed at once Another is to use the database features included within McIDAS eXplorer to select a certain image and the CD ROM volume on which it can be found There are two means of searching the database one is a generic d
159. ed with DEV F log file_name Alternately TFILE OPEN can be used to maintain a single log file record of the RUN output If any command aborts i e is terminated due to some error processing continues with the next command in the RUN file sie 2t 2 6 Keyboard For compatibility reasons McIDAS keyboard normally is in CAPS LOCK state All key ins are KEYWORD names are expected in upper case only Note that the McIDAS control program key board state in the command window is not always indicated by workstation s CAPS LOCK indicators Usually this is not a problem unless a UNIX file name is being specified in the Command window in which case the SHIFT key must be temporarily depressed All default McIDAS internal file names are in upper case The ESC key serves two functions within McIDAS X If this key is pressed while typing a command in the Command window the typed entry is cleared If however the key is pressed at any other time it prompts the user for a name of a file containing the script for a Function Key based menu interface If hit accidentally a simple ENTER will close that window and indeed this is necessary to return control of the keyboard to the user The key board state in other X windows is not affected and is consistent with the CAPS LOCK indicator light if any on the workstation 2 7 Programmable Function Keys Often used commands can be invoked quicker with the capability of programmable function keys The 12 functi
160. efix bytes are set to zero in the area directory by FILLO FILTER Spatially filter a digital image stored in a MclDAS eXplorer area using one of several two dimensional masks Left or Right edge enhancement smoothing Laplace gradient 3x3 high pass 3x3 convolution and sharpen A new output area is created the input can be either 1 or 2 byte per pixel data FILTERS List just the filters through which images in a range of areas were acquired WHERE also provides this information along with other relevant information FILTVGR Originally written for Voyager images this is a spatial contrast sensitive digital filter that is less sensitive to sudden brightness transitions e g in the neighbourhood of a bright limb The filter size shrinks as the domain approaches a sudden brightness transition FINDALT Determine on which PDS CD ROM volume Magellan Altimeter data from a particular orbit can be found As yet there is no command to determine the orbit number corresponding to a given Venus location FINDFF Find the names of the Magellan MIDR framelets containing a given geographic feature or a latitude longitude region on MIDR CD ROM s APPENDIX IIL 3 FINDMDIM FINDVGR FINDVO FITSKEY GEOM GETALT GETCPP GETFITS GETGO GETMDIM GETMGN Find a Mars Digital Image Model frame corresponding to a given latitude or longitude or containing a specified named surface feature Search the CD ROM index
161. efore hand AAMAP source_area dest_area frame_ PROJ lat lon km pixel lines ele where PROJ MERC or PS lin number of lines in the output area created by the command and Hele number if elements in the output area lat latitude of the area center lin 2 ele 2 and lon longitude of the area center A listing of the AAMAP macro will provide clues as to how the navigation is created using the MAKNAV command The AAMAP macro generates an output area of the specified size default is 480 x 640 with one byte per pixel data attaches to that area the directory information of the source area creates the required navigation information for the specified projection creates the output image using the navigation transformations and finally displays the output on the specified frame if different from zero in which case no call to DF is made to display the result The processing history is copied and an entry is made in the output area detailing the AAMAP If the source image is two bytes per pixel AAMAP uses the default BRIT calibration to convert the two byte pixel data into one byte pixel values resulting in a loss of dynamic range of the data Note that the default scaling of the two byte data to one byte brightness data is linear but can be changed using the SU command If the two byte range of the original image is to be preserved then the more elaborate recipe below should be followed Map Projecting Images Step by Step
162. er capability to execute a sequence of commands at a predetermined time in the future Although this is most useful in real time environments for acquisition of data the facility is useful to schedule processing resources intensive tasks at times when the workstation may be otherwise idle or less stressed DO Bd C T A EEE BENESET COSS ES CETE tqcthe AE i Figure 2 3 Another example of a display of a browse frame created from data stored in 180 areas which contained raw and mapped polar stereographic images from Pioneer Venus Orbiter Cloud Photopolarimeter The areas may or may not be consecutively numbered Each thumbnail image can be annotated either with the date time of acquisition or the area and band number as desired The browse area itself is tagged with day and time when the index was generated and can be seen on the frame annotation line at the bottom 2 5 Batch processing of commands A facility to execute commands from a file allows systematic repetitive processing of data effortlessly Any McIDAS command can be entered in a text file just as it would be entered from the key board The commands in the file can be executed using the scheduler capability or started from the key board with the RUN file_name command The file can be created using any text editor available on the workstation and should normally be in the mcidas data sub directory If a log of the processing is desired each command should be append
163. ere found within the cursor dimensions as located on the image display In the eXplorer version the size of the cursor is limited to 63 x 63 due to X window restrictions Consequently the edge points are now determined for the entire area or within a box specified by LIN and ELE keywords The command is meant to be used interactively and allows for addition deletion and listing plotting of the found points The file format LIMBnnnn is the same as that used by BRTCEN command and is recognized by the IMGNAV and IMGCTR commands LIMBPT LIMBPT is very similar to EDGES but uses a slightly more robust method of edge detection and therefore is less susceptible to noise than either BRTCEN or EDGES Another difference is that LIMBPT allows you to enclose the right or the left limb with a box using mouse button clicks to limit the search area for the edge detection The limb point file LIMBnnnn format is the same as that used by BRTCEN and EDGES commands and is recognized by the IMGNAV and IMGCTR commands PLAEDG PLAEDG is a more primitive limb finding command that was initially used for Voyager and Mariner 10 images of Venus to find a limited number of limb points for use with constrained fits to find the planet image center location It is restricted to finding no more than 25 limb points which are stored in a portion of the DDB rather than in a separate limb points file It is normally intended for the PLAN navigation type for Voyager images C
164. ering U of Wisconsin Madison 1992 HOW TO MEASURE CLOUD MOTIONS Measuring cloud motions on a sequence of navigated or aligned images involves recording coordinates of selected features in a two or more images as well as recording the time of observation of those features For framing cameras the time of observation is provided by the time tag that is attached to the individual images The convention used is this time tag notes the beginning of image data acquisition Typically the exposures are rarely longer than a few seconds and the intervening time interval and the spatial resolution of planetary images is such that the precise time more accurate than say a second at which the target is viewed in that image is not very critical This is usually not the case with images acquired using a scanning instrument which usually acquire an image of the target object over an extended period An extreme case is the NOAA AVHRR images for a whole orbit which are acquired over a roughly 90 minute period or Pioneer Venus CPP images which typically require 3 5 hours per full disk image In these cases the exact time when a feature is viewed by the satellite is calculable from the image navigation and these times are then used for the velocity computations There are two commands that accomplish this PCMW allows a feature to be tracked across a sequence of frames using visual location with the mouse driven cursor in each frame of a sequence Digital cor
165. es such as a VICAR label for instance that information will be stored in the McIDAS area header blocks or audit trail and can be scanned and used by McIDAS eXp keyins so the user does not have to be consciously aware of commonly used information Key parameters will also be extracted and placed in a separate Data Description Block DDB which can be easily listed by the command LISTDDB We need to carefully distinguish between the McIDAS words area image and frame An area is simply a numbered data file Like most low level data structures its coordinates are zero based and for the most part do not have to be known by the user An image is that subset of an area file which contains digital data values or digital numbers DN values An image is always assumed to be rectangular and to be composed of lines and elements or pixels Most images have the upper left pixel identified as line 1 and element 1 Some images are subsets of other images however so the upper left comer coordinates are somewhat arbitrary and they must always be defined in the directory block of an area A frame is what is displayed in a window on the video screen A frame is a subset of an image which can be displayed at varying degrees of positive and negative magnification Thus frame coordinates always start with the upper left pictel not pixel as line 1 and element 1 but to get back to image coordinates one must perform a linear transformation which in
166. es are delared as zero in the area directory MAKESU Create an enhancement table for 2 byte images The default conversion to brightness value is a linear function MAKESU allows different curves for the data number to image brightness conversion for display purposes MAKOUT Create an output area with the same directory entries as a given area Useful in setting up remaps MCLIMB Simulate view from orbit of a planet from a nadir looking instrument and plot instrument IFOV s MDCLAS Spectrally classify a multi band image MDM CLASSIFICATION USING SIG STATISTICS APPENDIX III 6 MINFIT MGNORB MOONSTAR NAIFNAV NAMES NAVCPP NAVUTIL NRMIMG NXTARA ORBVIEW PHYSCON PLAEDG PLANAV Determine Minnaert scattering Coefficients lo and R for a navigated planetary image I lo pp by both least squares and minimum absolute deviation methods Plot Magellan spacecraft s orbit track on a displayed MIDR image The program attempts to determine the orbit number based on a nominal orbit model Pinpoint the location of a star image brightness centroid a small moon or its shadow in an image Useful for optical navigation of the data Attach navigation based on the NAIF SPICELIB toolkit to an area Plot the names of Venus features on a displayed image Refine the navigation for a Pioneer Venus OCPP image by interactively determining the required adjustments for look angle and roll angle offsets
167. es the McIDAS area directory as well as the Data Description Block DDB attached to the area directory when saving the data to tape TGET performs the reverse task i e it copies the directory and the DDB from tape to the McIDAS data subdirectory when restoring the area Thus all of processing history and navigation data are restored as they were when the data were initially written to tape APPENDIX 1 95 TILES Display a Magellan BROWSE format image from an area and show the constituent sub frames or tiles or framelets area frame PARAME TERS arear frame KEYWORDS F Remakrs AREA RAME COL OFF SIZE Area containing browse image Frame to load and grid area_ area containing the Magellan browse frame frame_ 1 frame on which to display the browse area level color to write the sub frame id s in linoff ieloff pixel offset for the id pixels size of the sub frame id label characters Default is 7 pixels high This program is a combination of the OF keyin and a special gridding routine specifically used for Magellan browse images Normally this keyin is started by GETMGN but you may cail it separately to restore the browse image to the McIDAS screen if the browse frame was overwritten 7 x 8 tiles assumed The display frame can be any size TILES will display the area to fit the frame by appropriately scaling it down The location of the component tiles or sub frames or framelets is shown
168. escribes the spacecraft attitude instrument orientation and geometrical quantities needed to find points on the planet in the data Each group is detailed below Two asterisks after a word location indicate the datum location is mandatory if a DDB is present Mandatory entries are in the same place for every DDB regardless of spacecraft or instrument but they do not all need to be filled The DDB entries for a McIDAS eXplorer area are listed by the keyin LISTDDB Note that there may be several entries for a similar value such as for Voyager with the navigation north angle words 528 529 the SEDR data north angle word 516 and the north angle computed from a limb fit words 358 359 The navigation entry 15 the value used when the area is navigated An important note The navigation routines which rely on accessing the Data Description Block for navigation information NAIF RADC SPCE require that DDB word 124 contain the area number of the area Explorer keyins which copy or move data will update this number but a core Mcidas or Unix copy routine may not If an area contains a value in word 124 other than the area number the user MUST correct this using the NAVUTIL AREA area_number ID area_number command 5 14 o deii g m r m ee r r rer e r ma e r r r e O P ee n Pee k E r Y n r e n e eee P P e y e e y is dk s iie dk aiy m m ies Seis A deis e is frr i b Safe E rr be A re UU A e o m per be AB n Sebe k e 124 Area
169. escription Block Processing History User Interface McIDAS eXplorer Workstations Planetary Image Data Supported by eXplorer USING MCIDAS eXplorer Starting a session Starting the Graphical User Interface McIDAS Display McIDAS Command Syntax Keyboard Function Keys Environment Table Hardcopy output System Status Scheduler Batch Mode Operation Keyboard Programmable Function Keys Environment Table McIDAS eXplorer Commands eXplorer Tools mporting Data into McIDAS eXplorer PLANETARY DATA SUPPORTED BY MCIDAS EXPLORER VOYAGER IMAGES OF THE GIANT PLANETS AND THEIR SATELLITES Preprocessing of Voyager Images Removal of Geometric Distortion Removal of Photometric Distortion Voyager Image Navigation Center Finding Use of Voyager SPICE Kernels VENUS IMAGES MAGELLAN GALILEO AND PIONEER VENUS MISSIONS Pioneer Venus OCPP Images OCPP Polarization Maps Magellan Images of Venus Surface Magellan Altimetry Profiles Galileo SSI Images of Venus Kee t brek be pad ed bek kek rak pd pa t 1 oo oo C L e b Q KA KA mm th HA HA HA KA LA LA hA Uy Wh KA ked O O D D G G J Gh Ln A A LA Y bel allie K e A E Gh G Gh EHA LA Ke LQ LA G G Y 4 ae AS pa Sh U A A Z DB ud HM Se ho 4 3 4 4 4 5 4 6 A are 00 00 00 00 00 b e PUN m 0 IMAGES OF MARS VIKING ORBITER AND DIGITAL IMAGE MODELS HST WF PC IMAGES HOW TO IMPORT DIGITAL IMAGES INTO MCIDAS EXPLORER Magellan Radar Altimeter D
170. etary Sciences Meeting in November 1994 at Washington D C Limaye et al 1994 McIDAS eXplorer has been demonstrated at the AISRP Workshops in Boulder in 1992 and 1993 The eXplorer binaries for AIX IRLX HP OS and SunOS and OS 2 2 1 operating systems can be obtained from the Space Science and Engineer Center It is likely that the Software Support Laboratory at University of Colorado Boulder will also be an avenue for access to McIDAS eXplorer This final report describes the eXplorer software capabilities and includes a printed copy of the User Guide ee o Te A A AA mn fay impact parameter both of which are directty obtainable trom the frequency data am trajectory intormation Fjeldba Kliore and Eshleman 1971 ASTRON J 76 123 140 Occultation studies of the giant planets have demonstrated that departures from sphencal symmetry it not accounted for can result in senous errors Eshleman 1975 SCIENCE 1839 876 878 In the presem study we have analyzed and quamitied errors in temperature and pressure profiles due to large scale atmospheric tits in an otherwise spherical atmosphere including the role of occuttation geometry in enhancing or suppressing this error The effect of atmospheric tilt is to introduce an approximately constant bias in the temperature profile For example a horaontal tit of 0 6 mrad in the Martian atmosphere can bias temperature profiles by up to 0 3 Ketvins depending on the occultation
171. ety of reasons including backward compatibility eXplorer offers a choice of different means to accomplish the desired navigation transform These differ only in their approach to determining the precise instrument pointing by determining target object typically its center location in the data and then using the known imaging geometry to achieve the coordinate transform Target location usually requires the knowledge of its center which is generally found from the bright limb for low resolution images or offset from known surface features for solid bodies The location of the limb points allows the target center determination by unconstrained conic fits for most solar system objects If the target in the observing wavelength is known then a constrained fit can also be used Once the target center is known the instrument pointing is determined and then the coordinate conversion can be accomplished knowing the orientation of the different coordinate systems at the time the image was acquired There are three different approaches available in eXplorer as described below As they are completely independent any one or all three can be attached to a given image with one of them being active as selected by the NAVUTIL command Further a fourth navigation type allows the equatorial coordinates to be determined if the camera optic axis pointing and orientation are known SPICE Kernel Navigation For a subset of the solar system images acquired in the past and
172. eyword respectively For large images actual target size the image data can be sampled to speed up the computation The data can also be restricted to include only a certain range of latitudes and or longitudes Extended Minnaert Photometric Function for Thick Atmospheres For objects with thick atmospheres such as Venus and Titan the extension of the photometric terminator beyond the geometric terminator can be approximated within the Minnaert function by the introduction of a bias in the solar zenith angle Sromovsky 1989 4 15 lu lo pp B where p wot pl 1 y1 for po gt O and UX u1 exp uo u1 pl forpo lt 0 The function parameters are specified as the second third and fourth arguments of the FUNCTION keyword NRMIMG source_area dest_area spline size FUNCTION MINNEX intcpt slope muoffset Hapke Photometric Function NRMIMG source area dest_area spline size FUNCTION HAPKE abc HOW TO EXAMINE IMAGE DIGITAL DATA INA DISPLAYED IMAGE COTV COTY is a McIDAS core command that produces either a contour map 2 D or a three dimensional surface plot of the brightness values within the cursor location POPVAL POPVAL is an experimental command that runs constantly in the background once started and displays the digital data value at the cursor center location in the displayed image The data display is constantly updated as the cursor is moved or when a new frame stepping through the allocated frames or
173. eywords used in the label do not exactly match the FITS specifications use FITSKEY to map the keywords in the label to the expected keywords All other images Use MKIMG to import the images which have an unknown label format but whose header Jength and dimensions are known e g images in uncompressed TIF format 8 bit per pixel data only HOW TO NAVIGATE AN IMAGE OF A SOLAR SYSTEM TARGET McIDAS eXplorer has tools to navigate images of solar system targets such as planets their moons The term navigation refers to the process of converting the image or instrument coordinates to a different coordinate frame usually the native reference frame of the target object It may also include a different frame located at the observer s location such as the celestial frame right ascension and declination or ecliptic frame ecliptic latitude and longitude or any other reference frame whose orientation is known If the images are of planetary ring systems and asteroids the navigation tools will be added at a later date The navigation of moons depends also on whether the moon is reasonably modelled as a triaxial 4 4 ellipsoid In effect this means that the larger moons of the planets can be navigated and the smaller rocks and most asteroids including Ida and Gaspra which are highly irregularly shaped and for which a triaxial shape model is not very representative cannot be navigated as yet These objects require a detailed shape model is
174. fit to the image frame limb co ordinates See also LIMBPT for another similar command with a different edge detection algorithm APPENDIX 1 21 ELLIPS Draw signature ellipses from a USCLAS spectral classification of a multibanded image ELLIPS inarea LCLAS HCLASS MEAN STD Parameters LCLASS lowest class to display HCLASS highest class to display MEAN 1 to display class means only STD 2 is default Defaults are O to the number of the largest class present ellipses displayed The graphs are displayed in a new window which closes itself when all the graphs have been viewed APPENDIX I 22 EXPDOC EXPDOC On line help utility for MciIDAS eXplorer commands This command will bring up different user manuals in a new text window which can be viewed using the vi editor commands guide_name where guide_name REMARKS USERGUIDE introductory user guide COMMAND command help this section DATA data file structures The vi editor commands can be used to search for specific items Help Command_Name will list the help for that command APPENDIX I 23 FILLO Fill zeroes in scan lines due to data compression in Voyager Uranus Neptune images using the alternate side compression by averaging across lines that contain data area_in area_out OPT LINE BOX KEYWORDS NUMAVG 3 default BOX size MINDN 0 minimum DN used to compute average DN in BOX OPT LINE Default or BOX If OPT BOX
175. formats for storing and accessing the data are specified under McIDAS X such as image data two or three dimensional gridded data two dimensional gridded data sets e g output of numerical models which is usually much more granular than the image data and other single dimension data types such as time series etc The exact implementation of the different formats are dependent on the native operating system but McIDAS X provides a transparent and a common interface between the applications software and the native operating system The basic file system is called the Large Word array or LW format Both the digital image data and the grid data formats are based on the LW file system For both the gridded and the image data sets a directory service is provided to query the contents of the file McIDAS eXplorer uses certain extensions for planetary applications which are compatible with McIDAS X 2 3 stem Status As McIDAS X is a multiprocessing environment several application programs can be executed simultaneously The respective output can be directed to separate text windows or files Some of the applications such as multispectral classification of large images require significant processing time even on fastest workstations It is useful in such instances to determine the active applications A command SHFT provides a current snapshot of the processing load at any instance and an abort mechanism also exists to abort a user process from withi
176. g is twofold first McIDAS expects a valid time for the data stored in an area and one might as well tag the data with the most appropriate time possible and second the time helps distinguish between the three different cycles on which radar data were acquired and also in determining when the altimetry data were likely to have been acquired 2 Navigation information is attached to the area according to the information contained in the PDS label Thus the data when displayed can be overlaid with a map grid remapped into another projection composited etc 3 The MIDR data have already been corrected for the radar scattering function through the Muhleman scattering law The radar reflectivity can be computed from the digital data if the incidence angle is known at that location GETMGN stores the incidence angle table associated with each tile in the area so that the radar reflectivity can be computed on demand For C3 MIDR data however the incidence angle tables are not available and these data cannot be directly calibrated to radar reflectivity 4 MGNORB can be used to plot the Magellan orbit tracks on a displayed MIDR image to depict the nadir track or either the left or right look angle track that passes closest to a point indicated by the cursor position By assuming nominal orbital elements MGNORB also returns the orbit number on which the data were acquired accurate to within 1 or two orbit periods This is useful to determine t
177. geometry and on the onentation of the tit A much more severe siope of 4 8 mrad which might exist in the upper atmosphere at the boundary of the polar caps Pollack et al 1990 J GEOPHYS RES 95 1447 1473 and where most occultations of Mars Observer are expected ta occur could bias the temperature profiles by up to 3 2 Kelvins for an orbit opening of 30 degrees if such ettects were neglected Our approach in modeling the titts has been to assume the local atmosphere to be spnerically symmetne but with a ditterent cemer of symmetry This approach is satisfactory tor the case in which the ray penapsis doss not vary too much in lattude and fongtuce dunng the coursa of an occuttation Results from the NASA Ames GCM tor Mars suggest that honzontal vanations in pressure are much more severe across lattude than they are across longrude An axially symmetric figure of revolution should be a bener model for the shape of the Martian polar atmosphere than is a large scale tik The currem approach incorporates errors due to imprecise knowledge about the location of the transmmter the recever and the cemer of the occuring planet and is not restncted to any specitic occultation geometry 11 15 P McIDAS eXplorer A Vehicle for Analysis of Solar System Data S S Limaye L A Sromovsky R Krauss E Wright D Santek P Fry Spac Sci amp Eng Ctr Univ of Wisconsin Madison and R S Saunders JPL McIDAS eXplorer is a software environment
178. geometry the telescope optics projected into the focal plane at which the vidicon resided These reseau locations are found by keyin RF Voyager reseau finder The next entry contains the actual digital data values for the image arranged line by line with no record separators The length of the DATA block is computed using values within the area directory entry Word 34 of the area directory is the byte offset to the start of the DATA block within the file Image data stored in a McIDAS digital area is organized in a two dimensional array of lines and elements Each pixel in an area has a line number starting with zero at the top and an element number starting with zero on the left side of the line This line element number pair defines a coordinate system called the area coordinates for the elements in the area Note that the pixel count for areas but not for images or frames starts at zero not at one The line and element counting for images and frames 15 arbitrary and must be specified in words 6 and 7 of the area directory All McIDAS applications software must use this convention Finally after the image data we have a trailing entry which contains ASCII data that more fully identifies the data source and stores time stamped comments and notes from all applications programs or from the user using eXplorer audit trail utility keyin LISTAUD This provides an audit trail of variable length giving a full history of the processing Becaus
179. ges from WF PC camera on HST area_ This program is of limited interest because the actual alignment of the four component CCD chips is not precisely known and is significantly different from the handbook values and worse the calibrations of the four CCD s cannot be matched to each other making the exercise practically useless With the pending replacement of the WF PC camera the four chip format will be replaced with a single 800 x 800 CCD APPENDIX 48 IDMOON Interactive Mcidas Explorer routine to identify the shadows transit locations and relative positions of galilean moons from observer The user may also use the positions of the moons in the image to calculate the appropriate north angle and the pixel diameter of the primary pixel degree ratio is based on the pixel diameter of the primary IDMOON SCAN CUR default or BRIGHT REMARKS This routine requires a precise time of observation U T in the area to produce correct results If the user elects to calculate the north angle and pixel diameter for the image body he she may use either the cursor position to identify the moon or use a center of brightness scan over the domain of the cursor The routine will then display the moon name at the chosen position on the display and output the calculated north angle and pixel diameter of the primary This routine is designed to allow a user to predict the approximate position of Galilean moons in an image The image m
180. h image on frame 2 This sequence is useful for making mosaics from Magellan framelets or tiles Loz Hardcopy Text or Image output There are several ways of obtaining hardcopy text and image gray scale or color output from McIDAS X The simplest means of obtaining a print copy of the McIDAS command output is to use the redirect capability offered by the DEV keyword The output can be directed either directly to the workstation printer or to a file simply by appending any command by DEV P or DEV E filename respectively The text file can then be printed from the X window by any of the methods Note that this file is an LW file which really means that it lacks the carriage return LineFeed sequence and must be converted to a DOS or a text file by using DOSTOLW command and then sent to the printer One possible is to use enscript In the McIDAS Command Window DOSTOLW filename text_file OS enscript 2rG filename which will print the file as facing pages in the landscape format If a complete log of the McIDAS work session is desired user key ins and the McIDAS output can be also be copied to a log file using the TFILE command to open and close the log files at appropriate times as desired TFILE OPEN filename TFILE CLOSE The file can then be printed as before from the X window using the operating system commands A third means is to use a screen capture device to print out the screen display which may or may not incl
181. h of images of Venus from Galileo and for several weeks each year from the Pioneer Venus Orbiter At the other extreme we have the radar investigation of the surface of Venus from Magellan at a resolution of 120 meters providing mapping of a planet that is unmatched even by the data available about our own planet due to difficulties of mapping the ocean bottom 1 2 What is McIDAS Very briefly McIDAS provides a multiprocessing software and hardware environment for multiframe display and analysis of and interactive access to any multi dimensional data Data are rendered onto the two dimensional display device of the user workstation on as many frames as the hardware capabilities allow A user interface allows as many analysis tasks as practical limited by the workstation resources and animation Currently three different flavors of McIDAS are supported by SSEC They are McIDAS MVS that runs on mainframe computers capable of running the MVS operating system IBM or compatibles McIDAS OS2 for IBM compatible personal computers capable of running the OS 2 operating system and McIDAS X for UNIX workstations that support the X windows environment The MVS environment also typically includes satellite data ingestors for earth weather satellite data and a variety of inputs through other communication networks to ingest other types of data such as weather forecast model outputs conventional surface and upper air station data surface radar data lightning
182. hat upon completion the output area contains only the result of projecting the input image The SMOOTH option has two distinct targets The first response flag controls smoothing of the data in the output area by 2 3 1 3 weighting of the nearest two pixels a quick and dirty approximation to bilinear interpolation of the data The second flag controls whether the limb of the image in the output is to be generated without bilinear splines to remove the stair stepping effect caused by the fact that the spline domains span the visible edge of the output image such that some points within the spline domain are actually off the target such as in a full or partial disk of a telescopic image of a planet Regardless of whether a perspective view or a cartographic map projection is being generated the user needs to know and choose a few critical quantities for the projection such as scale of the output image in degrees per pixel or km per pixel the central longitude hemisphere etc The scale and extent of the source image are also important because wrong or incompatible values will result in an unsuitable output If a known photometric function is to be removed from the image at the same time that can be accomplished using the NRMIMG command instead of the REMAP command provided the coefficients for the photometric function are known At present only the Minnaert and the modified Minnaert functions are supported HOW TO GENERATE A THREE COLOR COM
183. he appropriate dark noise frame and the shading file for the specific camera filter combination is available in mcidas data sub directory and write the output in a new area Attach the NAIF provided SPICE kernels to a given EOM ed Voyager frame The frame must be re displayed to activate the navigation Determine the center of a star signature in a displayed image Strip or fuse an area into or from the DDB and image data component files DIRCxxxx and IMAGxxxx where Xxxx is the original 4 digit area number Currently used for data compression experiments Compute the observer and solar sub point locations on a target object using the SPICE kernels for a given date Restore one or more McIDAS area files from tape to disk i e in mcidas data sub directory from a DAT or an Exabyte cartridge written using TPUT Displays the framelets or tiles that make up a Magellan browse image created from C1 MIDR s as a grid pattern and numbers the tiles Normally started by GETMGN during retrieval of browse and full resolution images Will scale the displayed image to the frame size by integer sampling appropriately Lists areas on a tape written by TPUT SCSI tape drives only either DAT or EXABYTE Use TGET to restore data from tape to disk in the u1 mcidas data sub directory Save one or more McIDAS area files from disk to tape i e in mcidas data sub directory Track cloud features in a sequence of images and determine the mean veloci
184. he bottom the text message window to the upper right and the image window is on the left The graphics in the image window can either be independent either graphics or the underlying image can be toggled into view or merged with the base image The status line on the top of the Command Window indicates the current state of the display The GUI interface currently supported makes the use of McIDAS eXplorer easy for novice users An initial tool bar window allows selection of a particular function supported by McIDAS eXplorer Clicking with the mouse button left opens a newer window giving the user other choices that activate specific McIDAS commands and allow solicitation of input for command parameters This interface allows the help to be made available in a context sensitive manner and is independently controllable separate from the command itself and is being developed using the Tk Tcl scripting language An example of this interface is shown in Figure 2 ORIGINAL PAGE OF POOR QUALITY L dAd 0 AD D E N hada tO CE T TEA THAT AA AAO DLS i RET date gt F LELE IES SES TES E LEATA ES EI E K da RS d E KA KK K PPLE RE T E LALA eG P AP H e rent forte E d d d M gt d Z gt gt gt d d d d H Pad gt Pa Y LA d 7 z mA Z A K Z Y pl r 4 4 L gt 7 4 4 z va ed M x Fake Maney TSF Wire Mtatiro i RAAT im gt R N Rilke uno Sop AC G wae
185. he area The directory entries are as follows Data Description Block DDB The Data description block is a collection of numeric data in INTEGER 4 REAL 4 or REAL 8 numeric format that describes the attributes of a digital image stored in a McIDAS eXplorer file called an area These are frequently called metadata about the particular image The DDB as used within McIDAS eXplorer can have different types depending on the source and nature of the image data Typically each instrument has a characteristic set of parameters required for calibration navigation and analysis of the image and a specific type is defined for the corresponding data As many types of DDB can Glossary 6 be defined within McIDAS eXplorer as required and affected McIDAS commands modified as necessary LISTDDB WHERE are two specific commands which list information contained within the DDB and will need to be modified to reflect a new addition of a DDB type Specific formats of the different DDB s currently defined within McIDAS eXplorer are found in the document PLANAREA Data Number Data number generally refers to the raw value corresponding to a point in an image that is converted into a visual brightness For one byte image data the DN and the brightness value are generally the same For 2 byte image data the raw image data can have a value between 32766 and 32766 while the brightness value can only be between 0 and 255 a one byte number due to the video
186. he period when altimetry data could have been obtained on the nadir pass near the selected location 5 FINDALT can be used to determine the ARCDR CD ROM volume on which the altimetry data can be found for a displayed MIDR image E A A A 6 The complete PDS label attached to the browse image or a component tile can be listed for the data imported into an area with the LA area_ FORM AUDIT command 7 LISTDDB ALL command will list the same information as interpreted and used by McIDAS eXplorer 8 When a superbrowse area is created the brightness data are dynamically stretched based on the histograms so that the output area will have a nearly uniform contrast over all the component browselets Magellan Radar Altimeter Data on Venus surface Use GETALT to import data from PDS CD ROM volumes ARCDR_2001 ARCDR 2015 Note that these are the only non imaging data that are imported from the CD ROM volumes by McIDAS eXplorer GETALT allows the user to examine any of the 22 quantities available for each altimeter footprint For a single footprint all 22 can be listed on the screen or saved to a file GETALT will also provide a listing of all of these quantities for a given range of footprints along the orbit track in two files containing the first 11 and the last 11 variables respectively Typically one of eight selected quantities can be plot as an overlay graph on a displayed MIDR or a GxDR image The output file is an simple text file with a
187. hen ephemeris information should be recomputed for consistency using the REDONAV command If the ephemeris data are contained in the FITS label these may be used in lieu of the NAIF computations Please refer to the User Guide for more information on the use of REDONAV command Please see Generic Navigation Recipe for Framing Camera Images 4 7 The attached navigation can be examined by displaying the latitude longitude grid as drawn by the MAP command and or using the E key to list the coordinates for a point in the image at the cursor location Co ordinate transformations and zenith angles for points in the target image can be performed for individual points using the LISZEN command Cartographic projections can also be used to verify the navigation by remapping the source image into one of the many possible projections using either the AAMAP command or a combination of the MAKOUT MAKNAV or PLANAV and REMAP commands described elsewhere in this document HOW TO NAVIGATE VIKING ORBITER IMAGES OF MARS At present these images cannot be navigated or processed due to lack of calibration and SEDR data The processing required for these images is similar to that required for the images from the Mariner 10 and Voyager imaging systems namely the photometric and geometric distortion need to be removed Both of these steps require the respective calibration files which are not yet available within McIDAS eXplorer HOW TO NAVIGATE SPIN SCAN PIONEER
188. hotometric function combining multiple areas in some fashion etc IMGPRO and MC commands allow multiple areas to be arithmetically manipulated to create a new output area HOW TO OBTAIN INFORMATION ABOUT AN IMAGE AREA Each image stored in area files in McIDAS eXplorer contain a header record that describes the data Unlike the FITS format this header is in binary format and meant for system use A utility command allows the header information to be printed on demand as text The image data are followed by text records that document the processing history of that image Generally all the supplementary information present in the original data imported into McIDAS eXplorer e g from PDS CD ROM volumes is copied into the 64 word directory the Data Description Block DDB and or the processing history records The directory and the processing history can be listed using the LA command The contents of the DDB can be listed with the LISTDDB command and the audit trail that informs which commands have altered the area in some manner can be listed with LISTAUD LISTDDB area_ default area number is the area corresponding to the image displayed on the current frame LISTAUD area_ 4 19 default area number is the area corresponding to the image displayed on the current frame LA area default area number is the area corresponding to the image displayed on the current frame A quick one line text summary of the contents of one or m
189. ible whereas the the latter is not The compressed file is given a different name Use DECOMP to decompress the data The directory and DDB attached to the area is left untouched Fit a general conic to a set of points stored in a limb points file created using the key in LIMBPT Primarily useful for planet center determination if the pointing data is accessible Constrained fits are also used if the planet orientation and size are known Import tabular data into a database format Assumed that a separate file specifying the structure and field names is available Use DBL to search the database created List specified fields from a database file Database utility program A utility to insert entries into the Data Description Block or copy the entries from DDB for one area into the DDB for another area Decompress an image compressed by the COMP command and write the output in a new area Display a frame i e load the digital image data from an area onto a McIDAS display frame Various coodinate and scaling options are available to control the exact registration and resolution of the image within the frame This is a core McIDAS command The displayed frame s navigation can be displayed by overlaying the map or latitude longitude outlines with the MAP command A version of DF for the 24 bit version of McIDAS bp 24 option when starting a McIDAS session that allows 3 color composites DF3 will load a given frame in a specified color Red
190. ication is based on the Data Description Block DDB attached to the image area word 263 contains the NAIF id value The physical parameters for the object are obtained from a call to the eXplorer subroutine BODCON and allows for differentiating between radii for solid surface and different atmospheric levels for objects bearing extended atmospheres ASTAT The ASTAT command allows the user to obtain statistics on the digital data distribution in a portion of the area or the whole image one band at a time The area portion can either be an arbitrary closed outline or a box defined by the cursor location For more information please see the command reference IMGTS When a time series of digital data variation over a limited area at a fixed location in the image needs to be compiled from digital areas IMGTS is useful After it is compiled the time series data can also be shown as a plot For more information on how use this command please see the command reference HOW TO DIGITALLY FILTER AN IMAGE FILTER FILTER is a general application program to digitally manipulate the spatial frequencies in an image by means of a variety of digital filtering options has been 4 13 developed The object is to provide access to all The options to apply filters to images include the ones more commonly used such as High Pass Low Pass Laplacian Sobel Edge detection Smoothing and Median frequency filters Other options such as Fourier Kalman and
191. ide The syntax of the commands keyword explanations and examples are given along with some explanatory remarks A separate document containing etailed output from typical sessions is planned This manual can also be viewed on line from within McIDAS eXplorer using the EXPDOC command PLEASE READ MCIDAS commands accept both positional parameters as well as keyword values as inputs In this document the required positional parameters are indicated in italics Any KEYWORDS if needed or specified should be specified in upper case only unless explicitly Stated In general the keywords should follow the positional parameters Any global keywords e g DEV N or DEV P should be the last parameters on the command line A common positional parameter is the area_number for the image to be manipulates and is generally indicated by area_ If the result of the Operation is another area then the intial area may be indicated by source_area_ or input_area_ and similarly the result is indicated by destination_area_ or output_area_ In some cases the operation is performed on the image being viewed If the command is designed for Such use most are then the area number is not generally necessary APPENDIX 2 ANGLE Determine the north angle for a Jupiter image by measuring the tilt angle of the zones and belts for earth based images for which the north angle is not independently known ANGLE Parameters None Use the curso
192. ified They can be forced to other values by the user For Venus use VENUS SFC 297 or VENUS CLOUDS 298 diam Planet diameter in pixels default is LINES 50 radius Planet equatorial radius km ecc Planet eccentricity oblateness parameter 1 a 2 b 2 ANGLE north nadir na_azim north Spin axis tilt deg clockwise from vert def 0 0 nadir off_axis tilt of optic axis from planet to Spacecraft translation vector nadir angle na_azim Rotation angle of nadir angle about optic axis VIEWPOINT lat lon dist lat Planetocentric latitude at s c subpoint default 0 0 lon Planetocentric longitude at s c subpoint default 0 0 dist Distance s c to planet center in RADIUS def 10 0 DIST 1 000 is at planet or cloudtop surface Infinite distance yields orthographic projection LINE Line in area to put subpoint default area LINES 2 20 ELE Pixel in area to put subpoint default area ELES 2 SUN sub_sun_lat sub_sun_longitude DIRECTORY ss yyddd hhmmss yyddd Image day amp year default is current day amp year hhmmss Image time default is current time If the area exists prior to PLANAV call the existing SS YYDDD HHMMSS will be used as defaults ss MciDAS Spacecraft ID Default 50 REPLACE NAV NO AREA REPLACE NO merely generates CRT output of the navigation parameters default is REPLACE NO with default NAV 128 just lists nav NAV REPLACE NAV replaces only current nav block for area AR
193. ify a moon in an image of Jupiter and or use its position to determine the north angle as well as the image pixel scale Determine the center of a planetary image for which limb points have been written to a file LIMBxxxx where xxxx is the area using the LIMBPT command or any other process if the file conforms to the format by using a general conic fit The image center the two axes the orientation of the ellipse and the eccentricity of the ellipse are returned These values can be used in the PLANAV key in to attach navigation to an image e g ground based for which SPICE kernels may not be available if applicable Annotate a displayed frame with the day and time of acquisition default location is upper right hand corner This is useful for images which may be videotaped or published compile or display a file containing a time series of data from digital areas List area directory entries Compared to WHERE LA provides less information in a compact format Locate the planet s bright limb interactively using directional derivatives from displayed image and store the points in a file Primarily useful for planet center determination CONFIT for the purpose of image navigation Determines the limb location using the maximum local brightness gradient method and write the locations in a file LIMBxxxx where xxxx is the four digit area number Usually a first step in image navigation see IMGCTR and PLANAV Plot radial scans of da
194. ill Note that BODCON constants are based on the pck00003 tpc file except when more current data has been available in scientific literature APPENDIX 77 PLAEDG Find or list limb points in a displayed planet image or area calculate a best fit planet center and store the data with the area Gradients are calculated in vertical and horizontal at each pixel and the largest average gradient above the GRAD threshold is taken as the limb point PLAEDG area_ NUM PLAEDG area_ BOX YES NUM PLAEDG area_ BLOB mindn maxdn Iskip ieskip NUM PLAEDG area_ POINT GRAD LIN ELE NUM PLAEDG LIST Lists limb points for current area NOTES 1 If keyword BLOB is specified center of brightness and DN bounds are used to compute search limits for LIN amp ELE 2 lf BOX YES the box bounds define search limits gt AREA specification is optional if a displayed frame exists on which to plot limb points 4 area_ must be gt 30 if specified as a positional parameter to search for points def displayed area for frame in which case the first positional parameter is treated as a limb point number 5 If AREA is specified as keyword then it may be any valid area 1 9999 6 POINT 0 to FIND MULTIPLE limb points in area default gt O 7 To find a SINGLE limb point on the line LIN Jin added after last valid limb point found so number may be lowered on graphics overlay 8 POINT lt 0 to delete a SINGLE limb point KEYWO
195. image The Voyager calibration of shade corrected images then is reduced to converting the 2 byte data numbers into physical units which is a simple linear process with proper constants The amount of data required for geometric calibration is much smaller and the calibration block in the DDB for Voyager images in the eXplorer format is used to store these data These data are the position of some fiducial marks reseaus which are etched on the faceplate of the Voyager Mariner and Vikling cameras Keyin RF finds reseaus in Mariner and Voyager images and places a set of nominal or found reseaus at the end of the calibration block These reseaus are used by the GEOM keyin to produce a remapped image which has geometry very close to that of the focal plane image in the camera For the PDS solar system imaging data the eXplorer software generally reads the attached PDS labels and extracts the required calibration information and stores it in the DDB The same is also true for the attached navigation information Some data such as the map projected Magellan radar imagery of Venus must be calibrated using incidence angles related to the orbit data A single calibration block designed for a framing camera with a small number of pixels is not adequate for a large radar image mosaic We will provide special McIDAS eXp keyins to generate reflectivity and altitude maps from CD ROM data in the same scale and projection as the radar imagery Then it will be
196. imilar to that of other framing camera images First find the limb points using LIMBPT or BRTCEN If necessary edit the limb points file interactively with LIMBPT first assign the command LIMBPT DEL to a function key position the cursor over the points to be deleted and press that function key to invoke the command Next determine the image center using the IMGCTR command Use REDONAYV to update the navigation for ephemeris and the center or RENAVF to update the image center image coordinates only Usually the epehemeris data sub earth or sub observer point and the sub solar point on the target object in the target object s native reference frame and the range of the observer are computed using the NAIF toolkit corresponding to the date time entries attached to the image area It is assumed that these quantities refer to the time of acquisition of the data and are UTC values and not refer to any local time zone For spacecraft data available on PDS CD ROM volumes usually there is no ambiguity about the observation time However the earth based data read from FITS files may contain the observation time in any time zone Worse often the local time zone may not be noted in the FITS label and it if is the difference between the local time and UT may be ambiguous Also the one way light time correction may have to be applied for some observations If the observation date and or time are updated as can be done using the CA command t
197. ine of observer zenith angle cosine of solar zenith angle and a constant If the actual target behaves as a Minnaert surface then the plot of Ip vs ppo on a log log scale should be a straight line with Io determined from the intercept and 8 being the slope of the linear fit The applicability of the law is thus self evident over the puo limits by the linearity of the distribution and can be determined from the image either by least squares regression or by a robust fit The quality of the linear fit is given by the regression coefficient or by the mean absolute deviation of the robust fit MINFIT uses this scheme to determine the Minnaert coefficients intercept slope and measure of the quality of the fit by both methods If the image is perfect devoid of any noise then the regression and the robust fits will generally be very close Most imaging instruments however contain some systematic and or random noise an example is the presence of the reseau marks or their residue in Voyager images To the degree that such noise is present in the image data the regression and robust fits will differ somewhat with the robust fit being generally superior MINFIT stores the Minnaert coefficients and those for other photometric functions in the DDB for that image NRMIMG looks in those locations for removal of the brightness variation if the Minnaert Law is being used for removing the photometric function from the data as described be
198. ith SU option set up and use a transfer function file for displaving two byte images in McIDAS on a 8 bit display Then the core McIDAS keyin EB can be used to further adjust contrast and dynamic range linearly in the display Color composite images in McIDAS eXp require 24 bits per pixel as well as a 24 bit display such as the Silicon Graphics Indigo DA Part two consists of 1024 4 byte words 4096 bytes suitable for up to 10 bits pixel resolution in a lookup table of 4 byte floating point or scaled integer radiance values This transfer function is appropriate for doing calculations with physical quantities instead of DN values The McIDAS core D keyin is modified in McIDAS eXp so the table lookup or analytic conversion from DN to physical values is always done in the appropriate way for the data being displayed Thus when an 8 bit Magellan tile is displayed for example it 1s possible to obtain the latitude longitude alti tude orbit number incidence angle and radar reflectivity plus others for any pixel in the displayed image using the D keyin 3 Part three contains space for a set of 202 REAL 4 line clement reseau locations 1616 bytes Mariner and Voyager class spacecraft used vidicon sensors with electron beam readout subject to variable distortions from electromagnetic fields the spacecraft passed through The image geometry was preserved by etching reseau marks on the glass vidicon faceplate so one could reconstruct the exact
199. itude and longitude the distance of the observer from the target object the field of view of the instrument the number of lines and elements in the image or equivalently the pixel size in line and element directions and the orientation of the target object in the image where is the target object s North direction Much of this information is usually contained in the text labels attached to the image data and the importing programs try to decode it If the labels are in non standard format or if the information is missing the following key ins will allow the user to create the required navigation Finding the Limb Points and Image Center The limb points can be found by BRTCEN EDGES or LIMBPT commands The limb points can be edited using LIMBPT command The image center and the quality of the limb point fit can be examined using IMGCTR command without attaching the navigation information and should be used for testing the limb fits Specifying the Image Center Use NAVUTIL to specify the image center if known by other means Using the Target Image Center for Navigation Use IMGNAV To be combined from REDONAV and RENAVF to recompute the navigation from the specified center Until IMGNAV is ready use RENAVF to accomplish Re computing the Sub observer and Sub solar point data Usually the importing program will compute these data for the time of observation UT If that time is changed then IMGNAV REDONAV until IMGNAV is release
200. king EDR data are stored on the CD ROM s in a loss less compressed format without any other processing such as radiometric or geometric calibration In order to use these images for any quantitative analysis such processing must first be performed on the images At present the required programs or files for performing these steps do not exist within McIDAS eXplorer The Viking images can be imported into McIDAS eXplorer using the GETVO command Processed Viking images are also available on a set of CD ROM s through the USGS as Mars Digital Image Models These disks contain cartographic projections of the Viking data which have been pieced together and stored as sub sections of a global map These individual images can be imported into the McIDAS eXplorer environment using the GETMDIM command 3 13 AM SKO MARS SFC Figure 3 7 Example of a polar stereographic projection view of the Mars North polar region retrieved from one of the MDIM s displayed with a latitude longitude grid 3 14 Ze A T m v tran o aas lt we i 4 L U 3 15 HOW TO IMPORT DIGITAL IMAGES INTO MCIDAS eXplorer Before any image can be displayed or manipulated within McIDAS eXplorer it must first be imported into its database which usually resides in the default mcidas data sub directory on a workstation The process of importing the image creates an area directory and a Data Description Block DDB that contain informatio
201. l gt Instrument R 8 tape CDROM 572 589 3x3 Rot Matrix Inertial gt PicBody Cent R 8 SPICE Kernels etc 591 592 Tilt Angle of Optic Axis R 8 593 594 Azimuth Angle of Optic Axis R 8 595 600 S C Position Vector Picture Body Fixed R 8 RSC X Y 2 601 602 Sub S C Planetocentric Latitude R 8 RSC LAT 603 604 Sub S C Planetocentric Longitude R 8 RSC LON 605 606 Sin of half angle subtended by equat axis R 8 SINALP 607 608 Width to Height Pixel Ratio R 8 Ratio gt 0 609 614 Sun Position Vector Picture Body Fixed R 8 RSOL X Y Z 615 616 Sub Sol Planetocentric Latitude R 8 RSOL LAT 617 618 Sub Sol Planetocentric Longitude R 8 RSOL LON 619 624 Earth Position Unit Vector S C to Earth R 8 625 640 Spare 5 15 m m a s Bee r s s bk ce Po ge e f m TE UP rr r m A err m rap f p me drs i gg m mas de m mais g ger mr re r mr ee ae rrr r w m t ee rr P ee roy mn ma r m m es ee mr mas ie deia res WORD ITEM S C Image amp Instrument TYPE 131 132 Data Type S C Image Data Mapped c 8 RAW S C Raw Spacecraft Image 800x800 PROC S C Processed Spacecraft Image MAP PROJ Map Projection MOSAIC Mosaic 133 Spacecraft ID NAIF Code 1 4 134 Instrument 1D NAIF Code 1 4 135 136 Instrument ID c 8 137 138 Picture ID 1 FDS Cre 139 141 Picture ID 2 PICNO C 12 142 Picture Time Year I 4 143 Picture Time Day I 4 144 Month I 4 145 146 Picture Time hh mm ss c 8 147 Frame Size Pixels in scan direction I 4 14
202. lag ROLLOFF Parameters area area containing navigation block to be updated NCFF no center find flag 0 or any other number This parameter if non zero forces program to use planet center coor dinates already in the navigation block rather than perform a best fit to the bright limb points stored in the navigation block i e it forces the planet center position KEYWORDS ROLLOFF roll offset correction subtracted from north angle as determined from optical navigation by determination of the actual roll north angle by referencing a star or a satellite and noting the difference from the SEDR value of the north angle EXAMPLES CALCMA updates matrix for area last accessed CALCMA 1022 1 forces planet center for area 1022 will default to area last accessed APPENDIX I 10 CHANGECD Unmount mount a CD ROm volume in the UNIX workstation s CD ROM reader CHANGECD Remarks Most UNIX systems require that CD ROM volumes be mounted before they can be used to read data CHANGECD command makes this process simpler by allowing the user to unmount and mount a CD in the reader APPENDIX 11 CLEAN Remove Shot Noise and Line Dropouts from Images CLEAN nput_area output_area frame_ option threshold_DN DN_gradient Parameters input_area source area that contains the image of interest output_area new area to be written threshold_DN brightness above the neighbouring pixels beyond which pixel clas
203. lan orbit track on PDS CD ROM Volumes MG 2001 through MG _ 2015 Digital images stored in files in McIDAS or McIDAS eXplorer format are called areas The digital image data are preceded by a binary header called the area directory that contains information about image data image navigation and calibration The files are generically named AREAxxxx where xxxx is a 4 digit left zero padded integer number On a given system only 9999 areas can be resident in the default data sub directory mcidas data Additional areas following the same naming convention can exist on other sub directories where they are accessible to McIDAS commands by setting the proper path with the REDIRECT command The same numbered areas in different sub directories cannot be accessed simultaneously because the ROUTE command will accept only the first path for a given area Thus accessing both areas is possible by resetting the path with the ROUTE command for each area for each use The offsets for each of these quantities are flexible and are contained in the directory McIDAS eXplorer areas also contain a Data Description Block immediately following the 64 word directory that contains additional information about the target object contained in the image the imaging geometry as well as the details of the imaging instrument The image data is followed by an ASCII label that includes any text labels originally present information as to whether the image was importe
204. line element Default values are 1 1 Source_lines _source_ele respectively REMARKS Bilin does area subsection blowup blowdown using bilinear interpolation on pixel value vs pixel location currently max box size is 800 x 800 The routine may also be used to correct images with non square pixels e g many of the amateur telscopic images are acquired with Lynx or other cameras which have rectangular pixels Rendering the pixels square simplifies the navigation by not having to propagate the pixel aspect ratio throughout the navigation Examples 1 Project an image area 1111 with 165 lines by 192 pixels into a square field area 9999 BILIN 1111 9999 ASPECT 165 192 2 Magnify the same area 1 75 times BILIN 1111 9999 ASPECT X X 1 75 APPENDIX 1 5 BLEMEDIT An interactive program for editing blemishes in a displayed image The image data within the cursor are replaced by a bi linear average of the data in a larger box surrounding the cursor BLEMEDIT line ele BLEMEDIT FILE REMARKS The cursor size can be changed using the CUR key in to contain the blemish but the margin around it that defines the larger box cannot be changed except by exiting the command The cursor is placed over the blemish and a mouseclick then performs the data replacement Clicking the middle and the right mouse keys terminates the program If the blemish locations are previously known the command can be executed in the bat
205. list below These commands are in addition to the core McIDAS X commands supported Many of these commands can also be accessed via the eXplorer GUI and the core McIDAS GUI s AA ANGLE ASTAT AVG2D BILIN BLEMEDIT BOTSIM BROWSE BRTCEN CALCMA Copy an area containing image data to another This is a core McIDAS command Determine the north angle i e the orientation of the spin axis of Jupiter in an image by determining the slope of the zones and belts from cursor selected points on the zone belt boundary Useful when the north angle must be estimated from the image Measure image statistics from a displayed image e g histograms outlines etc Average multiple areas 1 or 2 bytes per pixel perform n x n averaging of data about each point and write the resulting output in a 2 byte per pixel area Useful for averaging Voyager dark frames Enlarge Reduce and image by any arbitrary scale factor s real or integer in either direction by bilinear interpolation Edit blemishes interactively in a displayed image by replacing the data within the cursor with a spatially weighted average of points within a larger box Navigate simultaneous Wide Angle Narrow Angle Voyager Image pair with one of them navigated Normally called by GETMGN BROWSE is designed for Magellan MIDR browse image files It calls DF to scale the MIDR browse image to the current frame and displays the 7rows x 8 column tile grid to identiffy th
206. lite data during the 1970 s when there was a dearth of adequate hardware and software tools While specific hardware elements are a key part of McIDAS it is primarily the suite of software tools that has made it particularly useful in national and international operational weather facilities for integrating vastly different data weather sources and providing a coherent access to the user Many of these capabilities are also applicable to the analysis of the planetary data returned by NASA s solar system missions of the past Viking Voyager Magellan current such as Galileo and Mars Observer and future such as and Cassini or the Pluto Fast Flyby However because of the different nature of the data and target objects many adaptations or modifications are necessary McIDAS eXplorer constitutes these adaptations and includes other specific tools for analysis of the planetary data This document is intended as a companion document to the McIDAS X or McIDAS OS2 User Guides For the most part however the need for documents is rare as majority of planetary data manipulation needs are addressed in this volume 1 1 Planetary Image Data While it may appear that the remote sensing data such as images returned from LANDSAT or SPOT satellites and data from weather satellites have much in common and hence the same analysis tools e g many of the Geographic Information Systems packages can suffice the differences between the two are apparent in the way thes
207. log for clarity band def current frame calibration units def original from area BRIT RAW RAD or TEMP ylo yhi xlo xhi modify x and y scales to new values Draws a line plot on the graphics of the data along the line at an azimuth of from the scan direction 135 deg and a distance of 200 pixels from the planet center to the planet center Only the first 100 pixels along that line from the point are to be plot The derivative of this profile is displayed in the right panel Three files are also created that contain the profile data LIMPRO LOGPRO and DERPRO These files are tagged by the FDS count and the scan end image co ordinates LIMPRO RAD 135 200 SCALE 10 1000 0 100 APPENDIX 55 LISCOM Lists contents of PLAN navigation common from navigation blocks LISCOM area CUR COD biknum LISCOM area CUR COD bikname LISCOM area CUR COD lists all blocks in CURRENT or CODICIL LISCOM area default is COD and all blocks NOTE All three parameters are positional only no keywords are used in this command Block Numbers blknum and Names blkname 1 SECTID Image identification 2 COMMVN Image geometry input 3 NAVVEC Navigation input 4 VNEDGE Bright limb points 5 VNTERM Terminator points 6 MOSTIE Mosaic link points to frames 7 MISLEN Odds amp ends 8 VNCOMM Navigation output constants 9 A Inverse navigation matrix 10 B Navigation matrix and vector 11 D Inverse vector 12 SQUASH Obla
208. low Hapke Photometric Function The determination of Hapke Photometric function parameters from a planetary image is under development Buratti Photometric Function The determination of the Buratti photometric function parameters is under development HOW TO REMOVE THE PHOTOMETRIC FUNCTION FROM AN IMAGE OF A PLANET OR A MOON NRMIMG NRMIMG removes the limb darkening due to scattering geometry variations using the Minnaert law Ideally the normalization of brightness should be done as a multiplicative process However the inadequacies of a good scattering model lead to some anomalies in the output brightness at high zenith angles For cosmetic reasons an additive correction is applied in NRMIMG such that the departure from the predicted intensity in the original image is added back to a constant brightness The output image can be contrast stretched linearly during this process The Minnaert coefficients are picked up from the DDB for the source area and can be overridden by specifying them on the command line NRMIMG source_area dest_area spline_size FUNCTION MINN intcpt slope Minnaert Photometric Function The Minnaert photometric function default can be specified in the NRMIMG command with the FUNCTION keyword The Minnaert fit parameters slope and intercept can be picked up from the source area s DDB if they previously have been computed and stored Otherwise they can be specified as second and third parameters of the FUNCTION k
209. ly most commands are task oriented and execute an operation once Since McIDAS is a multiprocessing environment in itself user always has the option of starting other processes via the command window while one is executing or via GUI or function keys Some commands however are interactive and require user attention via mouse button clicks or occasionally key board input A few commands are memory resident which remain active until the user either explicitly terminates them or they time out A command may or may not have any arguments have positional parameters or keywords or both The positional parameters are generally restricted to certain obvious situations but that is peculiar to the programmer while keywords are used to specify other specific inputs Such keywords are used by typing the keyword exactly ALWAYS in upper case followed by a comma or the equality sign followed by the value A keyword may accept as few as one or as many as 32 values entered consecutively on the command line The McIDAS eXplorer commands are expected to check the specified keywords for validity if any are misspelled or extraneous to the command an error message is printed out and the process is not executed The keywords come in two varieties global and command specific The global keywords are generally recognized system wide and share some commonality in use Examples are DAY and TIME or DEVice Generally the global keywords require only the fir
210. m deviation in pixels to discriminate between valid limb points and possible erroneous limb points default 5 REMARKS An unconstrained general conic fit in the image co ordinates returns the ellipse center major and minor axes eccentricity and the tilt with respect to the line direction The positive x axis is along the increasing line direction and the positive y axis is along the increasing element direction This is useful for navigating full disk earth based telescopic images of solar system objects using PLANAV if the sub earth point is known The format of the LIMBxxxx files is as follows It is a fixed length file 4001 words with the zeroeth word denoting the maximum index number of limb points stored in the file 4 byte binary integer The next 2000 words contain REAL 4 line numbers x coordinate of limb points and the next 2000 words contain the corresponding element positions of the limb points y coordinate The slots may not all contain valid limb points as some limb points may have been edited out Only non zero entries are taken as acceptable limb points either axis APPENDIX 50 IMGDAY Write the day and time corresponding to a displayed image on the graphics in a given size at a specified location Useful for annotation of frames being animated for videotaping IMGDAY area_ graphics_frame_ TV SIZE PARAMETERS area_ area number whose day time will be used to tag Default is area corresponding to
211. macro command In the three color mode the frame directory will eventually contain information about all three bands or areas being displayed The D key and the OD command will also list the digital data values for all three displayed bands Multispectral classification is a means of determining cross spectral spatial relationships in the image data It is an extension of the object of pattern recognition in a given image to the spectral domain Generally used in earth remote sensing applications such as crop analysis or mineral survey spectral classification is equally applicable to the solar system data if concurrent multi color imaging data are available e g Voyager multi color images of Jupiter which are near concurrent or Viking orbiter images of Mars surface For the purpose of classification it is not necessary that the data be obtained by an imaging instrument they could be processed data from a combination of sources or numerical models e g gravity and topography data composited from Magellan data The assumption is that there are only a discrete number of groups in which the features in a given area will fall into based on their spectral characteristics Classification can be accomplished in a number of ways Two common methods are unsupervised classification and supervised classification The latter requires some ground truth data and training sets For planetary applications this is not readily possible so far and onl
212. mages of Venus surface the Pioneer Venus Orbiter Cloud Photopolarimeter and Galileo images of Venus can be calibrated shading and geometry and navigated Support for other data products such as those from the Clementine Mars 94 and Cassini missions should also be possible once the data are available Support for navigation of irregular objects such as asteroids and the smaller moons and ring systems will be a o added as resources permit Once these data are imported within McIDAS eXplorer they can be gridded map projected animated brightness February 1994 lt Information Systems Newsletter a pal A at R L Y ime 16 36 Image Y 93356 normalized and filtered Three color composites and multispectral classifications of up to six bands are possible Calibrated and navigated image data can be used for areal cloud motion and other measurements using general tools Figure 2 shows an example of an Earth based telescopic image of Jupiter with an overlay latitude longitude grid and a view of some of the GUIs available Figure 3 shows a line plot between two arbitrary points in a Magellan SAR frame that shows the variation of the radar reflectivity dB along the path between those two points McIDAS eXplorer requires a copy of McIDAS X which is licensed by the Space Science and Engineering Center at the University of Wisconsin Madison For further information contact the author at 608 262 954 sanjaylO ssec wisc ed
213. mber can be specified following the first one if the same coordinate is to be converted for a consecutive range of areas all areas need not be present APPENDIX 60 LOCATE Identify the geographic locations on a displayed image by a graphic symbol as overlay graphics As an option the names of the locations can be annoated on the graphics in a specified font size The font type can be externally selected using the XFONTS command LOCATE filename symbol fontsize filename text file contaning the latitude and longitude locations symbol any key board character to be plot fontsize size of the symbol 1 gt n gt 99 REMARKS This comme 2 is useful when a large number of locations are to be identified on i e displated image The annotations are made only on the overlaid graphics display and do not affect the digital area containing the image data For a very small number of points the annotation can be accomplished using the PC E and ZA commands APPENDIX 61 LODSSP Display a single planetary image or a sequence of planetary images from a block of areas such that the center of the planetary disk is in the center of the frame Useful for registering a sequence of earth based or far encounter images for looping LODSSP first_area last_area frame_ magnification PARAMETERS first_area first area to display last_area last area to display total number of areas to be displayed should not exceed the number
214. mes Obtaining the software The general Explorer modules and the GEMVIS modules for Explorer or AVS men tioned above may be freely obtained from the anonymous ftp server at the National Center for Supercomputing Applications The address is ftp ncsa uiuc edu and the directory is SGI PATHFINDER Please see the README files there for additional information For additional information the Mosaic URL is http redrock ncsa uiuc edwPATHFINDER aisrp93 talk title html For other questions contact Robert Wilhelmson at 217 244 6833 McIDAS eXplorer A Tool for ines bald S saat S Data 7 G lt aa L Z aada aa Z A es gt Ii xe O y Sanjay Limaye Space Science amp Engineering Center SSEC University of Wisconsin Madison McIDAS eXplorer is an extension of McIDAS the Man Computer Interactive Data Access System an environment for analyzing weather data Besides the eXplorer version McIDAS Currently exists in three different flavors McIDAS X for X Windows under UNLX the version upon which the eXplorer has been primarily developed McIDAS OS 2 for the OS 2 operating system largely compatible with the UNIX version and McIDAS MVS for older mainframe computers using the MVS operating system Here when only the term McIDAS is used the reference is to capabilities in all flavors of McIDAS and when a suffix is used the text refers to the capabilities of that specific ver
215. meters area_ frame_ opt loc_x loc_y mag KEYWORDS COLOR BAND REMARKS Area to be displayed Frame_ to display the Area on Coordinate option E or A x coordinate to load at y coordinate to load at magnification factor ve for blowups negative for blowdowns Red Green or Blue Area band_ if it is a multibanded area A macro command DFC is available to load all three bands at once The format is identical to DF3 except that all three bands are specified with the RGB keyword instead of COLOR keyword APPENDIX 19 DS TNC E DSTNCE DSTNCE DSTNCE DSTNCE DSTNCE DSTNCE DSTNCE where opt is one of none CIR ROT STE E T PARAMETERS angle din distance inc lat lon line ele raster pictel KEYWORDS COLOR SIZE SYM UNIT Cuu my e e a eee eee eee Measure linear distances on a navigated and displayed planetary image optionally plot range circles for a given distance in km nm or miles on the displayed image opt CIR angle inc distance ROT angle inc distance STE angle din distance E fat lon fine ele T raster pictel measure distance between a pair of points or continuous segments indicated by mouse Clicks draw a circle around the initial cursor location beginning at a specified distance and angle draw all or part of a circle around the initial cursor location beginning at a specified distance and angle step the cursor away from
216. n CDPATH in string table must be CD ROM is assumed mounted as cdrom using the UNIX commands mountcd and or umountcd in the directory lut mcidas bin KEYWORDS FF 0 extracts 8 blowdown of entire mosaic default 1 56 extracts numbered 1024 x 1024 framelet CUR identifies framelet from displayed browse image ALL extracts all 56 framelets into 56 consecutive areas starting at designated area AREA nnnn AREA area number to wtite the image into between 1 and 9999 REQUIRED def 0 FRAMELET Any framelet number 0 56 0 means extract blowdown same as FF above DIRECTORY Any secondary directory in cdrom in the 8 byte format ciLLnNOOO where LL latitude and OOO longitude Remember that DIRECTORY and FILE NAME are case sensitive Also if FRAMELET is used DIRECTORY must be used CDPATH string table path including directory in which desired framelet cifFF resides e g TE cdrom c1XXnXXX this must be a blank string e g TE if the FILE NAME in the keyin includes the path since the FILE NAME is appended to CDPATH before the CD ROM files are opened Examples GETMGN AREA 23 FF 0 DIRECTORY c130n333 GETMGN AREA 1211 FF 23 DIRECTORY c110n130 GETMGN AREA 20 cdrom c130n333 c1f23 APPENDIX I 41 REMARKS This command is planned to be improved so that it stays resident if the browse frame is requested so that by indicating with mouse clicks the individual tiles or framele
217. n it is only necessary that the geometric distortion be removed Rather than work in virtual object 4 6 space where the distortion is accounted for on the fly McIDAS eXplorer assumes that the image to be navigated has already been processed GEOM command GEOM key in creates a new dataset or a new area in McIDAS parlance leaving the original area alone For GEOM to produce a reasonable looking output from images that either have excessive random noise or data compression gaps Uranus and Neptune encounters some preprocessing is generally desirable to correct for them CLEAN and FILLO are two commands that accomplish these tasks for the Voyager images If the image is to be used for any photometric measurements it should be processed with the SHADE9 key in to remove vidicon shading before removing the geometric distortion Finally the RF command finds the reseau locations in the Voyager images that are needed by the GEOM command RESEAU key in can be used to list or plot the found as weil as nominal and object space locations of the reseau marks in the Voyager images Note that the FIL_0 command also performs another task it strips off the 24 by te line prefix in the area that is not used by eXplorer commands and whose presence is sometimes problematic for some of the older McIDAS key ins in that the prefix presence can influence the data addressing HOW TO NAVIGATE EARTH BASED TELESCOPIC IMAGES OF PLANETS The procedure is s
218. n the data rate Since the NAIF SPICE kernels are computed for the FDS time this results in a an ambigous kernel set for the wide angle BOTSIM frame The SEDR information is actually more reliable in this instance Example SPICENAV OPT UPDATE 10 10 move the calculated center up 10 lines 10 elements right with no rotation APPENDIX i 93 STAR Determine the location of a star in an image in a region defined by the cursor Several options are availabel to determine the center center of brightness within the cursor edge detection or a brightness shape profile STAR AREA SKY KEYWORDS AREA Area number of the displayed frame SKY Brightness value for the background sky REMARKS The location of a star or a planetary moon if the image signature is small enough_ is frequently needed for the purpose of optical navigation The star signatures in most planetary image data do not appear as points but as bright blobs against a noisy background This command estimates the center of this signature as the best guess for the star location APPENDIX 94 TGET Restore one or more McIDAS area files from tape to disk i e in mcidas data sub directory from a DAT or an Exabyte cartridge winten using TPUT TGET ftarea1 tarea2 darea DEVNUM tarea beginning tape area required tarea2 ending tape area DEFAULT tarea1 darea beginning tape area required KEYWORDS DEVNUM i DEFAULT 0 REMARKS TPUT writ
219. n McIDAS X followed by the process identification number in the Command window An inventory of the data imported into McIDAS eXplorer is obtainable using WHERE and LA commands in condensed text form and visually as thumbnail images using the SCANA command SCANM a memory resident command allows some limited operations to be performed on the data areas displayed in a browse frame created by SCANA key in interactively y KAU it DES 2 LBA TAS p r j sabe PST Ss a H OT sree 515 CITE TO 2 sn ed GL ava Sup ak RRE MN DTU DSE YZ SLE UR LOT UT Pop hiret oN TUERTO A ON IPSS SU ams Wea coke WET ASLE THSRE IS IDEAS DIA 2itenmta Woo Ble dd 2934b AS PAS Cults nifa rks PEL LE ROZAS N NT E DP CE one E G S L RATA Wey aces gt Y 741 IEA OT Sar S AAA E EIT TITI KILT 7 FTT w 3 IBGE BOS Y 7 712 vnnt xi YT PLT AGELIS PAR hemp DES D FERR TES T vee ter ands K CU H PETE ENE N Ohne FORT TLE AT tices 14 KSE STE yor 22 Bias 25341 22 Mepit OD peer IS X es PEER cr o OLAN NANT IAN KSA PAORA DA ORERE ASI S VES YNOM ORK E SIN AS RES e ES AS TRUN F eae L SIT Wee ter E Posy K MCB LT Z E QA PESSI UG ELE bos 2430 IS KLL we RF PAN A be Fed SAAR AAA ADA RAAT KARAN A Figure 2 2 Example of a display for a browse area seated using SCANA to graen the area contents Practically as many as 400 images can be viewed in this format and used as an index to the eXplorer data contents 2 4 Scheduler McIDAS X has a schedul
220. n about the image source acquiring instrument imaging geometry or navigation information digital data calibration i e the conversion of the raw data units into some known physical units and brightness levels as well as any text descriptors As the source spacecraft and imaging instruments differ widely in their characteristics as well as in the exact format in which the images are stored McIDAS eXplorer has a selection of commands written specifically for certain known data types which are present in the PDS CD ROM collection There is also one general command which will read images with a FITS header e g earth based telescope images or HST WF PC images If the image is not in any of the recognizable formats it may only be possible to display and manipulate it without the abiiity to perform native reference frame navigation and calibration of the data The known data types and the commands that import those data are For most of the imaging data on PDS CD ROM volumes the McIDAS eXplorer commands allow the user to create or import browse mode images as well as import the full resolution images into the eXplorer environment When the full resolution data are imported the accompanying navigation and calibration information as well as the full PDS label are imported and attached to the data In general the task of importing or browsing the data is easily accomplished through the GUI provided but can also be performed readily from the command win
221. n scheme when not in use 3 1 4 Image Navigation Image navigation is the process of relating the image co ordinates of a feature to their planetary coordinates or vice versa For the Voyager images this step does not have the po tential to add photometric noise to the image However the procedures to bring out subtle image features such as color composites or image normalization require a precise navigation Thus navigation can indirectly add photometric noise to the processed image if the scattering angles are imprecisely or incorrectly computed There are two separate means of accomplishing the image navigation The simplest is to use the NAIF SPICE kernels if available The second is to utilize the SEDR information and determine the image center using constrained or unconstrained fit s to the bright limb as described below 3 1 5 Center Finding For objects whose surface is obscured by clouds such as Titan or the gaseous planets with no fixed surface features the navigation process relies on the observing geometry the camera characteristics and the physical shape of the object The first task is to determine the location of the center of apparent disk of the target object This is readily done for a spherical object by determining the position of the distinct gt eriphery of the object the bright limb Since the solid surface is not being imaged for most f Voyager data the visible limb does not have a sharp edge characterized by
222. n the image coordinates Thus if a sequence of images is displayed with the same image coordinates for all the frames the target image will in general move from frame to frame To discern any change in the images the human eye requires that the target image be frozen in the frame This can be done when the coordinates of the target image center which is coincident with the sub observer point on the target for far encounter observations for each frame are known LODSSP is a macro command that obtains the image center or more specifically the sub spacecraft point location from the DDB for each image and displays each image on successive frames such that this point is always at the same frame coordinate The default location is the frame center Optionally the images can be permanently registered in this manner by exporting them to new areas using LODSSP The images can be either magnified or scaled down by an integer factor for display or for exporting to a new area in which the image is centered This is an efficient means of creating an aligned sequence of images which all have the image center at a fixed area relative address assuming the areas are all the same size 4 11 NAVUTIL Frequently there is a need to modify some of the parameters used for navigation particularly for earth based images An example is when the planet image center line and element coordinates is known from some other means such as offset from a known star rathe
223. natural coordinate system Planetary Coordinates Latitude and longitude Unless the target object is Earth the latitude is planetocentric For spherical objects the planetographic and planetocentric systems are one and the same NAVUTIL command can be used to change between palnetary and celestial coordinate systems Satellite instrument coordinates see image coordinates above Window coordinates Under the X windows system the display buffer can be located anywhere in the window In X windows the cursor is software generated and can be positioned within the display using mouse movements McIDAS uses this cursor for the purpose of locating image coordinates upon demand The cursor type can be set to cross hair open box filled box and open box with cross hair X11Release 5 restricts the maximum cursor size to 63 lines by 63 elements The cursor type size and color can be selected using the CUR command D is a single letter command that lists the digital value of the image data at the cursor location in raw and calibrated units The OD command lists the data within the cursor in specified units Data within McIDAS implies digital information accessible to the McIDAS system that can be displayed as an image or displayed as a profile or listed as an observation Thus the data can be station data a profile or a two or multidimensional image Data Directory For each area a 64 word directory is used to identify the contents of t
224. nction Key 10 F 3 ASK1 area Which Area ASK1 frame Which Frame Solicit Input ASKI mag Magnification DF area frame X X X mag F 4 EB F 5 EU LIST ASK1 table Which Enhancement Table to Retore EU REST ftable F 6 ASKI table Name for the Table EU SAVE table 5 DATA STRUCTURES FOR MCIDAS EXPLORER INTRODUCTION In McIDAS Man computer Interactive Data Access System image data is stored in a data file called an area McIDAS areas contain 1 header blocks containing bookkeeping information which is needed for linking to all the McIDAS commands or keyins which manipulate the image data 2 the image data and 3 an audit trail showing the successive keyins which have been applied to massage and manipulate the image data This document describes the area file structure for planetary imagery analysis within the McIDAS X Unix X Windows environment The planetary image analvsis system built on top of McIDAS X is called McIDAS eXplorer or McIDAS lt Xp The current version of this documentation is stored in a plain ASCII text file called mcidas exp PLANAREA and can be read online by the McIDAS eXp keyin EXPDOC i e EXPDOC PLANAREA McIDAS is maintained by the University of Wisconsin Space Science and Engineering Center SSEC with support from the McIDAS Users Group MUG One of the aspects of McIDAS eXp philosophy is that if processing documentation travels with a data source on CD ROM or on tape fil
225. nd to execute the Batch file A third means is to compile a macro command that can accept both Standard FORTRAN statements for flow control and McIDAS commands and then execute that macro command MCIDAS is a multiprocessing environment on all platforms with the number of processes limited only by the available resources A typical UNIX workstation with 32 Mbytes of and a capable video board memory can run a McIDAS session with 16 frames of 1024 x 1024 in the full color mode A high end workstation can support multiple McIDAS sessions either on the same workstation or via X terminals It is even possible to network a number of workstations in a ring and share the data At the low end we have recently ported McIDAS to an Intel 486 DX2 66 MHz based PC equipped with a local bus video display card and a CD ROM drive and running the UNIXWARE operating system Except for the number of concurrent users Supported such a workstation is capable of being a satisfactory workstation for the individual scientist MCIDAS eXplorer has been developed under support from NASA s Applied Information Systems Branch Limaye S S L A Sromovsky R Krauss E Wright D Santek S Gorski and R S Saunders A Vehicle for a Analysis of Solar System Data NASA Science Information Systems Newsletter Issue 30 October 1993 in press S Suomi Wills Rds fos Sits Dima and Wi Smith doses A Modern Interactive Data Access and Analysis System McIDAS III J Clim
226. nding on the encountered planet so that the pointing of the camera system can be up dated particularly the roll angle APPENDIX 92 SPICENAV tility to calculate the position of an Voyager 2 with respect to a target body via the SPICE SP kemels retrieve the C pointing matrix from the SPICE C kernel and calculate inertial frame to body centered frame rotation matrix for the target body at image time These values are then written to the DDB for access by the nvxspce dim navigation routine The utility may also be used to fine tune the C matrix to improve the accuracy of the navigation SPICENAV area_number default displayed_image OP T option no default KEYWORD OPT UPDATE ine_adjust element_adjust roll_adjust in degrees Applies small rotations to an existing C matrix to translate or rotate the expected center of the picture body to better fit the data image After the new matrix is calculated the user may either replace tbe existing matrix with the new or store the new in the users section of the DDB REMARKS This routine may not return the correct state information for Voyager wide angle narrow angle cameras data if the data was obtained during a simultaneous narrow wide camera exposure The FDS number of both images should in principle be the same However because the narrow angle frame is always the first one read out the wide angle frame gets tagged with a later time stamp or FDS number where the delay depends o
227. ndow Unless the workstation is logged onto a host McIDAS CPU all commands are executed locally When the workstation is logged on to a host McIDAS CPU the commands can be executed either locally or on the host CPU Currently obsolete It used to display the image coordinates of the cursor now folded into E keyin Image frame graphics frame toggle It is not available in McIDAS X unless the independent graphics are running Toggle the image display on or off When it is off the display is set to black and cannot be set to any other color Any graphics if drawn and displayed remain visible Start and stop animation of frames within the frame loop set by LB or LS commands If viewing a single frame L starts animation and the next L stops it The frame dwell rate can be changed in units of 1 15th of a second using the DR command from 1 15th of a second DR 1 to as long as desired Different dwells can be specified for each frame in the loop If the workstation has insufficient memory for the number of frames activated then the animation may seem sluggish and the frames may drag for the faster animations The only solution then is to reduce the required display memory or upgrade the workstation CPU either by reducing the number of frames or by reducing their sizes Switch to opposite frame The specified number of frames is split evenly into two groups a displayed frame and its opposite Thus frames 1 and 3 and frames
228. ng viewed on a specific frame mcidas_command EXAMPLE SCANE WHERE AREA DF 5 This assumes that the frame being viewed corresponds to the SCANA area Choose a particular thumbnail image in that frame and click the right mouse button The output of the WHERE command corresponding to that area is displayed in the text window and displayed on frame 1 APPENDIX 1 90 SEDRIN Reformat SEDR data into navigation block for raw image SEDRIN area fds sedrfile target camera REPLACE Program will attempt to pick up all parameters from the area or displayed frame If navigation information already exists for the image the program will halt Use Kevin PLANAV to view the information SEDRIN stores in the navigation blocks for an area EXAMPLE SEDRIN 465 will search for a SEDR entry consistent with information stored with the image in area 465 SEDRIN 465 FDS 4386645 REPLACE YES repeat search with user specified FDS number KEYWORDS REPLACE YES Forces rewrites of navigation block for area AREA Area number to add navigation def displayed frame If navigation data already exists for the area the REPLACE YES keyword must be used FDS FDS number WITHOUT embedded decimal point a range of acceptable values may be specified to adjust for varied data rates since SEDR entries are given in starting FDS counts not ending counts Defaults to word 20 in area directory _SEDRFILE VGR1J VGR2J VGR1S VGR2S VG
229. ngle cameras data if the data was obtained during a simultaneous narrow wide camera exposure The FDS number of both images should match but this is not usually the case The fit made to the limb point data is an UNCONSTRAINED fit USE IMGCTR to perform a constrained fit APPENDIX I 71 NAMES Lists plots Planetary Feature names on displayed images Currently the name is GEOB and contains only the Venus database MIDR Mosaic Image Data Record Lists all features only LAT minlat maxlat LON minion maxion Selects features in region for plotting Features crossing 0 longitude must use 180 0 lt LOW lt 0 0 Default search bounds are LAT 90 0 90 0 LON 0 0 360 0 name searches for all feature name fragment matches P Plot all features on displayed MIDR image PLOT Plot all features on displayed MIDR image REMARKS There are 592 features named on Venus too many for a sceen printout to use DEV PPP to get a permanent listing if lat lon bounds aren t used or do a search using names or name fragments case sensitive to reduce number of features returned The names are stored in a file called geo tab on each MIDR CD ROM volume APPENDIX I 72 NAVUTIL Utility to list and or modify selected entries in an areas data DATA DESCRIPTION BLOCK DDB and audit trail intact NAVUTIL AREA area_number KEYWORDS NAVUTIL will list the current DDB values Defaults area_number area corresponding to current
230. nsion default 297 0 DEC Declination default 18 1 COLOR Plot color 3 is default TSIZE Text size default is 6 4 SIZE Star search region size default is current cursor size LIST 0 1 2 Generates more debugging output 0 is default These Keywords may be stored in the string table by using the TE command APPENDIX i 83 REDISP Re display an image being viewed such that it is centered in the McIDAS image display window over a point identifed by the cursor location on a specifed frame at a specified integer magnification or a blow down factor REDISP frame_ magnification frame_ where to display the frame mag blow up or blow down factor non zero integer ve for a blow up ve for a blow down REMARKS The area corresponding to the image to be re displayed must not have been quit APPENDIX 84 RESEAU Lists and or plots reseau data for Voyager spacecraft RESEAU option coord spcft camera KEYWORDS option LIST Lists coordinates on crt or DEV P S BOTH lists coordinates and plots on graphics May be abbreviated to L P OR B coord NOM OBJ OR FND Default is FND for raw images OBJ for GEOMED images May be abbreviated to N O OR F spcft A VOYAGER 1 B VOYAGER 2 def current frame camera WIDE or NARROW angle def current frame May be abbreviated to yy OR N KEYWORDS AREA Area number for FND reseau marks found reseaus are st
231. nvironment under OS 2 2 1 Thus any high end graphics card that has drivers for OS 2 2 1 can be used for running McIDAS on any bus microchannel ISA EISA or the local bus variants VL and PCI HIGHLIGHTS E Gy Cap e a ATA OC e NN T ES cR ER A GET e HR E DIT 0 NS mor o os ese O o RE l Sa E 3 Nicolle Zellner demonstrating McIDAS eXplorer to Nancy Chanover NMSU A Sanchez La Vega Spain and K Rages NASA Ames at the 25th DPS Meeting in Boulder October 1993 Co Investigator L Sromovsky is at right Major highlights of this last year include the successful demonstration of the eXplorer software environment at the 25th Lunar and Planetary Science Conference held in Houston March 14 18 1994 and at the 25th Meeting of the Division of Planetary Sciences in Boulder Colorado during November 1993 An abstract describing eXplorer software has been submitted for the DPS meeting to be held in November 1994 in Washington D C where it is anticipated that a workstation demonstration will also be held We demonstrated McIDAS eXplorer capabilities on a Silicon Graphics Indigo Extreme at both the meetings At LPSC the workstation which was set up in the exhibit area at the Lunar and Planetary Science Institute adjacent to the Johnson Space Center in Houston for the duration of the meeting Previously McIDAS eXplorer was demonstrated at the AISRP Workshor in Boulder Colorado during August 1993 An article describing eXpl
232. o the current cursor s position and size note the BOX keyword can be used to override the default cursor size 5 Lat Lon values may be entered in either a DDD xxx format or a DDD MM SS format 6 The program will display a time series of all LW file entries up to a maximum of 5000 7 The program can be set to screen for a user defined range of pixel values using MAX MIN keywords to define the upper and lower limits 8 The program calculates the LW entries for a ange of areas and stores them in the LW file in the order that the areas are sequenced regardless of the area s date and time 9 The program is designed to order the LW entires before it plots their time series from lowest to highest date APPENDIX 53 LIMBPT Program to determine the limb points from an area containing a planetary image for finding the center for the purpose of image navigation Particularly useful for ground based telescopic images of the planets as no navigation data are required either for EDGES or for IMGCTR Parameters option FIN ADD DEL PLT LIS KEYWORDS DER DER DER Remarks one of the following Find limb points from a displayed image and create a new limb points file to store the points and display them on the graphics frame Append more limb points to an existing file Delete limb points for locations within the cursor from the limb points file and erase them from the graphics display not in Mc DAS X Plot
233. of frames available for display No check is performed to verify this excees areas are not displayed i frame_ first frame to show load the first area on magnification blow up or blow down factors ve or ve integers respectively REMARKS This is a useful command to display a sequence of registered images for animation or for verifying the consistency of navigation between two or more frames in terms of center finding The program queries the navigation to determine where the sub spacecraft point is located in the image and uses the DF command to display using the EC option For close encounter images the disk center is usually not likely to be in the image but outside of it hence the display may look blank if a blow down factor is not specified such that the sub point is actually within the frame dimensions APPENDIX I 62 LINPLT LINPLT Display the data along a segment of a displayed image as a X Y plot The segment can be along an image line two arbitray points or restricted to the width of the cursor and along the line where the cursor center is located option KEYWORDS Parameter option KEYWORDS COLOR PLOT BAND UNIT UNIT SCALE Remarks Examples LP CUR LP SEG none to plot data along the line where cursor is located SEG a line segment of the image CUR a line plot using data through center of cursor color def 3 plot type SLD DOT or any ASCII char def SLD band def current frame
234. of the cameras was determined by measuring the output brightness level in terms of data numbers DN s for nine exposures for each filter and a coefficient determined for each pixel of the image that describes the response of the vidicon for the input brightness at for a given filter at that pixel and saved as a shading file Thus given an image that is exposed at an exposure within the bounds of the shading files the expected brightness at each pixel of the image can be interpolated from the actual vidicon response and the shading coefficients RZ T HUM 1 91 t 1800 ENUI ial E aed L as LINE PLOT o are RIA zo 320 nan apn s60 Ban 770 BDA A Si ie SS ALAT NA A A O TET T gY ero 21 NAAA Ty BT E AN N ITH ITE T apb SRB SRE BRB O P20 Figure 3 2 An example of a Voyager 2 Wide Angle camera dark frame A line plot across the image along line 800 shows the variation of the background brightness level The signature of the reseau marks is readily apparent The shading correction files are voluminous occupying nearly 12 mbytes per filter Their names are of type VGRnXm where n is 1 or 2 indicating Voyager 1 or 2 spacecraft X is the camera identifier N for narrow angle camera and W for wide angle camera and m denotes the filter number on that camera between 0 and 7 These files are normally expected in the default data sub directory They may be compressed to only about 24 of their original size using a loss less compressio
235. olarimetry Data These multispectral observations are available on tapes from NSSDC in a roll by roll format but with a significant difference The pixels are already navigated Because of the very low spatial resolution of these data an image can be created by two dimensional interpolation of the polarimetry mode data in a particular map projection 3 3 MAGELLAN IMAGES OF VENUS SURFACE AND ALTIMETRY DATA Magellan data is the largest component of the PDS CD ROM data with nearly 130 volumes of radar imagery of Venus surface and 15 volumes of nadir altimetry and radar reflectivity data on the Venus surface These two data can be linked in a displayed frame There are also two CD ROM volumes containing a global mosaic of the radar altimetry and radiometry data There are separate McIDAS eXplorer commands to import these data for analysis The radar images require no further systematic processing as the required processing has already been performed The only exception is if the radar reflectivity in calibrated units is required in which case a special command converts the image from raw data units into calibrated units The radar images are stored in three different formats as components of a global maps The individual components are mapped in a sinusoidal projection and are available at three different resolutions Each CD ROM volume also contains a 8 X reduced resolution browse frame to provide a larger context for a specific geographic loca
236. om space probes are limited One of the goals of the development of McIDAS eXplorer has been to provide a unified approach to the analysis of the target dependent data by accounting for the differences in their physical characteristics such as size shape etc To this end the Navigation Ancillary Information Facility s NAIF at JPL approach of assigning a unique identification tag to each object and spacecraft for that matter is adopted within McIDAS eXplorer with some enhancements Although McIDAS eXplorer is general enough to be utilized for most types of data its strength is in analysis of multispectral images or data that can be visualized as a two dimen sional image McIDAS eXplorer also has tools for analysis of atmospheric data such as temperature profiles which although are one dimensional individually are typically available globally for planets such as Mars Venus and of course earth The Infrared Radiometer Inter ferometer Spectrometer IRIS instrument on Voyager 1 and 2 provides spectra for the giant planets from which temperature profiles have been derived Object Identification The NAIF software developed at JPL uses an identification number for each solar system object for ephemeris purposes This same number is used within McIDAS eXplorer but with a small modification This identification process serves another purpose besides naming the object in the image it is used to retrieve the object s physical constants radii
237. omputed Rot Matrix Inertial gt PicBody R 8 432 433 Computed Optic Axis RA R 8 7 434 435 Computed Optic Axis Decl R 8 ls 436 Minnaert Fit Constant Max DN Used 1 4 437 Minnaert Fit Constant Calc Slope R 4 438 Minnaert Fit Constant Calc Intercept R 4 439 Minnaert Fit Constant Mean Abs Dev R 4 440 441 Picture Body Center Line R 8 If avaiable and 442 443 Picture Body Center Element R 8 necessary 444 445 Pixel Diameter of Picture Body R 8 446 447 Navigation Status 76 448 449 Navigation System Type CX D 450 451 Image Navigation Processing Status c 8 452 460 Spare WORD ITEM Supplementary Information TYPE COMMENTS 461 462 Supplementary Block Type Cres SUPL VGR 463 465 Data Source CD ROM Volume tape name CARE Satellite 4 Shadow Positions Star Locations Rings 5 17 133 Spacecraft ID ii ee d ee ee ee eee ee ee m ee m ee mr ee eee m ee eee e ee eee ee re eee ee ee drar ee eee ee eee ee ee eee ee ba S C Image amp Instrument 131 132 Data Type S C Image Data Mapped da FEEL CS 5 PES MIDR 134 Instrument ID NAIF Code 135 136 Instrument ID Name 137 138 139 140 141 142 143 144 145 146 147 148 149 150 Poi oe 133 182 Image Type Picture Location Tile or Framelet Number Number of First Orbit Number of Last Orbit First First First First Frame Frame Side Looking Direction Spare Orbit Ascending Node Orbit Ascending Node Orbit Ascending Node Orbit Ascending Node
238. on keys available on most workstations are named KEYF1 through KEYF12 and can be programmed using the TE command with a specific command e g E E pr ARE T KEYFI WHERE FRAME 1 4 Anytime the function key F1 is pressed the programmed command is executed It is also possible to assign multiple commands to a single key by separating them by a semi colon TE KEYF10 WHERE AREA 100 110 LISTDDB 10 05 Is cdrom Pressing the F10 key will initiate the sequential execution of the four commands assigned to that key and will first provide the McIDAS processor status list contents of areas 100 through 110 list the Data Description Block DDB for area 10 and send a command to the native Operating system to list the directory of the cdrom directory 2 8 Environment Table An environment table capability enables keyword parameters to be passed to commands that use that keyword The environment table basically consists of keywords used by McIDAS commands which can be assigned values using the TE command A McIDAS command will read this table to scan if any of the keywords used in that command exist in the table and use the value assigned if the keyword exists in the table If the keyword is also entered via the key board as part of the command then that value takes precedence over the environment table value TE DAY 79006 If the LA command is then entered from the keyboard with a certain range of area numbers to list then only the ones
239. on other labels such as VICAR labels as well as processing history and other mission specific labels or information McIDAS eXplorer tools to import the PDS data from CD ROM s in general will include the complete text label associated with each image file and also extract a set to encode into the DDB so that McIDAS eXplorer commands can use that information easily As work proceeds this approach will be adapted for other data types McIDAS eXplorer adheres to the general McIDAS X conventions for the file system Thus the data ingested normally reside in the mcidas data directory and the source is in mcidas sre directory etc Specific formats for storing and accessing the data are specified under McIDAS X such as image data two or three dimensional gridded data two dimen sional gridded data sets e g output of numerical models which is usually coarser than the image data and other single dimension data types such as time series etc The exact imple mentation of the different formats is dependent on the native operating system but McIDAS X provides a transparent and a common interface between the applications software and the native operating system The basic file system is called the Large Word array or LW format Both the digital image data and the grid data formats are based on the LW file system For both the gridded and the image data sets a directory service is provided to query the contents of the file McIDAS eXplorer uses certain exten
240. ond to the frame size so the index area can be displayed at full resolution SIZE lines elems set the size of the destination area in lines and elements def display line x display elem See comment about the GRID above POS position type image positioning ABS absolute REL relative def LABEL itype Itype tabel for each thumbnail one from AREA area number nnnn def e 9999 TIME time of image hh mm e 12 01 BAND band number bb ie 08 DAY date of image dd mm yy ie 4 NOV 93 JDAY date of image yyddd ie 93287 MEMO memo field from area 1 32 characters what ever fits TYPE satellite type 12 characters from sss code in area text plain text 12 characters not any of the above BAND bands specify band s to display or ALL for all bands def first band in channel map MISS brit specify the brightness value 0 255 used for missing data def 128 OPTS opt opt set program options from the choice below APPENDIX 87 Notes REMARKS GF FX HS SF Group Filter gt splits the dynamic brightness range between the source range groups Aspect Ratio Fill gt keep origional image aspect ratio Fill All gt best fit image to grid Histogram Stretch gt stretch the brightness range using the histogram of the data Set to image frame if IMA keyword is entered BAND uses range format described above example BAND 1 12 15 gt bands 1 through 12 and 15
241. ons such as digital enhancements filters Cartographic projections graphical overlays color composites McIDAS eXplorer is a multi processing environment and can run as many applications or user sessions as practical under the computing memory and peripheral storage resources availble Batch processing is supported as is the ability to create or use different user interfaces such as a function key te piate a graphical user interface or the command window A simple macro facility allows quick creation of specific command sequences that are used repititively In order to fully exploit the navigation calibration display and animation capabilities of McIDAS eXplorer the data are first imported into McIDAS eXplorer along with all available navigation and calibration data and stored in the workstation in a specific format Processing history records are kept for each image imported along with the entire text label that the image was tagged with e g the PDS or the VICAR label The supplementary calibration information for the radar images to convert raw data numbers into radar reflectivity is accessible to the system such that while roaming with the use of a mouse controllec cursor in a displayed image the full calibrated and navigated data can be retrieved at the cursor location These capabilities will be demonstrated on Magellan data at the conference APPENDIX II Copy of an article published in the February 1994 issue of the Scienc
242. onsuming as it requires a table interpolation at each point along the path to add back the angular dependence of the returned radar signal which was removed when the data were rendered as images If the image displayed is navigated then the physical distance along the path is expressed in km or meters as appropriate otherwise the distance is given in image pixels The default line plot is along the line at which the cursor is located The position parameters SEG and CUR allow the data to be examined along a path between two arbitrary points within the displayed image or along within the cursor limits along the line passing through the line where the cursor is located HOW TO ENHANCE AN IMAGE The appearance of an image as displayed can be controlled based on the digital data values that get translated into screen brightness This translation takes place internally in a look up table that assigns an output brightness level in each of the three colors red green and blue output of the display for the input image data Manipulating this table is the process of enhancement of an image and affects only the appearance on the display and not the actual data stored in the area Note that the appearance of the image can be changed in other ways such as by digitally modifying the data in some manner as well as spatial filtering In McIDAS eXplorer however the term enhancement is restricted to changing the look up table There is one look up table
243. ore areas or frames source spacecraft target object unique image identifiers can be obtained using the WHERE command as follows WHERE AREA begin area end area or WHERE FRAME begin _frame_ last_frame_ will annotate the displayed frames WHERE LIMB begin_ frame last_frame_ will list the areas images for which a limb points file is present HOW TO MAP PROJECT IMAGES Assuming that an area containing a navigated image exists a new area containing a view of that image in a different cartographic projection or a map can be generated If the source image is to be flattened or brightness normalized by removing the gradual shading due to the illumination and viewing geometry via a known photometric function at the same time please refer to the section for NRMIMG How to remove the photometric function for additional information The first task is to set up a destination area in which to write the Output projection There are three steps necessary create an output area attach proper navigation and create the required projected image In many cases a macro command AAMAP may be used to generate a few simple projections For other projections or assembly of composite or global mosaics the three steps can be used successively as described later Projections such as rectilinear polar stereographic or Mercator can be created using AAMAP when the image scale as well as latitude and longitude of the center of the output image are known b
244. ored with area calibration RANGE sets a min max range of reseau marks to use in plotting range must be COLOR a reseau box amp label colors defaults 1 2 HEIGHT height of reseau box label default 5 EXAMPLES RESEAU Plots reseaus on the current displayed frame RESEAU PN Plots nominal reseaus on the displayed frame RESEAU P RANGE 20 40 COLOR 3 3 Plots reseaus 20 40 in yellow APPENDIX 85 RE Locate reseaus in a Voyager image so that the vidicon geometric distortion can be removed using GEOM command area_ area_ RES RBEG REND TOL X XX BOX 15 NOM NO ZERO GEOM YES NO KEYWORDS AREA RES TOL BOX NOM ZERO GEOM UnGEOMed area in which to find reseaus required nt n2 Reseau number range Default is RES 1 202 x d Threshold displacement from polynomial fit above which reseaus will be adjusted to line up along line with neighbors default is TOL 0 6 so all reseaus deviating from polynomial by more than 0 6 pixels will be shifted n Maximum box size within which to search for a reseaux centered at its nominal position YES NO to file nominal reseau locations instead of the fitted locations default NO This implies reseaus are being found well beyond their nominal locations and we are having trouble fitting to specified tolerance The image may be of poor quality and the reseaus cannot be easily located in noisy or low contrast dark noise backgrounds YES default
245. orer was publishec in the NASA Information Systems Newsletter February 1994 cm e ea ie as ba A tory e Sie Saas Peo E T N GE E S erate McIDAS eXplorer being demonstrated to Jim Dodge of NASA s Office of Mission to Planet Earth at the AISRP Workshop held in Boulder August 3 6 1993 by Sanjay Limaye PI Onlookers include Bob Krauss and David Santek of SSEC left and front center who participated in the eXplorer development Photograph by Sandy Dueck JPL K an David Santek explains eXplorer capabilities at the LPSC conference in Houston using the poster display set up adjacent to the workstation in the exhibit area at LPI Q DO O ras Co Investigator Steve Saunders looks on while eXplorer capabilities for Magellan data are demonstrated on the SGI workstation at the LPSC conference above McIDAS eXplorer at the 25th LPSC Meeting Copies of the abstracts of papers describing McIDAS eXplorer are attached in Appendix I A copy of the article that describes McIDAS eXplorer is attached in Appendix II Finally the final version of the McIDAS eXplorer User Manual is attached separately as part of this report Acknowledgements Many individuals contirbuted to the development of McIDAS eXplorer Mr Robert Krauss Mr Edward Wright wrote a significant amount of code System support was provided by Mr Patrick Fry and Mr Steven rader Mr David Santek and Ms Sue Gorski assisted with core M
246. osition upper value range limit default 1 0E 35 lower value range limit default 1 0E 35 graphics panel selection 0 1 2 3 4 default 0 full screen NPT AVG STD MIN MAX plotting format options default AVG plot symbol can be any single alphanumeric character or DOT 1x1 box default DOT dispaly title up to 12 characters default blank internal calibration type unit default BRIT x axis label up to 12 characters default X min max div sdiv x axis area file plot parameters y axis label up to 12 characters default Y min max div sdiv y axis area2 file plot parameters where div of divisions sdiv of sub divisions zero pixel value option as MISSing or DATA or can indicate a specific non zero integer as the missing value code default MISS 1 If areas given then the program will calculate the average standard deviation minimum and maximum values for a user specified UNIT calibration type within a user specified target box location and size 2 If no areas given then program will display the selected PLOT option values of the user specified LW file 3 The program appends new values onto the specified Iwfile APPENDIX 52 4 The location and size of the target bex can be defined several different ways using the LAT LON BOX keywords using the LIN ELE BOX keywords using the LIN ELE keywords with double entries representing TV line and element ranges or using no keywords and defaulting t
247. ould appear as early as byte 2816 Spacecraft images occur in several different orms depending on the original data source They can be from framing cameras such as vidicons or solid state detector arrays or from spin scan cameras such as Pioneer They can be map projections or mosaics They can be multiple subsets of all of these as well We describe an image as a sequence of lines arranged each below the previous one and numbered from top to bottom the top line being number 1 Each line consists of a sequence of elements arranged across the line and numbered left to right the left most element being number An element may be an 8 16 or 32 bit quantity depending on the image source and format Most raw images are 8 bits while photometnically corrected images are 16 bits Color composites are normally 24 bits embedded in a 32 bit pixel Raw 10 or 12 bit imagery must be stored in McIDAS areas as two bytes per pixel Radiometricallv corrected images or composite multispectral images may have other formats but are generally limited in McIDAS to 4 bytes per pixel More than 4 bytes requires using the spectral band structure alluded to in the description of the area directory McIDAS data is not fully three dimensional because word 8 of the area directory 15 not currently used but the existing band structure and 32 bit pixels allow for building up layers of two dimensional images This line element numbering scheme determines a pair of
248. oyager 2 Saturn encounter SEDR file A catalog of Voyager 2 Uranus EDR tape cartridges Each cartridge contains 240 images 10 1600 bpi original EDR tapes SP kernel file for Voyager 1 Jupiter encounter limited coverage SP kernel file for Voyager 1 Saturn encounter limted coverage SP kernel file for Voyager 2 Jupiter encounter limited coverage SP kernel file for Voyager 2 Saturn encounter limited coverage SP kernel file for Voyager 2 Uranus encounter complete SP kernel file for Voyager 2 Neptune encounter Voyager 1 narrow angle shading files for filters 1 7 Voyager 1 narrow angle shading files for filters 1 7 Voyager 2 narrow angle shading files for filters 1 7 APPENDIX II 3 vgr2w0 through vgr2w7 verly vgr2 verls vgr2s vgr2u vgr2n Voyager 2 narrow angle shading files for filters 1 7 Extracted Voyager 1 Jupiter encounter SEDR file JPL Extracted Voyager 2 Jupiter encounter SEDR file JPL Extracted Voyager 1 Saturn encounter SEDR file JPL Extracted Voyager 2 Saturn encounter SEDR file JPL Extracted Voyager 2 Uranus encounter file JPL Extracted Voyager 2 Neptune encounter SEDR file In addition SPICE kernel files available from NAIF are required for navigation of Voyager and Galileo images using SPICE kernels APPENDIX II 4 APPENDIX IIT McIDAS eXplorer commands are described briefly below in alphabetical order Some often used core McIDAS commands are also included in the
249. p a call to MAKESU with FRAME set to that frame number Remember to click the mouse in the histogram window to restart the program after the program pauses to let you look at the histogram and transfer function 3 Thereafter you iterate by simply hitting SHIFT amp to recall the previous MAKESU command into the McIDAS command window using the editing keys to modify the parameters The program will continue to reload the displayed frame with each newly generated transfer function till you are satisfied It is best to modify the MAKESU parameters one at a time until one has feel for how the transfer functions are generated Once you understand what is happening you can usually select the proper function and get the parameters you want with three or four iterations within a minute or two APPENDIX 66 MCLIMB Simulate view from orbit of a planet from a nadir looking instrument and plot instrument IFOV s MCLIMB inarea outarea PARAMETERS inarea MAP AREA TO USE outarea OUTPUT AREA WITH ORBIT TRACKS KEYWORDS ECCEN ECCENTRICITY OF ORBIT DEFAULT 0 INCLIN INCLINATION OF ORBIT deg DEFAULT 155 PREC PRECESSION OF ORBIT deg day DEFAULT AUTO ORPSOL CRBITSPERSOL choose 1 DEFAULT 7 PERIOD ORBIT PERIOD l DEFAULT 211 0 2ND PARAMETER UNIT min hr day DEFAULT MIN GRAPH PLOT L LIMB ELLIPSE V VIEW VL VIEW WITH LIMBS B BOTH ALL DEFAULT VL NUMPER NUMBER OF PERIODS DRAWN DEFAULT 1 2ND P
250. p as soon as the multiplicative one at very high solar and viewing zenith angles Cao APPENDIX 1 75 NXTARA Find the first available or free area or a number of areas in the default data directoruy Locates the next available area or a consecutive block of number areas between the start and end area numbers specified default is between 1 and 9999 Useful before importing a lot of images from CD ROMs etc NXTARA number starting_at endging_at PARAMETERS number of free areas to search for default is 1 starting_at first area number to begin search at ending_at last area number to end search for a block number of free areas KEYWORDS FREE Number of free areas to search for BEGIN Starting area number of the range of areas within which find the free area s Default is 1 END Ending area number for the range of areas within which to locate the block of free areas Default 9999 APPENDIX 76 PHYSCON Program to obtain the Physical constants of an object Either the NAIF ID preferred or its name capitalized can be entered Radii and length of day are currently listed PHYSCON naifid PHYSCON OBJECT Parameters naifid the NAIF identificaiton for the solar system object or its name in UPPER CASE OBJECT Ifthe NAIF identification is not known the name of the object can be specified in UPPER CASE Only the first three characters are significant except for PHOBOS and PHOEBE TIT
251. patible personal computers based on Intel 80386 or later processors UNIX workstations and mainframe computers running MVS operating system with SSEC designed and built workstations The existence of a diverse user community implies user support and performance across platforms As the port to the X environment matures the interface is being modernized as more users move to the X Windows environment 1 3 What is McIDAS eXplorer McIDAS eXplorer is a software enhancement package for McIDAS currently only for the X version This is intended to provide support for analysis of planetary data acquired by NASA s numerous solar system missions As the missions to different planets have different instrument systems the planetary data span a large range in terms of data quantity type and global coverage It is neither possible nor desirable to provide support for all types of data The strength of McIDAS is in its ability to interact with satellite data for geophysical applications such as multispectral imagery surface network data and atmospheric soundings To that extent the enhancements described here provide support for planetary image data from missions such as Mariners Vikings Pioneer Voyagers and Magellan as well as from Hubble Space Telescope In addition other planetary data such as Magellan altimetry data Pioneer and Mariner 9 Mars occultation profiles Voyager IRIS can also be accessed and processed The tools developed to ingest the
252. per frame and hence each frame in a McIDAS work session can have a separate enhancement Further because there is only one table per frame the enhancement applies to the entire frame and cannot be restricted to portions of a frame Black and White Enhancement When all three colors are assigned the same output values the result is a black and white enhancement One of the simplest black and white enhancements is linear contrast stretch enhancement which linearly maps the input data range into an output brightness range This can be accomplished by using the EB command in one of two different ways The first way is to invoke EB without any argument the user is then prompted to move the cursor with mouse movements within the displayed frame upon which the look up table is updated in real time The line position of the cursor controls the input range of the image data while the element position controls the output brightness range A mouse click terminates the process leaving the last value of the enhancement table Caution The enhancement is changed only for the frame being displayed when EB is initiated If the display is stepped to another frame while EB is active and the cursor is moved the enhancement table for the original frame will continue to be changed until EB is terminated either deliberately or automatically if the cursor is not moved for a certain duration of time 4 17 A desired enhancement can be saved in a file E
253. planetary applications under USRA CESDIS contract No 5555 08 for the period July 15 1994 July 14 1994 USRA is supported by NASA under contract NAS5 32337 Prior work under the effort has been described in progress reports under USRA CESDIS Contract 550 80 and NASA GSFC Contract NAS5 31347 for the preceding two years respectively A Mci AS eXplorer User Guide has been produced that is the culmination of the work performed under NASA support and is attached to this report This User Guide is intended as a companion volume to the McIDAS X and McIDAS OS 2 Guides The third and final year of McIDAS eXplorer development has concentrated on porting eXplorer code to different operating systems streamlining the installation procedure identifying the operating system and version specific items implementing software revision control for the source code and adding support for some remaining Planetary Data System data products The progress in the last quarter is described below To provide a comprehensive overview the ca pabilities of the McIDAS eXplorer software are also summarized below McIDAS eXplorer User Guide is attached in Appendix I McIDAS eXplorer Overview McIDAS eXplorer consists of FORTRAN and C routines that conform to the McIDAS environment in terms of data structures user interface data navigation and calibration implemen tation For reasons of portability and software maintenance the new code developed strives to adhere to the mode
254. possible to make false color composites as 24 or 32 bit images and display on a Silicon Graphics McIDAS X workstation 5 6 AUDIT TRAIL To keep a history of the processing to which an image is subjected to most eXplorer key ins attach a one line record that includes the date time keyin name and keyin parameters used to modify the area in any way Those modifications include any changes to the navigation or calibration information The audit trail can be querid by using the LA FORM AUDIT command The first lines of the audit trail may contain an image identification block or IID block This identifies the spacecraft camera planet scan mode processing map projection constants VICAR header 5 27 etc for the image contained in the area It 1s of different length for different images McIDAS eXp keyin DDBTUIL will create a new planetary area with DDB Data Description Block suitable for the SPICE oriented navigation and two byte pixels from radiometric conversion from any standard McIDAS X McIDAS OS2 or McIDAS MVS format area The new areas remain completely backward compatible with the old as far as core McIDAS utilities and applications software is concerned 5 28 APPENDIX I APPENDIX McIDAS eXplorer Command Guide This section describes the McIDAS eXplorer commands that can be used with the planetary data in detail These are in addition to the McIDAS X commands which are described in the McIDAS X Users Gu
255. qor it 1313 LS rl R at LE wee ent PN b Cn y E za SA Y do T L P L Er 7 a e AV te an L i S ee E E T stretch contrast 0 7 Press RICHY mouse button to end procesg ii nass te Load Sum Spar ecrati Puert LOOSSP sows you to intey s weuere e of arved pte Lry majos Such that UM nage center H al Ow Irane center ef a specific Irene LODSSP e an ae be used to 1U0 5901 mages PLO another area Herreg Area Ender Area HRAME d MAG HIT ICATION WHERE Ka La te frare or area contents of the loaded mages EB Black and white enhancement completed 727 os e Bore m ae ee a nd E Par E S A LR E el a wie 8 57 aM AN E S EA ae tant Bounds Frame 1 4 te ye AU A Ee a ay og gt a MER Ap C a cea a e E S 9 ne e ha ke RE E 7 radiomeme calibration filters of various types navigation and cartographic projections image enhancement multispectral classification time senes analysis area and distance measurements and cross sections Map outlines and gazetteer files provide the ability to visually identify the geographic features General purpose utility applicanons provide housekeeping functions and data migration Two dimensional irregularly spaced data can be objectvely analyzed onto grids and gridded data themselves can be graphically displayed via contour plots and cross section plots as well as rendered into images A basic sprea
256. r filter dependent radii or radii defined at different optical depths etc The user must add these experimenter dependent atmospheric radii to mcidas exp BODCON FOR and recompile McIDAS eXp with shell script makeplan to make new body constants accessible to the McIDAS navigation routines Users can update or insert IAU data into BODCON at their convenience prior to recompiling McIDAS eXp The NAIF ID number which controls definition of all target body constants is the one in word 200 of the Data Description Block for an area This datum is mandatory for all image navigation in McIDAS eXplorer and is first set to a default value by GETXXX when reading a CD ROM or by DDBUTIL when the TARGET keyword is used In addition mcidas exp TGTANNOT must be updated to reflect the correct image annotation for the experimenter s new radit The current target ID numbers used in McIDAS eXp are shown in the table below 5 9 Contents of mcidas exp TGTANNOT e e ree mr ee er i et ee ee ee ee ee ee ee ror ee ee ee ee re ee ee e ee ee ee ee ee ee ee ee ee ee ee ee rr oe Target Object SSS Code Sun 99 Mercury 199 Venus Surface 299 Venus 2991 Moon 301 Earth Surface 399 Earth 3991 Phobos 401 Deimos 402 Mars 499 Mars 4991 lo 501 Europa 502 Ganymede 503 Callisto 504 Amalthea 505 Himalia 506 Elara 507 Pasiphae 508 Sinope 509 Lysithea 510 Carme SLI Ananke 512 Leda NE Thebe 197932 514 Adrastea 197971 515 Metis 197933 516
257. r than from a fit to the limb points default NAVUTIL will allow the user to enter the center coordinates into the DDB so that navigation programs can access that information NAVUTIL also lets the user specify the NORTH angle for the planetary image measured clockwise from decreasing line direction i e the up direction as seen on the display Finally NAVUTIL will allow the navigation reference frame to be selected when multiple reference frames are possible For example a planetary image can have observer based celestial navigation attached to it or the navigation referring to the native body reference frame For ringed planets a third choice RING navigation is possible not yet implemented SUBPNT SUBPNT computes observing geometry the sub earth and sub solar coordinates and ranges for a given image It assumes that the date and time attached to the image refer to UT when the image was originally acquired at the telescope The NAIF planetary constants file and ephemeris files must be available for this command leapseconds ker pck3mod tpc and del 18cd bsp files must exist in the mcidas data sub directory The values are stored in the DDB slots for those quantities and the navigation transform is computed so that the image navigation is accessible to the McIDAS eXplorer applications The image must be displayed after the IMGNAV command has been executed so that the frame directory contains the latest navigation state NAV
258. r to select several points along a linear feature A robust fit will be applied to the points to determine the slope of line indicated by the points with the element direction REMARKS This command should return a decent approximation to the orientation of the planetary image Jupiter and Saturn Because the command has no way of knowing which is north and south the required north angle for image navigation NAVUTIL command could be a 360 degree complement of the returned value APPENDIX 1 3 ASTAT Measure image Statistics on a displayed image optcoord KEYWORDS Parameters Keywords opt BOX CIR IRR LIN AREA BAND COLOR CUT TAIL HIST LAT LON ARC FORM output output output LEVELS REMARKS option type from one of the following rectangular outline default circular or ellipitical outline irregular shaped outline outline based on line between 2 points coordinate type one of the following image coordinates default All options are designed to run interactivly on the current image frame earth coordinates Station dist sfc station loc and radius km for CIR lat lon dist lat lon circle and radius km for CIR LAT lat1 lat2 LON Ion1 lon2 lat lon pairs for BOX hou ab H stn1 stn2 dist point to point corridor km for LIN area number spectral band default current frame or 1st band in area graphics color default 2 lo hi data range default 0 10000 tail percen
259. radius is defined Thus for Venus the NAIFID value of 299 is modified to 2990 for the solid surface and 2991 for the cloud level at the first wavelength 2992 at the second wavelength etc The mnemonic identification is also suitably modified as appropriate for example to Venus sfc or Venus_atm Object specific physical constants that are required for analysis or navigation of the data are obtained through a single subroutine The physical constants for each solar system target that are incorporated within McIDAS eXplorer can be listed with the PHYSCON command This subroutine contains the most recent published values of the triaxial radii and the length of the day for solar system objects If any of the data need to be updated then this subroutine needs to be recompiled after the required changes and all of the planetary code needs to be relinked as well This is done as a matter of precaution to ensure that the fundamental constants are not changed inadvertently as is possible if the constants were loaded from a data file there is no simple accountability if the file gets modified McIDAS eXplorer allows use of the SPICE kernels for the navigation of images and also provides tools to determine the navigation transforms when the kernels are not available but the basic trajectory and pointing information are available Data from the older missions such as Viking Orbiter and bulk of Voyager imagery fall in this category Digital Areas or Imag
260. ram Bell Amer Astro Soe vet gy 1 193 fp 0G3 Session 12 1992 Urey Prize Lecture C Pieters Moderator 1 30 2 20 pm Grand Ballroom 12 01 INV Harold C Urey Prize Lecture On the Diversity of Plausible Planetary Systems Jack J Lissauer Session 13 Invited Talk C Pieters Moderator ma 2 20 3 00 pm Grand Ballroom KOG s S Va A Pra 13 01 INV Breakthroughs in Ground Based Infrared Spectroscopy of Planets C de Bergh Observatoire de Pans Recent progress in infrared detector technology and instrumen tation and the development of infrared arrays have strongly ben efited the study of planetary atmospheres and surfaces using ground based spectroscopy We will review the most recent of these studies Three important breakthroughs will be more par ticularly discussed 1 the new study of the deep atmosphere of Venus by measuring near infrared radiation of the dark side of the planet 2 the monitoring of processes occurring in the ionosphere of Jupiter using Hf infrared emissions 3 the detection of nitrogen ice at the surface of Pluto Poster Presentation Posters from Sessions 14 15 3 00 3 30 pm Session 14 Comets MI S Hoban and J Crovisier Moderators 3 30 5 30 pm South Ballroom 14 01 No We Are Not in a Cometary Shower Paul R Weissman Jet Propulsion Laboratory The flux of long period comets through the planetary region will vary as a result of the magnitude and rate of extern
261. rdinates line element to planet centered coordinates latitude longitude The first 128 words in the planetary McIDAS area navigation block are designated as the current navigation for the area for use with any McIDAS compatible navigation software modules such as NVXGOES DLM Geostationary GOES Spin Scanners NVX LAMB DLM Lambert Conformal Projection NVXMERC DLM Mercator Projection NVXMSAT DLM Meteosat Spin Scanner NVXPLAN DLM Planetary Navigation Framing Cameras NVXPS DLM Polar Stereographic Projection NVXRADR DLM Weather Radar Projection NVXRECT DLM Rectilinear Projection NVXSIN DLM Sinusoidal Equal Area Projection NVXTIRO DLM Polar Orbiter Nadir Scanners In McIDAS the current navigation or map projection type is specified in word of the Navigation Block word 64 of t x area as a 4 byte ASCII string GOES for Gecstationary GOES Spin Scanners LAMB for Lambert Conformal projections MERC for Mercator projections MSAT for Meteosat Spin Scanners PLAN for Planetary Framing Cameras amp Perspective Views CPP for Pioneer 12 Venus OCPP spin scan images NAIF for Planetary Framing Cameras using SPICE position kernels SPCE for Planetary Framing Cemeras using SPICE C Matrix kernels RADC for Right Ascension and Declination navigation PS for Polar Stereographic Projections RADR for Earth Weather Radar Projections RECT for Rectilinear Projections SIN for Sinusoidal Equal Area Projections
262. re PLANET MAKNAV output_area 4 LAMB PLANET MAKNAV output_area MERC lin ele lat lon pixsiz PLANET MAKNAV output_area MOLL PLANET where PLANET is the name of the solar system object If a perspective view is required then instead of MAKNAV use PLANAV to simulate a view from an arbitrary distance specified in terms of planetary radius with arbitrary view direction aim point relative to nadir direction and rotation about the aim point relative to object s north direction PLANAV area Planet angle KEYWORDS where Keywords AREA LINES PLANET diam radius ecc ANGLE north nadir na_azim VIEWPOINT lat lon dist LINE ELE SUN DIRECTORY SS yyddd hhmmss REPLACE NAV AREA NAV MORE Output area number to define navigation for required line dimension if a new square area is to be created Default is LINES 1000 a 1000 x 1000 pixel area Name ID of a solar system object either the NAIF ID number or name is required RADIUS amp ECC will default correctly if the value of PLANET is specified They can be forced to other values by the user For Venus use VENUS_SFC 297 or VENUS CLD 298 Planet diameter in pixels default is LINES 50 Planet equatorial radius km Planet eccentricity oblateness parameter 1 a 2 b 2 north nadir na_azim Spin axis tilt deg clockwise from vert def 0 0 off_axis tilt of optic axis from planet to spacecraft translation vector nadir angl
263. re created by the system administrator If the X server is not running start it with xinit To start McIDAS simply enter at the prompt meida igy E RRP from your home directory This initiates execution of the mcidas profile file which sets the display environment flags such as of bits displayed number of frames created at start up size of the display frames etc The contents of the profile are described in the McIDAS X User s Guide Note that it is when starting a McIDAS session that the frame size and the number of gray levels displayed gets set leave it at 128 unless the workstation has more than a single 8 bit display plane Details of starting McIDAS with different numbers of frames and different sizes may be found in the McIDAS X Users Guide Note that the frame size defined here is the McIDAS display frame size The X window within which this display appears is initially set to this size and should normally not be changed Once the McIDAS session has started expanding or shrinking the display window or the image window for McIDAS has no real effect on the amount of data displayed by McIDAS in that window Thus the frame size should be set to the largest size of the image that needs to be seen at the full resolution since by integer sub sampling larger images can be seen in a small display frame McIDAS X creates several windows when a session is started typically four One of these is a command window which also includes
264. relation of the image data is feasible but not currently supported within McIDAS eXplorer to determine the motions The TRACK command records the native reference frame coordinates of selected target locations in a text file for later analysis PCMW The cursor can be trained to move at a certain rate in a certain direction based on the image interval The velocity vectors computed from a pair of position measurements in two images separated by the corresponding time interval are printed out when the measurement process for each target is complete over the image sequence Please refer to the command help in the User Guide for information on how to use this command TRACK The TRACK command is intended for more elaborate analysis of the feature motions in a subsequent process It records the coordinates and time of observation in a text file and graphically notes their locations in a graphics frame using the image navigation A linear fit is performed to compute the average drift speed and direction Please refer to the User Guide for information on how to use this command HOW TO EXPORT DIGITAL IMAGES FROM MCIDAS EXPLORER The format of files in which McIDAS stores its images is compact but unique Although these files can be exported as such many programs may not be able to make use of all the information stored in the accompanying header information When the destination workstation is not known it is better to export images from McIDAS eXplo
265. required before navigation can be supported A facility for handling navigation of irregular objects is feasible within eXplorer but not yet implemented The general approach of navigation of images of planets and regular moons is described below It is assumed that the images have been imported into McIDAS eXplorer either from the PDS CD ROM volumes or in some standard format recognized by McIDAS eXplorer such as FITS or in the case of Pioneer Venus Orbiter images the NSSDC format If the images were obtained from the earth or other non NASA spacecraft then it is assumed that the imaging geometry information is avaiicble in some manner If it is a full disk image the minimum information required is the position of the observing instrument relative to the target If the observing instrument is located on the earth or a planet then the Universal Time UT of observation is sufficient to obtain the relative geometry information using the ephemeris tools incorporated within McIDAS eXplorer SUBPNT command but the orientation of the image itself relative to the target must still be known which way is the north direction in the image For targets such as Saturn and Jupiter the north angle can be estimated either from the shape of the object and or the zones and belt patterns or occasionally from the locations of the parent planet s moons if they are in the same image frame But it should preferably be obtained using reference stars For a vari
266. rer in a format very similar to the FITS format Any single banded area can be exported into another file using the XPORT command which writes the directory data the DDB and the processing history as ASCII 80 character labels followed by the digital data For simplicity multibanded data can be exported as separate files by extracting individual bands using the same command XPORT source_area file_name BANDS band band2 band3 bandn 4 27 Alternately as described previously the data can be exported as GIF files HOW TO CREATE A FUNCTION KEY MENU The Function Key based menu system is described more fully in the McIDAS X Users Guide Multiple menus are possible to be created and used A menu is a text file containing Specific instructions for the text to be displayed and to relate a specific function key toa McIDAS command User input one item at a time can be solicited using the ASK1 command The menu script uses the first character on a line to define the instruction A portion of a sample menu exp is shown below For futher information please refer to the McIDAS X User s Guide Menu number Function Key 1 WELCOME to McIDAS eXplorer Text for Function Key 1 at 10 14 Query Database 2 Import New Images from PDS CD ROMs F2 Display an Image from an Area 3 Enhance Frame B W Restore an Enhancement Table Save an Enhancement Table BsSsashssssso ar lar iar Ler lor kar Lar kar kar Lar Lar lar Lar kar ie Fu
267. rmine the locations of the reseaus in a Voyager image which may or may not be displayed Generate a snapshot view of images contained within McIDAS areas Up to 484 areas can be scanned at a time in a grid as large as 22 x 22 Once this area is displayed the particulars of the images can be listed using the SCANE command SCANE also allows subsequent processing of the areas when the command is entered Access the digital areas corresponding to the image representation of the digital areas as displayed on a particular frame This is an interactive program which stays resident until the ALT G key stroke and can be used to query the contents of the individual images Access information about individual thumbnail images contained in an area previously created by the COBROWSE option in GETGO in a manner similar to SCANE APPENDIX Ill 8 SCANM SCANV SEDRIN SEDRRD SHADES SPICENAV STAR STRIPX SUBPNT TGET TILES TLST TPUT TRACK TRIM Access information about individual thumbnail images contained in an area previously created by the CDBROWSE option in GETMGN in a manner similar to SCANE Access information about individual thumbnail images contained in an area previously created by the CDBROWSE option in GETVGR in a manner similar to SCANE Reformat SEDR data into navigation block for raw image Load Voyager SEDR tape file records into LW file Remove the photometric distortion in a Voyager image if t
268. rn programming practices which have been amply described in Fortran Programming Standards and Guidelines JPL D 6613 and also to the standards followed by the NAIF toolkit McIDAS and eXplorer applications to accomplish specific tasks are developed as modules that are callable from a control program A module that would be traditionally a main program is a key in within the McIDAS environment The size statistics are as follows McIDAS X library modules eXplorer library modules NAIF Spice library modules Lines of code 939 Core McIDAS core 1291 This effort 515 developed at JPL McIDAS X 148 761 Core Version 2 0 eXplorer 161 872 New code thios effort For companion NAIF library 138 570 Developed at JPL Number of Keyins Core McIDAS X eXplorer Total eXplorer object library size is about 9 Mbytes 119 including single letter commands 82 New Space required for binaries both McIDAS X and Explorer IRIX 4 5 200 Mbytes IRIX 5 2 10 Mbytes shared object library requires larger swap space AIX3 2 5 130 Mbytes HP UX 9 03 230 Mbytes Produced by the Telecomminucations and Data Acquisition Office and the Space Flight Operations Center Jet Propulsion Laboratory Pasadena California September 1989 TDS Document No 890 218 SFOC Document SFOC0095 00 01 The operability of McIDAS eXplorer on different platforms has been a goal of this project from the beginning Besides the SGI and IBM RS 600
269. s resemble the Mariner 10 images of Venus taken during 1974 in terms of spatial and temporal coverage Both acquired images from a fly by trajectory and over a limited period The temporal and phase angle coverage is thus limited and the spatial resolution varies with time The main difference is that Galileo SSI has only one camera two on Mariner 10 and that the detector is a CCD chip rather than a vidicon Only about 81 images were acquired and these are contained on the PDS CD ROM GO_0002 These images were obtained with the glass lens cover of the camera system still in its closed position Therefore a number of blemishes diffraction images if dust specks on the lens cover appear on the Venus images which are mainly a cosmetic annoyance The blemishes can be subdued using the BLEMEDIT command interactively if needed These images like all other Galileo SSI images can be imported into McIDAS eXplorer environment with the GETGO command SPICE kernels are generally available for these images in the PDS label however the experience has been that the north angle is frequently in need of adjustment NAVUTIL can be used to make the desired changes 3 5 IMAGES OF MARS VIKING ORBITER IMAGES AND DIGITAL IMAGE MODELS MDIMs The primary sources of Mars image data are the Viking Orbiters available on PDS CD ROM volumes and the processed image products the Mars Digital Image Model data available on CD ROM volumes produced by the USGS The Vi
270. s the image and graphics to be looped independently or simultaneously B Back up the display to the previous frame in the frame loop Essentially this is the reverse of the A key Glossary 3 List in the text window current contents of the frame in terms of satellite id day and time of acquisition source area number display resolution sub sampled or repeated and the upper hand corner load point coordinates image Display the digital data brightness data number in calibrated as appropriate and raw units at the cursor location in a displayed image List the planetary coordinates latitude and longitude of the cursor in a displayed image if the navigation transform is defined The latitude listed in McIDAS is always planetocentric and the default format is DD MM SS for both latitude and longitude The format can be set to decimal degrees by entering the following command UCU POKE 17 1 Display the McIDAS display status The number of frames and their specified sizes cursor size and current cursor location are listed in the text window This keystroke is used by some resident programs e g SCANA SCANG DSTNCE PCMW wtc to exit in lieu of a double mouse click Toggle between host mode and local mode Most McIDAS eXplorer workstations will not have a host on which to log on When the host mode is set the Command Window status reflects it and it can also be discerned with the in the first column of the Command Wi
271. s the nominal reseau locations are retrieved within the program from the area DDB If the data are also to be corrected for radiometric distortion then the command SHADE9 should be used before removing the geometric distortion GEOM source_area_ output_area SMOOTH YES or NO Le PPA TOVAR A RRA RA A AA SALADA we etree See PEP EFLL POLE ARAS PARTE AA RARA TAR RRA AS ARANA EPL EL Ed b EG CN C LAAL v gt g Ag E Y z lt z z A f g y A E L LE we few L V ata EI A TEN body Haco 203 Tictuca Pot CULTO Tocbrf Paty Pirim Prey ota lunar Per fud flaw 1 204 BHT TET HT PTT TH D ha Matias kmo 2305 iria s Pitra tary nd acta tko SHI WWY Tar Nock Tepx 1 UA A Nowt LA La Typa 67 dL Vata gaused IEL KOR voles 923 1923 fagam Covyprone ion Af gur itie rot mopy ghee tthe ea wE Ge oC pa te TH OR RED Sow sb GLU ARIAS VW 44 T LISTELE Joie tue cuo WL FRE 2 E KASS KORT CLERGY D COLG D PAIT af PAZ MIZ BR S L S 182 YAM 2 ICIQ Io SIJA CO ORKE Jiu YR ESKARNE Y 720 d WL A ROO GU IRA RAR OTIR P SIA CDSEO P EUW VERGA ESO Y IRIRE fke i EC a C c yee L Sx are N s a eee AS CG x SESS RS ot RA es SSES 2 anaes PS OS O AS A RE DONA EA A E aiie ee Figure 3 1 Example of a Kres GEOMed i image with the reseau locations displayed on the image prior to filling them in with the RESREM key in The GEOM step uses the measured locations of the reseaux marks and their object
272. sified as noise DN_gradient brightness DN between pixel at same element addrees on preceeding and subsequent lines that tags the current pixel as a noise pixel opt Noise filter option Picjk one from NO OPTION IS LINE DROPOUT AND SHOT NOISE FILTER COMBINED BAD REALLY BAD NOISE SPIKES gt 1 PIXEL FILTERS OVER 5 PIXELS HORIZONTALLY WITH SOME RESOLUTION LOSS LIKELY DEFAULTS CLEAN lt area in gt lt area out gt 0 NOI 15 20 KEYWORDS FOR FRAME LOAD LOCATE DEFAULT AU YCOOR DEFAULT 0 XCOOR DEFAULT 0 MAG DEFAULT 1 REMARKS Program first checks to see if there is a smoother than gradient transition from the preceeding to the subsequent line f so and the middle line pixel exceeds the average of above and below pixels by threshold the middle pixel is replaced by the average This vertical interpolation removes correlated noise bursts along a line Then a shot noise filter is applied horizontally on the line to any pixel deviating by more than the threshold from its preceeding or following neighbor Thus gradient 0 gives an ordinary shot noise filter while setting it non zero turns on the vertical filter to remove correlated noise along a line APPENDIX 12 COMBIN Make a multiband area from several single band area MAY ALSO BE USED TO REDUCE 2 BYTE DATA TO 1 BYTE DATA COMBIN oufarea BANDS area1 area2 areaN PARAMETERS outarea area with N bands maximum 6 at present K
273. single header and is organized as a table suitable for importing into a spreadsheet or plotting using the SHOW utility plotting command Magellan Global Topography Radiometry and Terrain Data GxDR s Use GETGXDR to import images from PDS CD ROM volume MG 3001 and MG 3002 GETMGXDR is functionally very similar to the GETMGN command although the organization of the CD ROM volume is slightly different and there are four different data types topography slope RMS slope and emissivity Mars Digital Image Model MDIM s Data Use GETMDIM to import these images produced by the USGS from Viking Orbiter images of the surface of Mars VO_0001 through VO_0014 Viking images of Mars and its moons Use the GETVO command to import images published on PDS CD ROM volumes VO_1001 through VO_1014 Voyager images of the giant planets and their satellites Use the GETVGR command for data published on PDS CD ROM volumes 1 25 GETVGR accomplishes two tasks i generate a browse area from a range of images specified by FDS numbers for a given target maximum 56 and ii import one or more full resolution images into one or more areas for a given target object When importing full resolution images FILTER 0 through 7 or color and CAMERA WA or NA can be specified to limit the choices The Voyager images as published on the PDS CD ROM s do not have attached navigation and calibration data Additional steps are necessary to geometrically and 4 3
274. sion only The objective of McIDAS eXplorer is to bring to the planetary community the tools that the terrestrial meteorological community has been using to analyze weather data and model output While planetary data published by the 10 e February 1994 Information Systems Newsletter Planetary Data System PDS on CD ROM volumes are the primary source of solar system data acquired from spacecraft missions ground based and telescopic images of the planets are also accessible and manipulable via McIDAS eXplorer McIDAS was inspired by the need to have better means of analyzing the torrent of data from the geosynchronous weather satellites and to measure cloud drift winds McIDAS has been ported to UNIX and OS 2 Operating environ ments and can be used on IBM RISC 6000 Silicon Graphics Sun and Hewlett Packard workstations running the respective vendor s version of UNIX The software implementation of the McIDAS control program allows use of McIDAS in field experiments wherever and whenever some means of communication link to a McIDAS host site is feasible For example McIDAS was used to chart the flight paths of the research aircraft based in Bahrain to sample the smoke from the ol well fires in Kuwait McIDAS is currently used by the National Meteorological Center for routine weather operations and is at the heart of weather related activities for the space shuttle operations It is also used by weather services in Austra ia
275. sions for planetary applications which are compatible with McIDAS X Processing History Audit Trails Most spacecraft data undergo several specific processing steps some are mandatory such as radiometric or geometric calibration many others are optional such as map projections or multispectral classification In most instances wherein a large amount of data are being analyzed it is useful to maintain a processing history record for the data For the image data McIDAS eXplorer maintains an audit trail in which applications programs append an entry containing all the command parameters that were invoked in that particular processing step This processing history can be queried either by the user or by other programs to determine the processing status McIDAS has been ported to the OS 2 operating systems as well as to several versions of UNIX The primary application code is mostly written in FORTRAN with some C lan guage code To a large extent McIDAS acts as its own operating system and most housekeep ing activities can be performed from within McIDAS itself Nevertheless experience with the native operating system is useful but proficiency is not necessary As McIDAS predates most personal computers and certainly the windows environment it is not surprising that the pri mary means of interaction with the user is through the command line However other user in terfaces are possible and have been developed and implemented within McIDAS in the
276. sions to the outer planets Viking 1 and 2 Orbiter missions to Mars Magellan mission to Venus and Galileo Orbiter data collected during the Venus Earth and Moon encounters on its way to Jupiter These data are described briefly below 3 1 VOYAGER IMAGES OF THE GIANT PLANETS AND THEIR SATELLITES The imaging system on each of the two spacecraft was nearly identical each carried a wide and a narrow angle vidicon camera Each camera was equipped with a filter wheel with eight filters The filters on the two spacecraft were nearly the same with the exception of a methane band filter on the Voyager 2 wide angle camera that replaced the blue filter on the Voyager 1 filter wheel The face plate of each of the cameras was etched with a pattern of 202 reseau marks that were nominally 3 x 3 pixels wide Their positions were measured to a 0 001 mm accuracy on the ground The details of the imaging system and the calibration of the data can be found in the report by Benesh and Jepson 1978 The camera characteristics are summarized in Table 1 for completeness Table 1 Voyager Imaging System Characteristics Spacecraft VGR 1 VGR 1 VGR 2 VGR 2 Camera Narrow Angle Wide Angle Narrow Angle Wide Angle Focal Length mm 1502 38 1 37 200 47 0 39 1503 49 0 39 200 77 0 23 Frame Size 800 x 800 800 x 800 800 x 800 800 x 800 FOV 0 44989x0 44989 3 34888x3 34986 0 45022x0 45022 3 36174x3 36745 Pixel Size urad 9 12 68 34 9 11 68 23 Filters 6 5 6 5
277. space locations to remap the input image into another area that has the distortion removed The SMOOTH YES option smoothes the output image by performing a local average of the immediate neighbors 2 3 1 3 weighted Note that typically the radiometric distortion is removed BEFORE this step as the shading correction files are usable only in the original i e distorted image Further the averaging is speeded up through the use of a look up table that will currently handle DN values between 0 4095 only The output of the shading correction program is generally 2 bytes and is within this range if the data are normalized using the I OF 1 default option If the data are radiometrically calibrated to a greater dynamic range then the SMOOTH option should be turned off as it will not produce proper averaging If the resultant image is visually too granular then it can be smoothed by running a low pass filter with a small filter radius e g 2x2 3 1 3 Removal of Photometric Distortion Photometric correction requires removal of the dark current signal or dark noise and correction of the non linear response of the vidicon Both of these are image position as well as exposure time dependent The dark current however has another cause and that is dependent on the rate at which the image is read out by the data system the current starts building as soon as the image is exposed and keeps on increasing until the image is read out by the vidicon electronics
278. st three characters but command specific keywords may check the entire keyword the commands e entered in UPPER CASE oes Us recommended but ali keywords must The positional parameter is most often used to indicate to an applications program the area containing an image of interest Often it is desired to modify one image by some process and retain the original as well The syntax most often used and almost invariably in McIDASese is to specify in input area first and the output areaz second For example a command with a syntax given as REMAP from_area to_area and entered as REMAP 101 102 will remap the image contained in the file specified by the positional parameter from_area area 101 in this example and write the output in the file specified by the second positional parameter fo_area area 102 using the navigation transforms defined for the two areas The actual file names for the two areas are AREAO101 and AREAO102 but the user seldom needs to worry about the exact names except for system administration purposes A simpler example of the positional parameter is when only a single parameter is required such as in the LA command to list the directory for a given area so one can find out what the contents are LA 101 which produces a single line of output in the text window like ss yyddd hhmmss cor ecor lr er zr lsiz esiz 2 bands 101 48 89214 83159 If this is not sufficient one
279. sudden change in the brightness in a scan across the disk but a gradual one and requires the use of an edge detection technique to locate the limb The technique usually employed is the maximum brightness gradient one which usually is assumed to reflect the location of the level where the slant optical depth equals unity In the case of Venus and Titan this limb is a considerable distance above the solid surface determined from radar and radio occultation data respectively Further the height of the detectable limb of Titan has been measured to be different at different wavelengths from both Pioneer 11 observations Tomasko and Smith 1982 and from an analysis of Voyager images There is also evidence that the height of the detectable limb is considerably different at low i e backward scattering and high solar phase angles i e forward scattering for Titan To enable use of different radii at different wavelengths eXplorer uses a modified NAIF Object Identification code that allows a wavelength dependent radius to be used seamlessly for objects with extended atmospheres 3 1 6 Use of SPICE kernels If available the NAIF SPICE kernels for an image can be utilized to attach navigation transform using the GETSPICE command These kernels are available for a limited number of Voyager Jupiter and Saturn images from Voyager 1 and 2 and for all of Uranus and Neptune system images from Voyager 2 Note that with SPICE kernels some of the information
280. t 188 Ecliptic Latitude of Periapsis 189 Ecliptic Longitude of Periapsis 190 Altitude from Target Center at Periapsis 191 192 Image Compression Algorithm WORD ITEM Central amp Picture Body 193 195 Central Body Name 196 Central Body NAIF Code 197 199 Picture Body Name 200 Picture Body NAIF Code 201 Picture Body Rotational Period hrs 202 Picture Body Pole Right Ascension 203 Picture Body Pole Declination 204 Nominal Picture Body Eq Radius 205 Nominal Picture Body Pol Radius 206 Nominal Picture Body Cross Eq Radius 207 Color Dep Pict Body Eq Radius 208 Color Dep Pict Body Pol Radius 209 Color Dep Pict Body Cross Eq Radius 210 Picture Body Eccentricity SQRT e2 p2 p 211 215 OBJECT Name of object observed 216 217 EQUINOX Equinox in years for coordinates 218 219 Reference System 220 351 Spare 352 West Convention for Longitude WORD ITEM User Computed Quantities ee ee p eee ee ee ce ce eee ee eee ee Br ee eee 353 354 User Block Type MEXP VGR MEX P MGN MEXP CPP McIDAS exp Voyager McIDAS eXp Magellan McIDAS eXp Pioneer Venus 5 22 TIPE CES 1 4 1 4 CS C 20 C 20 Sn RY D R 8 C 20 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 c 8 TYPE E 12 EA CELZ 1 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 R 4 C 20 c 8 c 8 1 4 TYPE C 8 COMMENTS O for Earth Based O for Earth Based First 8 bytes N A Unused NONE HUFFMAN LZW etc
281. t For each frame that contains an image McIDAS keeps track of the image source its calibration and most important the navigation Overlay graphics can be drawn that can also be dynamically saved in independent graphics files for redisplay later The overlay graphics can be either merged with the image data or drawn as peelable graphics or transparency overlays allowing the user to peel off and on the graphics with a single key stroke Figure 1 shows a view of the McIDAS display illustrating the image display window with overlaid graphics a command window and a text output window The e Information Svsiems Newsletter MUS 139999 rine rpe NUS 1 9999 99904639 9990 VENUS MG 3001 SIM USIHAN USIMAN NAOHLY NAOHLY NAOHLY NAOMI T 1 9270 3 1716 BOTALT T HM TT VIOLET 155 HA ISS HA VIOLET LEHE HA 26846 11 1699U2 00 CLEAN IS5 NA 4 92 J piter a UU 12 1895 115 01072 s 73451 346 41 Jupiter l E E ra 930672 715085 336 86 Jupiter 0011 145 9455 C HIROHS 3k HE T E L A TT H 39 4309 ISS NA NAONLY gt ete toep a BLV m Da da 5 r EA m ft E VENUS FE 3001 SIM 300 1 1 Jupiler NONE 360 4 1 Jupiler HONE 4 970 4 3 Miranda NOME 72 880 kl Miranda barat E 920 1 LEM is ands HUHNE lt MOHE 170 7 1 Jupiter IRI ee PLAN you NG 0019 SIN E sees PLAN S ID PLAN gt ee PA VENUS TEE VENUS MG 0061 SIN ds 1 1 Jupiter NONE RI t AN
282. ta from a planetary images from the planet center to the planet limb APPENDIX III 5 LISTAUD List audit trail for a MciDAS area LISTDDB List the various Data Description Blocks DDB such as planetary SPICE navigation block etc for an area LISTHEAD List the text ASCII header of a FITS format file in the McIDAS text window LISZEN Compute solar and observer zenith angle for specified image coordinates for a single image or multiple images contained in a single area or sequential areas LOCATE Plot as an overlay graphic on a navigated image display the co ordinates of points from a text file LODSSP Display a sequence of navigated planetary image such that the image center is at the frame center beginning at a specific frame Can also be used to sub sect images into another area LP Line plot of Image Data at Cursor Location or between any two points on a displayed image MAKIMG Import an image from a TIFF format file into an area This is a McIDAS X commana MAKNAV Attach navigation for a cartographic projection to an area This is an adaption of the core McIDAS X version MAKOUT Create a new blank output area and attach the directory and teh DDB from another area This is useful for projection of images so that the supplementary information is tracked with the image This can also be accomplished with the AA command but avoids the overhead of actually moving the data NOTE The line prefix byt
283. tage 0 100 default 5 frame plot a histogram on graphics frame default no plot lo hi latitude range LON keyword must also be specified lo hi longitude range LAT keyword must also be specified lo hi angular segment of an circle CIR option only where deg1 degrees from 0 to begining of arc segment and deg2 degrees from 0 to end of arc segment output format of output Statistics 1 standard statistics default 2 standard stats BRIT bins 3 standard stats BRIT bins BRIT histogram nbin min max for UNIT BRIT only nbin number of bins defaults VGA 13 WWW 16 TOWR 16 min minimum brightness level default 0 max maximum brightness level default 255 This command allows the user to obtain statistics about the contents of an image or a section of it as determined by one of the many selection The IRR option lets the user draw an outline to enclose an area on a displayed image using the mouse The data units are user selectable as well APPENDIX I 4 BILIN Scale an image in line and element direction by any arbitrary factor by bilinear interpolation source_area_ output_area_ ASPECT INPUT Parameters souce_area area number containing the image to be scaled in x and y dimensions output_area_ output area number that will contain the scaled image KEYWORDS ASPECT line_factor element_factor magnify Defaults values are 1 1 1 respectively INPUT start_line start_ele
284. te planet correction APPENDIX 1 56 LISTAUD List the audit processing trail for a McIDAS area LISTAUD area_ Remarks Most McIDAS eXplorer applications programs that modify the contents of an area make entries in the audit trail The processing that an image has undergone can be determined by examining the processing trail APPENDIX 57 LISTDDB List the Data Description Block for a McIDAS eXplorer area LISTODB area_ type PARAMETERS type MAN to list the mandatory data target source block type SC to list the spacecraft and camera specific block GEOM t list the map projection and image geometry block SPICE USER to list user computed quantities for that area NAV to list the older PLAN type navigation block BOD to list the target object specific block ALL to list all blocks APPENDIX 58 LISTNAV Lists any or all planetary SPICE navigation blocks for an area LISTNAV block type area PARAMETERS block_type can be any of the following SC spacecraft 4 camera block def lt ult block BOD central amp picture body block IMG maging geometry block USER user computed quantities block ALL list 31 SPICE blocks for area SC BOD IMG amp USER area navigation block words 128 511 CUR list current navigation block if PLAN otherwise uses the LWU LIST AREAXXXX 64 191 format PLAN list PLAN navigation block 512 639 area area number for which to list the blo
285. ted image identifiers such as filter camera etc for areas displayed frames and limb point files LIMBnnnn FRAME 1st_frame last rame KEYWORDS AREA begin_area_ ending_area_ LIMB begin_area_ ending_area_ KEYWORDS MISSION mission ID VGR VO GO or MGN TARGET name of a solar system target Remarks If the FRAME option is used each of the displayed frames are annotated on the graphics frame with a one line summary of the displayed image if any and the area_ which was used for that frame display Similarly if the AREA option is specified then if that area has been displayed on a particular frame then that frame number is also indicated on the one line summary of each area APPENDIX I 100 XPORT Routine to write a Mcidas area into a FITS format file XPORT source_area_ FITS_file_name Paramaters source_area_ area number from which to copy the image data into a file with a FITS header FITS_file_name name of the output file containing the image data with the FITS header REMARKS This command allows images stored in the eXplorer area format to be converted into a file with a FITS header that contains the pertinent image information from the area DDB Example XPORT 9999 image dat APPENDIX I 101 APPENDIX II McIDAS eXplorer Data Files A number of data files are required by some of the commands that form McIDAS eXplorer in addition to those files required by the core McIDAS These files exist in
286. tered using the ALT key and generally control the display state Examples are the A and B key commands which respectively advance or back up the display to the next frame in the sequence McIDAS also makes use of user defined string tables to facilitate simpler input to ap plication programs as well as argument passing between different application programs These string tables are created by a simple string editor and stored in the user profile and can be saved and deleted Multiple versions can be stored under different names for different applica tions and can be shared with other users Besides the single command execution or action of application tools McIDAS applications can be executed in a sequence for repetitive tasks in one of two distinct ways One of them is as a macro command that is precompiled A Mcl DAS macro program accepts as input standard FORTRAN statements with some exceptions and can call other McIDAS applications Once compiled the application executes the sequence described within the macro The second way of simplifying repetitive tasks is to use the REPEAT command which executes a command string a given number of times with any number of numeric arguments For example TE MAPIT 1 2 MERGE YES DF 2 1 REPEAT MAPIT 100 TO 200 BY 1 300 will map images contained in areas 100 to 200 and map into a given projection and merge the output into a single output area 300 and display the result after the addition of eac
287. termine which CD ROM volume the data can be found on FINDFF will list all CD ROM volumes that PRIMA PAGE BLANK MOT FH MER contain data over the specified region in either the LEFT or the RIGHT look modes and over all three cycles GETMGN can be used to accomplish three tasks i create a super browse image from all the browse images contained on a given MIDR CD ROM volume and write that image in an area ii import a single browse image into an area and iii import a single tile or a framelet from a selected directory or a browse image The MIDR data are published at four different resolutions F MIDR at 225 m pixel C1 MIDR which is once compressed F MIDR data C2 MIDR which is twice compressed data and C3 MIDR thrice compressed data Each of the compression steps results in a 8X reduction in spatial resolution and compasses larger and larger area GETMGN will work with all four versions of the data However there are some differences as noted in the remarks below l GETMGN tags the imported data a browse frame or a a single component tile of the browse image with a nominal time tag in the area directory that indicates the time UT of acquisition of the data As these are images are mosaicked from many orbits there is no single time that is appropriate for the image The time tag corresponds to the periapsis time for the first orbit number noted in the PDS label for the data that are being imported The purpose of this time ta
288. th and be the last entry on input line ANY VALID McIDAS AREA NUMBER 1 9999 The complete path i e cdrom f226axx f226aNN imq must be included in the FILE NAME field and String Table entry CDPATH must exist and be a blank field If the reseau location files and the shading files are availble the images may be processed to remove the geometric and photometric distortions and navigated if the SEDR data are also available The FILTER command with the MEDIAN type filter will remove most of the random noise found in these images APPENDIX 1 45 GUI Start the Graphical User Interface from the Command Window REMARKS This is the simplest way to start the GUI APPENDIX 46 HSTTOMC Import Hubble Space Telescope WF PC image from a FITS format tape file into a McIDAS area HST FILES ARE WFPC FITS FORMAT USUALLY WITH 4CCDS OUTPUT AREA HAS ONE BAND FOR EACH CCD HSTTOMC infile outarea PARAMETERS infile HST FITS file COH or DOH extension gt gt ENTER THE FIRST 8 LETTERS only lt lt outarea MCIDAS multi band AREA KEYWORDS DATA DATA RAW uses DOH raw data DATA CAL uses COH calibrated data EXT File extension after INFILE s 8 chars Overrides the DATA keyword value DEFAULT t_cvt cOh PIXSIZ DATA TYPE OF OUTPUT FILE 1 OR 2 BYTE DEFAULT 1 APPENDIX 47 HSTKNIT HSTKNIT Remarks Program to create a single area 1600 x 1600 containing four component 800 x 800 CCD ima
289. that contain images acquired on day 6 of 1979 will be listed as DAY is a valid keyword for LA The environment table can be listed with the TL command and saved restored in from a named file with the TU command Thus a user can create multiple environment tables for different types for data analysis 2 9 McIDAS eXplorer Commands A variety of tools or commands are available to manipulate the data within McIDAS eXplorer For solar system image data these include geometric and radiometric calibration filters of various types navigation and cartographic projections image enhancement multispectral classification time series analysis area and distance measurements cross sections etc Map outlines and gazetteer files provide ability to visually identify the geographic features General purpose utility applications provide housekeeping functions and for data migration Two dimensional irregularly spaced data can be objectively analyzed onto grids and gridded data themselves can be graphically displayed via contour plots and cross section plots as well as rendered into images A basic spread sheet capability allows arithmetic operations on the gridded data to compute other derived quantities Spectral data can be displayed averaged and staged for further processing as desired for temperature retrievals or other analysis Many of these commands are part of the core McIDAS X on which eXplorer is built McIDAS commands are generally written in ei
290. that is provided in the Voyager SEDR record is not available directly and hence the DDB entries for those quantities will not be filled unless GETSEDR is also used for that area Sometimes it is desirable to improve upon the SPICE kernel navigation either to update the planet image center location or the north angle NAVUTIL can be used to update the navigation In future a utility to output the SPICE kernels in the NAIF compatible format from any eXplorer image navigation would be useful 3 2 VENUS IMAGES MAGELLAN GALILEO and PIONEER VENUS MISSIONS There are four US space missions which have returned a significant amount of VEnus images and most of which is available on PDS CD ROM volumes Mariner 10 obtained nearly 5000 images using two vidicon cameras over a period of about 8 days on a fly by trajectory to Mercury its ultimate target These data are not yet available on PDS CD ROMs In 1978 the Pioneer Venus Orbiter began acquiring images of Venus from orbit using a spin scan technique The Orbiter Cloud Photopolarimeter OCPP instrument acquired nearly 4000 images of Venus cloud cover over a time approximately 7 years in reflected sunlight and filtered through a narrow band 365 nm filter It also acquired many full disk polarimetry maps at 270 365 550 and 935 nm over a longer duration As Venus is completely covered with clouds images in reflected solar light acquired by Mariner 10 and Pioneer Venus reveal only the cloud features of Venus
291. the initial cursor location at a specified distance and angle step the cursor away from the initial cursor location by the specified latitude and longitude increments step the cursor away from the initial cursor location by the specified line and element increments step the cursor away from the initial cursor location by the specified raster and pictel increments moves the cursor away from the original location by this meteorological angle def 0 increment to step the cursor along its straight line path distance to move the cursor from its original location angular increment in degrees degrees of latitude to move the cursor northward is positive degrees of longitude to move the cursor westward is positive number of image lines to move the cursor downward is positive umber of image elements to move the cursor rightward is positive number of lines rasters to move the cursor downward is positive number of TV elements pictels to move the cursor rightward is positive graphics color level of the characters typically between 1 and 7 but as permitted for the workstation Default 2 height of the plotted characters in pixels def 5 character to mark points with def Allowable symbols are o distance units one of KM kilometers default MI statute miles NMI nautical miles APPENDIX I 20 EDGES Program to determine the limb points from an area containing a planetary image for finding th
292. ther FORTRAN or C and compiled Users may write their own applications in the McIDAS environment making use of the subroutine libraries provided as part of the McIDAS X license 2 10 Right Tool for the Task McIDAS eXplorer has tools to import process and analyze planetary images from PDS CD ROM volumes Currently Voyager images of the giant planets and their satellites and ring systems Magellan SAR images of Venus surface Pioneer Venus Orbiter Cloud Photopolarimeter images of Venus clouds can be calibrated shading and geometry and navigated Support for other data products such as Galileo SSI images and hopefully Mars Observer will be added in the near future Once these data are imported within McIDAS eXplorer they can be gridded map projected animated brightness normalized and filtered Three color composites and multispectral classification of up to six bands are possible Calibrated and navigated image data can be used for areal cloud motion and other measurements using general tools Although many of these commands are quite general in that they can be used for data from any solar system object or spacecraft mission some of them are very specific to a particular mission and data For example there are a set of specific commands that are limited to data from Voyager 1 and 2 missions to perform tasks related to the analysis of the images 2 10 which have very specific properties requiring specific processing Similarly the Magellan
293. tion The steps in displaying a region of interest are briefly described below FINDFF GETMGN and TILES These three commands collectively enable the user to locate and import a radar image into McIDAS eXplorer FINDFF searches the cumulative index from the last MIDR volume MG 0123 to determine the CD ROM volume containing a region given by latitude and 3 10 longitude or by a feature name if known The NAMES command can be used to list the named surface features on Venus Once the CD ROM volume has been located and mounted in the CD reader GETMGN will import that frame into a McIDAS area from which it can be displayed using the DF command If useful the browse frame can be imported first in which case the user is provided the option to import a full resolution image of one of the 56 component pieces also called tile or a framelet or chip of a browse frame by selecting a specific number from the displayed image The tiles can be re drawn using the TILES command 6 SO MAGELLAN RAJAR CLBROWSE 0 DUL 1 50006 MAGELLAN 1 SEP 22245 164414 GO00S 02 0 Figure 3 5 An example of a Magellan browse frame with the individual tiles shown The tile numbers and locations are drawn by the TILES command on a C1 MIDR browse frame With SCANM key in any of these tiles can be retrieved from the CD ROM in specified areas SCANM is an interactive command and can be used to import more than one tile from the displayed browse frame from the mounted
294. toaa i E i 7 To gt UT 22 er ey e ee GAD STATG ALU OF SUNY ana iann ps Rois Pixel rito end tie 7 32 E NN SN 22 l an re ASS Sree E l i i T gt oy ae See A SS RR AER AAA Bett Cunt eC Yoru sitios Hch tae Mick Tepe Mo Ct See HGD TLR oo E Nes S RS LL a K E ar AAA ET T C E 9 l T S CoN 4 IIIS SSS Blan ld BAL Ricos Catat 2 EY L 2 P oc Mesas Fil TRR Sta rn tal cote S 130 103 ret W P S N y TS Y Hone Aurelia A EUT ESODTET BL nN as Oe ae EO Nae eae Se Figure 3 3 A navigated roll by roll OCPP Venus image with the latitude longitude grid is shown in the image window The text window shows a portion of the output of the LISTDDB command listing the DDB contents pertinent to that image Usually the nominal navigation performed using the spacecraft and instrument geometry data can be refined by interactively determining the look angle and roll angle by matching the expected location of the Venus bright limb with the observed location The improved roll and look angles can be input to the DDB attached to that area using the NAVCPP command Venus due to orbital motion in its eccentric orbit the images can be mapped into a more suitable projection using either MAKNAV or PLANAV projection navigations and either REMAP or NRMIMG NRMIMG requires that the Minnaert scattering coefficients be known and can be determined using MINFIT aL aire ET SELYS AE ME A A INTERC 2 ER RERA oak MINNHERT
295. tput It currently exists in three different versions McCIDAS MVS for the mainframe system McIDAS 0S2 for the OS 2 operating system for personal ccmputers and McIDAS X for the UNIX workstations The eXplorer version is compatible with both the X and 0S 2 versions of McIDAS A prime objective of McIDAS eXplorer is to Provide access to the planetary data now available on nearly 200 CD ROM volumes published by the Planetary Data System PDS and the US Geological Survey These CD ROM volumes contain image data collected by missions such as the Viking 1 and 2 Orbiters Voyager 1 and 2 Magellan Radar mission to Venus and the Galileo Orbiter still in transit to Jupiter These data comprise all the planets except Mercury and Pluto as well as many of the planetary satellites and ring Systems and soon two asteroids McIDAS eXplorer provides a common approach to the access analysis and display of the data on these different targets in terms of data manipulation and navigation McIDAS provides tools for three data categories i graphic or image data ii gridded data and iii station data The image data can be multispectral and have either 1 or 2 byte depth The gridded data are distinguished from the image data in that the data values may be real 4 or 8 byte and generally have dimensions smaller than the image data and may have missing elements The station data are generally a single geographical location data vector with as many components as ne
296. ts that make up the browse image can also be imported into McIDAS by moving the cursor and clicking over the browse frame Individual tiles are indicated by the comamnd TILES which is called by GETMGN to display the numbered tiles APPENDIX 42 GETMDIM Reads CD ROM format Viking Mars Digital Image Model MDIM or Digital Terrain Model DTM Images to a McIDAS eXp rea GETMDIM area_ FILE_NAME write file to area GETMDIM LIST FILE_NAME list header for image file KEYWORDS AREA ANY VALID McIDAS AREA NUMBER 1 9999 FRAME ANY VALD McIDAS FRAME NUMBER amp MAGNIFICATION defaults are no frame load and magnification 2 REMARKS The complete path i e cdrom mi30sxxx mi30s182 img must be included in the FILE NAME field and or String Table entry CDPATH must exist and be a blank field To generate CDPATH use the keyin command TE CDPATH path name FILE NAME ANY VALID SOURCE FILE NAME Must begin with and be the last entry on input line EXAMPLES GETMDIM AREA 345 FRAME 2 3 FILE NAME write to area 345 and display on frame 2 at 3X blowdown APPENDIX 1 43 GETVGR Import a compressed Voyager image from CD ROM and write a McIDAS area containing that image KEYWORDS FILE_NAME area_ FILE NAME KEYWORDS CDPATH FILE NAME FDS TARGET FILTER CAMERA AREA EAMPLES Enter path in the string table using TE command Should be blank if 1 CD ROM format image is in mcidas dat
297. ty by regression and robust estimation Trim the spline sized rectangular edges at the limb of a remapped planetary image APPENDIX Ill 9 USCLAS WHERE XPORT Spectrally classify a multi banded image using unsupervised multispectral classification Currently assumes 1 byte per spectral band data 2 byte data can be used after using COMBIN to use the calibration to convert to 1 byte data List image identifiers for a range of frames areas or limb points files LIMBxxxx format contents in the text screen using data specific information Export a McDAS eXplorer area into a FITS format file by writing the DDB information in a FITS compatible header so that other programs may be able to access the image data unlike a GIF format file created by SVGIF key in APPENDIX Ill 10 GLOSSARY A QS SES AA AAA ETE Glossary Animate McIDAS display is a multiframe display A time sequence can thus be displayed on the available frames as a loop The loop bounds can be set with the LB command for sequential frames to be displayed or with the LS command for arbitrary frame numbers to be displayed in a sequence The animation can be started or stopped with the L key entered either as Lf r or ALT L The dwell rate can be controlled using the DR command Altimeter Radiometer Composite Data Record ARCDR The Magellan Mission Altimeter data on Venus surface topography is archived for altimeter footprints under the Magel
298. u McIDAS EXPLORER A PLANETARY ANALYSIS AND DISPLAY SYSTEM PERIAPSI ar npr 3 nuz vk CUESSED ITA 1990 3149 13 URET CUESSED VIEH 1994 21 186 ORD AE CARSSED VIF 23442 11 f f Tt 25 ORNIT ey TN TT T NT 1997 3748 th TGAN e SELECT LAT LOM 331 011 109 PERIAP LAT LON 9 11 uy DATE OFT PTRIAP 194 701 f f 70 HOMINID GIT YT SCAN 2506 779 URDATAL PIOD HIM 19 572 11 FO od AL DI PLL A mere et TT AAs PR LARA a lt n r Ps ea Pr y lt r L C Jx e a Leer aa P N AN P PTA teh ne Ta G r a vua 1T Space Science amp Engineering Center University of Wisconsin Madison ee McIDAS EXPLORER A PLANETARY ANALYSIS AND DISPLAY SYSTEM Developed under support 7rom the Applied Information Systems Research Program NASA Space Science amp Engineering Center University of Wisconsin Madison 1225 West Dayton Street Madison Wisconsin 53706 608 262 9541 sanjayl ssecmail ssec wisc edu September 1994 McIDAS X is a licensed product available from the Space Science and Engineering Center For licensing information Contact S S Limaye SSEC UW Madison 1225 West Dayton Street Madison Wisconsin 53706 608 262 3755 sanjayl ssec wisc edu K Keh kea Whe Un b 2 0 2 1 pee bere ee 0 0 9 4 G Lh E LA HA NN Table of Contents INTRODUCTION Planetary Image Data What is McIDAS What is McIDAS eXplorer Object Identification Digital Image Files Data D
299. uch a mis orientation of the planet in an image as specified by the SPICE kernels is usually obvious when it is viewed in a time sequence with a constant orientation as can be arrived at by remapping the images to force a constant north angle in the output images It can also be occasionally verified by the presence of stars or satellites in the particular image which allow the true orientation of the imaging instrument to be determined independently SPICENAV command can be used to update the SPICE kernel based navigation IDMOON key in offers a means to determine the image orientation and also the image scale information for images of Jupiter provided at least one moon is visible in the image As econ as the P kernels for satellites of Saturn and other planets are available the key in in can be extended to include those planets satellites If multiple moons are visible in the image maximum accuracy is achieved in both the north angle determination and the image scale size if the furthest satellite is used HOW TO MEASURE DISTANCES and AREAS WITHIN AN IMAGE OF A PLANET OR A MOON DSTNCE This application allows the user to measure distances on any displayed and navigated image between pairs of points in the image or along a multi segment path in physical units meters km nm or miles The command obtains the proper scale factors based on the same physical constants as are listed for the target object by the command PHYSCON The target identif
300. ude gray scale or color images using such as a TOYO printer which is connected to the display device of the workstation Finally the image displayed on a McIDAS frame can be printed by saving it as a GIF format file using the SVGIF command The GIF file can then be saved as a PostScript file using the XV utility from a X Window session either as a color image or as a black and white image The PostScript file containing the image can then be sent to the system laser printer to get either a black and white gray tone image or to a color printer to obtain a color print The GIF file can also be exported to other systems such as high resolution cameras or image editing programs to add annotation change color balance etc Frequently an X window is also required for direct interface to the operating system although most commands can also be sent to the operating system from the McIDAS command window through the OS command followed by a string i e preceded by the double quote symbol containing the operating system command syntax Exceptions are commands that require authentication as the su command OS pwd queries the system for the current directory The output is directed to the current McIDAS text window lulimcidasIdata McIDAS eXplore adheres to the general McIDAS X conventions for the file system Thus the data ingested normally resides in the mcidas data directory and the source is in mcidas src directory etc Specific
301. umes containing Magellan SAR mosaicked images Altimeter data or Global composite data Similarly GETVGR imports Voyager 1 and 2 images of the outer planets and their satellites and GETGO and GETVO are used for Galileo Orbiter and Viking Orbiters 1 and 2 images respectively The GUI also allows a means to mount and unmount CD ROMs Importing Planetary Data from other than PDS CD ROMs Planetary data from other than PDS CD ROM sources can be imported into McIDAS eXplorer if the target data is in a FITS format file using the GETFITS command This enables the attached FITS header to be decoded to use the calibration and navigation information if any If the data do not come with a FITS header then assuming the size of the header is known and the data are stored in a simple binary format one or two bytes per pixel signed integers only MAKIMG can be used to import the data Any supplementary information about the navigation can then be attached manually using commands such as DDBUTIL and NAVUTIL The different planetary data for which there is explicit support within McIDAS eXplorer are described in the next section 2 12 3 PLANETARY DATA SUPPORTED BY MCIDAS EXPLORER The primary data supported by McIDAS eXplorer are the imaging data from NASA s various missions to solar system targets that have been published by the Planetary Data System PDS on CD ROMs To date the missions whose image data are available include the Voyager 1 and 2 mis
302. using TGET onto another workstation if McIDAS X and the the eXplorer extensions have been installed APPENDIX 98 USCLAS Spectrally classify a multi banded image using unsupervised multispectral classification inarea outarea KEYWORDS PARAMETERS inarea area to classify outarea Classified area with M spectral classes KEYWORDS BANDS BANDS BAND1 BAND2 BANDN Band numbers from the area to classify up to 6 Default is all bands present in the area CLASES initial of classes presented Default is 100 SKIP Pixel skip factor for iterative classification Specified numbers of lines and elements are skipped MUST BE lt 8 DEFAULT IS 4 ITER Maximum of iterations allowed Default is 35 MERGE Cluster Merging factor 0 TO 2000 If a divergence lt MERGE then merge two classes 0 NO MERGING DEFAULT IS 1400 SPLIT SPLITTING FACTOR 1 TO 10 IF BIG SMALL DIMS gt SPLIT SPLITTING 0 NO SPLITTING DEFAULT IS 3 0 NULL DATA DROP OUT DECISION ANY CLASSIFY AS ZERO IF ANY BAND HAS 0 ALL CLASSIFY AS ZERO IF ALL BANDS 0 DEFAULT IS ALL smallest of pixels required in a class DEFAULT 0 01 OF DATA LINE or STRETCH Output color stretch type LINE Linear stretch for class colors HIST histogram equalization stretch DEFAULT HIST MINPIX STRETCH APPENDIX 1 99 WHERE List inventory of the image data imported within MclDAS eXplorer as identified by target object spacecraft source and selec
303. ust be partially navigated in that the observer position vecter the picture body center information and time are available If the north for the image is also in the DDB then the routine can display the exact moon positions Caution Do not use when the moon is near the limb of the disc APPENDIX I 49 IMGCTR Determine the center using a conic fit of a planetary image for which limb points have been previously stored in a file LIMBxxxx where xxxx is the 4 digit area number using EDGES or other programs IMGCTR area_ KEYWORDS KEYWORDS FILE usually LIMBnnnn where nnnn is the area number Expected file format is described below If the displayed frame contains the image of interest the area_ need not be specified nor the FILE keyword as the LIMBnnnn file corresponding to the displayed image is read by default OPT BAD to list the points that deviate from the least squares general conic fit by more than the MAXDEV see below pixels REPLACE to replace the limb points in LIMBxxxx file with the edited points that match the fit criteria i e all points that are bad due to excess deviation from the fit are excluded COL graphics color level for the fit quality display GRAPH LIMB for displaying the limb points on the image CONIC to show only the quality of the conic fit or ALL to show both the limb points and the conic fit quality deviation in pixels for line s of points default MAXDEV Maximu
304. utput image by moving the data by displaying the area on a given frame and displaying the latitude longitude grid on it If that area was created using MAKOUT the screen will most likely be black i e no visible should be visible as all the data values are still null If the output area was created using AA then the source image will be displayed but with the new navigation attached 3 Actually writing the remapped image into the output area The third and final step is to remap the source area into the output area using the REMAP command REMAP source_area output_area spline_size where spline_size size of the bilinear spline block square in pixels Default is 50 which is a good number for an input image size of about 1000 lines x 1000 elements The minimum spline size allowed is dependent on the size of the source image and should be generally about 1 of the larger dimension Larger spline size results in a faster generation of the output at the risk of perhaps losing some accuracy in the projection KEYWORDS MERGE YES or NO SMOOTH flag flag where flag is YES or NO Depending on whether or not the output images is being assembled as a composite the MERGE option should be set to YES in which case the output of the remapping process is digitally merged with the data already in the area if non zero or above a certain digital number value or NO in which case any existing image data in the destination area is overwritten so t
305. vised when using this option Consult PLANAREA documentation for type size and adress information REAL CHAR or INTG size of entry on DDB in bytes 4 8 12 16 etc 4 bytes 1 DDB word address of the beginning of the entry value to be placed in the DDB only valid for PUT Examples To see the integer value stored in DDB address 200 NAVUTIL DDB SEE INTG 4 200 To see the double precision value stored in DDB address 517 NAVUTIL DDB SEE REAL 8 517 To input a double precision value of 100 into ODB address 517 NAVUTIL DDB PUT REAL 8 517 100 To input a 12 charcter string PARKER into DDB adress 142 NAVUTIL DDB PUT CHAR 12 517 PARKER Note FOR ENTRY TYPE CHAR WHEN THE OPERATION IS SEE THE ENTRY SIZE MAY BE ANY ARBITRARY VALUE EVENLY DIVISIBLE BY 4 WHEN THE OPERATION IS PUT THE ENTRY SIZE MUST BE 12 8 OR 4 shift_command L R U D B S The SHIFT option allows the user to interactively alter the stored values for the line element coordinate of the body center and the body pixel diameter A shift in any value will change the value by 0 5 pixels The effect of these changes is most easily seen with the MAP command L R move the center left or right U P move the center up or down B S increase or decrease the body pixel diameter Note When modifying the ddb of a displayed area the user should APPENDIX 74 NRMIMG NRMIMG NRMIMG Brightness Normalize an image using an analytical limb darkening fun
306. with the ESC key The user can create custom menus for different applications and invoke them as needed 1 4 McIDAS eXplorer Workstations The foremost requirement for McIDAS eXplorer is to have convenient access to the current and future planetary datasets Data from missions such as Voyager giant planets Viking Mars Galileo Earth and Venus and Magellan SAR imagery of Venus and surface altimetry reflectivity emissivity data are available on CD ROM s through the Planetary Data System and the National Space Science Data Center NSSDC The workstations required to use McIDAS eXplorer are the ones that can run McIDAS X with the exception that a CD ROM reader needs to be available either locally or over a Local Area Network LAN A typical configuration is a UNIX based workstation SUN SGI IBM RISC 6000 HP with 32 mb or more memory 1 Gb or larger capacity disk and a DAT or an Exabyte tape drive in addition to the CD ROM reader A color display preferably with 24 bit display capability is desired but 8 bit display support is adequate for many applications Similarly a CD changer such as the Pioneer DRM 604X can also be useful to provide access to as many as 6 CD s simultaneously not synchronously of course but not necessary and of course can be expanded through the SCSI interface to handle as many as 48 CD s on line up to 8 of the minichangers daisy chained to the SCSI port simultaneously 1 5 Planetary Data supported under
307. y data to be published on CD ROM volumes by the Planetary Data System beginning with Voyager 2 Uranus System images Volumes 1 3 continuing with selected Voyager 1 and 2 images of Saturn System Volumes 4 6 selected Voyager 1 and 2 images of Jupiter Volumes 7 8 and of the Neptune System 9 12 The entire collection of Voyager 1 and 2 images of the giant planets and their satellites and rings are now being systematically issued on Volumes 13 25 Since the Voyager project began before the SPICE navigation system was developed the images on volumes 7 12 and subsequent volumes do not have SPICE kernels available These images can be navigated using the Supplementary Experiment Data Record SEDR information directly until the SPICE kernels are available The SEDR data for the Voyager missions can be obtained through the Planetary Data System Further for photometric calibration of the Voyager data raw dark noise frames can be found on individual Voyager volumes however the shading correction files themselves have are not yet available on CD ROM s Assuming that the SEDR data is available in the encounter specific formats the respective images can be navigated as described below Pre processing of Voyager Images Voyager images were obtained using vidicon cameras Consequently they suffer from both geometric and photometric distortions The removal of these distortions is described elsewhere in this document For the purpose of image navigatio
308. y the unsupervised classifier is presently available within McIDAS eXplorer USCLAS Classification of a Multispectral image is relatively easy however requires several iterations to understand the results It generally is fairly CPU intensive The first step is to identify a region of an image that is to be classified Since the classification is a purely brightness signature driven process the shading due to varying illumination geometry if any should be removed in each spectral band If it is a planetary image this can be accomplished using NRMIMG if an analytic photometric function is known High Pass filtering may be sufficient in many cases as well Note that the classifier uses only the brightness values 8 bits Therefore if the original data are 2 byte per pixel the appropriate range of the data should be scaled into the 8 bit pixel domain using a suitable linear or a non linear transfer function using MAKESU The command COMBIN will enable multiple areas to be combined into a single area of desired spectral bands of 1 byte pixel data Once the input area is ready USCLAS will classify the image and write a new area containing the classified image with an appropriate color table The spectral classes themselves can be examined using the ELLIPS command For further reference look up A comprehensive Unsupervised clustering technique for the classification of remotely sensed data G Peltzer M S Thesis Civil and Environmental Engine
309. y defaulted by MAKESU for one or two byte per pixel areas but can be overridden by the user with the AREA keyword MAKESU contains five possible transfer functions SIGMOID the default middle level expanding EXP exponential or high end expanding LOG logarithmic or low end expanding INVSIG inverse sigmoid or range compressing and ENDSIN the industry standard percent ends in transfer function using the image histogram If an unrecognized TYPE is input a simple one segment linear function is generated The ends in stretch generates a five segment linear function with the middie segment being the largest covering the part of the histogram between the two percent values and the end segments displaying a mild degree of saturation The other four functions have a gamma parameter which changes the slope of the transfer function and a vertical or horizontal dn_value which controls the offset SIGMOID and EXP offset in the horizontal direction while LOG and INVSIG offset in the vertical Because of their shapes you will find that EXP and LOG are more effectively APPENDIX 65 controiled by the gamma value alone while you will often use both the offsets and slope for SIGMOID and INVSIG It will probably be necessary to iterate MAKESU several times to obtain the desired transfer function This is accomplished as follows 1 Keyin DF to load the desired area to a frame then keyin SF to display that frame 2 Set u
310. y from the McIDAS command window using the MAKFRM command The frames that are created dynamically can be of any size as limited by the available workstation memory McIDAS eXplorer User Interface McIDAS X typically creates four windows on the workstation screen when a session is started One of these is a command window which also includes a status line Figure 1 and is the primary user interface to McIDAS There are multiple text windows 1 and 2 of which only one is active at any moment selected by clicking on a mouse button in the par ticular window or from the numeric keypad by pressing 1 or 2 key The window active when a command is entered contains the output from that command The fourth window is the image display which is sized according to the frame size specified in the start up procedure McIDAS eXplorer supports various forms of user input text or command oriented supplemented by function keys and single letter key strokes and a Graphical User Interface GUI The function keys are user programmable to fit the particular application needs as weli as utilized in a a menu system which is invoked with the ESC key which prompts the user for the name of a menu file The user can communicate his input to eXplorer in two other ways besides the Command window The GUI is based on the Tcl Tk script and is user tailorable as well as a Function Key based menu system which can also be adapted by the user as needed These two
311. y record for the data that contain enough informaton to inform the user of what was done to the data For image data McIDAS eXplorer maintains an audit trail in which applications programs append an entry containing all the command parameters that were invoked in gt ormation Systems Newsletter Februur The objective of A A AA AX e ee e re McIDAS eXplorer is to bring to the planetary es community the tools rn ao Se a that the terrestrial PP _ r meteorological ee r Krr A community has been using to analyze AA mm a er oe oe weather data and model output U CD E a eE 294 e 17 Figure TA ie A s HE S tr y AT ES gren UHRE MISC 2 McIDAS image display window ORIGINAL PAGE Y 12 L February 1994 POOR QUALITY TE 929 RU RADAR GEBROWSES O Eom 70317 18 106787 O8 VIOLET CLEAN A 70581 77 012032 00 UVW 7 199 NA S HA C2 T UFF Te AE TRT T Le 93067 7i 65922 gt ci wibR 2 Ei 1019 943 MAGES LAM RADARS 9 C URONSE O OONIAG ele E lt E E on 8 S TA laud a gt es Aa P Ima ge 44 68 that particular processing step This processing history can be queried either by the user or by other programs to determine the processing status McIDAS display screen The display frame contains much more information than just the visible image in the McIDAS environmen
312. ype band defaults are displayed area BRIT band 1 except for 2 byte data where calib_type 2BYT frame magnification frame on which to display image using NAME ODNin hiDNin loDNout hiDNout hes and output limits for stretch function defaults are 0 255 0255 APPENDIX 64 REMARKS Tutorial A stretch table is generated using the plotted function and is stored under the indicated NAME That name can be used as the SU argument to the DF keyin to guarantee that the dynamic range of the display is used to maximum advantage If FRAME and AREA are set the DF Kevin will automatically load the area to that frame using the NAME stretch table It is often useful to iterate several times in order to reach an optimum set of parameters for the stretch table Often one has to cc npress or expand the dynamic range of an image to fit the dynamic range f the display screen or printer output This is often referred to as changing the gamma of the display medium Many times this is true for one byte data but it is especially true for two byte data which generally has a dynamic range much too large for a CRT to adequately display with good contrast resolution One then has to choose what small portions of the brightness dynamic range in the original image will be displayed on the CRT MciIDAS merely defaults to a simple one segment linear enhancement from the frame buffer to the screen which may be modified with the EB command

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