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Texas Cookbook - Caltech Submillimeter Observatory

1. 10 11 Now stop the data reduction processes If the merging is finished type c in the the slicing window and q in all the other IDL windows c tells the slicer that it is the last observation of the night and will slice it without waiting for the next observation to be written Then type exit in all IDL windows and then close them Back up the data observer allegro Do tape back ups observer allegro observer allegro Eject the first tap you don t need to backup_home_disk data00 backup backup day yyyymmdd Note the total number of Mb written to the tape on the case insert tape eject e insert copy 2 and repeat You can leave the second tape writing wait for it Point the dome East UIP gt az 90 and exit the UIP Go get some sleep you ve earned it 34 10 Observing with SHARC II written by MMD June 2006 updated by NJE Dec 06 further updates by MMD June 2008 10 1 Setting Up SHARC 10 1 1 Before Leaving Austin Prepare a list of calibrator sources visible at different times throughout the night see the SHARC II webpage for information on suitable calibrators Load new sources you know you are going to observe into catalogs and make sure existing sources have the correct coordinate information See Section 10 2 2 for information on how to do this Bring a blank SHARC II log sheet with you Sometimes there aren t any blank ones left up at the telescope 10 1
2. 545 0 5 0 912 0 11 0 545 0 14 0 544 0 5 5 534 0 5 0 459 5 6 0 540 0 5 0 JT obser K 134 5 3 2 134 5 3 2 134 5 3 2 134 5 3 2 134 5 3 2 134 5 3 2 134 5 3 2 134 5 3 2 134 543 2 134 5 3 2 134 5 3 2 134 5 3 2 134 5 3 2 134 5 3 2 399 9 9 343 5 9 9 399 1 10 2 399 E L0 2 3595 9 10 2 356 0 10 2 356 6 10 2 V GHz 211 2 211 2 215 4 218 2 218 4 219 6 219 6 220 4 220 4 225 7 225 7 244 9 342 9 342 9 244 9 335 0 338 5 345 7 348 3 349 3 356 0 For moon measurements we list the number of days since new moon Uncertainty assumed to be 4 596 Extrapolated from 1990 model predictions 4 Old 230 GHz receiver before 10 91 NMB 0 540 024 0 60 0 03 0 53 0 044 0 564 0 044 0 46 0 044 0 51 0 024 0 72 0 03 0 554 0 024 0 68 0 02 0 50 0 044 0 53 0 034 0 45 0 034 0 45 0 04 0 38 0 05 0 833 0 03 0 76 0 02 0 78 0 02 0 78 0 01 0 77 0 01 0 70 0 01 0 78 0 02 Measurement made at the subsolar point so age given as 15 0 days full moon 79 Table 5 2 Average CSO Main Beam Efficiencies Before about 1993 Source Receiver average nmg of measurements Mars 345 0 57 0 11 7 Jupiter new 230 0 71 0 02 7 345 0 53 0 05 18 Saturn old 230 0 51 0 05 9 new 230 0 67 0 06 3 345 0 41 0 05 2 Moon new 230 0 83 0 03 1 345 0 76 0 03 6 76 18 8 Things We Always Assume But Don t Always Measure In the following two sections we look at two aspects of
3. 21 3 Computer Hang up or Crash This happens much less often in January 2002 after both the antenna computer and the backend computer have been replaced In the case of the antenna computer a crash will leave the time not updating on the antenna computer monitor the big TV screen It s probably a good idea to push emergency stop Read the instructions for the new antenna computer on the CSO web page First check for memos to see what the latest variation on the procedure is If the terminal is out of control and cntrl C does not get you a UIP gt prompt you have to break out of UIP Type cntrl Y Then reenter UIP and follow the above procedure You will also need to reopen catalogs and set acquire limits as well as checking all your other parameters especially note FAZO and FZAO 85
4. 9 3 Real Time Data Reduction les 9 4 Pointing Corrections ooo 9 5 Trouble Shooting 2 5 deeg Roc ee ber Ree MIR ee RUE RP an E 9 6 Shutdown Procedures e 10 Observing with SHARC II lO I Sett ng Up SHARG 2 face udi e ee Ee 10 1 1 Before Leaving Austin I0 1 2 At the telescope ci eed eo edo seb ox E a E e SR 10 2 Observing Unchopped us lea A equ DeC Be ead 10 2 1 Calibration and Pointing es 10 2 2 SOUPCES uu Sot A e VR INTR ia Rer geek eee p Eoo RECH 10 3 Data Red ction s i ue Aa ne Tere ER aote o ne 41 etd e ets 10 4 Shutdown ix ok Ree Ae EE RN PASE tk RC 11 13 13 13 16 16 17 19 19 19 20 21 21 22 23 23 23 25 27 27 29 29 30 31 33 10 5 SHARC II Problems 4 4 sss 10 5 1 Can t Get a Good Level 10 5 2 What To Do If You Can t Connect to the DSOS 11 The Tipping Meter 11 1 Measuring 7 Manually suig nna ae led EU Pc lee Se is 12 CLASS Notes 12 1 Sample CLASS Session 2 2 ee 12 2 How to See Your Last Scan ee 12 3 Advanced Classis accen ete e Dux OUR An Ee qoe dote OAS 12 4 Changing Sidebands 2A 12 5 Mapping Data Reduction e 13 List of CLASS Macros in TEXAS PROC 14 List of GREG Macros in TEXAS PROC 15 The CLASS Startup File 16 CLASS and GreG Macro Descriptions and Directory Management 16 1 CLASS Macro D
5. Thus most of our observations were incorrectly DSOS corrected The point is that this is not a perfect solution It might work and it might not so don t blindly follow this assuming everything will be fixed But if it s the middle of the night and the weather is good and you have no other option go ahead and follow this procedure It just might work 44 11 The Tipping Meter There is a tipping meter mounted on the shed and working at 225 GHz It automatically measures the transmission periodically and stores the results These can be used directly if you are at a similar frequency There is some information on scaling to other frequencies in a memo by Colin Masson but beware that the meter may not be reliable at very low values of r It probably bottoms out around 0 027 So if you are lucky enough to see numbers close to that you won t know just how good it is There is a 350 micron tipper running as well It is more realistic at low 7 The current 7 data are on the antenna computer screen but it is usually good to average a bit Various plots are accessible from the CSO web site Follow the links for Observer information weather information etc The web gives you a nice visual display but not numbers We have a program called tauupdate in the bin directory on the UNIX machines that should be accessible from any window on a UNIX machine It will provide the most recent values along with some statistics If the taumeter gets hung up
6. 4 50 50 50 50 60 60 60 UIP gt OTF 110 110 2 10 10 10 cal foc for each position aGddddddddaddad 21 7 4 Chop slewy For weak sources or sources with wide lines it may be appropriate to use the chop_slewy command In this mode the secondary chops while the telescope takes observations in a nodding mode The basic nod pattern is The basic command is UIP gt chop slewy n FOC TCAL ATT LO where n is the number of cycles that you want For instance if you setup with SPEC 20 the do chop slewy 2 you will have 160 seconds of total ON integration time Before you can start the chop slewy command you must set up the chopping secondary This is accomplished with the command UIP gt secondary c f tolon toloff where c is the chop throw in arcseconds f is the frequency in Hertz and tolon and toloff are the tolerances in the ON and OFF positions If you make these too small you will have trouble getting any data but if you make them too large you will smear the beam around Using tolerances of 6 arcseconds is reasonable for chops of 90 arcseconds or less We have typically used 1 123Hz in the past it is not a multiple of any common frequencies and has good efficiency When you are finished with your chop slewy observations make sure to type UIP gt secondary stop to stop the chopping secondary UIP gt secondary c f tolon toloff cruncher will tell you how
7. just hit cntrl C and the macro will continue There is also a macro called ADD which will look for new data so again you may need to use cntrl C find all the scans with the data selection parameters you have chosen e g source name offsets line name sum them smooth them take out a baseline plot them and show you the zero line and the rms noise 12 3 Advanced Class If you have written your scans to a reduced data file you can do various more sophisticated things To do this it is often convenient to run a second CLASS job in a separate window Make the input file the file you used to write your reduced scans in in this example we will use the file name x red Note that you will not be able to do this until you have finished writing into x red and changed the file out on the main CLASS job You can list the scans in x red with the list command and send the output to a file and print it on the laserwriter by typing list output x lis system Ip x lis The second command says deal with what s in quotes at the system operating system level and lp is the unix command to send a file to the laserwriter So in this case the quotes really need to be there 48 A slightly more exciting possibility is to print out the results of the Gaussian fits using the following commands print fit output x fits system Iwprint point 6 x fits The qualifier point 6 switches to small print which will be hard to read but w
8. you have to restart the tipper by going out to the shed green key unplugging and plugging back in the power cord to the tipper get someone to show you where it is Look up the Mini how to page on the CSO website under Local Information for instructions on how to restart the transfer of files The availability of the tipping meter has made doing your own tipping nearly obsolete unless you are working at an unusual frequency 11 1 Measuring 7 Manually To measure 7 manually we need to measure the sky temperature at different values of airmass Macros have been defined that allow you to move the telescope to airmasses 1 1 5 2 3 4 and 5 without needing to calculate the zenith angle Actually 1 airmass is usually unnecessary Simply type UIP gt M where can take the values 1 1 5 2 3 4 or 5 Let the telescope sit for a few seconds at each airmass so that you can measure the sky value in DC voltages off a meter Then insert a hot and cold load into the receiver measuring the load values in the same manner as the sky values Actually it is a good idea to check the hot and cold loads at each air mass to check for receiver level shifts with air mass When you are finished you may be able to plot them and get a fit UIP gt TAUPLOT Follow the instructions 45 this page left blank 46 12 CLASS Notes CLASS is the data reduction package developed at Grenoble and used at the IRAM 30 meter It is a reasonably nice packa
9. 1 9 3 849 250 165 5 2 5 2 865 110 145 1 2 3 3 870 57 139 5 8 3 Saturn 31 uu 133 0 4 2 1 90 149 3 4 1 1 150 137 0 11 0 1 310 130 134 5 3 2 2 451 270 137 0 4 0 2 580 420 122 2 1 1 2 666 170 112 3 3 2 2 724 625 119 2 1 2 2 849 250 112 9 1 1 2 References 1 Ulich 1981 AJ 86 1619 2 Hildebrand et al 1985 Icarus 64 64 3 Griffin et al 1986 Icarus 65 244 70 18 7 Using the Moon as a Calibration Source There s a moon in the sky It s called the moon And everybody is there including Saturn Mercury Saturn Venus Saturn Mars Saturn Jupiter The Van Allen Belt There s a Moon in the Sky Called the Moon The B52 s The properties of the thermal radio emission from the moon are determined by the conditions under which the surface layer becomes heated and cooled during the course of a lunation The behavior of this emission as a function of lunar phase is determined by the electric and thermal properties of the lunar surface material Following Krotikov and Troitskii 1964 Soviet Phys Usp Engl Transl 6 841 and Linsky 1966 Icarus 5 606 1973 ApJS 25 163 we assume that the lunar surface is smooth and uniform with temperature and depth independent thermal properties The surface temperature as a function of depth longitude latitude and time T x w t can be found by solving the equation of heat conduction OF OT x V t where p c x t and amp x t are the density specif
10. 2 At the telescope Login to kilauea in the control room as texas with the usual password Make a run directory as usual Type uip to start the User Interface Program Make sure the telescope is pointing east and also load the SHARC II calibrators catalog uip gt za 45 uip gt cat sharccal cat Open Shutter e Check for obstructions out in the dome e Pull out the big red stop button in the control room e in UIP type shutter open e If the sun has not yet set only open to 50 or 60 of the maximum and MAKE SURE the dish does not receive any direct sunlight Open a new terminal For a display of the sky at the CSO type orrery amp Prepare to start the DSOS Dish Surface Optimization Software On Desktop 2 open two terminals In this guide the notation winX Y means terminal Y on desktop X Thus win2 1 means you are in terminal 1 on desktop 2 To start the DSOS type win2 1 ssh visitor0128 171 86 102 password Dishm3 DSOSdaemon DSOSserver win2 2 ssh visitor0128 171 86 102 password Dishm3 35 If the control room computer is unable to connect to visitor 128 171 86 102 see Section 10 5 2 Power up SHARC II go out into the dome on the second floor control room level e Change alidade power controller from charge to operate on the the panel near the door e On the back of the instrument next to the cryostat you should see two green lights and one yellow light Flip the power switch to on yo
11. 5 5 4 170 5 5 4 170 2 5 4 168 8 5 7 168 8 5 7 168 5 5 8 168 5 5 8 168 2 5 8 GHz 330 5 345 7 345 8 345 9 345 9 393 0 356 7 218 2 218 2 218 4 219 6 220 4 244 9 278 7 330 6 332 3 335 0 341 3 342 9 345 8 345 9 348 3 349 3 354 6 354 8 355 0 356 0 362 7 362 7 364 1 364 1 365 4 NMB 0 46 0 02 0 663 0 03 0 69 0 02 0 50 0 03 0 42 0 02 0 66 0 04 0 64 0 02 0 73 0 02 0 67 0 02 0 74 0 01 0 72 0 03 0 71 0 03 0 71 0 02 0 69 0 02 0 58 0 02 0 46 0 01 0 51 0 03 0 47 0 01 0 54 0 01 0 55 0 02 0 52 0 01 0 52 0 02 0 54 0 01 0 57 0 01 0 44 0 01 0 59 0 01 0 47 0 01 0 57 0 02 0 55 0 02 0 603 0 03 0 54 0 03 0 53 0 03 Source Date Saturn 08 91 10 91 08 91 08 91 08 91 08 91 10 91 08 91 10 91 07 91 08 91 08 91 07 91 10 91 Moon 08 91 03 90 03 90 07 90 01 90 01 90 03 90 beq x Opol arcsec 18 3x 16 5 17 2x15 6 18 2x16 5 18 3x16 5 18 3x16 5 18 3x16 5 17 1x15 5 18 2x16 5 17 1x15 5 18 5x16 7 18 3x16 5 18 3x16 5 18 5x16 7 17 2x15 6 13 9 days 17 6 days 15 0 days 15 0 days 15 0 days 15 0 days 15 0 days Table 5 1 continued Dun arcsec 33 0 33 0 32 3 31 9 31 8 31 7 31 7 31 6 31 6 30 8 30 8 28 4 20 3 20 3 28 4 20 8 20 5 20 1 20 0 19 9 19 5 Ti planet K 24 5 0 5 24 5 1 0 25 0 2 0 27 0 2 0 220220 25 0 1 0 31 0 1 0 2 O10 29 5 0 5 26 0 2 0 27 02 0 26 5 2 0 46 5 4 0 34 5 3 5
12. If the A D light is illuminated use aaa aa which is 0 25 degrees greater than the current AAZ If the light goes out you may be back in business so restore the normal limits with UIP gt LIM If the ultimate limit light is illuminated you have exceeded the hardware limits You must be very careful not to make a mistake here Again type the appropriate AZ command to move in the correct direction but the antenna won t move until you depress temporarily the switch labeled ULTIMATE LIMIT DOME BYPASS on the right of the control box Watch what happens and be prepared to hit the emergency stop Once you have it back within the hardware limits you won t have to depress the switch and once it is back inside the software limits you should reset them as above Once you have completed these steps try some small moves in azimuth only first If the TLENGTH does not stay close to zero or if you again exceed the limits the next thing to check is the circuit breaker for the dome motors It is found in the UPS room directly under the control room and is in the tall skinny grey cabinet immediately to your right as you enter The dome motor breaker is number 1 If a relay indicator light in the locker on the other side of the UPS room is red the breaker needs to be reset Switch it off and back on If this was the problem you may hear the dome motors start up If all this fails you may 84 as well reload the antenna microcomputer see next section
13. Plots CO 3 2 and 2 1 spectra and ratio on same page Reads a file produced in CLASS with the command GREG name FORMATTED Author NJE START Startup macro which prompts for and opens the graphics environment and the input file and also initializes variables Author NJE TAILER Macro called at the end of all macros which sets the SIC variable VERIFY to ON Author JGM WINGS Makes contour plot of line wings Simpler version of 2WINGS GREG Author NJE 98 16 3 How to Add a CLASS or GreG Macro to texas proc If you have a CLASS macro that you think is of general interest the procedure for putting it into the texas proc area is as follows 1 Make the macro as general as possible This means that you should take out commands such as FILE IN 99DORK91 DAT which tie the procedure to a specific input file 2 Call the macros HEADER and TAILER at the top and bottom respectively of your macro These two macros set some variables which will make your macro run in a prettier fashion and therefore will be quite attractive to others Use p header and 9p tailer 3 Insert a short description of the macro in the text file USER TEXAS PROC MACRO TXT This text file is used as a look up table for finding macros 4 Tell Neal Evans that you have added a new macro to the general procedure area if you don t do this it is quite possible that during a future observing run Neal will suddenly become possessed by Bertha the Cleaning L
14. SOCTO91 is 500 2311 32 E DE 50 1824 28 SOCTO91 de 500 2252 3l Ve ES s 50 1776 28 3 2 4 a Feb92 1328 500 3179 31 ur ad 1329 50 3179 311 CS7 6 5140 July90 1781 500 1449 3 8 DR210HJM Nov90 1354 500 1304 10 4 m La d 1355 50 918 9 0 CS5 4 5140 HNOV89 1657 500 920 5 6 du 1963 500 1720 6 0 e eg Nov90 2119 500 3102 6 5 M e A E 0583 TU These were corrected upward by about 5 K to account for higher baseline placement 79 on these noisy spectra 80 19 Transferring Files to Austin To transfer files to or from Austin use ftp from the unix machines This usually goes smoothly To transfer the data files you can be in your run directory and use the unix ftp to ftp to Austin The basic data files should be put in data8 CLASS Data which can be accessed from any of the group computers You will need to know the password for user class If you do not just put all the data in some space that you control and ask someone to sort it out Reduced data should NOT be put in data8 CLASS Data Put those files in your own personal Class space 81 this page left blank 82 20 Using ASTRO to make Plots of Source Elevation vs Time It s always useful to be able to predict the elevation of a source at a given time on a given day This is easily done by using ASTRO which is one of the complementary packages that comes with CLASS To make things even easier we now have a macro called ELEV_PLOT ASTRO which resides in h
15. a problem it is probable that the power is too low The symptom will be zeroes or very small values for the attenuation The problem probably lies in the IF Converter Box The first thing to check is whether the various switches are set correctly to feed power to the AOS You can check this with a program ifpmon which shows the settings or by the lights on the panels The panels also have test points for the various power supplies It is not uncommon that they are not correct Check them with a voltmeter If not nominal power cycle the top box that is mounted in the rack labeled 4 8 GHz IF Processor Unit DC Power Unit Then check the voltages again If you still lack enough power your only recourse is to get more power from the receiver Failing this give up EEE ccc cec 15 6 3 Tuning Frank s Receiver The main issues with Frank s receiver are getting a lock and the fact that you have to do B field checks by hand since there is no computer to scan for you We are using an SMA lock loop which is indicates a lock by a green light coming on There are also two yellow lights on either side which indicate that you are close but not really locked If you get the yellow lights out and only the green light on that is ideal However the lock system is quite fussy about power levels So tune the Gunn based on tuning curves and watch the spectrum analyzer for a strong signal If you get one that you can make go away by detuning you are
16. at zenith angles lt 10 and gt 65 Note though that the measurements at these low and high zenith angles were taken during the same observing run so that further measurements of yg at these extreme zenith angles should be made to confirm this result 18 8 2 Possible Errors in the T From AOS Compression To monitor any contribution to the T4 scale made by the AOS measurements of the Von Vor Vnot and Maud voltages on Jupiter during a position switched scan were made during the February 1992 observing run at the CSO This is meant as a comparison between the T scale which the AOS gives us and the T4 scale which we can calculate directly from the voltage measurements from a total power detector The measurements spanned a range of frequencies and zenith angles Two separate skydip measurements were made from which we are able to derive 7 and mot giving us a measure of the consistency in the sky conditions for this data set Each measurement was done following a check of the pointing which was very stable throughout this observing run In the data below T4 has been calculated using the equation listed in 86 1 From these measurements we find that T4 AOS TA direct A plot of the individual ratios which went into this calculation is given in Figure 6 4 Therefore the difference between T measured through the AOS and T measured directly from the receiver is lt 5 1 02 30 05 78 18 9 Line Calibration Tests We have c
17. duration of the test The pointing was checked at the beginning in the middle and at the end of the test with the following results FAZO 19 9 FZAO 267 9 at the start of the test FAZO 19 7 FZAO 268 8 in the middle of the test FAZO 25 3 FZAO 275 7 at the end of the test mean values FAZO 21 6 3 2 FZAO 270 8 4 2 Therefore the pointing was stable throughout the duration of the test with an rms uncer tainty of 0 8 The results from this test are shown in Figure 6 1 For zenith angles less than 68 T4 124 842 5 K which indicates that the CSO main beam efficiency at 220 GHz varies by 2 for zenith angles lt 68 Note that this value for T4 is about a factor of 1 4 lower than other values for T derived from other 230 GHz receiver measurements made during this observing run This is probably due to a zero offset in the mixer Therefore the T4 values derived from this analysis should not be used to derive ry T 2 0 x 280 0 x 77 Analysis 2 Individual measurements of nmg from our measurements of Jupiter and the moon are shown in Figures 6 2 and 6 3 The data in Figure 6 2 indicates that for the 230 GHz receiver 7p varies by 5 for Jupiter measurements made at zenith angles between 25 and 60 There may be a decrease in Nu for zenith angles lt 20 but more measurements need to be made to confirm this Figure 6 3 shows that for the 345 GHz receiver yg falls by 15 for Jupiter measurements made
18. example it will now use the FFTS If you are working at high frequency you may have better luck pointing with the chopping secondary running 8 1 Using a continuum source If you have a continuum source e g a planet as your pointing source then just type UIP gt off position 300 altaz asym UIP gt acq 3 60 UIP gt spec 10 nobaseline UIP gt five 1 2 one where 1 is step in arcseconds for the five point map half the beam diameter if the pointing source is small half the source size if it is large and 2 is the number of channels on either side of the center that you want to average over 200 is a reasonable choice If you have more than one backend and you want to use e g the FFTS1 you need to add the qualifier FFTS1 at the end of the five command If the Spectrometer passband is well behaved you can leave this number blank and it will use the entire spectrometer passband If the planet is weak you may want to be more careful The qualifier ONE tells it to take one OFF position and use it for all the ONs If you leave that off you will get a separate OFF for each ON This will take twice as long but may give better results If the planet is strong e g Jupiter and you have a good system temperature you can use a shorter integration time NOTE if the NOLO does not stop the Gunn Frequency from changing and you are tuned for a source with a large velocity you can keep the Gunn locked by using the LO command with
19. for an offposition 10 away we changed the tolerance to 1 for the off position using the command UIP gt ACQUIRE_LIMITS 3 60 where the first number is the limit for the on position and second is for the off position We also found that integrating longer in the spectrometer gave good baselines under good conditions The longer you integrate between position switches the less dead time but you may get bad baselines Up to 60 sec has worked but 10 sec is a good fall back time You can just take a calibration scan by typing UIP gt TCAL offset equatorial where equatorial tells the computer to step the telescope in Right Ascension You may also step in declination by typing UIP gt TCAL offset 0 equatorial offset is the number of arcseconds that you want the telescope to step before doing the calibration scan Parameters are no longer sticky so type this full command each time you want to take a cali bration scan Note that the new UIP seems to take the calibration scan at the off position so you can type TCAL with no qualifiers and if you have put in an off position UIP gt OO where is the number of cycles of integrations to perform both on and off the source 4 is a good number to start with if things go smoothly you can increase it The total integration time in the on position will be the number of cycles times the integration time per cycle set by the SPEC command If you want to make a simple fiv
20. image sideband to which he is switching the line name to be assigned to the corrected scans and the output file to which the corrected scans are to be written Inputs can also be entered directly using the command SIDEALL VRAD FREQ LNAME FILEOUT Author SZ START Startup macro which prompts for and opens the graphics environment and the input file and also initializes variables START is now a combination of the macros INIT and SYMBOLS Author RIP SUMALL Searches an area around a source for scans and sum all scans for a identical offsets You may want to set source and line before executing the marco User is prompted for the RA offset range for the search the DEC offset range for the search the spacing of the positions that you want to add to the list and the name of the output file to which the summed scans will be written Note that it will do a find all at each offset so previously dropped observation numbers will reappear and all version numbers will be found Can also be run using ASUMALL I1 I2 J1 J2 SPACING FILEOUT where I1 and I2 are RA range in units of SPACING J1 and J2 are DEC SPACING is in units of ARCSEC Author SZ TAILER Macro called at the end of all macros which sets the SIC variable VERIFY to ON Author JGM ZLINE Plots a zero line on the current spectrum Author JGM 57 16 2 GreG Macro Descriptions 2WINGS Makes contour plot of line wings Author NJE 4SPECNJE Used for making contour maps
21. of outflows From a file produced in CLASS using PRINT FIT will produce a contour plot of the red and blue wings of an outflow Author NJE 4SPECTRA Plots 4 spetra with Gaussian fits overlayed on the same page Reads from a file written in CLASS with the command GREG name FORMATTED Limits for all boxes are based on the first spectrum in the file Author NJE CHANNELMAP Makes spectral channel contour maps Reads a file produced in CLASS with the command PRINT AREA v1 v2 Author RIP CHAN A more user friendly version that also works with files produced in class with the command PRINT AREA v1 v2 Author MC CONTOUR General contour map making routine Reads a file produced in CLASS with the command PRINT FIT Author RIP CON General contour map making routine which tells you the range of your data and lets you select contour levels interactively Reads a file produced in CLASS with the command PRINT FIT Author MC HEADER Macro called at the begining of all macros which sets the SIC variable VERIFY to OFF and sets the ON ERROR variable to QUIT Author JGM OUT Produces laserwriter hardcopy of the screen graphics To check laserwriter queue type DCL SH QUE LW when inside GreG or SH QUE LW at the VMS level Author NJE PLOT Simple two dimensional plotting routine Will plot X versus Y for any two columns defined by the user Reads a file produced in CLASS with the command PRINT FIT Author RIP RATIOS
22. off and set the alidade power controller to charge Shut down the DSOS 41 win2 2 control c stop agent from running DSOSbase Power down the eight power supplies win2 1 control c close DSOS status display Turn off scanning and chopper as necessary uip gt sweep stop uip gt sec stop Set up a delayed He cycle if necessary Log out of all terminals and then log out of kilauea Sit and stare at the shutter status display because chances are you are very tired and ready to leave but it is still closing because it is really slow When it finally finishes closing push the red stop button Turn off all lights lock the doors and drive down the mountain If it is not your last night eat breakfast grab a few hours of sleep and do it all over again the next night If it is your last night eat breakfast grab a few hours of sleep and head to the beach 42 10 5 SHARC II Problems 10 5 1 Can t Get a Good Level In Dec 2006 we noticed a problem when we first tried to level SHARC II Half the array never changed color on the displays After several tries at leveling we exited from Sharc Server etc and from the window where one starts the DSP We then went through all those steps again and this cleared the problem Based on advice from Melanie if that had failed we might have had to also exit from the DSOS programs because SHARC and DSOS communicate Do the end of night shutdown on DSOS in particular DSOSbas
23. peakT4 CS7 6 peakT 4 CO3 2 peakT 4 CS7 6 The difference between these two tunings was then about 13 The pointing was good to about 4 08 5 so pointing is not likely to significantly affect the measurement of the sideband gain ratio Therefore this estimate of the variations in the sideband gain ratio would imply an accuracy of about 1096 Note that previous tests in which the receiver was deliberately mistuned produced much larger differences so careful optimization is probably a required but not sufficient condition for having the response in the signal and image sidebands be equal For common lines in the 345 GHz range you should observe a standard source from the paper by Wang et al These sources were observed with a sideband filter The paper with these sources should be available at the CSO If not complain loudly 3 29 0 12 for tuning 1 2 86 0 14 for tuning 2 63 18 Measuring Telescope Efficiencies by Jeff Mangum March 24 1992 updated by NJE January 2 2010 18 1 The Procedure Since we often use Mars Jupiter and Saturn as continuum pointing sources measurements of the telescope efficiency can best be made immediately following a pointing check on one of these objects The lunar brightness should also be measured a couple of times during an observing run if it is available To measure the planetary and lunar telescope efficiency use the following procedure Mars Ju
24. possible with UIP gt REPLY ENABLE 6 5 Switching from Wide Band to Sidecab Receivers To switch from one of the wideband receivers to the sidecab receiver is fairly easy but there are a few steps to remember For this example we assume that you were observing with Frank s receiver with the secondary chopping and the wideband AOS you are switching to the 230 GHz sidecab receiver using the 50 MHz AOS AOS2 and not chopping First attenuate Frank s receiver always a good idea to protect multipliers and SIS from tran sients Then execute the following commands JIP gt SECONDARY STOP JIP gt OBSERVE sourcename JIP gt LO linename IF 1 5 LOCK NEW JIP gt SPEC 5 AOS2 NOAOS5 JIP gt TERTIARY SIDECAB JIP gt POINTING 230 SIDE Then enter any previous values for FAZO and FZAO Check for Eccosorb in the optical path often put in when using receivers at other foci and remove as needed Then you can tune point observe If you get the SYNTH FAILURE 06 message the usual trick described above may not work IF you are keeping the same line So give an LO command that selects a different sidecab receiver and then another that puts it back to the one you really want au ec ane eni eni 17 this page left blank 18 7 Taking Heterodyne data Texas Style This section assumes that you have entered UIP and set up your data file the receiver the spec trometer etc If not read the section on starting up the CSO computer F
25. real time Observe a pointing source using pointing w rot mac This will take two observations each scanning in perpendicular directions If you ve entered the source name in the files described above then it will automatically reduce when it s finished Once the observations has gone through the first four auto windows slice_files clean Dles ptg map files ptg centroid_files you can then determine the pointing cor rections to make using a simple idl script In the idl window type IDL gt boresight source name obs num UT date in yymmdd fazo fazo used for observa tion fzao fzao used for observation This will open an idl plot window showing the source and the position of the peak of the source In the bottom right hand corner it gives the new pointing offsets In the upper right hand corner you ll find the calculated shifts between current and new FAZO and FZAO On ocassion the scripts won t be able to centroid for various reasons the source is offset by too much the maps look funny etc this should not be a large concern unless it happens to a large majority of your pointing observations We usually take the offsets found by the first of the two observations and don t worry about the second Use whichever you can if one is bad it s no big deal For the July 2007 run we realized that there is a huge sine wave in the FAZO and FZAO versus azimuth and a smaller linear variation with zenith angle There is a directory home kilau
26. similar Va and that FREQUENCY is in MHz 5 Intensity calibration and make plot you need to rescale data according to the tele scope efficiencies and then make plots using the your favorite package Here is an example reducing CO3 2 data from 21DEC89 DAT observed with CS7 6 L setup from the source GL2591 1 Frequency Calibration FILE IN 21DEC89 DAT FIND ALL P FCALL 511 9 0 495 21DEC89 2 Baseline Removal FILE IN 21DEC89 MODIFY 51 3 4 5 SET LINE CS7 6 L SET SOURCE GL2591 FIND ALL SET WINDOW 40 160 CO line is very wide QP BASEALL 1 GL2591 NEW Linear Baseline Switching Sidebands FILE IN GL2591 BASE FIND ALL P SSIDE 24 3 345795 97 CO3 2 U GL2591 Combine scans at each offset FILE IN GL2591 SIDE P SUMALL 36 27 27 27 9 0 GL2591 9 arcsec spacing Make a grid of spectra FILE IN GL2591 SUM FIND ALL SET MODE X 100 100 SET MODE Y 2 15 P MAPCSO If you have problems please report them to Neal Evans 52 13 List of CLASS Macros in TEXAS PROC 50 CLASS sets TELESCOPE to CSO 50MHz for data selection 500 CLASS sets TELESCOPE to CSO 500MHz 2 for data selection 1500 CLASS sets TELESCOPE to CSO 1 5 GHz to get the 1 5 GHz AOS ADD CLASS Sums smooths and plots ADDOTFS gt adds OTF scans undocumented alien COPYALL CLASS Copies all scans in index to output file BASEALL CLASS Removes baselines from all in lis and writes FFTALL CLASS Allows interactive rem
27. stops tracking and the TLENGTH number in the bottom right of the antenna computer will flash Your observation will hang and you ll have to kill it To fix this follow the instructions in the troubleshooting section 821 Antenna Computer Timeout When this happens the UIP will beep give a message and the observation will hang First kill the macro Then exit the UIP if it s frozen ctrl y will boot you out Then outside of UIP type run uip exe locks Get the antenna proc id stop id Proc id Go back to the uip and restart the antenna computer UIP gt ant restart nosync Go back to observing 9 6 Shutdown Procedures A more detailed description of the shutdown procedure can be found on the CSO Bolocam webpage 1 Start dome closure 2 Stop DAS On Andante via remote login from ahi hit the large red stop button in the DAS LabView window 3 Move the telescope to zenith angle of 25 UIP gt za 25 4 Move the telescope to az of 90 make sure sun has set first UIP gt az 90 5 Stop tel util on allegro and close the four associated windows observer allegro kill tel util 6 Set the rotator to a standard angle of 10 15 degrees If the dewar is not at the proper rotation angle the fridge cycle will not be successful observerGallegro interactive gt 888 If it is not already between 10 and 15 degrees move it there gt 15 Check to make sure it made it there by typing 888 Then exit by typing 999 33
28. temperature calibration which are always assumed to be of minimal importance but are rarely measured 18 8 1 Zenith Angle Dependence of the Primary Beam Response Two separate analyses of the change in zenith angle of the primary beam response have been made In the first I present the results from a dedicated experiment where I measured the change in T for Jupiter as a function of zenith angle during one night In the second analysis I have extracted the zenith angle dependence from all of our nmg measurements using Jupiter and the moon Analysis 1 On February 7 1992 measurements of the total power emission from Jupiter were made at zenith angles ranging from 33 to 72 with the 230 GHz receiver tuned to a frequency of 220 3987 GHz The measurements were made by consecutively monitoring the total power emission of the planet a position free of source emission located 5 away from the planet in azimuth and the emission from a hot load inserted directly in front of the receiver This allows us to directly calculate T4 Von Vof Vhot T Vof where the factor of 2 0 puts T on the single sideband scale and we assume to be consistent with the CSO on line system that the hot load temperature is 280 0 K Skydip measurements were made at the beginning and end of the test which yielded the following results 7 220 3987 0 078 at start of test T 220 3987 0 060 at end of test Mer 0 60 Therefore the atmosphere was quite stable for the
29. 102 password Dishm3 DS0Sdaemon DS0Sserver Go about all the other steps of the setup as listed above and when it comes time to start the DSOS leave out the step where you start up the DSOS monitor In other words type DSOSinit Then follow the steps to power up the power supplies and finish by typing DS08agent Basically you are doing exactly the same as you would have done except you are doing this on tpick itself instead of remotely from the control room and you are leaving out the DSOSmonitor command that starts the status display To shut down simply control c to stop the agent from running run the base command as described above log out from the visitor account and turn off the power supplies 43 This should only be used as an absolute last resort the fact that you were unable to connect to tpick in the first place means something is wrong In March 2005 the problem didn t interfere with the actual operation of the DSOS once we started it locally it knew what ZA it was pointed at and corrected the dish surface as expected However in June 2005 we encountered the same problem and thus followed the procedure just described Unfortunately it turned out that tpick was not communicating with the antenna computer at all meaning it had no idea what the ZA was at and perpetually corrected the dish surface assuming it was at 49 degrees the last measurement it recorded before the two computers stopped communicating
30. 2 92 02 92 06 92 02 92 01 91 03 90 03 90 02 92 02 92 01 89 01 90 01 90 02 90 03 90 01 91 03 90 11 91 02 92 02 90 02 92 02 90 Gen X Opol arcsec 12 3x 12 2 8 3x8 2 8 3x8 2 8 3x8 2 12 8x12 8 8 3x8 3 8 3x8 3 34 1x31 8 44 2x41 3 33 7 x31 6 44 2x41 3 44 2x41 3 44 2x41 3 36 4x34 0 43 9x41 1 45 5x42 5 39 8x37 3 39 3x 36 8 43 8 x41 0 44 2x41 3 43 8 x41 0 46 6x43 6 46 6x43 6 43 3x40 5 39 3x 36 8 45 3x42 3 39 8x37 3 34 1 x31 8 44 1x41 2 42 5X39 7 44 0x41 1 42 5x39 7 Table 5 1 CSO Main Beam Efficiency Dun arcsec 21 0 20 1 20 1 20 1 20 1 19 7 19 5 31 9 31 9 31 8 31 7 31 6 31 6 25 0 21 0 20 9 20 8 20 4 20 2 20 1 20 1 20 0 19 9 19 6 19 6 19 6 19 5 19 2 19 2 19 1 19 1 19 0 Ti planet K 30 01 1 5 31 5 1 5 33 5 1 0 24 0 1 5 5 1 0 39 5 0 5 33 0 0 5 126 0 1 0 157 0 3 0 125 0 1 0 172 0 5 0 170 0 5 0 185 5 2 0 168 0 2 0 182 5 7 5 147 0 5 0 153 0 8 0 140 5 3 5 171 0 3 0 173 0 7 5 163 5 3 0 165 0 7 0 170 5 1 0 176 0 2 0 131 5 2 5 186 5 2 0 142 5 2 5 159 0 5 0 171 5 2 5 185 0 7 0 166 55 5 164 0 9 5 74 tana K 196 3 9 8 227 6411 4 227 6411 4 228 0411 0 196 34 9 8 227 6411 4 227 6411 4 169 9 5 1 169 9 5 1 169 9 5 1 170 9 3 9 170 9 3 9 169 9 5 1 169 9 5 1 175 7 5 1 173 9 5 1 174 1 5 1 173 4 5 1 173 0 5 1 172 4 5 2 172 4 5 2 171 9 5 2 171 7 5 2 170 5 5 4 170
31. A COOKBOOK FOR THE CSO Neal J Evans II Department of Astronomy The University of Texas at Austin Last Modification July 2010 OUnderground Publishing Corp This document can be produced at the CSO by typing latexit on the unix machine in texas nje Cookbook followed by lp template ps if you want to print it In Austin type latexit data8 mmgrp NewCSOcookbook followed by lp template ps if you want to print it Contents 1 2 A Night at the Telescope Texas Directory Management Current Status of Texas Directory Setting up Catalogs Logging in to the CSO computer and the UIP Instrument Choices 6 1 Switching from Heterodyne to Continuum a soaa a 6 2 Switching from Continuum to Heterodyne 6 3 Tuning Frank s Receiver a ss 6 4 Using the Wideband AOS AOS5 6 5 Switching from Wide Band to Sidecab Receivers Taking Heterodyne data Texas Style GE Mapping e sr SE o e 1 2 Comments ara a A A pd LER E a a A ds uo 73 On the Fly Mapping e 7 3 1 Extending an OTF Map 7 3 2 Quadrant Mapping BIG oke LA ChopssleWye mosto decla De oe ge AA ROB dup DA etes How to check the pointing Heterodyne 8 1 Using a continuum source aa e a e e a a e a a al Bee a OSY 8 2 Using a spectral line source 2 8 3 Comments oA aoe etd A A ERR a e eee x Ned e Texas User Guide for Bolocam 9 1 Start up Procedures 2222s m EEN 9 2 Galactic Plane Survey Macro Generation Procedures
32. Hz AOS data will be selected Author NJE e 1500 Sets the telescope to CSO 1 5 GHz so that only the 1 5 GHz AOS data will be selected Author NJE e ADD Looks for new data finds all selected scans in a data file then sums smoothes baselines and plots the result Useful to keep up with how you are doing on a source with more than one scan No inputs Author NJE e BASEALL Smooths and fits baselines to a list of scans and write these baseline fitted scans to a file with default extension BASE User is prompted for the baseline order and an output file name Author SZ e COPYALL Writes scans in the current index to a previously opened output file No inputs Author SZ e GETOFF For a given positional offset finds sums smooths and plots the composite spectrum Inputs are X and Y offset Author NJE e HEADER Macro called at the begining of all macros which sets the SIC variable VERIFY to OFF and sets the ON ERROR variable to QUIT Author JGM e MAP Makes a map of the scans in whatever data file you happen to be in at the moment Maps are made to be full screen size When procedure is done the plot window is reset to normal size No inputs Author RIP e MAPZHOU A nicer version of MAP it automatically puts the source name and line name on the plot and for reasonably shaped maps will label the upper right spectrum with the temperature and velocity scale Be sure that you have set MX and MY Will leave
33. Lellouch Encrenaz and Combes 1984 A amp A 140 405 for details The most dominant absorption lines are from HCN PH3 and NH3 In the 230 and 345 GHz windows the frequencies to watch out for are 266 GHz HCN J 2 and PH J 0 and 354 GHz HCN Ji 23 The HCN JL 2 and PH J 0 transitions subtract gt 10 of the brightness temperatures for Jupiter and Saturn in the frequency range 350 v lt 355 GHz The HCN J 2 transition subtracts gt 10 of the brightness temperature of Jupiter for 264 v 268 GHz and of Saturn for 257 v lt 275 GHz Note that both of the estimates for Jupiter neglect the possible importance of H5S on the jovian infrared spectrum see Lellouch et al 1984 18 6 Saturn s Rings Ulich 1981 AJ 86 1619 Hildebrand et al 1985 Icarus 64 64 and Epstein et al 1980 Icarus 41 103 have analyzed the effects of Saturn s rings on the measured brightness tem perature of Saturn Basically when the rings are at low inclination 2 lt inclination 20 they block a small fraction of the Saturnian disk since the rings are colder than the planet surface For larger inclinations the rings begin to add emission to the disk because the rings begin to be projected off the planetary disk In general based on the Epstein et al models these effects represent lt 10 corrections to the millimeter continuum brightness temperature of Saturn for ring inclinations lt 30 Unfortunately the 3 mm continuum
34. Linsky 1973 so that 1 Ro 1 These two assumptions reduce our equation for Tr A to the following Ti 0 1 28 4 262 A Measurements of the radio emission from the moon extrapolated to A 0 have been used to derive values for D 0 in terms of To 0 and A Linsky 1966 finds that n er and 41 A 0 24 A A in mm Therefore our equation for Tr A becomes Tr A To 0 cos amp A 0 0 0 77 Ty 0 Tr A To 0 i 14 048A 0 11423 cos x ELA 0 0 where xe dh Ls since new moon x 360 180 period of moon 140 24 X period of moon 29 530589 days This equation should be applicable throughout the radio and infrared wavebands Values for To 0 from Linsky 1973 table 6 are given below Table 4 1 Values for T 0 amp 4 0 0 tan 0 24 A 12um 17 5um 30um 100um 300um 1mm 3mm To 0 213 9 b6 0 212 7 E6 2 213 748 7 216 1 6 9 217 6481 219 1 6 3 22T T E8 9 T2 5 The Measurements Table 5 1 lists the measurements of nmg that have been made since 1989 Each entry has been calculated using the following technique For each measurement of the planet an eyeball Ti planet and rms uncertainty have been estimated When a scan was taken in dual AOS mode the average between these two measurements is used yp was then calculated for each measurement along with an uncertainty based on the noise Then for a given observing run
35. SS header is 511 5 and the default channel width Df in the CLASS header is 500 MHz 1024 channels or 0 4883 MHz In August 1991 Taco modified UIP so that when a data scan is taken the most recent FCAL solution is applied to the scan before it is written to your data file Therefore there is no longer any need to worry about frequency calibrating your data UIP takes a weighted average of five channels around each peak to get the position of each peak in the FCAL comb It then uses the position of the central peak as the solution to the center channel for the 500 MHz AOS and the average of the two peaks nearest the center for the 50 MHz AOS To get the frequency resolution UIP takes an average of the widths of the FCAL comb peaks A comparison between this method of solution and ones which use a parabola Gaussian and teepee fit to the FCAL comb peaks to find the solutions has shown that there is little sensitivity to the method used 61 17 1 Frequency Calibration of Data taken at the CSO Before Aug 91 It is possible to use CLASS to analyse the FCAL spectra and thus measure the actual center channel and frequency resolution of the AOS It is usually necessary to modify the default frequency scale due to shifts in the AOS The default center channel for the 500 MHz AOS IO in the CLASS header is 511 5 and the default channel width Df in the CLASS header is 500 MHz 1024 channels or 0 4883 MHz To determine the actual center channel call
36. a statistical average rpg an rms uncertainty calculated from the uncertainties in the individual measurements and a standard deviation calculated from the variance of the individual measurements was calculated from the individual measurements for a given frequency These average values are given in Table 5 1 where the uncertainty for each entry is the greater of the rms uncertainty and the standard deviation of the individual measurements In general the standard deviation is more than twice the rms uncertainty suggesting that systematic effects like pointing sideband gain atmospheric stability etc are the main sources of uncertainty In the calculation of nmg from Jupiter measurements I have used a linearly interpolated value for Tpianct from the measurements of Griffin et al 1986 see Table 3 1 Martian brightness temperatures are taken from calculations done by Karl Stapelfeldt used for the CSO bolometer calibration A plot of the average np values given in Table 5 1 as a function of frequency is shown in Figure 5 1 Since nmg measured using a given calibration source is reasonably constant within the tuning range for a particular receiver we list in Table 5 2 average values for nmg applicable to each receiver along with the standard deviation from dispersion from run to run and over frequency for a given receiver 73 Source Mars Jupiter Date 01 91 07 90 07 90 01 89 01 91 07 90 07 90 11 91 02 92 11 91 02 92 0
37. ackslash separating them VERIFY has other uses To list all the sources in all the open catalogs type VERIFY NODEFAULT The is a wildcard which means take anything So means list all sources The NODEFAULT prevents you from having to watch the whole enormous default catalog which is always open To correct a source use a text editor To delete a source in catalog n use a text editor Since a source might be in several catalogs with the same name but different positions or velocities check that the coordinates and velocity are the one you want If not close catalogs until the source is found in only the catalog that you want Record the catalog in which the source was found in the log sheets this page left blank 10 5 Logging in to the CSO computer and the UIP First find out which of the many computers littering the control room now runs the show As of January 2010 this is kilauea Login to it USERNAME texas PASSWORD This is our little secret The computer will give you a prompt Now go into whatever directory you are using The top level directory is home kilauea texas and for example if the directory for this run is dec99 then you switch to this directory by typing cd dec99 For a display of the sky at the CSO type orrery amp Now type UIP This will put you into the User Interface Program from where the telescope is run The prompt in UIP is UIP gt The following assumes that you ar
38. ady and delete your wonderful macro 59 this page left blank 60 17 Frequency Calibration at the CSO One disadvantage of using Acousto Optic Spectrometers AOS for backends is that they lose the very high frequency accuracy inherent in heterodyne receivers They must be frequency calibrated as would an optical grating spectrometer This is done at the CSO by taking a special scan called FCAL You should do this at the start of each night of observing and at least once every hour thereafter the UIP system will automatically take an FCAL scan whenever you make a long slew This command turns on a phase locked temperature stabilized oscillator which injects a frequency comb into the AOS For the 500 MHz AOS the oscillator puts out 100 MHz and then is run through something which generates all of the harmonics This produces peaks that occur at various frequencies in the band For the 50 MHz AOS the oscillator puts out 10 MHz and similar things happen The peaks are shifted from the center because the IF signal is further down converted for this AOS and the new central frequency is something like 75 MHz whatever it is it is not a multiple of 10 MHz but ends in 5 MHz It is then possible to analyse this spectrum and thus measure the actual center channel and frequency resolution of the AOS It is usually necessary to modify the default frequency scale due to shifts in the AOS The default center channel for the 500 MHz AOS 10 in the CLA
39. alues not what you may have determined previously on the run uip gt inst sharc2 tells the telescope that you are using sharc2 check that the pointing file is correct and that the focus mode is constant uip gt tertiary to check that it is in position if not do tertiary nasmyth2 uip gt observe sourcename replace sourcename with name of the calibrator this slews the telescope and may take a few minutes depending on how large a slew it is uip gt sweep 20 14 142 y 20 20 altaz sets up the sweep pattern this is only an example see SHARC II webpage for more information set integration time to 120 seconds in the sharcClient record the current value of FAZO you will need it soon uip gt fazo 1000 moves the telescope off source so that you can level level the equipment click level hardware and then click grab leveling frame both arrays should turn mostly green uip gt fazo current current is the value you just recorded moves telescope back to the source 38 Click start in the sharcClient to take the image Once the integration finishes you will want to check the pointing Open a new window on desktop 4 win4 1 and execute win4 1 ssh Y sharc kilauea password 350mu_m cd src crush crush point scan replace scans with the actual number also don t execute this command until the words copy complete appear in the sharcClient If you get a Gains did not converg
40. and the ENTIRE line NOT just the word FIVE a few times and averaging the values before inputting the new values of FAZO and FZAO by typing UIP gt FAZO UIP gt FZAO 24 where is your chosen offset 8 3 Comments Even though FAZO stands for Fixed Azimuth Offset it isn t always so Both FAZO or FZAO may vary with both time since opening the shutter and zenith angle Trust no one check the pointing often and if you see significant changes make your own pointing curves A convenient GreG macro for keeping track of pointing corrections is POINT GREG If you copy the files POINT 230 and POINT 345 from the working directory of the previous run or from TEXAS MINHO and update them as you do the pointing you can use GreG to plot the FAZO and FZAO versus Azimuth and Zenith Angle If they have changed a lot since the last run you can ignore some of the previous lines by modifying the GREG macro Since the POINT GREG macro assumes you have both 230 and 345 GHz pointing data there is now a macro called POINT230 GREG which assumes you have only 230 GHZ data Since limits are hardwired into these macros you will probably have to edit them 25 this page left blank 26 9 Texas User Guide for Bolocam written by Miranda Nordhaus June 2006 last updated July 2007 9 1 Start up Procedures 1 Login to kilauea username bolocam password bem rtu Note you should only be logged in as bolocam on one machine at a time All b
41. and writes the reduced scan into orion red along with the baseline and the the results from the gaussian fit If this is all you want to do you then exit 12 2 How to See Your Last Scan One of CLASS s more irritating features has been that scans that are taken after you open an input file done in the above session by the fi command are not available for viewing The command NEW DATA rectifies this problem Need to check if this still works There are also macros which allow you quick access to a new scan Since the AOS resolution is about 2 channels it is recommended to smooth the data with a boxcar This command is smooth box 2 or more briefly smo bo 2 A macro called p plt does this after getting your scan and plots the data You type Ap plt Once new data come in it will list them and prompt you to say what scan number you want If you have set up your window for baseline removal you can also remove a baseline after smoothing with the macro Qp pb For the really ambitious you can try Gp pbg which removes a baseline plots the spectrum fits a Gaussian and displays the results of the fit Since Aug 91 these macros will invoke the command NEW DATA which will look to see if new data have come in since you last did the file in command This is convenient for looking at the scan that just finished but if you are looking at old data and there are no new scans these macros will hang up waiting for new data To get past this point
42. ansform Spectrometer or AOS2 the 50 MHz AOS for Galactic sources or AOS5 the 1GHz times 4 AOS for extragalactic sources As a practical matter AOS5 can be used with the wideband receivers such as Frank s receiver or with the sidecab receivers The FFTS1 is generally the best choice for narrow lines as it provides better spectral resolution AND broader velocity coverage with 8192 channels The spectral resolution is essentially equal to the channel spacing so there is no need to smooth to make channels independent A wideband FFTS called FF TS2 is expected in the future When using FFTS1 for narrow lines you want to specify BAND 0 5 and remember to include this qualifier if you have to restart the FFTS1 If you forget and you use the velocity offset lines will appear at strange velocities For using the FFTS1 a very helpful document can be found in http www cso caltech edu docs hiro ffts FFTS Instruction html For using AOS5 a very helpful document can be found in http www cso caltech edu docs hiro wideband aaos html Similarly check the following for help using the wideband receiver http www cso caltech edu docs hiro wideband wideband html Pdf files for both are available by replacing html with pdf Copies of these from Dec 2006 are in the cookbook at summit under Memos If using AOS5 you must choose a suitable IF in the LO command For Frank s receiver it could be 4 5 GHz to center in the first part channel A of AOS5
43. bove you would type LAS MODIFY RECENTER 510 LAS MODIFY WIDTH 0 5 if the data is in the LSB Or LAS MODIFY WIDTH 0 5 if the data is in the USB There is a CLASS macro in the texas proc directory called FCALL CLASS that will perform these modifications for all the scans in the index 62 17 2 Sideband Gain Ratio In the chopper wheel calibration scheme that we use at the CSO one of the assumptions is that both sidebands of the receiver respond equally to a given signal In general one cannot easily check that the signal and image sideband gains are equal before taking data It is possible though to get an estimate of the equality of the sideband gains that existed during a particular observing run if you have made repeated lower sideband measurements of the CS 7 6 transition toward a certain source For an IF frequency of 1 4 GHz with CS 7 6 in the lower sideband CO 3 gt 2 appears in the upper sideband By taking the ratio of the peak T for these two transitions one can get a rough estimate of the sideband gain stability during an observing run During July 1991 the CS 7 6 and CO 3 gt 2 transitions were used to monitor the sideband gain ratio of the 345 GHz cassegrain SIS receiver at CSO In the course of making a map of a source which spanned two separate tunings between which the receiver was tuned to a different frequency the ratio of the CO 3 2 and CS 7 6 transitions varied as follows peakT4 CO3 2
44. cale see Kutner and Ulich ApJ 250 341 for a detailed discussion of temperature scales The two scales are related by mul HEI where n is the source coupling efficiency and mg is the forward spillover and scattering efficiency In general will depend on the coupling of the telescope beam to your source For this reason it is convenient to factor 7 into two terms a source filling factor fs and a term which describes the coupling to a source which just fills the main beam which we will call n main beam Ne fj main beam This allows us to define the main beam efficiency Nu NMB n main beam nfss One can tie this definition to the original definition of the beam efficiency ng by noting that rg includes the rear scattering and spillover efficiency Mss Therefore mp is actually NB Nrss By measuring T on a planet or the moon one can derive yg using the following planet beq 2 A eq pol Rue coe eae Ee 223 TOR J vs Eeer Weg J vs age exp 5 ONE which is the convolution of a Gaussian telescope beam with a uniform disk source The terms in this equation are defined as follows Ji Tg Planck function at frequency v and brightness temperature Tg hy ie pues x T planet single sideband antenna temperature of calibration source e Ty brightness temperature of calibration source Tembr brightness temperature of the cosmic microwave background about 2 78 K eq equatorial diame
45. ccess these is by sitting on the floor and scooting back til you are looking up at them Use the knurled knobs to tune and read the result from the dials If you see the SIS current get above about 10 attenuate Tune for a maximum in total power Iterate between the two knobs Then climb out and adjust the attenuator to get between 10 and 12 on SIS current check latest instructions in receiver tuning manuals Then touch Bfield on the blue box This will sweep the voltage and you should see two or more peaks The one on the right is the one you want and those on the left are due to Josephson noise which you don t want Suppress those by turning on the B field box and increasing the B field until they are minimized Now check the I V curve by pressing IVSweep If the slope after the main step is negative you may have bad baselines so detune the Eplane tuner a bit This has not been much of a problem lately Stop IVSweep Measure the power on hot load and cold load use the absorber on the handle dip the absorber in LN and put it in front of dewar window taking care not to touch the delicate wire grids The ratio of the two powers is the Y factor Values between 2 5 and 2 8 are good on the 230 sidecab receiver Check all your settings and see if you can get an FCAL and a CAL Before doing anything serious re issue the SPEC command to not allow it to take data when the Gunn is unlocked UIP gt SPEC 5 AOS5 RESTART NOLOCK NOSHUT_UP If you still have
46. ceiver Barney who lives in a garish purple dewar a 1 or 2 mm continuum camera Bolocam and a 350 micron camera SHARC II All but the sidecab receivers require prior arrangments You can have SHARC mounted at Nasmyth 2 and either Bolocam or Frank s receiver at Cassegrain It is also possible to have Bolocam at Cassegrain and Frank s receiver at Nasmyth 2 ZSpec or Zeus low Res but very wide coverage systems may also be or may become facility instruments Finally there is a polarimeter for SHARC called SHARP A treasure trove of information that is not obvious from the main CSO web page is found in http www cso caltech edu docs hiro Generally to switch between systems requires a few steps It is easy to forget something so we will provide a few examples to illustrate the steps 6 1 Switching from Heterodyne to Continuum To switch from heterodyne to continuum one generally uses the INSTRUMENT command followed by the name of the instrument UIP gt INSTRUMENT BOLOCAM or UIP gt INSTRUMENT SHARC2 Another useful command is TERTIARY Issued alone it tells you the current position of the tertiary which is now encoded Or you can issue it with a value which can be SIDECAB NAS MYTH2 or CASSEGRAIN Finally you want to choose the correct pointing file which could be 230 SIDECAB or similar commands for the other sidecab receivers For SHARC II at Nasmyth it is UIP gt POINTING SHARC2 NASMYTH The INSTRUMENT SHARC2 c
47. d only a tenuous atmosphere it is generally used as the flux calibration standard for far infrared through millimeter wave lengths Using results from the Mariners 6 and 7 spacecraft Neugebauer et al 1971 AJ 76 719 see also Wright 1976 ApJ 210 250 Wright and Odenwald 1980 BAAS 12 456 Simpson et al 1981 Icarus 48 230 developed a model of the Martian far infrared thermal emission This model does not include the influences of a dusty atmosphere or of the Martian polar caps At wavelengths shorter than 40 um atmospheric dust storms may have a direct influence on the Martian thermal continuum emission These effects should be negligible at longer wavelengths because of the A dependence of the continuum optical depth although as pointed out by Griffin et al 1986 Icarus 65 244 the thermal emission at longer wave lengths may be diminished due to the reduced solar insolation during a dust storm With these provisos in mind a reasonably accurate calibration scale can be constructed based on the model predicted continuum brightness of Mars It is instructive to point out that Ulich 1981 AJ 86 1619 showed that the Martian brightness temperature at 3 3 mm is given by Ro T R DA where Ro 1 524 AU mean Martian heliocentric distance T Ro 206 8 5 8 K T R Martian brightness temperature at heliocentric distance R Brightness temperatures predicted by the Neugebauer ef al model are usually within 1096 of those predict
48. describe the typical sequence of events during a night at the CSO opera Opening night has a few special features surrounded by 1 10 11 Look for memos notes on the board in the control room etc For example there may be a note saying to keep within certain limits on zenith angle Log in to the current control computer Kilauea as of this writing Respond to the login prompt with our user name TEXAS It will then request the password See section on starting up the CSO computer for more information Tf it is the first night of the run create a directory for the run using the conventions explained in Texas Directory Management If it is not the first night just go to the previously created run directory by typing cd dirname Enter the user interface program by typing UIP Tf it is the first night you have to set up a data file See the section on Computers If it is not the first night type STATUS this will tell you what the data file and next scan are If these are correct you are all set If not use the instructions in the Computers section but give a scan number which is one number greater than the last scan number of the night before If the sun is not hitting the dome start opening the shutter so the telescope can cool down First check that everything is OK and then pull out the big red stop button Then type in UIP shutter open To decide which instrument to use check t
49. e error when trying to reduce bright calibrators try the following crush point gainrounds off scan Check the image in the show window when it pops up the image should be centrally peaked and symmetrical If it isn t you may need to change the focus See the documentation on the SHARC II webpage for information on how to do this Check the resulting pointing if the pointing is far off the suggested FAZO and FZAO may be meaningless Update the FAZO and FZAO from the result of crush and record the changes on the logsheets Repeat the 120 second integrations and pointing checks until the pointing looks good the position errors should be small but more importantly the pointing should be stable As a reality check make sure the source looks like it is in the center of the image that pops up You will want to check the pointing throughout the night especially in the beginning while the telescope is still cooling down Since it doesn t take long you should probably check the pointing each time you image a calibrator since you will be imaging these often throughout the night for your flux calibration or at least you should be For the first pointing if your calibrator is strong and point like check the focus using FOC OFF xx commands to move by 0 1 or so Optimize signal but also check beam size and sidelobe level to find best values The SHARCII website has examples 10 2 2 Sources Load the source into a catalo
50. e and a 3x1b takes approximately 52 minutes To enter a new source in the catalog type in the uip source cat n source name nocon vert to 1950 Then enter the coordinates in J2000 0 You only need to enter the coordinates and epoch you can enter 0 for the rest of the fields In fact most field centers were entered without noconvert so they have been converted to 1950 To see the original 2000 0 coordinates use the new qualifier on verify As of July 19 2007 we are using positive longitude notation so that we have a source macro and parameters named 1351 instead of Im009 9 3 Real Time Data Reduction The data reduction start up procedures described above will not be the final reduction It creates a sav file which serves only as a sanity check are you getting good data or is something wrong with your observing macros You can access the data from the home bolocam directory by gt cd data mapped This path is linked to the actual location of the data as of 6 21 2006 bigdisk bolocam 200606 mapped Within this directory you will find a folder for each source observed The slicer IDL window titled run run auto slice files looks for the next observation number before reducing the current obser vation For example if you are integrating on observation one the slicer will wait until observation two has begun being written before it will reduce observation one Once the reduction process has begun but before it has f
51. e but you don t need to shut down the power supplies Just start it up again according to the sequence on the web under DSOS Users Procedure 10 5 2 What To Do If You Can t Connect to the DSOS In March of 2005 we found that we were unable to connect to tpick the computer that controls the DSOS from any of the computers in the control room this is the computer you log into with the ssh visitorQ128 171 86 102 command If you run into this problem the first thing you should do is a series of simple checks Is tpick on it is the computer in the glass case next to the 8 DSOS power supplies Does it look like network cables have come unplugged Did you type everything correctly If you can t find the problem your next course of action should be to contact somebody that might know what the problem is The best place to start would be the CSO pager You can also contact other people using the numbers listed next to the phone in the control room use your best judgment about whether or not your problem is serious enough to wake people up if it is the middle of the night If all else fails you can do what was done in March of 2005 run the DSOS from tpick locally instead of remotely This means going out of the control room and using the keyboard and monitor hooked up to tpick to start the DSOS You will not be able to run the status display but you will still be able to have the DSOS in operation To do this on tpick type ssh visitor0128 171 86
52. e called with the sign in front of the macro name or if the macro is in the proc directory use P startx The startx macro is described more fully in the section on CLASS Directory Management The second line asks the program to get a particular scan number 1001 It is conventional at the CSO to begin with scan 1001 Next we plot it The initialization sets you up to see all the channels Usually you want to restrict the range so the next command sets the range on the horizontal axis to cover 20 to 40 km s Then we prepare to take out a first order baseline by setting a window The baseline will use all channels within the range set by set mode x but EXCLUDING the channels in the window The baseline routine also measures the area in the window after removal of the baseline so if you set your window carefully you get the integrated intensity of the line Next we plot the result of the baseline removal The next step is to fit a Gaussian One can fit several Gaussians and control what 47 is varied but in this simple form the command just says to fit the strongest thing To see the Gaussian on top of the data type fit The command P hardy sends the plot to the laserwriter Finally you may want to save your processed scan in another file here called orion red This file is created here by the command file out orion red new After the file has been created you can re open it by the same command without the parameter new The write comm
53. e point map in RA DEC you can type UIP gt FIVENJE 4 30 where the step size is 30 arcseconds and you want to do 4 cycles of on off It will cal once adjust the attenuator wait 1 minute for the AOS to settle down and then take all the positions using the same cal To fill in the corners of the box use UIP gt CORNERS 4 30 If you know in advance that you want the whole nine point box use UIP gt NINE 4 30 7 3 On the Fly Mapping written by Yancy Shirley 7 30 99 update by NJE on 6 30 08 On the Fly mapping OTF can be a particularly efficient method of mapping extended sources The procedure for an OTF is as follows UIP gt SPEC xx where xx is t N t AZRes Speed Num of azimuth pts in map N AZsize 10 UIP gt OTF AZsize ALsize Speed Rampt AZRes ALRes cal des foc AZsize size of map in Azimuth in arcseconds ALsize size of map in Alititude in arcseconds Speed speed in arcseconds second that the telescope moves in Azimuth Rampt time in seconds to wait for antenna computer to acquire next position AZRes the step sixe in Azimuth in arcseconds 20 ALRes the step size in Altitude in arcseconds cal foc take a TCAL and focus UIP gt SPEC 17 debase UIP gt OTF 110 110 2 10 10 10 where we have chosen the Speed 2 with Ramp Time 10 the default for Speed below 5 s smaller values of Ramp time may be used but I usually just use this value 7 3 1 Extending an OTF Map To make a
54. e shutter stow the antenna push the emergency stop button turn off instruments and lock the doors At the end of the run ftp the data file to Austin see Miscellaneous section for ftp in structions Clean up your working directory for the run transfer any modified or new and generally useful and DOCUMENTED class or greg procedures to the texas proc directory for safe keeping Transfer any undocumented things that you like to your own directory Re member that this working directory could be deleted if space issues become a problem Head for the beach 2 Texas Directory Management In order to keep our Texas directory at the CSO in reasonable condition we will abide by the following rules T Each observing run will operate in a subdirectory of the TEXAS directory on Kilauea labeled by month and year e g Dec99 To create a subdirectory called in this example Dec99 type mkdir dec99 Both the night data files themselves as well as all the other observing files night reports etc will now go together in this one directory unlike before when there was a separate directory on user_vax for the data files The data file in this directory will have a name labeled by day month and year and have a DAT extension e g 15DEC99 DAT The file may be deleted by the CSO staff or by the next group unless they are notified otherwise Use CLASS only on the UNIX machines The macros for class are in texas proc These are
55. e using the heterodyne receivers If using SHARC or Bolocam go to those sections Now type for example UIP gt SPEC FFTS1 BAND 0 5 where is the integration time in seconds per on source cycle typically 10 or 20 For this example we have assumed that you are using the Fast Fourier Transform Spectrometer FFTS in its high spectral resolution mode which gives a bandwidth of 0 5 GHz This is now the spectrometer of choice for high resolution The option for still wider lines is a broadband AOS called AOS5 To turn off an AOS use the NOAOSn qualifier where n is the number of the AOS that you want to turn off Likewise NOFFTS1 will turn off the FFTS There is an FFTS2 coming soon with a wider bandwidth If this if the first night of the run you need to set up the data file UIP gt DATA filename scan number where filename is the file you wish to store the data in e g 24JULY98 a DAT will be supplied by UIP scan number is the scan number you wish to start at 1001 if you have just started a file but 1 plus the last scan number if you are opening an old file Tf this is not the first night you can just check that all is well by typing UIP gt STATUS Warning don t ever try to access the current data file from VMS e g with a COPY command because DCL commands can block data recording from UIP Now set up your local oscillator frequency by typing UIP gt LO line where line indicates w
56. ea bolocam GalacticPlane Pointing which has the information There is a directory with pointing analysis for July2007 and one for Sept2006 The Pointing directory also has a file with information on the master field project called Masters A ReadMe explains what is there Based on analysis of the nights when many pointing sources pcals were done Neal constructed a pointing 30 model that is implemented by a fortran program called pointme f compiled to pointme in the bolocam top directory Further experiments with pointing models are in the Pointing directories compiled to Pointing bin So the procedure to observe a source is to observe sourcename in UIP get the requested AZ and ZA from the antenna computer screen run pointme providing those values and change FAZO and FZAO as directed This is the outcome of the pointing model If the source is a pointing source pcal analyze the outcome with the IDL routine boresight described above and record them in the logsheet and edit pointing 20070704 bolo to add these results However do NOT correct FAZO and FZAO because the next source may be at a significantly different AZ and ZA Instead use pointme on EACH SOURCE We can analyze the offsets to consider improvements in the pointing model 9 5 Trouble Shooting Rotator problems First never be in interactive on allegro while executing a macro which uses the rotator The macro and interactive will both be trying to control the rotator and
57. ed by the expression above The T Ro agrees well with the Neugebauer et al model for the far infrared emission indicating that the global temperature changes very slowly with increasing wavelength and that the Martian thermal emission closely approxi mates a blackbody at millimeter and submillimeter wavelengths In the calculations presented in Table 5 1 I use Martian brightness temperatures pre dicted by a model calculation done by Karl Stapelfeldt using software developed by Don Rudy These are the same brightness temperatures used for the CSO bolometer calibration 18 5 Molecular Absorption Lines in the Spectra of Jupiter and Saturn Most of the measurements of the brightness temperatures of Jupiter and Saturn are broad band continuum measurements The bandwidths in these measurements are generally some 100 s of GHz we have one brightness temperature for the entire 345 GHz window for exam ple Since models of the atmospheric continuum emission at millimeter wavelengths indicate that the the brightness temperature changes very little over a given band broad band mea surements of Tplanet are sufficient One physical effect that the broad band measurements 68 cannot measure though is the existence of molecular absorption features superimposed on the continuum emission spectrum of the planet At selected frequencies these features can decrease the planetary brightness temperature by as much as 1596 for Jupiter and 4096 for Saturn see
58. escriptions ee 16 2 GreG Macro Descriptions 16 3 How to Add a CLASS or GreG Macro to texas proc 17 Frequency Calibration at the CSO 17 1 Frequency Calibration of Data taken at the CSO Before Aug 91 11 2 S1debarid Gait Ratio nai a oue CENE Eas Erde Ves 18 Measuring Telescope Efficiencies 18 1 The Proc d re iogree eek Rem Re AR A AA I8 2 The Technique 03 oe Ad Voy ect 18 3 Calibration Source Temperature 18 4 Mars Brightness Temperaturen 18 5 Molecular Absorption Lines in the Spectra of Jupiter and Saturn 18 6 Saturn sR ungs doe me RE RG t ee PA ew 18 7 Using the Moon as a Calibration Source 18 8 Things We Always Assume But Don t Always Measure 18 8 1 Zenith Angle Dependence of the Primary Beam Response 18 8 2 Possible Errors in the T From AOS Compression 18 9 Line Calibration Tests 19 Transferring Files to Austin 20 Using ASTRO to make Plots of Source Elevation vs Time 21 TROUBLE SHOOTING as of December 2006 21 1 UIP Very Slow Things Hang 2000000200005 21 2 DOME POSITION UNSAFE e 21 3 Computer Hang up or Crash aoaaa 45 45 47 AT 48 48 90 51 53 54 55 56 56 58 59 61 62 63 64 64 66 68 68 68 69 71 77 77 78 79 81 83 this page left blank 1 A Night at the Telescope The following is an attempt to
59. eter for both the ON and OFF positions and write them down This will allow a check of the T scale 64 5 4 When the OO scans are done go out to the cassegrain focus above the 345 GHz receiver and measure the HOT load and COLD load voltages Write them down with your ON and OFF voltage measurements To check the temperature scale in your measurements run the program beameff or eta these can be found in home hapuna texas bin or in ug mmgrp obsutil in Austin The program eta will allow you to change the beam size from the default diffraction limited values and is preferred This program will prompt you for the voltages you measured above along with 7 and the zenith angle of the measurement from which it will calculate Von Vos T CSO 2 0 x 280 0 x A Vnot be Vog and Mon Wa Voff 2x Thot Tola Vhot V cold NI assuming Thot 273 0 and T 80 0 K Compare these T values with those from your position switched scan and note all three on the log sheet The three measurements should agree to within 1096 or so Ti cold exp 7 sec ZA 65 18 2 The Technique Quite often it is useful to compare spectral line measurements made at the CSO with those from other telescopes Since the raw data you get at the CSO is written in the telescope dependent T temperature scale one must measure the beam efficiency in order to trans late ones data to the telescope independent Tg s
60. g if not already done The easiest way to deal with the catalogs is to open a second uip on desktop 1 This won t control the telescope only the first uip that you open will do this If you want to override this however and make this new uip be in control type uip gt pundit true To add a source to a catalog type the following in the second uip 39 uip gt cat spitzer cat This will load the catalog named spitzer cat other catalogs can be loaded in the same way uip gt cat this will give a list of all catalog names and numbers Add sources to your catalog with any editor You don t need V_lsr for SHARC II obser vations but if you know it you should enter it as you do need it for heterodyne observations uip gt ver source name altaz gives current position of source uip gt ver source name elev 30 gives rise and set times above and below elevation of 30 any value can be used in place of 30 Now that the source is loaded into the catalog you are ready to observe it Back in the first uip the one that actually controls the telescope type uip gt observe source name uip gt sweep 20 70 7 y 50 20 altaz only an example of a possible sweep pattern to use Level the hardware in the manner described above Move to a FAZO of 1000 level the equipment and then move back to the current FAZO value If the weather is good you will probably want to use a 10 minute 600 second integration If it is bad 5 minutes 300
61. ge provided that you have developed some macros to make life easier The main reason you need macros is that CLASS uses a rather sophisticated data base type method to specify which scans are available to be acted on This can be useful but is incredibly frustrating if you just want to see the last scan the telescope has taken If you are in the Texas group you should only run CLASS on the UNIX machines NOTE in January 2009 a new fortran90 version of CLASS is running at the CSO with substantial changes Some of the steps described below or in macros may not work Macros developed by the Texas group reside in the texas proc directory for the UNIX machines These can be copied to the directory you are working in or accessed from the appropriate proc directory by prefixing P to your call to the macro see sample CLASS session below You can also make your own macros the file should be name CLASS where name is the name you want to use when calling it from CLASS 12 1 Sample CLASS Session Enter CLASS by typing class You will then get a prompt that looks like LAS We begin with the first call to a macro which initializes everything and sets up abbreviations symbols for some commonly used commands P startx fi 14jun93 dat get 1001 plot set mode x 20 40 set window 5 15 base 1 plot minimize visualize hard plo file out orion red new write exit This basic session illustrates some of the operations that one typically does Macros ar
62. he NRAO tipping meter which measures the 7 at 225 GHz and sends a file to the control computer The latest value is displayed on the antenna computer monitor You can also see plots by going to the CSO weather page and selecting tau plots Before tuning the receiver set up the local oscillator by observing a source to set the velocity and selecting the line See Starting up the CSO Computer and Taking Data Note that if you change receivers the mirrors will not move unless the zenith angle is less than 45 degrees If the receiver you plan to use is already set up and turned on just tune it up following an appropriate tuning sheet in the Receiver notebook and recording your results on a new tuning sheet Be sure the correct pointing files are loaded for the receiver you are using These are accessed with the following command POINTING 345_SIDE for the 345 receiver Use 230 SIDE etc for the other receivers Check the pointing on some suitable source See How to Check the Pointing If you are pointing on a planet make a measurement of the beam efficiency See Measuring Telescope Efficiency section Check the pointing and efficiency again about 1 hour later since they are likely to change as the dish cools off If you can t think of anything else to check try taking data See Taking Data section 12 13 At the end of the night follow the shutdown procedures in the latest CSO manual or memo Be sure to close th
63. he SHARC II documentation recommends giving multiple scans to crush rather than using coadd to get the best combined dataset coadd should be fine for quick looks at the data while observing Several options can be added to crush Some of them are listed below along with when they should be used Brightness modifiers verybright moon etc bright 710 000 100 000 Jy default 1 10 000 Jy faint lt 1 Jy can be extended deep lt 7100 mJy assumed somewhat compact Size modifiers these appear after the brightness modifiers when both are used default pretty much anything try not using a size flag first extended gt 2 may increase baseline compact lt 20 may decrease baseline 10 4 Shutdown Due to the fact that the sun rises behind the summit of Mauna Kea we typically observe for at least a half hour past sunrise Once the sun is up be very aware of the position of both the sun and the telescope do not let direct sunlight hit the dish When you are ready to close up for the night first start closing the shutter as this will take quite awhile Park the telescope with uip gt stow This will slew the telescope so that it is facing east toward the rising sun and at a zenith angle of about 45 degrees So make sure the dome is shut if the Sun is up Exit out of the Data Acquisition software win3 2 Control c gets you out of the sharcServer Power off the instrument Switch the power switch to
64. hich fits all the data on the page Now for a real thrill you can get a grid of all your spectra on a source First you may want to leave certain scans out of the grid You can do this by typing drop 1322 which says to ignore scan 1322 in whatever you do next Now to make a grid you must first set the x and y ranges to definite values not auto So do set mode x 50 50 set mode y 1 10 to set up for a velocity window of 50 to 50 km s and a temperature range of 1 to 10 K Now type map grid number where the grid qualifier says to put a box around each spectrum and the number qualifier says to put the scan number on each spectrum The number is now written rather large so this is marginally useful For a macro that makes a reasonable display try P mapcso You can then make a hardcopy in the usual way There are also a number of macros which can batch process all the selected scans See the sections on Mapping Data Reduction and CLASS Macro Directory Management for more information on these 49 12 4 Changing Sidebands Suppose you set up the system to observe line A and and there is another line say line B in the opposite sideband You can get the correct velocity scale for line B by switching the sideband Although the commands MODIFY BANDS MODIFY FREQUENCY frequency let you switch sidebands and enter a new line frequency you need to pull a few tricks to get the correct velocity scale for line B The macro SIDE is w
65. hich line you wish to observe Note that the FFTS misses one channel right at the center so it is a good idea to move your line off center by adding V_OFF yy with 11 yy in km s We found yy 20 to work well Line setups are kept in a catalog default catalog and in a private catalog You can use the verify command with the LINE qualifier to see the line set up Type in UIP VERIFY CO LINE for example to see all the lines for CO Note that the multiplier and the sideband are also specified For many lines we have entered more accurate frequencies in our private line catalog so use these if you have a choice The antenna computer display now shows enough digits so when you go to a new line write the rest frequency with all the digits on the log sheet Now you should check that your receiver is locked and tuned See the latest receiver tuning instructions and tuning sheets Also be sure to turn on the IF processor which is in the tall tan rack in the room labeled Receiver Lab Otherwise you are unlikely to get an power into your spectrometer To see how to observe a source see section on Taking Data 12 6 Instrument Choices There are now many choices of instruments many of which are available only if you have requested them ahead of time As of summer 2008 you have all the sidecab receivers 230 345 490 650 except that the 490 receiver is broken Frank s wideband 230 GHz receiver now known as Z Rx a wideband 345 GHz re
66. ic heat and conductivity of the lunar surface material The most convenient form for the solution to this equation is a Fourier series T v 9 Y t vie H 1 T DEEN cos n n dn SE d Therefore the thermal radio brightness temperature at position V is given by Tr 0 Y t 1 Hiel T x 9 Y t ky sec r exp xk sec r dx SN TT d ame 2c E30 cos 12801553 x cos n nd bn EnlA Q V where R V reflection coefficient ky coefficient of electromagnetic wave absorption 71 r angle between the normal to the surface and the direction at the point of reception To w average over one lunar period brightness temperature n 1 n 2 an On A s ratio of the thermal attenuation coefficient for the Fourier component to the electromagnetic attenuation coefficient EE RU UP n phase shift relative to insolation for the n Fourier component of the surface temperature m 1 An Al cos r Enl 0 V tan neon component of the radio brightness temperature At the center of the lunar disk o ail 0 0 and for a given time t this equation reduces to the following phase shift relative to insolation for the nt Fourier 40 0 R 0 E2750 a ae c M E bn EnlA 0 0 EE The harmonic amplitudes for n gt 1 are only a small fraction of the n 1 harmonic amplitude and can be ignored Also Ro lt 0 05
67. in lock even if the lights are not on However the system does not know it is locked so you won t be able to integrate unless you tell the AOS to ignore the lock using UIP gt SPEC LOCK IGNORE UIP gt REPLY DISABLE The first command tells it to ignore the fact that it doesn t think it is locked and the second stops all the messages about that and other things This solution is far from optimal so first try the following Decrease the power coming from the HP synthesizer that is mounted near the receiver and which is supplying a reference frequency for the lock Push local power 10 Dbm to set the power to 10 Dbm The Dbm button is most prominently labeled GHz but Dbm is selected when you have pushed power This worked in Dec 2006 but one may need to experiment We also needed to attenuate the signal going to the harmonic mixer There is a separate attenuator for that turn counterclockwise as usual to attenuate After we attenuated enough the lock light came on After you have a lock you need to tune the receiver Since there are no tuners your only variables are the power main attenuator the bias voltage and the magnetic field Be sure to read the memos about this receiver in the Memos section of the cookbook or on the web Deattenuate enough to have some SIS current 30 75 mA and change the voltage bias to manually sweep the power versus V curve Find the peaks at low V and adjust the B field to minimize those Do not a
68. inished a Jeck file will appear in the mapped folder In order for the observations to be reduced the source must have an entry in the following files 29 directory bolocam cvs pipeline automation params cleaning params 200706 txt mapping params 200706 txt science fields txt ptg srces all txt The cleaning params file must have the correct entries in order to clean the file properly The easiest way to do this is to find a similar source already in the file and copy the line For example if you use G34 3 as a pointing source find another object used for pointing Uranus maybe and copy all the flags in that objects line If the object is a normal observation enter its name in science fields but not ptg srces all and vice versa if it is a source used for pointing To view the images you ll first want to convert the sav file to a fits file and view it with ds9 In the same directory as the sav file start idl IDL gt sav2fits filename sav IDL gt exit gt ds9 filename fits amp Alternatively you can restore the sav file in idl and then use atv to view it In that case open idl then type restore filename with path To view the map type atv mapstruct map zoom 2 or mapstruct mapconvolve for a less noisy version Pointing sources and science fields will be reduced by different windows the names should give it away 9 4 Pointing Corrections As of September 2006 we are now correcting for pointing offsets in
69. ip pro contains all of the texas macros each macro is now a separate file with file name macro uip for example fivenje uip All the above listed directories and files are of general utility and should NOT be deleted Also if one puts something in one of them it should be documented with internal comment statements or in some other way They are meant to be generally useful not peculiar to a particular person The second group of directories are data directories Finally we have personal directories which are now too numerous to mention Since we now have the luxury of using unix machines we keep all these directories there There is a proc directory for unix versions of class and greg procedures These are copied from Austin and some are modified to work at the CSO The VAX directories can be accessed from the unix machines with cd user vax texas at least until these ancient VAX machines receive their well deserved euthanasia 4 Setting up Catalogs Putting sources in catalogs is now done using a text editor to directly modify the catalog files which are stored at uip cat See the section on starting up the CSO computer and entering UIP There is a huge default catalog which is basically the OVRO catalog with some additions however you should not add your source to the default catalog All our catalogs are kept in the uip cat directory As mentioned above sources are now added to catalogs using a text editor When yo
70. irst make sure that you have selected the proper catalog and are pointed at the desired object by typing UIP gt CAT catalog name UIP gt OBSERVE object This will start driving the telescope to your object if indeed your object is in one of the open catalogs Note that if your source name has characters like or the source name will have to be placed in quotes Note that when you go to a new source offsets offpositions and velocity offsets are removed To keep a velocity offset when using FFTS1 you need to reenter the LO command In the following we assume a certain mode of observing the off position is specified relative to the on position by offsets in RA and Dec the cal scan is taken in the off position a cal is taken for every scan all scans start in the off position and the local oscillator and spectrometer attenuator are set for each scan If you want to do this you can use the following convenient macros designed for familiarity to old MWO observers If not some more general explanation is given below and you are invited to decipher the CSO manual entry for the OO SCAN command Now select an offset position for the telescope to take an off scan note that this is different from the standard UIP command OFF POSITION in that it specifies that the offsets are equatorial and that only one asymmetric off position is used by typing UIP gt OFFPOS 1 2 where 1 is the offset position in arcseconds East 2 is
71. it will get confused Whatever the problem try these steps A kill macro if executing one UIP gt kill UIP gt status The status command will tell you if a macro is executing or not Use this to check if the kill command worked properly B stop tel_util observer allegro kill_tel_util Then close the five windows associated with tel_util C Check rotator angle with interactive observer allegro interactive To display the current angle gt 888 To set the angle to 10 basically just get it moving gt 10 To make sure it moved to 10 gt 888 31 Exit interactive 999 lobserver amp allegro home home will bring the rotator back to zero This will prompt you to check the position of the silver tab on the dewar If it successfully went to 10 it should be just to the right of the sensor a small black box labeled as home on the side of Bolocam if you re standing with your back towards the control room If it looks good type g and hit enter The rotator limits are effectively 35 to 35 so if it s outside those limits there s a problem D Reset the Bolocam logic flags in the UIP window UIP gt flsignal 255 reset E Restart tel util Look in data00 encdir yyyymmdd and grab the mod number from the last file written Use that when restarting tel util observer allegro start Tel util yyyymmdd 1 1 1 mod F Resart merge When you restart the merge process you need to give it the current file
72. k and start up DSOS hardware go out into the dome on the third floor one level up from the control room On each side of the dome there are 6 valves and two temperature readouts Do the following e Check that both temperatures are about O degrees they don t have to be exact especially if you have just opened the dome and the telescope is still cooling down e Check that the pressure readouts show about 8 psi e Check that all six valves are fully opened counterclockwise 37 e Check that the flow of coolant is better than a trickle e Check the two additional temperature displays one is to the right of the amplifiers and one is above the amplifiers They should each read about 5 degrees e Turn on the power supply for all 8 amplifiers e Press menu on each of the 8 amplifiers e In pairs simultaneously press enter Now return to the control room Wait for the DSOS temperatures to settle all but 1 3 readings on the DSOSmonitor should be white win2 2 DSOSagent Wait for all but 1 3 DSOS temperatures to settle before observing Check to make sure the tertiary mirrors are in place for SHARC II You are now ready to observe with SHARC II 10 2 Observing Unchopped 10 2 1 Calibration and Pointing First you will want to image a calibrator both for flux calibration and for pointing To observe the calibrator do the following commands check the fazo fzao and foc off after inst sharc because it will load standard v
73. ll other macros ZLINE CLASS Draws zero line 53 14 List of GREG Macros in TEXAS PROC 2WINGS GREG Makes contour plot of line wings 4SPECNJE GREG Plots 4 spectra on same page in uniform fashion 4SPECTRA GREG Plots 4 spectra on same page CHANNELMAP GREG Makes contour maps of spectral channels CHAN GREG Nicer one for channel maps CONTOUR GREG General contour map making routine CON GREG Very nice contour map making routine HEADER GREG gt Header macro used in all other macros MACRO TXT gt Description of all macros PLOT GREG Simple 2 dimensional plotting routine POINT GREG Plots pointing data for the run POINT230 GREG Plots pointing data for the 230 Receiver RATIOS GREG Plots CO 3 2 and 2 1 spectra and ration on same page START GREG Startup macro TAILER GREG Tail macro used in all other macros WINGS GREG Makes contour plot of line wings 54 15 The CLASS Startup File The current 06 06 version of the CLASS startup file START CLASS is listed below This file should be run immediately after entering a CLASS session using the command Gp start This listing can be used as a quick reference guide to the short hand symbols defined within START CLASS The current symbols can also be listed by giving the command SYMBOL in CLASS This macro can be used for each time you start a new session with class To use just type Gstart or p start depending on whether
74. llow the trace to smear from a point to a line which indicates instability Go back to the main peak and adjust V for a peak and B for a point like steady trace Check the Y factor 6 4 Using the Wideband AOS AOS5 This is a very nice AOS but it has some quirks See Hiro s writeup in the Memos section of the Cookbook or for the latest look in http www cso caltech edu docs hiro wideband aaos html It has 4 IF units each covering about 1 GHz with 2048 channels If your line is not extremely wide it is best to center in one of the IFs IF1 was the best in Dec 2006 This is selected by the IF qualifier on the LO command IF 4 5 selects the first IF IF 5 5 selects the second etc Note that this choice does not prevent the other IFs from being stored in the data file or from being displayed on the spectrometer display To select only the IF you want with CLASS use the set telescope command and put the exact name e g CSO 4GHz IF1 in quotes Then FIND will retrieve only the first IF To display only the first IF on the AOS screen type the following no spaces between tildes and numbers UIP gt TO A 8 9 0 2047 Likewise to show the first 3 IFs use 16 UIP gt TOA 8 9 0 6143 The higher IFs especially IF4 often lack enough power so you will get continual complaints about the RF power being too low You can disable this with the following rather dangerous command UIP gt REPLY DISABLE This should be undone as soon as
75. ly equal in size to the calibration source size For example nmg calculated using Jupiter is not really appropriate for objects gt OjuprrER Or objects Ojuprrgn Under these circumstances one of the following calculations must be done 1 1 For objects lt lt Ojuprrgn one should use nmg measured on a smaller planet like Mars and correct the temperature measurements by the filling factor for your source and beam bs ye Ysmall source up MARD 7 MB 2 2 For objects gt yuprrer one should use nyg measured on a larger planet Unfor tunately there are no planets larger than Jupiter so one must use up derived from moon measurements Tlarge source up MOON Note though that because the moon is so large 30 use of a moon derived Nu will under estimate TR because of the inclusion of the beam sidelobes in the Ti measurement Note also that if you use the moon as your calibration source you will actually be measuring just Ness Since main beam 1 for sources much larger than the beam Information regarding the use of the moon as a calibration source is given in 84 67 18 3 Calibration Source Temperatures In the following we discuss a few things that one should be aware of regarding the use of Mars Jupiter and Saturn as calibration sources In Table 3 1 we list brightness temperatures for Jupiter and Saturn 18 4 Mars Brightness Temperatures Because Mars is bright compact and has a solid surface an
76. mea surements of Ulich 1981 do not agree with the model predictions of Epstein et al and are instead consistent with no ring emission Our own measurements of the main beam efficiency using Saturn during a period when the ring inclination was about 20 are generally lower than efficiency measurements made using measurements of Jupiter or Mars see 5 Our current recommendation is to avoid the use of Saturn as a calibrator until these effects are understood Update In June 2008 run we observed Saturn and Mars at the beginning of each night and Jupiter a few hours later We compared the efficiencies measured on Saturn to those measured on Jupiter At this time the inclination of the rings was relatively large at about 8 6 degrees so the effect would have been a maximum Yet we found essentially no effect with n Jupiter nSaturn 0 99 at 230 GHz 1 06 at 245 GHz and 1 04 at 279 5 GHz As far as we can see Saturn works fine with an assumed Tplanet 135 in the 230 to 280 GHz range 69 Table 3 1 Jovian Planet Brightness Temperatures Planet Mean Frequency Bandwidth Thlanet Reference GHz GHz K Jupiter 31 ht 152 4 4 8 1 86 ein 180 4 4 7 3 90 Ee 172 5 1 4 3 90 T 179 4 4 7 1 150 E 167 0 12 0 1 150 50 be 341 3 22 Y 70 170 9 9 279 75 169 9 5 1 3 310 130 175 0 10 0 2 337 150 174 3 5 1 3 392 75 162 5 2 0 3 451 270 167 1 2 1 2 580 420 149 9 2 6 2 666 170 135 0 5 0 2 674 90 148 5 4 9 3 724 625 155 3 1 3 2 808 200 143 7
77. n extension of size E to a map of size A in the direction you are expanding with spacing S then you can calculate the new center position of the extension by que ES A Then issue and RAO FIELD x or DECO FIELD x command before issuing the OTF com mand e g I want to make a 70 x 70 extension to the west on an existing map with an western edge of 50 and a spacing of 10 Then z 29219 50 90 The commands would be UIP gt SPEC 13 debase UIP gt RAO FIELD 90 UIP gt OTF 70 70 2 10 10 10 cal foc 7 3 2 Quadrant Mapping BIG OTFs For very extended sources it is more practical to split up the OTF into 4 quadrants For an OTF 110 110 it takes 18 minutes with overhead OTFs bigger than 130 x130 are probably not practical as sky conditions change the source airmass changes and especially if you don t know the extent of your source The quadrant method can produce a 210 x 210 map in 72 minutes while doing 4 CALs In general if you want to produce a map that extends to A with S spacing then the commands to produce 4 quadrants are IP gt RAO FIELD 44 IP DECO FIELD 4 JIP gt OTFAA21088 JIP gt RAO FIELD 4 IP gt DECO FIELD 4 IP gt 21055 IP gt RAO FIELD 4 IP gt DECO FIELD 43 IP 21055 IP RAO FIELD 4 19 IP gt DECO FIELD 42 JIP gt OTFAA21088 e g for a map that extends 100 x 110 with 10 spacing the center positions of the quadrants would be 60
78. nd sharcDSP again See the SHARC II User s Manual for more on this Now start the acquisition software 36 win3 2 ssh sharc sharcii password 350mu_m cd 7 ire sharcServer wait until the sharcServer stops starting up before proceeding you will know it has stopped by the fact that it stops displaying new messages Open a new window on the second kilauea display display 0 1 Execute the following ssh sharcOkilauea password 350mu_m cd irc sharcClient The messages about the polarimeter being unavailable are normal By request of the SHARC II staff please make sure to fill out the Observation Options fields wavelength observer project etc Important Check the SHARC II cheatsheet on the SHARC II webpage to see if you should use sharcClient Test or sharcClient This opens a graphical interface to the acquisition software If the bolometer array does not show any data quit and restart the sharcClient If this still does not work try restarting the DSP In the window you should have e mode single preset time e DSP Convergence 200 0 mV e max iterations 5 e stabilize delay 2000 msec e Display leveling constant e filter 350 ym The final thing to do is to start up the DSOS The dome should have be open at least 45 minutes prior to executing the following so that the telescope has had enough time to cool down Make sure the telescope is at ZA 45 win2 1 DSOSmonitor win2 2 DSOSinit Chec
79. number so that it doesn t get stuck on files that don t contain any data The easiest way to do this is to look in the das_data folder on Andante The numbering of the files should jump Type the following command where x is the first file number AFTER the jump on kilauea or wherever you started the merge start merge yyyymmdd x F Restart your macro Watch the rotator window that opened when you started tel util If the same error message appears at first it s alright The rotator window shows what is being written to the log and it may be a bit behind Watch for a bit it should return to normal operation IDL reduction processes crash A To restart the slicer IDL gt run_auto slice_files yyyymmdd obsnum x B To restart other windows IDL gt run_window_name Just type run once not twice like in the name of the window If you end up with a bad observation you should move the sliced file into a bad folder within the field s sliced folder Otherwise the cleaning and mapping software will get hung up on it If the cleaning crashes on an observation you might want to go into the cleaned directory and delete all files associated with that observation If there are no files in the cleaned folder 32 the cleaning software will reduce the observation as if it were new which is often what you want when it crashes TLENGTH error This is when the telescope and the dome get out of alignment When it happens the telescope
80. ollected data from our CSO archives regarding the issue of whether there are sys tematic differences in calibration between the two different AOS s The effort was motivated by the warning of dynamic range problems in the 500 MHz AOS The largest data set was for 140 but we have added some other data as well as collected in the accompanying table The data for the CO J 3 2 line were sufficient to do some statistical analysis The average value for the line as seen in the 500 MHz AOS is 31 9 2 1 K while the 50 MHz AOS gave 29 9 1 5 K One can also use the table to compare values taken at the same time The results usually agree very well The same is true of the CS J 5 4 line given the lower signal level on that line We have also plotted the 74 value versus system temperature and find a possible slight trend for lower T4 at lower Tsys but it is barely significant The con sistency of the results is encouraging in several ways First it suggests that dynamic range has not been a problem at least during the times that these data were taken This does not mean that continued caution and checks are not necessary Second it seems to imply that different tunings will not produce vastly different sideband gain ratios at least for the lines considered here TABLE 1 Line Temperatures ine ource un can sj H K K 3 2 140 uly90 1781 900 1449 28 10CT91 3925 500 2063 33 3926 50 1600 3l 500 2076 34 50 1608 30 500 2095 34 oc M 50 1632 3l
81. olocam accounts share one home directory so if you login from more than one place and try to access the same directory the computers will become confused Things will slow down and severe aggravation will follow 2 From kilauea Telnet into alphal username bolocam password 1sttry 3 Start the User Interface Program UIP on alphal by typing uip Then type UIP gt instrument bolocam 4 Next check the fridge cycles and disk space on Andante You access Andante through a remote desktop on ahi the windows machine in the control room Andante is located in the dome You cannot kill programs on Andante from ahi you must do so directly on Andante For those not familiar with windows machines hit ctrl alt delete to open the end task window Select the task you wish to kill and hit the end task button A Check the temperatures for the fridge cycles You should expect to see a drastic increase in temperature followed by a leveling out at a colder temperature Make sure that the UC temperature in the bottom right hand corner of the fridge control window is at approximately 0 250 K This is the part that actually cools the detector Another location to check the temperature of the detector is on the same rack as Andante in the dome To the right of Andante there will be a read out of resistance After a succesfull cycle this should read approximately 45 kQ If this instead reads a few tens of 2 the detector is too hot resistance increases as
82. ome kilauea texas proc on the CSO computers This macro will do all the work for you The CSO format catalog files are now compatible in format so you can just use those catalogs The format is simple sourcename rahours ramin rasec decdegrees decmin decsec For example L1630 05 39 12 01 55 42 To run the macro it is first necessary to enter ASTRO Type ASTRO You will now be in the ASTRO program Ignore the messages displayed on the screen Then type the following ASTRO gt QP ELEV PLOT Some messages now appear on the screen describing the setup that the macro will use as well as a reminder of the format required for the source catalog The macro will prompt you for the relevent information such as the date and the minimum source elevation It will now plot elevation vs time for the planets and then will ask if you wish to plot specific sources as well as the planets If you answer N the macro will end If you answer yes you will be asked to enter the name of the source catalog you wish to use enter the full name including the extension The next prompt asks for the source names You can enter as many source names as you wish as long as they are separated by a space The plot will appear and the macro will end To make a hard copy type HARD PL at the ASTRO gt prompt 83 21 TROUBLE SHOOTING as of December 2006 211 UIP Very Slow Things Hang A likely suspect is the VMS computers Believe it or not there are still 3 of these dinosa
83. ommand does this for you but be sure to check It also sets the focus mode to constant It may or may not get the tertiary in the right position so check that with the TERTIARY command You will need to set FAZO FZAO and FOC OFF to your last values if different from the pointing file and you will need to start the sweep again see 810 for details about switching to SHARC II or 89 for details about Bolocam If you will not use the heterodyne system for awhile it is a good idea to shut it down For all receivers you should attenuate before doing anything else to protect the multiplier It is also good to turn down the magnetic field and turn off the switch on the magnetic field box Also there is an absorber that fits in the sidecab port to keep RF signals from the sidecab from entering the other instruments You may want to turn off the receiver more completely depending on the receiver For the sidecab receivers at least press Rx DL toggle switch on touch screen and then MAIN 6 2 Switching from Continuum to Heterodyne For heterodyne instruments the instrument command sets most things but not the tertiary UIP gt INSTRUMENT RX230 13 will select the 230 sidecab receiver and set the sidecab mirrors appropriately Alternatively using the SPEC command tells the UIP that you will be using heterodyne mode It also of course selects which spectrometer you will use The practical choices as of January 2010 are FFTS1 the Fast Fourier Tr
84. or 5 5 for channel B or 5 0 to center between them for very wide lines If IF is chosen that is greater than 2 GHz the UIP will assume that you are using one of the wideband receivers whichever is suitable for your line frequency So for example to switch from using SHARC II at Nasmyth 2 to Frank s receiver at cassegrain use UIP gt SPEC 10 AOS5 RESTART UIP gt LO linename IF 4 5 LOCK SMA FORCE UIP gt TERTIARY CASSEGRAIN Be sure to check the heterodyne data file name and scan number with Status command in UIP Then you could issue the tertiary command to see where it is If you get a synthesizer error maybe FAILURE 06 on antenna computer monitor it is probably the synthesizer in the sidecab which feeds a 109 MHz signal to the synthesizer connected to Frank s receiver In the sidecab find the HP synthesizer go to local push blue button program for 200 MHz and the status light should start flashing Turn the synthesizer off wait 10 seconds then turn back on wait for status light to stop flashing then program for 109 MHz If the status light does not stop flashing after about 5 seconds repeat the procedure While the procedure outlined above may work there can be problems especially if you are observing a galaxy with a substantial velocity offset Then the velocity won t be set until you observe the source so the Gunn probably won t lock and the AOS may hang because it wants to take a frequency calibration but it won
85. or not you have a copy of start class in your working directory p header sic edit vi sic help page SET FORMAT ORIGIN ON set angle second set telescope set line set source set offset set number set mode x auto set mode y auto set plot histogram set format long set unit V F set align v set map clear set match 3 set box 2 27 2 15 Now set up some abbreviations for some commonly used CLASS commands sic verify on symbol mx set mode x symbol my set mode y symbol ss set source symbol sl set line symbol ssc set scan symbol so set off symbol b1 base 1 symbol sw set window symbol fi file in symbol fo file out symbol st set telescope Ap tailer 55 16 CLASS and GreG Macro Descriptions and Directory Man agement The texas proc subdirectory contains CLASS and GreG macros which are of general use to most of us Below is a listing of the macros currently residing in texas proc along with a short description of what each one does To run these macros within CLASS or GreG give the command texas procprocname or the shorthand command Ap procname 16 1 CLASS Macro Descriptions e 50 Sets the telescope to CSO 50 MHz so that only 50 MHz AOS data will be selected Author NJE e 500 Sets the telescope to CSO 500MHz so that only 500 MHz AOS data will be selected Author NJE e 502 Sets the telescope to CSO 500 2 so that only second 500 M
86. oval of ripples FITS PRO CFITS program to write a FITS tape FITALL CLASS Does fits to all scans in index interactive GETOFF CLASS Sums smooths and plots scans for an offset position HCL CLASS Jaffe receiver macro HCLN CLASS Jaffe receiver macro HEADER CLASS Header macro used in all other macros HICAL CLASS Jaffe receiver macro HICALOLD CLASS Jaffe receiver macro HLOOK CLASS undocumented alien HTRANS CLASS Jaffe receiver macro MACRO TXT Description of most macros MAP CLASS Makes grid map of spectra MAPCSO CLASS Same as MAP but with labelled x and y axes ON OFF CLASS Jaffe rec macro OTF_PROC_DES CLASS For reducing OTF data OTF PROC DES 50 CLASS For reducing OTF data PB CLASS Smooths and removes baseline PBG CLASS Smooths removes baseline and fits Gaussian PBJM CLASS Interactive version of PB PLOT CLASS Smooths and removes 1st order baseline PLT CLASS Smooths and plots PLTSIG CLASS Writes sigma on bottom of plot READFITS PRO CFITS program to read a FITS tape RENEW CLASS Jaffe Rec macro RNW CLASS Resets parameters and gets new data RMS CLASS undocumented alien SIDE CLASS Switches sideband SIDEALL CLASS Switches sideband for list of scans START CLASS Startup macro SUBTRACT CLASS Jaffe receiver macro SUMALL CLASS Sums positions in a map TAILER CLASS Tail macro used in a
87. piter and Saturn measurements 1 1 If possible hook up a digital voltmeter to monitor the total power from the re ceiver This is generally not easy anymore but it can provide a reality check on the spectrometer linearity 2 Following a check of the pointing do three separate OO scans of the planet in whatever spectrometer you are using SPEC 10 OO 2 The three separate measurements will allow a check of the consistency of the measure ments and using your actual spectrometer will effectively calibrate through the same system used for your data 3 While the OO scans are being taken note the total power voltage from the digital voltmeter for both the ON and OFF positions and write them down This will allow a check of the T4 scale 4 When the OO scans are done go out to the receiver and measure the HOT load and COLD load voltages Write them down with your ON and OFF voltage measurements Moon measurements 1 1 If possible hook up the digital voltmeter to monitor the total power from the receiver 2 Go to the moon and do a scan using the OO command PLANET MOON SPEC 5 DEBASE OO 2 CAL Note that the OFF position will be 1 in azimuth away from the ON position As with the planet measurements the three separate measurements will allow a check of the consistency of the measurements 3 While the OO scans are being taken note the total power voltage from the digital voltm
88. rent position of the tertiary You can change the position by typing for example UIP gt tertiary cassegrain 7 Start the reduction processes On kilauea or whichever computer is logged in as bolocam in the home directory type gt start merge yyyymmdd This should open a window titled merge When copied from Andante to data00 the data is still in separate files for each mod My current understanding is that the merger puts the time stream from the bolometers back together and the slicer one of the idl scripts described below then slices the time stream into a separate file for each observation Then type 28 gt start autos This should open eight IDL windows which will process the data and produce a sav file This quick data reduction is described more below 8 You are now ready to observe 9 2 Galactic Plane Survey Macro Generation Procedures To make the observing macros for the Galactic Plane Survey gt cd home kilauea Bolocam GalacticPlane gt idl IDL gt bgps make macro coord b cord This will automatically create six mac files which will be saved in user_vax bolocam and readily available to execute The naming scheme L 1Bbbb_Ixbd mac lis the number of degrees in covered by the scan and 6 is the number of degrees in b d represents the scan direction it will be either an lor a b The files produced are 3x11 3x1b 1x3l 1x3b 1x1l and 1x1b A 3x1l takes approximately 42 minutes to complet
89. ritten for your convenience To use it simply type P SIDE Vg FREQUENCY after calling up a scan in CLASS where Va is the earth velocity Vradia at the CSO in km s and FREQUENCY is the rest frequency of line B in MHz Plot the spectrum to check the velocity scale write to a file if you are satisfied If you have problems it is most likely that you are at the 14000 foot level There is also a version of this SIDEALL which will do all the scans in your index 50 12 5 Mapping Data Reduction Reducing mapping data can be quite confusing especially when you have data from several observing runs Here we assume that you have raw not frequency corrected data from CSO and that the telescope efficiency did not change from one run to another For generality we also assume that you want to change sidebands If your data is already frequency corrected skip step 1 if your data was taken in the sideband that you want to examine skip step 4 In each step you are required to choose the correct input file using FILE IN and then build up an index of interest using SET and FIND 1 Frequency calibration please refer to the relevant section for details This step is not needed for data taken after Aug 1991 If you need it you can use a macro to correct all the scans assuming you have reduced the FCAL data and know the correct center and width Briefly you can type P FCALL CENTER WIDTH FILEOUT where WIDTH is positive and has units of MHz FCAL
90. seconds is better Note that these only apply for sweep mode observations If you are using box scans set the integration time based on the values given on the SHARC II website Click start to start the integration Don t forget to log all of your observations 10 3 Data Reduction This section describes the type of data reduction you will be doing in real time at the CSO It does not describe the detailed data reduction you will eventually perform back in Austin Raw data are kept in home transfer sharcii data 2004Sep 2004Sep replaced w current month Reduced data is kept in src data fits fits is the output from crush Open a new window on desktop 4 win4 2 To reduce a scan convert it from a scan into a FITS file coadd reduced FITS files and look at the images type win4 2 ssh Y sharcOkilauea password 350mu_m cd src crush crush options scant this will take several minutes with the eventual result being a fits file If you have more than one scan of the same source you can reduce them all at once by the following although it might crash if you give it too many and you run out of memory 40 crush options scans scan 2 scan 3 win4 2 coadd data 1 fits data 2 fits data 3 fits win4 2 show data imagename fits use Z and z to zoom use B and b to change brightness scale leftclick to select area use f to print out flux and rms middle click to select a beam size Note that t
91. t do that while the Gunn is unlocked This can prevent you from ever getting to observe the source so you can only control Y out of UIP To avoid that problem here is an example of how to switch from SHARC II to Frank s receiver at Cassegrain 14 with the AOS5 and a galaxy with a large velocity offset The idea is that you locked the Gunn on this earlier and now you want to go back to it JIP gt SWEEP STOP JIP gt OBSERVE NGC4175 IP gt LO linename IF 4 5 LOCK SMA FORCE JIP gt SPEC 5 AOS5 RESTART LOCK SHUT_UP IP gt TERTIARY CASSEGRAIN IP gt POINTING BARNEY_CASS IP gt FAZO XXX IP gt FZAO YYY IP gt FOCUS STEALTHY IP gt DATA filename nextscannumber JIP gt STATUS Then you need to actually get the receiver of choice going Remove the absorber in the sidecab port if it is there We will assume here that the receiver has been turned off There are manuals on receiver tuning What we give here is a generic set of steps for the sidecab 230 receiver Use the blue touch screen box to choose the receiver Lock the Gunn by reading Flock on the antenna computer screen consulting the sheets posted on the wall for the Gunn setting the micrometers close to the values indicated and tweaking til you get a lock signal Then put in a hot load deattenuate clockwise til you see some increase in SIS current and total power Then tune the SIS backshort and E plane tuner upper and lower knobs behind dewar for a maximum The best way to a
92. t two steps If not take a calibration scan UIP gt TCAL offset 300 altaz Now take an OO scan with 1 cycle This is done just to get a quick scan which will allow you to see where your baseline window should be set UIP gt OO 1 noatt nocal UIP gt SPEC 10 Now set the baseline window by typing UIP gt SPEC 1 2 3 4 5 Where 1 is the integration time in seconds usually set to 10 sec for pointing The purpose of the other four numbers is to exclude everything below 2 and above 5 from the baseline calculation It will also exclude everything between 3 and 4 basically this excludes the line from the baseline calculation These numbers are read off the Spectrometer display screen after the OO scan has been completed The baseline intervals should be small less than 50 channels and close to the line Now we do the five point map by typing UIP gt FIVE 2 3 ONE CENTER 1 where ONE tells the computer to do only one off scan CENTER 1 sets the center of the line at position 1 read off the display screen 2 is the distance in arcseconds that each scan will be displaced from the central position normally 10 for the 345 GHz receiver and 15 for the 230 GHz receiver 3 is the HALFWIDTH of the line The computer will now happily chug along and eventually spit out its suggested corrections to FAZO and FZAO then ask you if you want to input these to the computer It is a good idea to repeat the FIVE comm
93. tart tel util yyyymmdd 1 1 1 A quick aside These processes are responsible for copying the data from Andante to data00 recording telescope parameters that aren t included in the data files etc The rotator window tells you the current rotator position The write log window tells you which log file is being copied over The dirsync window tells you which data file is currently being transfered over it usually runs a few minutes behind write log All observations are written to a one file per minute so the file name corresponds to the minute since midnight UT For example the write log window will say wrote encoder log entry to file data00 encdir 20060621 060621 0946 dat on Wed Jun 21 15 46 02 2006 In this example the minute of day mod number is 0946 Because dirsync typically runs a few minutes behind write log the pipeline will wait for dirsync to catch up before it begins the reduction making it a not quite real time reduction D Go back to Andante and Start DAS In the labview window First change the output directory field to include the current UT date It should say D das_data yyyymmdd Then click on the arrow button at the top of the window just underneath the Edit and View menus to start the DAS There will be a short delay but the plots should begin update and plot the output from a few of the good bolometers 6 Check the position of the tertiary mirror In the UIP type UIP gt tert This will return the cur
94. temperature decreases A very detailed description of the fridge cycle procedure as well as an image of a successful cycle can be found at http www cso caltech edu bolocam Fridge html B Check the amount of available disk space located in D das_data by double clicking on the shortcut to My Computer located on the desktop If not enough space is available delete the oldest folder in Adas data folders are named with the UT date ie yyyymmdd Data is automatically backed up elsewhere so don t worry about losing data 5 The Data Acquisition Software DAS is run from Andante To start the DAS double click on the BCAM DAS 20061119 icon on the desktop During the July 2007 run we ve been leaving the DAS open on Andante so check if it s already open before you click StartDAS A First create a folder in Mas data with the name corresponding to the UT date yyyym mdd There s a quick link to das_data on Andante s remote desktop 27 B Next you must synchronize Andante s clock with Hau Do this by double clicking on the time in the task bar When the Date and Time Properties window opens go to the Internet Time tab Select hau and click Update Now Wait for a message to appear in that window saying it was successful then click OK on the bottom C Now back on kilauea you ll need to do start tel util which will begin 5 procedures and open a window for each ssh observer allegro password 503 dvc observerQallegro s
95. ter of calibration source poi poloidal diameter of calibration source e yp telescope main beam FWHM 66 Tpianec can be found in the literature see 83 Aq and 054 can be found in the Astronomical Almanac and yg can be derived from the following relation assuming a diffraction limited beam with a uniform illumination pattern and 10 dB taper on the edges A 72348 267 Hun 117 5 radians arc seconds D vD where v is in GHz and D in meters 10 4 for the CSO Note that the beam is not diffraction limited and you should check the CSO web pages for the most recent values of the beam size but do not take the quoted efficiencies you find there at face value The term involving Tembr takes into account the fact that when you position switch on an opaque object like a planet you are actually measuring the difference between T planet and the temperature of the cosmic microwave background radiation The cosmic microwave background term contributes lt 1 to the J vs T planet J Vs Tembr term so can generally be ignored Using the Rayleigh Jeans approximation to Ji Tplanet results in an 2 6 overestimation of this term for measurements of Mars Jupiter and Saturn in the 200 365 GHz range To first order yp as calculated above is appropriate for objects with sizes equal to up hence the term main beam efficiency To second order as calculated above is appropriate for objects approximate
96. the offset position in arcseconds North The following macro will take a cal scan and a position switched scan UIP gt CAPS where is the number of on off cycles that you want 4 is a reasonable first guess if the spectrometer integration time is set to 20 this will give you 80 sec on source and 80 sec off If you want to take another position switched scan using the same CAL just type UIP gt PS where gives the number of on off pairs as before 7 1 Mapping To map we need to move the telescope to offset positions This is very easy to do thanks to some macros that have already been defined They are UIP gt E Moves the telescope arcseconds East of the reference position UIP gt W Moves the telescope arcseconds West of the reference position UIP gt N Moves the telescope arcseconds North of the reference position UIP S Moves the telescope arcseconds South of the reference position Note that these are NOT taken with respect to the current offset but with respect to the reference position Thus typing N 10 when you are already 10 seconds north will have no effect 7 2 Comments If your off position isn t very close to your source position you may spend a lot of time moving the antenna and yourself This dead time can be partially reduced by relaxing the limits which 19 determine whether the antenna has acquired the off position as long as your off position is far enough away For example
97. the only ones being maintained These procedures should not be changed except with approval of Neal Evans If you want to modify them copy them to the run directory and make versions suitable for the particular run At the end of the run if you have improved some of these or created new ones that you think are generally useful check with Neal Evans about adding them to the proc directory Be sure to comment them and follow the instructions in the section on CLASS Macro Descriptions and Directory Management Delete others or move them to your private directory Catalogs are kept in uip cat They should be accessed there by typing from within the UIP cat name cat or cat uip cat name cat They are now simple text files and can be modified with any text editor Each person can have a subdirectory for storing idiomatic stuff Generally useful stuff should be documented and placed in appropriate directories To delete for example the DEC99 directory go to the directory above the one you want to delete from a unix machine and type rm r dec99 Current Status of Texas Directory As of January 2010 the Texas directory on Kilauea at the CSO has the following generally useful subdirectories uip cat contains source catalogs There are also two files locations of general relevance gag init init uip contains definitions of macro names and locations of macro files that are loaded upon starting the uip u
98. the output file set to JUNK BUR for technical reasons No inputs Author SZ 56 PB Smooths and removes a baseline of pre determined order to a scan and plots it Baseline regions must be pre set User is prompted for the scan number or the scan number can be input at the pb command Input is the scan number Author NJE PBG For a given scan smooths removes a baseline of pre determined order fits a gaussian and plots Same input as for PB Author NJE PBJM Smooths interactively removes baselines and plots Same inputs as PB Author JGM PLOT Smooths removes a first order baseline and plots a scan Assumes that baseline regions have been preset User is prompted for scan number or scan number can be entered directly at the plot command Input is scan number Author NJE PLT Smooths and plots a scan User is prompted for scan number or scan number can be entered directly at the plt command Input is scan number Author NJE RNW Resets all data selection parameters and gets any new scans from the input file No inputs Author NJE SIDE Switches sideband and sets velocity scale for image sideband Inputs are the Earth s radial velocity and the frequency of the line in the image sideband to which you are switching Use Gside VRAD LINFREQ Author SZ SIDEALL Same as SIDE but switches the sideband for the scans in the current list User is prompted for the Earth s radial velocity the line frequency in the
99. the qualifier JN OFFSET set to your source velocity The computer will now happily chug along and eventually spit out its suggested corrections to FAZO and FZAO then ask you if you want to input these to the computer It is a good idea to repeat the FIVE command the ENTIRE line NOT just the word FIVE a few times and averaging the values before inputing the new values of FAZO and FZAO by typing UIP gt FAZO UIP gt FZAO where is your chosen offset When you are well peaked up do a quick OO scan switching in azimuth just type UIP gt oo 1 the offposition will still be 300 arcseconds in azimuth from the above off_position command Make sure the cal is done off the planet When you get a chance reduce the data and calculate an efficiency using the equations in the Calibration section This is a good way to see if something is wrong at the time Keep a record and summarize your efficiency measurements in the run report when you get back to Austin When happy reset SPEC to the value used for observing 8 2 Using a spectral line source This description applies to spectral line sources such as CO in evolved stars These are listed in the binder called CO Point Stars and their positions can be accessed by typing 23 UIP gt CAT CO_POINT_STAR CAT Then type UIP gt off position 300 altaz asym which sets the offset to 300 arcseconds in azimuth If you know how to set up the the spectrometer for this source you can skip the nex
100. to set the controls on the secondary and optimize the input wave form to create the best output wave form While it is optimizing the BSW part of the antenna display will flash This may take several minutes You can find out the status by typing SEC with no parameters or qualifiers and it will tell you its current status When it is optimized the first three things listed will say TRUE Once you have it set up for a given throw and frequency you can use the command UIP gt secondary reload and it will reload the last setting If it has been a long time it will ask you whether you want the computer to reoptimize This mode will turn the chopper off when you do a CAL or when you slew to a new source but it will turn it back on afterwards 22 8 How to check the pointing Heterodyne At the beginning of the night and occasionally throughout the night especially until the telescope has cooled down it is desirable to check the pointing of the telescope by making a five point map This is easily accomplished by using the UIP function FIVE This section describes how to do this for a continuum source and gives the general theory of how to do spectral line sources Note that the instructions below set up for switching in azimuth so to return to offsets in RA and DEC you will have to execute something like OFFPOS when you are finished or type OO JUST NOCOORD The system will point with whatever spectrometer you put first in the SPEC command For
101. u add a source you must specify source name epoch coordinates and source velocity Look at one of the existing catalogs for the proper format Names and qualifiers can have up to 20 characters but note that some characters notably and cannot be used unless you enclose them in quotes Thus G34 3 0 4 should be entered as G34 3 0 3 After adding a source to a catalog using a text editor the following sequence of commands from within UIP will open a catalog find out the number assigned to that catalog and check that the source has been added correctly CATALOG GAL CAT VERIFY CEPA The first line opens the catalog Catalogs may have any name but the extension CAT will avoid confusion The second line allows you to see what the UIP has made of your catalog entry It will show all entries for CEPA in any open catalog Enter either EQ 1950 00 or EQ 2000 00 depending on whether your coordinates are 1950 or 2000 This only affects the display and what is written in the header As far as we know the accuracy of the pointing is the same whether you stay in J2000 or convert to B1950 An important use of qualifiers is in absolute position switching to do this it is best to enter an off position in absolute RA DEC coordinates into your catalog with the same name as your source but with the qualifier of OFFPOSITION you must type out the whole word since it is part of the source name The qualifier is added right after the name with a b
102. u should now see an additional two red lights e Check the filter setting on the black knob on top of the cryostat you will need to climb the ladder to do this Don t forget this step or you could spend the entire night observing at the wrong wavelength The settings are 250 350 um 500 450 um 750 850 um Configure amplifier electronics and multiplexer Open two new terminals on desktop 3 and execute the following win3 1 ssh sharc SHARCII password 350 cd fpga go Reset the SHARC II DSP as follows cd DSP For some reason this did not work in June 2005 we instead had to type the full path which is cd home sharcii sharc DSP sharcDSP wait a minute s2 status You should see the number 12 twelve times and the number 36 two times status A bunch of numbers will print out to the screen including the UT Type status a few times and make sure the UT is updating and not frozen at a certain time If it is not updating try again a few times If it still isn t updating see below If it is updating type quit If the UT is not updating when you type status wait a minute and try again If it doesn t work after a few tries type conf4290 If this still does not work after a few tries push the small reset button about half way down the Pentek board on SHARC II located in the lounge Be careful to get the right one as there are several reset buttons on the computer Then execute conf4290 a
103. up the FCAL scan in CLASS and change the x axis units to channel number by typing LAS SET UNIT C Then make a gaussian fit of the central spike the results of which will give the center channel e g 510 instead of 511 5 To determine the frequency resolution measure the separation between two arbitrary spikes in channel number Then take the separation between the two spikes in frequency and divide by the separation in channel number For example since 5 spikes are injected into the 500 MHz AOS we will use the first spike and the last spike which we know to be separated by 400 MHz Assuming we measure the centre of the first spike to be at channel 100 and the last peak to be at channel 900 We find the frequency resolution to be 400M Hz MHz 900 100 channel All or at least a reasonable sample of the FCAL scans should be reduced and checked for consistency So far we have found a single correction can be applied to the whole week s worth of data Note that the process has to be done separately for the two different AOS s if you are using both Note that the 500 MHz AOS sets the value of the central channel to that with the centermost spike while the 50 MHz AOS sets it to the mean of the two centermost spikes See the discussion in the section called Calibration Memos Now to actually modify the data we use CLASS First get the spectra that you wish to modify Assuming you want to use the values from the examples a
104. urs here alphal alpha2 and poliahu Alphal is obvious as the big beige box near the bookshelfs with an ancient VT240 monitor attached Poliahu is a smaller box on the shelf of the bookcase and its own monitor Alpha2 is lurking by the door leaving the control room going to the lounge It s keyboard and monitor are on the shelf along the hall They all have to be rebooted in a certain order Check web or call Ruisheng for instructions I could not find instructions on the web but they could be somewhere Once you have them all rebooted you will have to restart the NFS server and the taume ter If you forget the first step the taumeter will run and write data but the antenna computer and the web won t know about it For instructions check the Mini how to page last item For instructions on the taumeter also check the Mini how to page first item 21 2 DOME POSITION UNSAFE If this message flashes on the antenna display screen check the lights on the control panel If the ultimate limit light is NOT illuminated you have only exceeded the software limits on the dome antenna misalignment Look at the lights labeled A D and A D on the left of the control panel If the A D light is illuminated the antenna is ahead of the dome in azimuth Disable the software limits and move the dome to a lower azimuth by typing UIP gt NOLIM UIP gt AZ aaa aa where aaa aa is 0 25 degrees less than the current ACTUAL azimuth AAZ on the antenna monitor
105. will figure out the sideband infor mation for you The output file has a default extension of MODIFY 2 Remove baseline use SET to find the SOURCE and LINE then plot the data and SET a WINDOW for the line The macro QP BASEALL BLORDER FILEOUT NEW OLD will go through each scan you FIND smooth with BOX 2 remove a baseline with order BLORDER and write into the output file called FILEOUT The output file has default extension BASE Use NEW if this is the first run and old if you are working on data from a second run 3 Sum scans The macro P SUMALL I1 12 J1 J2 SPACING FILEOUT does everything for you The macro assumes you have SET the WINDOW for the region where line appears and that you have removed baselines It will go through RA offsets I1 to I2 and Dec offsets J1 to J2 in steps of SPACING where all the quantities are in units of ARCSEC At each offset it will SUM up with WEIGHT set to S igma and write out to the designated output file The output file has a default extension of SUM For scans with different setups alignment in velocity is assumed To combine data taken before Nov 1989 you need to SET CALIBRATION OFF because the header was incomplete 4 Switch sideband please refer to the relevant section for details The macro P SIDEALL Vg FREQUENCY LINENAME will go through scans in the index switch sideband set the new LINENAME and write to output file default extension SIDE Note that all scans in the index must have

Texas Cookbook - Caltech Submillimeter Observatory

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