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1. After Tile and GS AOS star generation VISTA s xml files can become very long To view them it 1s recommended that you use a viewer editor that recognises xml structures and allows them to be collapsed to a shorter more readable form e g a web browser such as Firefox 8 6 2 Xml Schema The xml schema is included as cfg vista sdt xsd The schema must be recognised by P2PP when it imports xml files made in SADT Users must not edit this file 8 6 3 Structure of SADT xml files The xml file is structured as follows for a VISTA survey lt SURVEY gt element which contain one or more lt SURVEY AREA gt elements which contain one or more lt TILE gt elements which each contain typically 6 lt PAWPRINT gt elements which each contain lt REFSTARS gt elements giving coordinates and magnitudes of the guide and aO stars which are converted into paf files attached to the OB lt REFSTARS gt lt PAWPRINT gt lt TILE gt lt SURVEY AREA gt lt SURVEY gt 8 6 3 1 Example Survey Areas not Tiles yet As an example the xml file saved for the Survey Areas defined in Figure 4 1 after pressing View Update is as follows lt xml version 1 0 encoding UTF 8 standalone no gt lt SURVEY backtrackStep 100 0 id Fig_4 1 ip VIRCAM 1 25 maxJitter 15 0 tileAngle 0 tileOverlapxX 60 0 tileOverlapY 60 0 gt lt SURVEY AREA coordSys Galactic exclude false height 2 2 lat 2 0 long 32 0 number 1 p
2. You can then work with the converted file as with any other VISTA SADT XML file 6 7 Saving Surveys for use with P2PP Once generation of a survey with all its guide aO stars has been completed then the survey areas tiles pawprints and guide aO stars generated should be saved as a file in XML format with extension xm for later import into P2PP to enable produce all the OBs Observation Blocks needed to implement the Survey This process is defined in the P2PP manual this outline is included only for convenience but the P2PP manual must be consulted for a definitive description In P2PP the user constructs a single Parent OB 1 e chooses filters their DIT NDIT Nexp jitter pattern etc to be used for all the Tiles If not all the Tiles will use the same Parent OB the user will need to make appropriate subsets The user provides P2PP with the xml file from SADT containing the N tile positions pattern and guide aO stars P2PP conceptually at least does the following 1 Makes N copies of the Parent OB VISTA Survey Area Definition Tool User Manual for VISTA a 2 Copies into each 1 through N the appropriate telescope pointing coordinates for the tile derived from the saved SADT xml file 3 For each of the N tiles each with n default 6 pawprints generates n paf files containing the guide and aO star coordinates amp magnitudes for each pawprint within each tile as derived from the saved SADT xml
3. 5 4 1 Zooming The zoom options are 1 Zoom In 2 Zoom Out 3 Reset Zoom Select one of these and then Left Mouse click on the point in the plot about which you want to zoom in or out The zoomed plot will be centred on the spot you clicked on This offers a means of selecting the area being viewed It does not matter where you click for Reset Zoom VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG 5 4 2 Display Coordinate system The options are 1 FK5 J2000 2 FK4 B1950 3 Galactic 4 Ecliptic 5 SLOAN N B SLOAN mode is not required for VISTA and has not been tested Note this option only affects the displayed plots changing the display coordinate system is not a way if converting the coordinates displayed in the Survey Areas Table between systems 5 4 3 Plot type The options are 1 Cartesian Plot default 2 North Polar Plot Not useful for VISTA 3 South Polar Plot The plot type should be chosen to be sensible Le South Polar Plot for areas close to the South Pole etc 5 5 Exclude Survey Areas Individual areas may be excluded by ticking the Exclude box in Column 8 4 1 4 6 They can also be re included by unticking the box 5 6 Example Figure 5 2 displays the same area as Figure 5 1 but with the Geodesic Rectangle area excluded the Aspect Ratio set variable the Coordinate System set to Galactic and the window size aspect ratio changed by dragging a corner You can see t
4. AG Faintest acceptable guide star for this chip If a user feels any of these values are not suitable for his program he should contact ESO s VISTA Instrument Scientist for to request a change in these values MINPMER 5 0 for GSC 2 only Minimum value of proper motion proper motion error ratio for which SADT applies proper motion correction If total proper motion is lt MINPMER times its total error then the guide star is not proper motion corrected by SADT Guide stars are not rejected based on their proper VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG 8 5 Configuration Files amp xml Schema Instrument parameters required by SADT are read from the Instrument package s default isf file sadtdirectoryname cfg vista contains the xml schema defining the format of the xml files SADT writes for ingestion by P2PP The same directory contains two configuration files in which various configuration parameters are set 8 5 1 sad xsd The xml schema is included as cfg vista sdt xsd The schema must be recognised by P2PP when it imports xml files made in SADT Users must not edit this file 8 5 2 sadt cfg Configures most defaults in SADT An explanation of all these properties is provided in the sadt cfg file itself 8 5 3 skycat cfg The guide aO stars are searched for in a selected catalogues over the Internet and skycat cfg sets up the available catalogues appear in the catalogue choice box of th
5. 475 0 475 0 475 0 475 0 475 0 475 SEQ TILE OFFSETY 0 475 0 475 0 0 0 0 0 475 0 475 SEQ TILE OFFSETROT 0 0 0 0 0 0 0 0 0 0 0 0 Tile6s A Figure 8 6 Tile6s VISTA Survey Area Definition Tool User Manual for VISTA a 8 2 1 5 Tile6zz VISTA Tile6zz corresponds to FAEBDC left diagonal up left diagonal up left forming two z s on top of each other written as zz a VIS MAN QMU 0001 0003 Visible amp Norm Astronomy SEQ TILE NAME 6 step zz zig zag pattern SEQ TILE OFFSETX 0 475 0 475 0 475 0 475 0 475 0 475 SEQ TILE OFFSETY 0 475 0 475 0 0 0 0 0 475 0 475 SEQ TILE OFFSETROT 0 0 0 0 0 0 0 0 0 0 0 0 Tile6zz Figure 8 7 Tile6zz 8 2 1 6 Tile6ss VISTA Tile6ss corresponds to AFBECD right diagonal up right diagonal up right forming two s s on top of each other written as ss SEQ TILE NAME 6 step ss zig zag pattern SEQ TILE OFFSETX 0 475 0 475 0 475 0 475 0 475 0 475 SEQ TILE OFFSETY 0 475 0 475 0 0 0 0 0 475 0 475 SEQ TILE OFFSETROT 0 0 0 0 0 0 0 0 0 0 0 0 Tile6ss Figure 8 8 Tile 6ss VISTA Survey Area Definition Tool User Manual for VISTA a 822 Npaw 3 patterns a VIS MAN QMU 0001 0003 Visible amp Norm Astronomy There are two n 3 patterns which define contiguous strips like the one shown in Y but not in X 8 2 2 1 Tile 3nx SEQ TILE NAME 3 step nx negative x pattern SEQ TILE OFFSETX 0 475 0 475 0 475 SEQ TILE OFFSETY 0 4
6. 66 2 49 SEQ JITTER OFFSETY 9 89 4 65 4 11 3 19 4 87 6 68 4 35 5 17 1 83 0 94 4 27 8 02 7 95 8 11 4 76 5 40 8 78 2 31 8 16 7 51 8 55 9 94 5 19 2 57 8 39 5 64 9 29 4 03 0 84 4 00 Jitter3Or1 VISTA Survey Area Definition Tool User Manual for VISTA a a VIS MAN QMU 0001 0003 i ail 8 4 Instrument package settings for SADT The file default isf in the VIRCAM Instrument Package contains inter alia information some of which SADT reads Much of this 1s to do with the geometry of the IR detectors and CCDs and will not be discussed here Another part deals with parameters that SADT reads separately for each of the 2 AG and 2 LOWFS CCDs which define how SADT will find the potential guide aO stars in the catalogues it is searching The relevant values and their seeting as of VIRCAM IP 1 44 are Set NUMIN Minimum number of stars SADT should find NUMAX Maximum number of stars SADT should find SEPMIN Minimum separation arcsec from neighbouring stars whose 25 magnitude difference is less than MAGDELTA MAGDELTA Smallest acceptable magnitude difference to neighbouring stars within distance SEPMIN MAXECC for GSC 2 only Maximum eccentricity allowed motion regardless of whether or not the proper motion 1s corrected Brightest acceptable guide star for this chip Brightest acceptable guide star for this chip Faintest acceptable guide star for this chip MINMAG LOWFS MAXMAG LOWFS MAXMAG
7. 8 3 8 JitterS5n SEQ JITTER NAME 5 position pattern n shape with centre rotated 60deg cw SEQ JITTER OFFSETX 0 0 8 66 5 0 8 66 5 0 SEQ JITTER OFFSETY 0 0 5 0 8 66 5 0 8 66 8 3 9 JitterSz SEQ JITTER NAME 5 position pattern Z rotated 30deg cew SEQ JITTER OFFSETX 0 0 3 66 13 66 13 66 3 66 SEQ JITTER OFFSETY 0 0 13 66 3 66 3 66 13 66 jitter5z VISTA Survey Area Definition ST Tool User Manual for VISTA i a 8 3 10 Jitter9s SEQ JITTER NAME 9 position pattern square shape rotated 30 deg cew SEQ JITTER OFFSETX 0 0 13 66 8 66 3 66 5 0 13 66 8 66 3 66 5 0 SEQ JITTER OFFSETY 0 0 3 66 5 0 13 66 8 66 3 66 5 0 13 66 8 66 Jitter9s 8 3 11 Jitter25s SEQ JITTER NAME 25 position pattern square spiral rotated 30 deg cew SEQ JITTER OFFSETX 0 0 4 33 1 83 2 5 6 83 4 33 1 83 2 5 6 83 11 16 8 66 6 16 3 66 0 67 5 0 9 33 13 66 11 16 8 66 6 16 3 66 0 67 5 0 9 33 13 66 SEQ JITTER OFFSETY 0 0 2 5 6 83 4 33 1 83 2 5 6 83 4 33 1 83 0 67 5 09 33 13 66 11 16 8 66 6 16 3 66 0 67 5 0 9 33 13 66 1 1 16 8 66 6 16 3 66 Jittter25s Z IST VISTA Survey Area Definition d Tool User Manual for VISTA a 8 3 12 Jitter30r1 SEQ JITTER NAME 30 position pattern random numbers SEQ JITTER OFFSETX 5 66 9 10 9 37 2 73 4 77 6 63 9 56 7 53 3 14 5 63 8 22 4 91 2 24 3 61 6 70 2 66 5 65 6 16 3 59 0 88 2 24 1 16 3 11 7 61 9 96 7 85 4 86 5 02 6
8. Note that some tiles may then not have GS AOS stars for all the pawprints and the OBs will not successfully complete without operator intervention With Backtrack Step 0 set in the GUI when tiling with guide star search is executed the catalogue is queried but if no guide star is found no backtracking is applied and the current position of the pawprint is retained The result is a set of tiles with the same coordinates as if no guide star search were performed but with additional REFSTARS information that was retrieved from the catalogue In addition to the geometry there are several other parameters set in the Instruemnt Package which influence whether guide aO stars will be found These are described in 8 4 3 3 Main GUI Menu Help Clicking on the Help menu brings up the following Window User Guide About 3 3 1 User Guide Refers the reader to the location of the User Manual this document The latest version should always be avialble at www vista ac uk observing sadt 3 3 2 About Gives the version numbers of SADT and Instrument Package version currently being used together with terms and conditions of use and a disclaimer 3 4 Main GUI Box Survey ID Define a name for your Survey in the Survey ID box This will be the default name used in saving or exporting files from SADT It will also form part of the name of the parameter files ceated for your survey by SADT P2PP so use something brief but clear If nothing is ent
9. Visible and Infrared Survey Telescope for Astronomy 1 3 VISTA focal plane layout Figure 1 3 shows VISTA s focal plane consisting of 16 Science IR Raytheon detectors s 1 16 shown in green The number in brackets after the detector number gives the ID number 1 4 of the IRACE board controlling the detector and the letter A D gives the channel in that IRACE board 2 Autoguider CCDs AG PY amp AG NY shown as blue rectangles 2 active Optics or Low Order Wave Front Sensor CCDs LOWFS PY amp LOWES NY shown as blue squares VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA i suwnjoo 10798480 Science detectors controlled by IRACE Figure 1 3 Focal Plane layout looking down onto it Note the definition of X and Y directions N B When looking out onto the sky the detectors are painted on the sky in the mirror image with 1 in the top right The IR detectors are not contiguous so a single sky exposure known as a pawprint shows the gaps between the detectors As is explained in detail in Section 8 1 to make an image without gaps it is necessary to combine together several typically 6 pawprints with position offsets chosen so as to cover the gaps and form a filled tile Six is the minimum number of pointed observations with fixed offsets required for reasonably uniform and completely contiguous coverage and exposes each piece of sky away from the upper and lower edges in
10. axes of the focal plane and which detector is which To toggle this Tick Untick the Draw Aux Detectors option on the Options menu 3 2 5 Include Overlap On Off If this option is selected then tiles which lie partially in an included survey area and partially in an excluded survey area 4 1 4 6 are included Otherwise they are excluded To toggle this Tick Untick the Include Overlap option on the Options menu VISTA Survey Area Definition Tool User Manual for VISTA a 3 2 6 Configure Preferences Select Values a VIS MAN QMU 0001 0003 Visible amp More Astronomy Clicking on Configure in the Options menu brings up the Window in Figure 3 1 which shows the GUI window for setting these parameters AO Configuration preferences Amount by which adjacent tiles should overlap arcseconds gt 2x sampled overlap in X 60 0 gt 2x sampled overlap in Y 60 0 Maximum jitter amplitude i e O to max min which will be used in the survey arcseconds Maximum Jitter Amplitude 15 0 Tile Y axis orientation degrees Tile Orientation 0 ES Backtrack step if not enough guide aO stars found arcseconds Backtrack Step 100 0 Figure 3 1 Configuration preferences global value setting interface The default tile to tile overlaps of 60 arcsec are recommended for ease of tieing together adjacent tiles during data processing Before changing Tile to Tile overlaps from the default parameters consult the Appendix i
11. coordinate system shown in Figure 4 1 would look like Figure 5 1 Survey Areas displayed in FKS 2000 Cartesian Plot Zoom 1 01 00 mem 00 00 00 TT 01 00 00 il 02 00 00 ii 03 00 00 II T ei y amp ae II 19 20 00 19 16 00 19 12 00 ien e 19 La 00 19 per 00 18 Li 00 18 a 00 18 48 00 Figure 5 1 View of Survey areas of Figure 4 1 displayed with the Fixed Aspect Ratio ticked in Options One area of each type Geodesic Rectangle Circle Coordinate Range each defined in a different coordinate system 5 3 Coordinates at mouse in display system You can find the coordinates of the current mouse position in the current display coordinate system by pressing the middle mouse button over a position in the survey area display and keeping it pressed pop up window will display the coordinates Z IST VISTA Survey Area Definition ess Tool User Manual for VISTA Page 29 of 64 Ji 5 4 Changing plot display parameters The Aspect ratio of the plot displayed can be toggled between fixed or variable according to Window aspect by Ticking Unticking the Fixed Aspect Ratio menu item under the Options Menu 3 2 2 A Right Mouse click anywhere in the survey area plot display window except in a selected light blue tile and the following popup menu will appear Zoom In Zoom Out Reset Zoom FKS 12000 FK4 B1950 Galactic Ecliptic SLOAN Cartesian Plot North Polar Plot South Polar Plot
12. defined can be saved as an xml file for future reference or for later re import by selecting Save As on the File menu and choosing a location and file name ending xml The saved XML file without any tiles pawprints can used as a log of what Survey was defined and can be reimported into SADT for further work 8 6 3 1 VISTA Survey Area Definition Tool User Manual for VISTA my VIS MAN QMU 0001 0003 ail Visible amp Ee Astronomy ae rn Xml files are in plain text with extension vm and have a file structure is as governed by the schema in the Appendix at Section 8 6 5 9 Reading Survey Areas without Tiles Pawprints xml files containing exported Survey Areas as described in 5 8 may be reimported into SADT by selecting Open on the File menu and selecting the directory and xml file name must end xml required This will overwrite any existing Survey Area definition in the GUI and then behave as though the area had been entered via the GUI All the SADT facilities to display and inspect survey areas make tiles and create and output guide aO stars are all available to the imported Survey Areas Survey Areas generated by hand can be imported as long as they conform to the xml schema standard in 8 6 2 6 Tiles Pawprints Create Show Refine amp Save Given the user has already set all the parameters required SADT will create the Tiles and their component pawprints and if enabled find all the guide stars GS
13. in cases where an area is defined to include an integer number of tiles in both directions For a given RA Longitude range the number of degrees on the sky will vary with Dec Latitude and this makes use of this mode less intuitive than the geodetic rectangle mode and it is not recommended at very high gt 60 Dec Latitude VISTA Survey Area Definition Tool User Manual for VISTA a Keeping each tile aligned to its Dec produces awkward effects a high Dec as explained in 1 6 4 a VIS MAN QMU 0001 0003 i ail 1 6 4 Choosing between the 3 input systems especially at Dec Lat above 60 Because using coordinate ranges 1 6 3 inevitably produces different shaped areas at different declinations latitudes and because SADT aligns the bottoms of coordinate range tiles along lines of constant Dec Latitude or at an angle relative to Dec Latitude there will inevitably be significant problems in automatically covering areas completely when the areas have been defined as coordinate ranges especially at high Dec Latitude Therefore in general it is recommended that geodetic rectangles 1 6 1 be used as the most reliable way to cover sky fully and efficiently For example to tile the whole Southern hemisphere requires 13 029 tiles in Geodetic rectangle mode and 13 235 tiles in Coordinate Range mode which actually fails to cover the S pole region completely It is recommended that geodetic rectangles should be used in prefer
14. is no Random paf file but is generated with a given user defined amplitude when the OBs are created 8 3 2 Single Single Jitter pattern is not an actual pattern there is no Single paf file but rather an indication that no jitter pattern should be executed 8 3 3 Jitter2d SEQ JITTER NAME 2 position pattern diagonal left to right down SEQ JITTER OFFSETX 10 0 10 0 SEQ JITTER OFFSETY 10 0 10 0 Jitter2d VISTA Survey Area Definition Tool User Manual for VISTA ay VIS MAN QMU 0001 0003 Visible amp Ee Astronomy BEER 8 3 4 Jitter2u SEQ JITTER NAME 2 position pattern diagonal left to right up SEQ JITTER OFFSETX 10 0 10 0 SEQ JITTER OFFSETY 10 0 10 0 Jitter2u 8 3 5 Jitter3d SEQ JITTER NAME 3 position pattern diagonal left to right down SEQ JITTER OFFSETX 0 0 10 0 10 0 SEQ JITTER OFFSETY 0 0 10 0 10 0 Jitter2d VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA Page 55 of 64 i 8 3 6 Jitter3u SEQ JITTER NAME 3 position pattern diagonal left to right up SEQ JITTER OFFSETX 0 0 10 0 10 0 SEQ JITTER OFFSETY 0 0 10 0 10 0 12 Jitter3u 8 3 7 Jitter4u SEQ JITTER NAME 4 position pattern U shape rotated 30deg cew SEQ JITTER OFFSETX 3 66 13 66 3 66 13 66 SEQ JITTER OFFSETY 13 66 3 66 13 66 3 66 Jitter4u VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA Page 56 of 64 BEE
15. the Y direction of the tile to at least 2 camera pixels 1 4 Definitions To use SADT effectively and understand how SADT works it is necessary to appreciate the following definitions as used in SADT e Survey A survey corresponds to the total area of sky that needs to be observed A survey may consist of a number of non contiguous survey areas which may be of various different types and defined in various different coordinate systems SADT is not concerned about what observations are carried out at each position in a survey except SADT must be given the Tile pattern 8 2 to be used to determine the order in which the pawprints will be observed and the maximum jitter amplitude used 3 2 6 3 to ensure the GS and AOS stars stay on the CCDs during jitter moves Definition of what observation is carried out at each position is handled by P2PP VISTA Survey Area Definition Tool User Manual for VISTA my VIS MAN QMU 0001 0003 ail Bee e Survey Area Each survey area is a contiguous area of sky A survey consists of one or more sets of survey areas which may be non contiguous In general each will consist of multiple VISTA tiles e Tile A tile is a filled and fully sampled area of sky formed by combining multiple pawprints Because of the detector spacing the minimum number of pointed observations with fixed offsets required for reasonably uniform coverage is 6 which exposes each piece of sky away from the edges of the
16. the VISTA IR Camera VIRCAM Instrument Package IP which SADT must read Note the path to the directory containinp p2pp on you local system e g on the manual writers Mac with an old version of P2PP containing an old version 1 25 of the IP it is Applications p2pp_v3 3 1beta5 eso instruments VIRCAM 1 25 2 2 2 Download SADT Go to www vista ac uk observing sadt where the latest version of SADT will be available as sadtfilename tgz where sadtfilename tgz represents the actual name of the file 2 2 3 Linux Unix instalaltion Download sadtfilename tgz into a directory and cd into the directory and type gunzip sadtfilename tgz a tar file will then appear tar xf the tar file and a directory called sadtdirectory appears where sadtdirectory represents the actual name of the directory which should contain at the first level a bin lib cfg and tsf 2 2 4 MS Windows instalaltion Download sadtfilename tgz into a directory SADT understands MS Windows file names containing blanks so you can install under My Documents Double click on sadtfilename tgz and unpack the directory structure called sadtdirectory where sadtdirectory represents the actual name of the directory which should contain at the first level a bin lib cfg and tsf VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA Page 15 of 64 Ji 2 2 5 MAC OS X Installation Download the sadtfilename tgz and unpack it 2 2 6 Configure loc
17. the number of pawprints in the tile and xx is a mnemonic for the tile pattern defines a tile pattern for the VISTA Camera and these are used by observation templates to sequence the telescope offsets The tile patterns define absolute offsets from a reference position in units of detector size The user must choose which one is to be used from the drop down Tile Patterns menu For example e For standard Npaw 6 pawprint tiles Tile6n Tile6s Tile6ss Tile6u Tile6z and Tile6zz define the same pattern of 6 pawprints observed in different orders as suggested by the mnemonic suffix letters Section 8 2 1 e For Npaw 3 pawprint tiles Tile3nx and Tile3px define the same pattern of 3 pawprints covering half a tile only observed in different orders in the X direction as suggested by the mnemonic suffix letters Section 8 2 2 e For single Npaw 1 pawprints Section 8 2 3 Tilel 00 contains only I null offset 0 0 and so the order is not relevant Tilel 00 is equivalent to the Single tile pattern available in P2PP but SADT itself does not recognise single When using SADT for defining Single pawprints use Tile pattern Tilel 00 and use the same pattern in P2PP The patterns defined in the IP are now described in more detail 8 2 1 Npaw 6 patterns The pattern names n u Z s ZZ or ss are meant as a mnemonic for the user to visualize the pawprint order To explain this notation consider labelling the six pawprint positions need
18. 1 475 degrees 88 5 arcmin at VISTA s nominal pixel size Combining the 2 X and 3 Y offsets an area of 7 65 5 275 X Y 40 354 detector areas is contiguously and almost uniformly covered by a minimum of 2 pixels as shown in light green in Figure 8 2 which shows the resulting exposure map assuming no jitters corresponding to 1 475 1 017 1 501 deg sky at VISTA s mean pixel size Figure 8 2 Exposure map for Tile6 tiles Exposure Colour key Light green 2x Dark green 1x Magenta 3x Red 4x Yellow 6x The dark green areas at top Y and bottom Y of Figure 8 2 are each 0 135 sq deg 1 475x0 092 and can be overlapped by corresponding areas from adjacent tiles for many surveys Assigning only one of the two 0 092 deg overlap top amp bottom to each of the two tiles involved in an overlap the result is that each tile when part of a filled larger area covers 1 475 1 017 0 092 1 636 deg at least twice VISTA Survey Area Definition Tool User Manual for VISTA my VIS MAN QMU 0001 0003 ail Visible amp Ee Astronomy ae rn Table 8 1 summarises the various dimensions in units of a VISTA detector and in degrees using VISTA s mean pixel scale e a simple uniform effective pixel scale although the real pixel scale is not uniform across the field A Y Area A Y Area Adopted mean pixel size 0 339 arcsec true size varies over Focal Plane det det det deg deg deg Step size 0 950 0 475 0
19. 1832 0 0916 Single Detector l l l 0 1929 0 1929 0 0372 Ouer oundary Ob Uk dass Sel 1990110173 4 3145 Pawprint Diagonal of 1 unfilled Pawprint 8 5273 1 6445 6 pawprint Tile Outer dimensions Sg engl Weg Deeg ae 7 650 6 225 1 4753 1 2005 1 7711 6 pawprint Tile size covered twice 7 650 5 275 40 354 1 4753 1 0173 1 5009 6 pawprint Tile top amp bottom Y 7650 0 475 3 634 1 4753 0 0916 0 1351 strips covered once 6 pawprint Tile covered twice if one of the two 0 475 Y overlaps iS 7650 5 759 43 988 1 4753 1 1089 1 6360 matched by a neighbour tile in large survey Table 8 1 Summary of dimensions unit of 2048 pixel side detector and degrees VISTA Survey Area Definition Tool User Manual for VISTA my VIS MAN QMU 0001 0003 ail Visible amp Ee Astronomy ae rn 8 2 Tile Patterns In principle the pawprints making a tile pattern can be executed in any order although in practise the available orders are restricted to minimise overhead during movements As an example the order illustrated in Figure 8 1 is known as Tile6n from the n shape of the line joining positions 123456Tile patterns are chosen from drop down menu The VIRCAM instrument package contains inter alia the default isf file and all the defined tile patterns VIRCAM TileNpayxx paf files Only tile patterns defined in the VIRCAM Instrument Package maintained by ESO s VISTA Instrument Scientist are executable Each TileNpawxx paf pattern where Npaw IS
20. 4 MANGUBOS SURVEY ID ennn E a R 23 35 MAIN GUI CHOICE TILE PATTERNS iiccsswsessectetutesaacsebuinilondiswadadntnsdnedadaanuuinicaduaedaausdetentadsdeelwanedsdetavinabenddeies 23 30 MAN GUI CHOICE CATALOGS ataie iore a E aa A E T E 24 A SURVEY AREAS TA E e Nu LE 24 A ADI SG TAR EE 24 E E 24 GE E E 24 215 Column E 25 EE GEER EN 25 AA Column2 RA Long RAL Lon ebe 29 4042 Column Dees liDELI Nav 26 4 143 Column4 Width Circle diameter RA2 Long 0 irronneen ennen ennon ea aAA RENERE NEERA ES EAEE ERAR RREN 26 4 1 4 4 Column 5 Height Dec2 Lat2 snonsooeseessessssssseeeesseessesssesssessssssssssssseseeseerssesseessressesssessssssseersseess 26 4 1 4 5 Column 6 Angle Survey Area relative to SKY rrrrrnrrnnvvnvrnnvvnvvvnvrnrensressrensnnsvnnsnnnsnnssnnsnnvensvnnssnssnnsnnssnnes 26 NEE PSN 26 TT NN 21 AL FN EE 2 Ao VERRE SURVEY EN 2 5 SURVEY AREAS VIEW UPDATE amp SAVE es 28 EE a et EEE ee E EE EE 28 AE EET EE RE EEE EN 28 5 3 COORDINATES AT MOUSE IN DISPLAY SYSTEM sesrernevnevnvnnvvnennevnennevnennvvnennuvnennuvnennuvnennuvnennuvnennuvnennunnennunneen 28 5 4 CHANGING PLOT DISPLAY PARAMETERS s ssssnsnseseseseesenessrsesesesensesesensrsrsererersesesessrsrsesenensesenessrsesesenenss 29 ET LNR 29 542 Display GEL ANE EEE ENE 30 NN PN 30 DF ESN 30 SEE SD GA SEE NE EE ee tT ENE ENN eee en amen Oe Or nT See mee er er eres 30 5 7 INTERPRETING SHAPES DISPLAY ED wsccasianinaasonasacssasaenspdacaassacinseisdnceian
21. 75 0 0 0 475 SEQ TILE OFFSETROT 0 0 0 0 00 Tile3nx Figure 8 9 Tile3nx 8 2 2 2 Tile3px SEQ TILE NAME 3 step px positive x pattern SEQ TILE OFFSETX 0 475 0 475 0 475 SEQ TILE OFFSETY 0 475 0 0 0 475 SEQ TILE OFFSETROT 0 0 0 0 00 Figure 8 10 Tile3px IST VISTA Survey Area Definition ir Gl Tool User Manual for VISTA Data Flow System 8 2 3 Npaw 1 patterns There is one n 1 pattern Tilel 00 which defines a single pawprint SEQ TILE NAME I pawprint pattern SEQ TILE OFFSETX 0 0 SEQ TILE OFFSETY 0 0 SEQ TILE OFFSETROT 0 0 VIS MAN QMU 0001 0003 11 September 2009 Tilel 00 is equivalent to the Single tile pattern available in P2PP but SADT itself does not recognise Single When using SADT for defining Single pawprints use Tile pattern Tilel 00 and use the same pattern in P2PP VISTA Survey Area Definition Tool User Manual for VISTA my VIS MAN QMU 0001 0003 ail Visible amp Ee Astronomy ae rn 8 3 Fixed Jitter Patterns The Jitter patterns available are define in a series of VIRCAM Jitter paf files in the Instrument Package These include the set of OFFSETX and OFFSETY values in arcsec which define each pattern During OB definition in P2PP the scale of jitter offsets in a pattern may be scaled by setting the multiplicative factor Jitter Scale Multiplier to a value other than 1 0 8 3 1 Random The Random Jitter pattern avialable in P2PP is not a fixed pattern there
22. E REE EN EN 44 ELT NNN 47 TNT 47 0 EG T RE ER EE EE EE re er Ree ee 48 E dee RE NE EE EN 48 KN VU 49 EG Dee EEE ER viaeeeen 49 NN TU 50 PL VE 50 vr NT E 51 gt RE Ek RENEE EE ERE EE a ee tt ee 51 B222 NN 51 Nr 52 dr FDITR PN erreen scent assesses cates auras eal nana essere eset ee EEEE 53 roe E EEN 53 EE 53 E Er EEN 53 JE E 54 VM 54 arrests ec acorn rs eet EEE EEE nasa einen eke 55 JER e E 55 EEE 00 EE 56 JE 0 EE EEE SKEE EE EEE NN EEE 56 NNN 57 JE DE 2 EE 57 JE SEE 2 EE 58 8 4 INSTRUMENT PACKAGE SETTINGS FOR SAIT 59 8 5 CONFIGURATION FILES amp XML SCHEMA o iscocacnsonssveenesensuvnrseeeadssedenanat vaaxeeesescassavnsiauacswusdevcbesbsasnaniveneesees 60 EEE 217 EEN 60 Eeer eebe 60 NNN 60 LNR 61 SOT TV 61 GN 61 0 STENEN SADT Gasa 61 8 6 3 1 Example Survey Areas not Tiles yet ecciccccccccsccssegsicscesaussearcnocesexeceacesongacionssdbessnwececestescesseseeseadedeenseaeeeiees 61 8 6 3 2 Example Survey Areas with tiles pawprints and Guide aO stars 62 KD me Pay E 63 Sood Example REIN EE 64 een Visible amp Infrared Survey Telescope for Astronomy Data Flow System I Introduction 1 1 Purpose VISTA Survey Area Definition Tool User Manual for VISTA VIS MAN QMU 0001 0003 11 September 2009 This document is the User Manual for the Survey Area Definition Tool SADT for VISTA The SADT user manual for VST will be covered in a separate document The main functions of
23. O CCDs in arcsec which are read from the Instrument Package 8 4 the Maximum Jitter Amplitude values define the area over which guide stars will be sought This ensures the guide aO stars found will remain on the guide aO CCDs during the maximum jitter offsets If the value is set wrong there are two possible consequences 1 If Maximum Jitter Amplitude is set larger than necessary the area over which Guide aO stars will be sought will be smaller than necessary which could be a problem especially in regions of low star surface density 2 If Maximum Jitter Amplitude is set smaller than the actual maximum jitter amplitude used some guide aO stars may fall off their CCD during a jitter causing OB execution to take longer wasting time whilst the operator intervenes or possibly to fail VISTA Survey Area Definition Tool User Manual for VISTA a a VIS MAN QMU 0001 0003 i ail The Maximum Jitter Amplitudes set in SADT MUST not exceed those implicitly chosen by choice of Name of Jitter pattern and Jitter Scale Multiplier in the P2PP OBs that you will create Pattern arcsec shown in Section 0 Single 10 Nojitter S Jitter30r1 10 Jitter Scale Multiplier 30 point jitter generated with random number generator Random Use value set for amplitude of This is not a fixed pattern but generated the random jitter pattern with a given amplitude when the OBs are created Table 3 1 Maximum Jitter Amplitudes 3 2 6 4 Tile Orien
24. PrimitivePattern class survey vista VistaTileCenterIO replacing class survey util TileCenterIO class survey vista VistalO replacing class survey util SdtXML class survey vista VistaGuideSearch replacing class survey catalog DetectorSearch Using standard format Creating a plastic manager No local USNO catalog available Other catalog s will be used If a bug occurs at anytime go to this terminal Window then right click and select the Select All option to select all the text Copy and paste this into a simple text file to document the problem when you report it The window also displays progress information on tiling and finding guide aO stars GS AOS If you did not set INSTRUMENT PACKAGE PATH in sadt cfg to a valid location containing the VIRCAM IP see 2 2 6 you will see something like the window shown in Figure 2 1 Could not find VIRCAM Instrument Package files VIRCAM Instrument Package directory home user VIRCAM 120 vcotsf config is invalid A Please ensure you have an up to date version of the VIRCAM Instrument Package and that the location of Z its top level directory is correctly entered into the SADT s configuration file If you continue the program will use its own copy of the VIRCAM instrument files which are potentially out of date Abort and exit Figure 2 1 Window seen if Instrument Package not found in P2PP VISTA Survey Area Definition a VIS MAN QMU 0001 0003 Visible amp de Astr
25. RINT dec 020840 200 id 1 1 3 offangle 27 9127 offsetx 0 475 offsety 0 475 ra 185718 072 gt lt PAWPRINT gt lt PAWPRINT dec 02033 1 320 id 1 1 4 offangle 27 9173 offsetx 0 475 offsety 0 475 ra 185756 952 gt lt PAWPRINT gt lt PAWPRINT dec 020822 560 id 1 1 5 offangle 27 9189 offsetx 0 475 offsety 0 0 ra 185807 248 gt lt PAWPRINT gt lt PAWPRINT dec 021314 160 id 1 1 6 offangle 27 9205 offsetx 0 475 offsety 0 475 ra 185817 568 gt lt PAWPRINT gt lt TILE gt lt TILE dec 011302 640 id 2_1 offangle 27 9015 priority 0 ra 185545 072 gt lt TILE gt lt SURVEY_AREA gt lt SURVEY_AREA coordSys Ecliptic exclude false lat 19 5 long 288 0 number 2 posangle 0 0000 radius 1 47 type Circle gt lt SURVEY_AREA gt lt SURVEY AREA coordSys FK5 J2000 exclude false lat1 01 00 00 lat2 00 00 00 long1 19 03 00 long2 19 14 40 number 3 posangle 0 0000 type Coordinate Range gt lt SURVEY AREA gt lt SURVEY gt Done pr Within the lt Pawprint element the id is constructed as Tile ID PawprintNumber VISTA Survey Area Definition Py ai Kl Tool User Manual for VISTA Page 64 of 64 BEE 8 6 3 4 Example REFSTARS The REFSTARS element of the first pawprint of the first Tile from the same ouput file is shown below expanded fully lt REFSTARS gt lt CDATA PAF HDR START gt Start of PAF Header PAF TYPE paramfile
26. Tiles from covering some of it when they overlap into it from a non excluded area The actual behaviour depends on the setting of Include Overlap 3 2 5 The Excluded surveys areas are not removed from the GUI or memory If Exclude is unticked the area will be displayed and used again in subsequent SADT operations This saves typing the area in again later VISTA Survey Area Definition ST Tool User Manual for VISTA 4 1 4 7 Notes Whenever changes are made to the values in the text boxes defining the Survey Areas SADT assumes new areas are required and after asking you if you wish to do this will delete all the tiles and guide stars created 4 2 Example Figure 4 1 shows the survey definition box for three defined survey areas one of each type all in the FK5 system and with the Geodesic rectangle row selected Column headers will differ for other Type System combinations Survey Area Definition Tool VISTA File Options Help Survey ID Survey Areas Bd ach Lat WEI deg Height deg Angle deg System Exclude Geodesic Rectangie EE eA EE 1 TTI 0 19 5 0 Ecliptic be Coordinate Range 19 03 00 01 00 00 ef 00 00 00 OFKS J20 PE GE ee E Add Survey Area amp Delete Survey Area Tile Patterns VIRCAM Tile6n v Catalogs GSC 2 at ESO 2 View Update Start Resume 7 to Reset amp Plastic Figure 4 1 Example for a 3 area survey one of each Type and System with
27. Type of PAF PAF ID FiLg_6 5 1 1_1 1 20090911142035 Unique ID for PAF PAF NAME Fig_6 5 1 1_1 1 paf Name of PAF PAF DESC Telescope guide star candidates for Pawprint 1 Short description of PAF PAF CRTE NAME SADT v3 04 CVIRCAM 1 25 Name of creator PAF CRTE DAYTIM 2009 09 11 14 20 Civil Time for creation PAF LCHG NAME SADT v3 04 Name of person application changing PAF LCHG DAYTIM 2009 09 11 14 20 Timestamp of last change PAF CHCK NAME Name of application checking PAF HDR END gt End of PAF Header TPL FILE DIRNAME INS_ROOT INS_USER MISC VISTA OCS SADT CAT ID Gutde AO star candidate catalogue OCS SADT IP ID SADT v3 04 VIRCAM 1 25 Creator version TEL AG START T Start autoguiding TEL AG GUIDESTAR SETUPFILE Select guide stars from this setup file the default TEL AO START T Start active optics TEL AO AOSTARA SETUPFILE Select LOWFS_PY stars from this setup file Cthe default TEL AO AOSTARB SETUPFILE Select LOWFS NY stars from this setup file the default gt lt REFSTARS gt Here the unique ID is derived by adding the date and time to the Parameter file paf Name The name consists of SurveylD Fig 6 5 SurveyAreaNumber 1 TilelD 1 1 PawprintID
28. Vist Visible amp Infrared Survey Telescope for Astronomy Data Flow System Document Title Survey Area Definition Tool User Manual for VISTA Document Number VIS MAN QMU 00001 0003 Issue 2 0 Date 11 September 2009 Document Jim Emerson Signature Prepared By QMUL and Date Document Jim Emerson Signature Reviewed By VISTA PI and Date Document Jim Emerson Signature J j m Digitally signed by Jim Emerson DN cn Jim Emerson o Queen Mary University of London ou Astronmy Unit Released By VDFS Project Leader and Date Emersop Trives VISTA Survey Area Definition Tool User Manual for VISTA Data Flow System Vi E i A VIS MAN QMU 0001 0003 Change Record Manual Date SADT Section s Description of Change Change Request Issue version Affected Reference Remarks release date 0 2009 09 11 2009 07 07 A iie after testing at VISTA prior to ESO Science Verification VISTA Survey Area Definition Tool User Manual for VISTA a VIS MAN QMU 0001 0003 i ail Visible amp de Astronomy ea TABLE OF CONTENTS CHANGE EE 2 1 INTRODUCTION see 6 RON 6 UE SE E E KR Re 7 EAS OC AI TLAN LA E WE i NTN NN 8 ENN 9 ko VANNS een 10 1 6 1 Rectangular Geodetic areas via GUI in a choice of system 10 162 Circular areas via GUI in choice Of Systems cassis icasaiesaedndapsiaissexhextuntubinetbntsheaneesdcaesiteensbedeoassadexs la 1 6 35 Coordinate Range areas via GUI in a cho
29. ai Kl Tool User Manual for VISTA EG Section 6 6 explains a partial workaround if this is conflicts with the users needs 6 6 Saving Tiles as Individual Survey Areas Some users may want to save their Tile positions fixed within their Surveys areas so that the area is not retiled and the user s work adjusting it undone when SADT is next asked to Tile the survey e g to find GS AOS for such a complex set of tiles Use File Create survey areas from tiles in xml file 3 1 to select an already saved xml file containing the Survey Areas and Tiles that you wish to work on again in SADT You will be prompted for the name of an output xml file The resulting output file will define each individual Tile as its own Survey Area containing a single Geodetic Rectangle thereby protecting each Tile from being changed by SADT s Tiling algorithms For each survey area tileOverlapX and tileOverlapY will be set to zero but the original tile overlaps will remain preserved in the positions of the geodetic rectangle survey area tiles The width and height of the Geodetic rectangle made will depend on whether a Tilel Tile3 or Tile6 pattern is selected for that tile Approximate values as shown in Table 6 1 Width X deg Height Y deg Width X deg Height Y deg Tilel pawprint 1 292117 1 017301 1 292117 1 201 1 292117 1 017301 1 475 1 201 1 475 1 017301 Table 6 1 Width and Height of single geodetic rectangle tiles
30. and active Optics aO stars AOS needed for observing the pawprints for each tile 6 1 Finding Tiles Pawprints 6 1 1 Note The user should always carefully check the settings of all the configuration parameters before running any tiling 6 1 2 Start Resume Pressing Start Resume begins the process of filling the defined survey areas with tiles pawprints and if Find Guide AO stars option on the Options menu 3 2 1 1s on it starts finding guide aO stars It is recommended that Guide aO allocation be kept turned off until you are ready to find guide aO stars If guide aO star selection was selected this may take some time depending on the location of the catalogue chosen SADT has mainly been tested at VISTA using GSC 2 at ESO especially if your network is congested Start Resume should also resume this process where it left off after an interruption using Stop Users are advised to be careful in this mode as there have been reports that some material may sometimes be lost during a Start Stop Resume sequence Check that tiles or guide aO stars have not gone missing around the sky position you pressed Stop at VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA Page 33 of 64 gd When the process is finished an summary information window like that in Figure 6 1 will appear Finished Number of tiles in the survey areas s 11 Number of pawprints in the survey areas s 66 Number of times backtrack
31. and deselecting tiles Tiles are can be selected and deselected with the mouse in various ways similar to a file manager program on a computer e Select Tile s o Left Click into a tile o Drag mouse along tiles o Drag mouse along a closed path to select all tiles inside the path If closed loops of tiles are selected then all the tiles inside the loop will be selected as well o To add to an already existing selection press the Control button and keep it pressed while selecting new tiles equiv on Mac OS X TBD Selected tiles appear in the colour cyan light blue e Deselect Tiles o To deselect all tiles left click outside the survey area o To deselect a single tile press the Control key and click on the tile Equivalent key on Mac OS X is TBD VISTA Survey Area Definition Tool User Manual for VISTA a 6 3 2 Tile operations on selected deselected tiles a VIS MAN QMU 0001 0003 i ail Visible amp de Astronomy Selected tiles can be deleted restored with or without a priority or have an internal 4 step priority set in the integer range 0 3 with each priority associated with a different colour O red default 1 purple 2 light blue 3 dark blue e Delete Selected Tile s Exclusion of Survey Areas was covered in 4 1 4 6 Right click on the selected tile s gives the Delete Tile option Selecting it removes the tile leaving only the location of the centre of each pawprint This 1s achieved through se
32. ation of IP for SADT Once SADT has been installed use a plain text editor to open sadt cfg in sadtdirectory cfg vista and set the location of the VIRCAM IP on the machine you are using to e g for the example location in 2 2 1 INSTRUMENT PACKAGE PATH Applications p2pp_v3 3 1beta5 eso instruments VIRCAM 1 25 and save the modified file Note it is very important to do this to ensure use of the same versions of the IP 1 25 in this example in both SADT and P2PP If not differences in the two IPs used could result in OBs that will fail to execute correctly For trial SADT runs whose output will not be used to produce executable VISTA OBs locally defined tile patterns in sadtdirectory tsf vista vcotsf config can be used These are set to be the same as those in the instrument package at time of the SADT release so that users without P2PP installed can still carry out explorarory test work 2 3 Run 2 3 1 Unix Linux To run type sadtdirectory bin sadt 2 3 2 MS Windows To run Start gt Run and browse to e g My Computer gt C gt gt MyName gt sadtdirectory gt bin gt sadt bat so the box reads C MyName sadtdirectory bin sadt bat and click OK or navigate to e g C Name sadtdirectory bin sadt bat and double click on sadt bat 2 3 33 MacOS X To run click sadtdirectory bin sadt You can also navigate to sadtdirectory bin and make an alias of sadt Move this to a convenient place say D
33. cal coordinate system as in b with a red dot marking the centre The dark blue grid generally represents RA Dec The yellow angle shows the position angle when looking out from the inside of the fixed system VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG The algorithm used to construct the tile pattern starts from the lower right hand SW corner of the area to be filled and then fills in from right to left goes to the next row up fills it from right to left and continues this until the whole area is filled N B In general this means that the area produced will look different e not be just reflected about the equator if one flips the sign of the declination latitude the area is centred on The exception is in cases where an area is defined to include an integer number of tiles in both directions It is recommended that geodetic rectangles should be used in preference to coordinate ranges or circles at high Dec Latitude above 60 deg This should ensure the most complete and efficient coverage especially at very high Dec Lat above 60 where the coordinate range method s need to follow Dec Latitude lines can produce poor coverage as the modulus of Dec Lat gets closer to 90 1 6 2 Circular areas via GUI in a choice of systems In Circular mode the central position and radius of the areas are defined in the chosen coordinate system 1 6 3 Coordinate Range areas via GUI in a choi
34. canton snseasdunnsdanardedaorinanevedsseacsausdssdnanwens 31 5 8 SAVING SURVEY AREAS WITHOUT ITULESBAWPRINTS 31 5 9 READING SURVEY AREAS WITHOUT IILESBAWPRINTS 32 6 TILES PAWPRINTS CREATE SHOW REFINE amp SAVE eoeeosesevnsvvvnsvvvnsvvnnsvvnnsvvnnsvvnnsvvnnsvvnnsnnnnseesee 32 6 1 FINDING TILES PAN NN 32 EE REE EEE EE 32 C SS EE 32 EE JERNET EEE ea 34 EE EE 35 GE EEE 550 EEE REE EEE EE E 35 old GONNA eee 35 6 1 7 Inspecting catalogue entries on guide aO detector footprint dieplou 37 MN OVN 37 6 3 OPERATIONS ON INDIVIDUAL OR GROUPS OF TILES enesvnvnnvnnennennvnnennvnnennvnnennennennennennennennennennennennennennennenn 37 6 31 NNN eee r re 37 6 3 2 Tile operations on selected deselected les 38 6 4 SAVING TILES PAWPRINTS WITHOUT GS AOS STARS 39 6 5 WHAT HAPPENS WHEN SADT READS IN AN XML FILE eronvnnrnernnnnnrnnnnnrnnnnnvnnnnnvnnnnnvnnnnnsnnnnnsnnnnnsvnnnnsvennnenne 39 66 SAVING TILES AS INDIVIDUAL SURVEY AREAS cssssacessdscessenqaswutantdancoadesabnraandeausbenanbavacatnedouadeslvaanatwasncnseanes 40 Gy SAVING SURVEYS FOR USE WITH Eege 40 6 8 READING SURVEYS READY FOR P2PP 00 0 ec ce cece ceceecceccccceccecceccsccscceccncceccecceccnccscesceeccscescesceesesceesencescancees 41 T TILES PAW PRINTS PLOTTING IN ADA DIN wisccceccsarecesvscinnsisociestecisiscactsansteceusaaentnes cataaucusstponseesssanseess 41 VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG PNI NNN 44 8 1 EH Ce E KL EE
35. ce of systems In Coordinate Range mode the upper and lower bounds of the areas are defined in the chosen coordinate system The angle relative to the coordinate system is fixed at 0 deg as any other value would be inconsistent with the coordinate range given Figure 1 4 a shows a green coordinate range painted on a spherical coordinate system with a red dot marking the centre Figure 1 4 c shows a green coordinate range defined m a different rotated spherical coordinate system painted on the different light blue rotated spherical coordinate system with a red dot marking the centre The dark blue grid represents RA Dec The yellow angle shows the position angle from the RA Dec frame to the new frame and is used internally in SADT The tiling algorithm used constructs the tile pattern starting from the lower right SW corner of the area to be filled e when defined in RA Dec system the lowest RA and lowest Dec In that example RA Dec system the equivalence in other systems included rotated ones is obvious it then fills the first row from right to left increasing RA at constant Dec and then fills in the next row up higher Dec left to right and continues this until the area is filled Always starting from the SW corner means that in general the area produced will look different and not be just reflected about the equator if one flips the sign of the declination latitude the area is centred on The exception is
36. deleted tiles remain plotted so they can be found and undeleted if required 6 4 Saving Tiles Pawprints without GS AOS stars The survey defined can be saved as an xm file for future reference or for later re import by selecting Save As on the File menu and choosing a location and file name ending xml The saved XML file with tiles pawprints can used as a log of what Survey was defined and can be reimported into SADT for further work The saved file will not include any deleted tiles or excluded Survey Areas 8 6 3 2 6 5 What happens when SADT reads in an xml file It is important to appreciate that SADT as designed works at the Survey Area level In particular if Start Resume is pressed SADT will operate on the Survey Areas defined computing new Tiles Pawprints etc and ignoring any Pawprints guide aO stars it may already have So when Start Resume is pressed after a previously saved xml file has been read back in any changes made to the Tiles that SADT originally generated will be lost As soon as Start Resume is pressed SADT starts to generate a new set of Tiles Pawprints overwriting in Memory those that were produced before For example a user who kept the same survey area but generated a complex geometry with many deleted Tiles or by editing the xml file would find that SADT would recompute all the tile positions based on the Survey area and the users carefully made changes would be undone VISTA Survey Area Definition e
37. desic Rectangle opposite sides have an equal number of degrees on the sky at any Declination Latitude Given that the VISTA field of view is itself rectangular on the sky neglecting barrel distortion this is the most natural and efficient way to cover the sky N B a rectangle on the sky tangent plane projects to a pincushion on the focal plane In Geodetic Rectangle mode a survey area centre position is defined in the chosen coordinate system and the number of degrees extent in two orthogonal directions are given together with an angle relative to the coordinate system used i IST VISTA Survey Area Definition Tool User Manual for VISTA A ke ge L de vr NM Ai I Fa p ESR FS c EN Figure 1 4 Areas defined by Geodetic tiles b amp d and Coordinate Ranges a amp c and showing rotation angle The darker blue lines represent a fixed coordinate system e g RA Longitude Dec Latitude in all four diagrams The lighter blue lines in c amp d represent the rotated coordinate system in which the survey area was defined Figure 1 4 b shows a green geodetic rectangle with position angle zero projected on a fixed spherical coordinate system dark and light blue grid with a red dot marking the centre Figure 1 4 d shows a green geodetic rectangle defined in a different rotated light blue spherical coordinate system and projected on the fixed spheri
38. e amp de Astronomy ee Te 2 Configure 3 2 1 Find Guide aO Stars On Off If this option is switched off SADT s algorithm creates tiles pawprints without any guide aO stars This is useful of you want to see roughly how a survey area is filled with tiles without having to wait the sometimes long time it takes to download guide aO stars for all tiles from an online catalogue To toggle this Tick Untick Find Guide AO stars option on the Options menu 3 2 2 Fixed Aspect Ratio On Off The Aspect ratio of the displayed plots can be toggled between fixed or variable according to Window aspect To toggle this Tick Untick Fixed Aspect Ratio option on the Options menu 3 2 3 Draw Pawprints On Off If this option is selected then the shape of all science detectors component pawprints of each tile is drawn on the survey area display If this option is not selected a dot marks the central position of each pawprint in a tile If the survey area is large then these detectors become very small and it might be clearer if they were not drawn To toggle this Tick Untick the Find Guide AO stars option on the Options menu 3 2 4 Draw Aux Detectors On Off When Draw Pawprints is set On setting Draw Aux Detectors On will display the positions of the 2 Autoguider AG and 2 aO Low Order Wavefront Sensor LOWFS CCDs CCD AG PY is shown in black In conjunction with Figure 1 3 this is allows determination of the directions of the X and Y
39. e SADT The guide aO CCDs have I band filters so guide aO stars should ideally chosen by their magnitude in I band Not all of the catalogues accessible via skycat cfg are suitable as guide aO star catalogues e g IRAS NED ABELL 2MASS One should select a suitable catalogue for the guide aO stars The current recommended catalogue is GSC2 at ESO This list of catalogues available was based on the entries of serv type catalog contained in the standard skycat cfg in Dec 2003 In principle SADT can also read other catalogues that can be read by tools such as GAIA and JSkyCat Adding a new catalogue can be done as follows e Create copy edit a skycat cfg file such as this distribution s e Put all the catalogues you want to use into the skycat cfg file e Edit the entry jsky catalog skycat config cfg skycat cfg in the sadt cfg file of this SADT distribution so that the value of jsky catalog skycat config IS the path of the skycat cfg you want to use e GAIA SkyCat JSky catalogues can be online as well as in a local file conforming with the GAIA http star www dur ac uk pdraper gaia gaia html SkyCat http archive eso org cms tools documentation skycat JSky http archive eso org cms tools documentation jsky catalogue conventions N B The use of local GAIA SkyCat JSky catalogues has not been tested VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG 8 6 xml Files 8 6 1 Viewing xml files
40. e range of catalogues avialable in SADT offers the possibility to find guide aO stars using 2MASS Abell IRAS NED QSO ZCAT do not do so VISTA commissioning work has been done using GSC 2 at ESO which is believed to be the most appropriate catalogue for finding VISTA guide aO stars 4 Survey Areas Creating 4 1 Add Survey Area To define the survey areas press the Add Survey Area button 4 1 1 Tooltips Many input widgets of the SADT buttons tabs etc have tooltips that are displayed when the user hovers with the mouse over them 4 1 2 Column 1 Type Select the Type of Survey Area required by single left clicking on one of the entries in the Type column and using the drop down menu to select Type from V Coordinate Range Circle Geodesic Rectangle These 3 types were described in 1 6 Il Geodesic Rectangle 1 6 1 The default height and width correspond to the area covered at least once in a single Tile6 tile see Table 6 1 and Table 8 1 2 Circle 1 6 2 3 Coordinate Range 1 6 3 Z IST VISTA Survey Area Definition ess Tool User Manual for VISTA EG Note in particular the pros and cons of each type as explained in 1 6 4 Geodetic rectangles are recommended The descriptions in the column headers running rightwards from Type change according to the Type in the row selected for that Type 4 1 3 Column 7 Coordinate System Select a Coordinate System for your input by single left clicking on the column valu
41. e remote catalogue and can be hours for large numbers of tiles After hitting the Stop button it is possible to save intermediate results to the file in the same way as for non interrupted results 5 8 A file with suffix xm1 should be used This file can later be opened again using the File gt Open menu The generation of pawprints can then be resumed where it had stopped before N B Be careful in this mode as there have been reports that some material may sometimes be lost during a Start Stop Resume sequence Check that tiles or guide aO stars have not gone missing around the sky position at which you pressed Stop VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG 6 1 4 Reset Resets the plots and deletes any tiles etc made Does not affect the surveys defined in the GUI just the display The user is asked to confirm he does want the plotted tiles deleted from the plot N B It is sometimes necessary to use Reset before finding of GS AOS will work e g if they have just been toggled on 6 1 5 Display The survey areas as defined in the survey areas text box are displayed in light green as described in Section 5 SADT s algorithm tries to retrieve suitable guide aO stars tile by tile pawprint by pawprint starting at the bottom left SW corner of each survey area AS soon as a guide aO star has been found for a pawprint the pawprint is displayed as pink dot This pawprint is provisio
42. e under System and using the drop down menu to select System from V FKS 2000 FK4 B1950 Galactic SLOAN Ecliptic 1 FK5 J2000 default requires input in RA and Dec 2 FK4 B1950 requires input in RA and Dec 3 Galactic requires input of Galactic Longitude and Latitude 4 SLOAN requires input of Longitude and Latitude N B SLOAN mode is not supported for VISTA and has not been tested and may not work 5 Ecliptic requires input of Ecliptic Longitude and Latitude The descriptions in the column headers running rightwards from Type change according to the System in the row selected for that Type 4 1 4 Other fields Double left click on the other relevant cells without drop down menus in turn to highlight them for entering a value The value input is only saved when the cell is closed Press carriage return to close the cell or single click elsewhere to achieve the same effect The fields available depend on the Type amp System selected for each Survey Area row and are described here by column Tooltips are displayed when moving the mouse over the Survey Area table header 4 1 4 1 Column 2 RA Long RAI Lonl Depending on survey area Type amp coordinate System RA RAI use HH MM SS SS or HH MM S SS Long Lonl use Decimal degrees not decimal hours VISTA Survey Area Definition Tool User Manual for VISTA a 4 1 4 2 Column 3 Dec Lat Decl Latl Depending on survey area Type amp coordinate System D
43. eady finished a VIS MAN QMU 0001 0003 i ail Visible amp de Astronomy 6 1 7 Inspecting catalogue entries on guide aO detector footprint display Catalogue entries can be selected in the guide aO detector footprint display if you are quick enough Click in the centre of any on the circles representing the catalogue entries being careful to be very close to the middle of the circle with the mouse The catalogue ID and the RA DEC are then displayed as the frame title of the display window 6 2 Missing guide aO stars As already explained see Backtrack Step 3 2 6 5 if SADT cannot find suitable guide AO stars for pawprints at the tile positions it generated it will attempt to move the tile centre by the amount specified in BackTrack Step until it does without leaving any gaps in the survey N B This will modify the tile centres and these modifications may depend on the guide aO star catalogue used This behaviour can be stopped by setting BackTrack Step 0 but then some pawprints may not find any guide aO stars and the OBs will stall 6 3 Operations on individual or groups of Tiles The user may select assign individual tiles or groups of tiles and delete them Changes may be undone The user can set an internal priority of 0 4 which can be used to label tiles by colour however currently such priorities will have no affect on the priority of executions of the OBs created as the priorities are not used by P2PP 6 3 1 Selecting
44. ec Dec 1 use DD MM SS SS or DD MM SS SS Lat Lat I use Decimal degrees pan VIS MAN QMU 0001 0003 i ail Visible amp de Astronomy 4 1 4 3 Column 4 Width Circle diameter RA2 Long2 Depending on survey area Type amp coordinate System Width Diameter Long2 use decimal degrees not decimal hours RA2 use HH MM SS SS or HH MM SS SS 4 1 4 4 Column 5 Height Dec2 Lat2 Depending on survey area Type amp coordinate System Height and Lat2 use decimal degrees Dec2 use DD MM SS SS or DD MM SS SS 4 1 45 Column 6 Angle Survey Area relative to Sky The position angle degrees on the sky between North in the selected coordinate system and the Height axis of the survey area Angle is measured increasing Eastward from North on the sky SADT applies the Angle and Tile orientation to derive the offangle in the output XML file that must be sent to the Telescope Control System TCS in an OB Note that offangle correctly obeys the ESO TCS convention and is not a conventional net astronomical position angle 4 1 4 6 Column 8 Exclude Ticking the Exclude on survey areas excludes those areas from being further processed in SADT 5 5 In SADT s plots the excluded Survey Areas are shown outlined in red with no infill Exclude can also be used to define a sub Survey Area to be excluded from within the bounds of a larger Survey Area Excluding a survey area does not necessarily stop
45. ence to coordinate ranges or circles at Dec Lat above 60 This should ensure the most complete and efficient coverage especially at Dec Lat above 60 where the coordinate range method s need to follow Dec Lat lines can produce poor coverage as Dec Lat gets closer to 90 In any case it is strongly recommended to do a visual check that the tiling algorithm has succeeded in producing adequate coverage of the areas intended before saving the output xml file 1 6 5 Surveys input as an xml file SADT can also read in xml files describing surveys In general these files will have been previously written by SADT The skilled and very careful user can create his own xml files to input complex surveys These are described in the following sections and in 8 6 2 Installation and Start up 2 1 Requirements SADT is a java application that is required to run under Scientific Linux running java 1 4 or higher This can be downloaded at java sun com j2se As a java application it should also run under Unix Mac OS X or MS Windows OSs running java 1 4 or higher but is no support is guaranteed on other systems Given that running P2PP requires java 1 5 it is suggested that SADT is also run under java 1 5 The script files which run the SADT need to be able to run Java therefore it is advised that your PATH environment variable should include the directory path to the Java executable 2 1 1 Memory SADT keeps all the informa
46. era pixels 0 95 detector widths v awprint 3 0 475 detector widths H int 2 D Kei 3 e 4 wm EN BEER SEE HUNN Dn 220E HETE E Pawprint 6 a b c Figure 8 1 Tile6 o Six overlapping pawprints in order o make up one contiguous tile d D I gt As shown in Figure 8 1 these six pawprints whose order is set by the Tile pattern file used 8 2 consist of a Three positions offset in Y by 0 475 of a detector in Y In Y this covers two outer strips of 0 475 detector once two strips within these of 0 475 detector twice nine strips of 0 425 detector twice and 10 strips of 0 05 detector 3 times The resulting 4 strips in X each cover a twice covered contiguous area in X Y of 1 5 275 detector each corresponding to 0 193 1 017 degree 11 57 61 04 arcmin at VISTA s mean pixel size of 0 339 arcsec The once covered strips correspond to 0 193 0 092 degree 11 57 5 5 arcmin or 694 330 arcsec at VISTA s mean pixel size VISTA Survey Area Definition S Tool User Manual for VISTA ae rn b Two positions offset in X by 0 95 of a detector in X In X this covers two outer strips of 0 95 detector once six strips within these of 0 90 detector once and seven strips of 0 05 detector twice This corresponds to at least single coverage in the X direction over 7 65 detector widths with double coverage in the 0 05 deg strips This corresponds to
47. ered then Survey ID defaults to survey or whatever may have been set as the default in the sadt cfg configuration file 3 5 Main GUI Choice Tile patterns The pattern of pawprints that will be used to make a Tile must be selected from the Tile Patterns drop down menu in the lower left of the main GUI screen The Tile patterns are shown in Section 8 2 Note that SADT does not recognise the Single Tile pattern available in P2PP this means take a single pawprint The Tilel 00 pattern available in SADT and P2PP is entirely equivalent to Single When SADT is being used single pawprints can only be defined using the Tilel 00 pattern VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG The Tile pattern used in SADT must be the same one that the user will use in the corresponding OBs in P2PP Otherwise the guide aO stars will not be associated with the right pawprints and so the GS and AOS stars will not appear on the CCDs at the telescope leading to failed execution of the OBs 3 6 Main GUI Choice Catalogs The catalogue choice box is underneath the survey areas text box guide aO star The catalogues are discussed in the Appendix about skycat cfg in Section 8 5 3 where it is explained how further catalogues can be added Note that the AG LOWES guid aO CCDs are filtered for I band 0 60 0 87 micron and so use of catalogues that do not provide equivalent magnitudes should be avoided For example although th
48. esktop and run by clicking on the alias to sadt N B sadt cannot be put on the application launching toolbar as it is a java file not an app file 2 4 Start up Windows When the SADT starts up the first window which opens is an information log window which just after start up contains VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG for WinXP something like path sadtdirectory bin gt echo off path sadtdirectory bin gt java classpath lib sdt jar lib vecmath jar lib jsky jar lib log4j jar lib diva jar lib util jar lib fits jar lib image jar lib el jar lib jfreechart jar cfe vista survey app SurveyDefinitionTool Plugins loaded class survey vista VistaTiles replacing class survey area PrimitivePattern class survey vista VistaSurveyAreaDisplay replacing class survey area SurveyAreaDisplay class survey vista VistaGuideSearch replacing class survey catalog DetectorSearch class survey vista VistaTileCenterIO replacing class survey util TileCenterIO class survey vista VistalO replacing class survey util SdtXML Using standard format Creating a plastic manager No local USNO catalogue available Other catalogue s will be used for Mac OS X in Terminal java 80x24 something like Plugins loaded class survey vista VistaSurveyAreaDisplay replacing class survey area SurveyAreaDisplay class survey vista VistaTiles replacing class survey area
49. file 4 Saves the resulting N OBs each with their n associated paf files One SADT file will have spawned N OBs and N n associated paf files a VIS MAN QMU 0001 0003 i ail Thus the combination of SADT and P2PP enables the astronomer to make OBs for a survey in an efficient manner Other ESO tools based on scheduling containers allow for time and priority linkages between OBs In due course the OB may be scheduled for execution Then the Broker for OBs BOB interprets the OB and passes the necessary files to the VISTA IR Camera VIRCAM for execution Caution If either of X coord of pointing or Y coord of pointing set to non zero values in OBs in P2PP SADT Guide AO stars will NOT work as SADT does not take any account of such offsets 6 8 Reading Surveys ready for P2PP xml files containing exported Survey Areas with Tiles amp Pawprints amp even GS AOS stars may be reimported into SADT by selecting Open on the File menu and selecting the directory and xml file name must end xml required This will overwrite any existing Survey Area definition in the GUI and then behave as though the area had been entered via the GUI All SADT s facilities to display inspect survey areas make tiles delete tiles and create and output guide aO stars etc etc are all available to the imported Survey Areas 7 Tiles Pawprints Plotting in Aladin Aladin http aladin u strasbg fr 1s an interactive software sky atlas allowing the u
50. he pawprints are sent over and you should see their centres in Aladin If other PLASTIC managers are running in addition to Aladin the tiles can be exported to these by choosing between Aladin and the other tools using the selection button at the upper middle right of the GUI in Figure 7 1 Aladin should display the pawprint centres as rhombs as in Figure 7 2 Aladin v5 0 D Da ar kW Location PLASTIC 9 15 9 09 9 03 Nic Ie g 3 00 00 Ke 009 S KR ilter 00 PP gt o KA gt gt x lt A 5 T 02 00 sl La i oa A PLASTIC e Iss m Zoom 2x sd ZS tt TO 03 00 del 6 5 x 4 6B 4 wy N ar e TINN TTT f gt WI gt KW k G 33 d multiview match Search Osel 66src 10Mb Ei Figure 7 2 Pawprint centres in Figure 6 2 plotted in Aladin using the Plastic button ll VISTA Survey Area Definition Tool User Manual for VISTA If you want to see the outlines of the pawprints rather than just their centres you have to Right Mouse click over the PLASTIC plane on the right hand side of Aladin and open the properties window of the plane with the pawprints as shown in Figure 7 3 EN EN EN Properties Properties of the plane PLASTIC PlanelD PLASTIC _ als WETTER el m Default shape rhomb s Source 66 Origin plastic uk ac starlink plastic RmiAgent 2e8204 3 VISTA_Survey_Area_Definition_Tool_Plastic_Ma
51. he red outline of the excluded Geodesic Rectangle VISTA Survey Area Definition Tool User Manual for VISTA Data Flow System Survey Areas displayed in Galactic Cartesian Plot Zoom 1 Vi E VIS MAN QMU 0001 0003 x di E 36 000 35 000 34 000 33 000 32 000 31 000 30 000 Figure 5 2 As Figure 5 1 but with the Circle area excluded the Aspect Ratio not fixed and displayed in Galactic Coordinates 5 7 Interpreting shapes displayed SADT s default display is simple Cartesian not a spherical projection Shapes of areas plotted must be interpreted with this in mind North Polar and South Polar projections are also available The shapes seen will also depend on the System Type Aspect Ratio and values set and the projection used Be careful not to jump to incorrect conclusions about your tiles based on the plots Two examples are 1 In the Cartesian plot a Geodesic Rectangle and a Coordinate Range will look similar close to the equator however near the pole a range will still look like a rectangle whereas a geodesic rectangle will look like a slice 2 Ina Cartesian Plot a coordinate range defined in a particular coordinate system appears as a rectangle in the survey area display only if the same coordinate system 1s selected as display coordinate system 3 Equivalent but different considerations arise when plotting in S Polar projections 5 8 Saving Survey Areas without Tiles Pawprints The survey
52. ice of systems rrrrnrnrnrnnrnnnnrrrrnnrrrrrrrnrrrrrrrrrrrrrrrrrrrrnrnrnnne 12 1 6 4 Choosing between the 3 input systems especially at Dec Lat above ef 13 NNN 13 2 INSTALEATIONAND START UP susen 13 2 1 REQUIREMENTS cccccscccosccsssccccccessecessceccecsscessecsuscessescscessecuscessesesssesessusceseseaesessecsuscesesescessessuseenseseaes 13 TINN 13 NNN NNN 14 EEE ENO ERE ERE NE RE RR ER 14 Zad A E EN 14 OVI ON SDI REE EEE EE 14 EEE OAL OL SSE EE none ee ee er ae 14 224 MS Windows instalaltion pve ctccdsssnesacednslceoonie tinued veardda cede nas aa e aaaea esau TA AEE ii 14 SMN 15 2 260 Configure location of IP Jor SAD Pasadena dad E Ena a 15 KR 15 e GE EE EE 15 e P DEG ERE REESE EE NE A EN 15 LE EEG ON EEE EN eee eee ee 15 TSR een 15 3 SETTING CHOOSING OPTIONS Lenne egENege 17 ENN 18 Ehe 18 SE 18 313 Crealesurvey areas from iles MAML EE 18 IA Comet Be AMLE TEE 18 NNN 18 GE ENE NERE EE EE 18 SS NNN SION 19 TONE ONO en 19 PENN jr 19 ETL AE LON cg Le OL Lic EEE EE EEE mene ee eae 19 Iaa Draw Aur DCIS EE 19 SE Overlap JONO EE 19 3 2 6 Configure Preferences Select Values EE 20 GJ EEE EGG de M EE 20 3202 e E G EE REE ER 20 3203 VNR 21 3 2 64 Tile Orientation Tile relative to Survey ATCA sicdiccscasissacsasasnnscencsaceaceasenvessananesa nen dnneenteowaieeanadaedcnnoanescedes 22 NE NA 22 SG MENN Ne 23 VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG EE O EE 23 PEER ER 23 5
53. ing had to be used to find a guide star after the pointing creation was started or resumed 0 None or too few guide aO stars Type None Found Too Few Found LOWES PY 66 tiles P tiles AG ee tiles o tiles LOWFS_NY 66 tiles o tiles Please save the results Figure 6 1 Information message on completion of tiling as in Figure 6 2 Figure 6 2 shows the tile found for the areas defined in Figure 4 1 The default 60 arcsec tile to tile overlap in X has in this case caused 5 more tiles to be produced than are needed This is an edge effect due to the small area being surveyed These 5 unnecessary tiles could be removed by rerunning with TILE OVERLAP X 0 In general however overlaps should be retained for later matching up tiles across boundaries in data processing Pa IST VISTA Survey Area Definition ess Tool User Manual for VISTA a Survey Areas displayed in FKS J2000 Cartesian Plot Zoom 1 01 00 00 00 00 00 01 00 00 D eet 02 00 00 03 00 00 04 00 00 05 00 00 19 20 00 19 16 00 19 12 00 19 08 00 19 04 00 19 00 00 18 56 00 18 52 00 18 48 00 Figure 6 2 Tiles created for Survey Areas in Figure 4 1 without using guide stars 6 1 3 Stop Stops the process of making Tiles Pawprints and finding guide aO stars This may be necessary if Internet connection to the catalogue is slow or the run is taking longer than expected Run length is limited by finding guide aO stars from th
54. lumns start at 1 1 in the bottom right hand corner of each Survey Area VISTA Survey Area Definition Tool User Manual for VISTA oe N B Offangle is NOT the position angle input into P2PP as discussed in 4 1 4 5 8 6 3 3 Example Pawprint The same ouput file is next displayed showing the expanded first Pawprint of the first Tile Mozilla Firefox J LG Lal ft a file Users jim Desktop Fig_6 5 xml 47 Y is g Goo Q Most Visited Bookmarks Toolba Observingv Documents software astro v VirtualSkys VISTA ESO v file Users jim ktop Fig_6 5 xml ke This XML file does not appear to have any style information associated with it The document tree is shown below lt SURVEY backtrackStep 100 0 id Fig 6 5 ip VIRCAM 1 25 maxJitter 15 0 tileAngle 0 tileOverlapX 60 0 tileOverlapY 60 0 gt lt SURVEY_AREA coordSys Galactic exclude false height 2 2 lat 2 0 long 32 0 number 1 posangle 35 0000 type Geodesic Rectangle width 475 gt lt TILE dec 021057 000 id 1 1 offangle 27 9166 priority 0 ra 185747 808 gt lt PATTERN gt Tile6n lt PATTERN gt lt PAWPRINT dec 021823 040 id 1 1 1 offangle 27 9160 offsetx 0 475 offsety 0 475 ra 185738 688 gt lt REFSTARS gt lt REFSTARS gt lt PAWPRINT gt lt PAWPRINT dec 021331 440 id 1 1 2 offangle 27 9143 offsetx 0 475 offsety 0 0 ra 185728 368 gt lt PAWPRINT gt lt PAWP
55. ment tree is shown below lt SURVEY backtrackStep 100 0 id Fig 6 5 ip VIRCAM 1 25 maxJitter 15 0 tileAngle 0 tileOverlapX 60 0 tileOverlapY 60 0 gt lt SURVEY_AREA coordSys Galactic exclude false height 2 2 lat 2 0 long 32 0 number 1 posangle 35 0000 type Geodesic Rectangle width 475 gt lt TILE dec 021057 000 id 1 1 offangle 27 9166 priority 0 ra 185747 808 gt lt TILE gt lt TILE dec 011302 640 id 2 1 offangle 27 9015 priority 0 ra 185545 072 gt lt TILE gt lt SURVEY_AREA gt lt SURVEY_AREA coordSys Ecliptic exelude false lat 19 5 long 288 0 number 2 posangle 0 0000 radius 47 type Circle gt lt TILE dec 030108 760 id 1 1 offangle 7 0712 priority 0 ra 190754 240 gt lt TILE gt lt TILE dec 015524 240 id 2 1 offangle 7 1045 priority 0 ra 190744 904 gt lt TILE gt lt SURVEY AREA gt lt SURVEY AREA coordSys FK5 J2000 exclude false lat1 01 00 00 lat2 00 00 00 long1 19 03 00 long2 19 14 40 number 3 posangle 0 0000 type Coordinate Range gt lt TILE dec 002358 920 id 1 1 offangle 0 0000 priority 0 ra 190557 000 gt lt TILE gt lt TILE dec 002358 920 id 1 2 offangle 0 0000 priority 0 ra 191147 064 gt lt TILE gt lt SURVEY AREA gt lt SURVEY gt Done Within the lt Tile element the id is constructed as TileRowNumber TileColumnNumber where the rows and co
56. n Section 8 1 3 2 6 1 Tile to Tile Overlap in X gt 2x sampled overlap in X Set a value for the tile to tile overlaps in arcsec required in X TILE OVERLAP X for areas covered twice or more with a default Tile6 pawprint pattern Overlaps double and greater coverage in adjacent tiles in X by 60 arcsec 1 e 60 arcsec in X at the sides is common double coverage to adjacent tiles in X 3 2 6 2 Tile to Tile Overlap in Y gt 2x sampled overlap in Y Set a value for the tile to tile overlaps in arcsec required in Y TILE OVERLAP Y for areas covered twice or more with a default Tile6 pawprint pattern Overlaps double and greater coverage in adjacent tiles in Y by 60 arcsec The value of the Y overlap shown in the GUI is the same value that is stored or retrieved from the XML file For internal calculations however the Y overlap used is the Y overlap from the GUI plus the value of the parameter 1x STRIP Y from sadt cfg 1x STRIP Y is set at 330 0 475 2048 0 339 arcsec which just overlaps the singly exposed edge strips of VISTA Survey Area Definition Tool User Manual for VISTA a adjacent tiles in Y This is to ensure that the 1x covered strips in the Y direction are covered twice as should be the default for efficient surveys a VIS MAN QMU 0001 0003 i ail Visible amp de Astronomy Examples e TILE OVERLAP Y 60 overlaps adjacent doubly exposed tiles in Y by 60 arcsec 1 e 60 arcsec in Y is common do
57. nager See catalog info Associated FoVs Show all associated FoVs Hide all associated FoVs Figure 7 3 Aladin s Plastic properties window Clicking on Show all associated FoVs should now show the outline of the boundary of each tile but not the individual detectors as in Figure 7 4 BG Aladin v5 0 Location ICRS full SS PU SE grid multiview match Search e TIP Resize the measurement columns click amp drag the header Osel 66src 17Mb KE Figure 7 4 SADT pawprints with their Field of view plotted in Aladin It should be possible to overlay the pawprints onto an image of the field loaded into Aladin VISTA Survey Area Definition Tool User Manual for VISTA EG pan VIS MAN QMU 0001 0003 i ail Visible amp de Astronomy 8 Appendix 8 1 Making a Tile The 4x4 array of IR detectors in VISTA s focal plane are not contiguous Figure 1 3 so a single sky exposure shows the gaps between the detectors known as a pawprint To make an image without gaps it 1s necessary to combine pawprints with position offsets together so as to cover the gaps and form a filled tile Given that detector spacing in the X 0 9 detector and Y 0 425 detector directions are different six 6 pawprints is the minimum number of pointed pawprints required for reasonably uniform and completely contiguous coverage of an area and exposes each piece of sky away from the Y and Y edges of the tile to at least 2 cam
58. nal until guide aO stars for all the pawprints in the tile have been found Then the pawprints become permanent and are displayed in black When plotting a large area the plot may become confused by the black pawprints To mitigate this uncheck Draw Pawprints 3 2 3 in the Options Menu and only the red outlines of the Tiles will be displayed with black dots at the pawprint positions For very large survey areas the dots representing the pawprint might appear merged together You can use the zoom facility 5 4 1 to zoom in on the detail 6 1 6 Guide aO star finding display While the SADT is filling the survey areas with pawprints it searches the selected catalogue for suitable guide aO stars if the guide aO star search mode is enabled The catalogue entries and the guide aO detector footprint currently being searched are displayed Figure 6 3 amp Figure 6 4 while this process goes on The AG LOWES windows will if you don t have a slow connection to the catalogue flash by very fast so it will usually be too quick to see much A log of difficulties encountered is output in the terminal window 2 3 IST VISTA Survey Area Definition Tool User Manual for VISTA Visible amp Infrared Survey Data Flow System Detector AG NY at 19 12 27 174 01 06 18 24 a OC Ee y GE eg ye Ze G Qas CAS Sy te Of CR AGE don x Soy e Figure 6 3 Autoguider star search window Figure 6 4 aO star search window The following colour c
59. oding is used for catalogue entries in the guide aO display windows green The entries that are selected as the guide aO stars Note that no green entries are displayed if at the time of the display it is not yet known which entries will be selected as guide aO stars Example First the SADT looks for suitable candidate entries for guide stars on both autoguider chips without displaying any as selected guide aO stars Only after that the SADT decides which of these are selected as guide stars cyan Entry in autoguider range and valid Entry in autoguider range and invalid blue Valid but not in autoguider range magenta Not valid and not in autoguider range and the following for the background colour in these windws ee eee grey Normal mode of operation Ge red No guide aO star found yet Backtracking pink Backtracking was successful KE Ki red and yellow No guide aO star found Backtracking unsuccessful Leaving flash this pawprint empty It sometimes happens that the change of background colour of the detector display is not exactly as described here especially when the algorithm is interrupted by clicking the Stop button and then can briefly assume it is in backtracking mode and trigger the display to be VISTA Survey Area Definition Tool User Manual for VISTA a painted red although backtracking is subsequently not really executed Similarly if the detector display might sometimes stay red even though backtracking has alr
60. one at Angle 35 Column headings for Geodetic Rectangle Survey Area row 4 3 Delete Survey Area A complete Survey area row can be permanently deleted use Exclude to merely stop an area being plotted and used to generate Tiles from the table by selecting the row via any cell in the row with the mouse and pressing the Delete Survey Area button to the right of the Add Survey Area button You will be prompted Are you sure you want to delete the selected survey area and can answer Yes or No After deleting an area click on View Update Areas to refresh the display ist VISTA Survey Area Definition Tool User Manual for VISTA Data Flow System 5 Survey Areas View Update amp Save 5 1 Overview SADT allows the user to view the surveys tiles pawprints in several coordinate systems and projections to zoom to graphically exclude or delete regions and to query the coordinates of a point and iteratively adjust and replot the survey areas and tiles 5 2 View Update Pressing the View Update Areas button allows viewing of survey areas specified in the text box without starting generation of pawprints and allocating the guide aO stars the areas are shown in Green with a selectable coordinate grid overlaid Also use View Update after making a change the survey areas defined in the Survey Area table The Survey with 3 types of area geodesic rectangle circle and coordinate range in this example each in a different
61. onomy Tool User Manual for VISTA Page 17 of 64 EISE Answering Yes will terminate SADT Answering No will allow you to continue using the version of the IP included with SADT but for version control reasons the SADT file that you make may not be usable in P2PP but will be useful for practise If you did set the correct path to P2PP s VIRCAM IP the window in Figure 2 1 will not appear Now the window from which the SADT is driven opens Figure 2 2 Survey Area Definition Tool VISTA File Options Help Survey ID Survey Areas Type RA Long Dec Lat Width Long An Height Lat2 Angle System Exclude Add Survey Area Tile Patterns l VIRCAM Tile6n e Catalogs GSC 2 at ESO KR View Update Start Resume Reset Plastic Figure 2 2 Command Input GUI window on opening 3 Setting Choosing Options The user must configure some parameters before generating any survey areas tiles pawprints of guide aO stars SADT does not remember the last values used when it was last shutdown so these options will need to be set each time SADT is started up As SADT cannot know what you intend to do in P2PP you must provide it with information on the Tile pattern you will use in your OBs 3 5 and the maximum jitter amplitude 3 2 6 3 VISTA Survey Area Definition a LL Tool User Manual for VISTA EG you will use in your pawprints If this information is not c
62. onsistent with what you actually do in P2PP your OBs will fail 3 1 Main GUI Menu File Clicking on the File menu brings up the following Window Open Save As Create survey areas from tiles in XML file Convert Existing XML File To Gnuplot Network preferences Exit 3 1 1 Open Open xml files written by SADT 3 1 2 Save As Save current survey definitions as an xml file 3 1 3 Create survey areas from tiles in XML file Convert tiles within a survey area saved in an xml into multiple survey areas one for each tile 6 6 3 1 4 Convert Existing XML file to Gnuplot Igonore this no longer supported option It was for debugging by a software engineer in debug mod and wrote the coordinates of the tile centres pawprints and guide stars to files that ccould be read by Gnuplot and created a Gnuplot script that read all these files 3 1 5 Network Preferences Specify a proxy server if required e g in connection with firewall 3 1 6 Exit Exit the SADT program N B The parameters set in the menus are not stored within SADT between invocations of it Be sure to save your work as an xml file or note your settings VISTA Survey Area Definition Tool User Manual for VISTA a 3 2 Main GUI Menu Options Clicking on the Options menu brings up the following Window Find Guide aO Stars Fixed Aspect Ratio Draw Pawprints Draw Aux Detectors Include Overlap a VIS MAN QMU 0001 0003 i ail Visibl
63. osangle 35 0000 type Geodesic Rectangle width 1 475 gt VISTA Survey Area Definition Tool User Manual for VISTA H Visible amp Infrared Survey Telescope for Astronomy i lt SURVEY AREA coordSys Ecliptic exclude false lat 19 5 long 288 0 number 2 posangle 0 0000 radius 1 47 type Circle gt lt SURVEY AREA coordSys FK5 J2000 exclude false lat1 01 00 00 Lat2 00 00 00 Longi 19 03 00 Long2 19 14 40 number 3 posangLe 0 0000 type Coordinate Range gt lt SURVEY gt Witin each defined type lt gt parameters set are written in alphabetical order The meaning of these should be clear from earlier section of this manual except for lt SURVEY id which is Survey ID name of the whole survey lt SURVEY AREA number an integer ID conter for each survey area 8 6 3 2 Example Survey Areas with tiles pawprints and Guide aO stars As a more complex example the xml file saved for the Tiles defined in Figure 6 5 is as follows with guide aO star finding switched off and everthing under the Tile elements collapsed using Firefox at the viewer Mozilla Firefox LG GA L file Users jim Desktop Fig 6 5 xml LI Y ins a Lk Q Most Visited Bookmarks Toolba Observingy Documents software astro v VirtualSkys VISTAv ESO v _ file Users jim ktop Fig 6 5 xmi hard This XML file does not appear to have any style information associated with it The docu
64. reparation tool P2PP It also provides facilities to plot the pawprints on VO tools communicating via a PLASTIC hub such as Aladin SADT is not concerned about what observations are carried out at each position in a survey except SADT must be given the Tile pattern to be used to determine the order in which the Pawprints will be observed Sec 0 and the maximum jitter amplitude used 3 2 6 3 to ensure the GS and AOS stars stay on the CCDs during jitter moves Caution If either of X coord of pointing or Y coord of pointing set to non zero values in OBs in P2PP SADT Guide AO stars will NOT work as SADT does not take any account of such X Y coord offsets VISTA Survey Area Definition Tool User Manual for VISTA a To implement a survey the positions of the component tiles that VISTA will have to observe must be defined Each filled tile will consist of typically six overlapping pawprints and for best image quality autoguiding and active optics should both be used a VIS MAN QMU 0001 0003 i ail For each pawprint in each tile suitable candidate guide stars GS and active optics stars AOS must be preselected ready for use when the observation is made This ensures that survey speed is not limited by frequent tedious and sky time wasting operator intervention For guide star acquisition there must be at least one GS this can be on either of the two autoguider CCDs AG PY AG NY see Figure 1 3 For active optics opera
65. ser to visualize digitized astronomical images superimpose entries from astronomical catalogues or databases and interactively access related data and information from the Simbad database the VizieR service and other archives for all known sources in the field SADT can export Tiles and for plotting in Aladin SADT does this using a PLASTIC manager PLASTIC the PLatform for AStronomical Tool InterConnection http plastic sourceforge net is a VO protocol for communication between client side astronomy applications Once you have created tiles you should be able to send them to Aladin from SADT s PLASTIC dialog Aladin should be started with Plastic hub manager on the same machine as the SADT before you attempt to exports any tiles Aladin V4 and V5 launched a PLASTIC manager by default Aladin V6 will by default launch a SAMP internal hub and not a PLASTIC internal hub To launch PLASTIC internal hub you have to specify in advance the plastic parameter on the Aladin command line http aladin u strasbg fr java FAQ htx T0C34 EE VISTA Survey Area Definition Tool User Manual for VISTA ist Page Paora Data Flow System The Plastic button in the SADT GUI brings up a Plastic dialog as in Figure 7 1 Plastic HUB up Aladin 2 Send Survey Tiles 4 Cancel d Figure 7 1 SADT s plastic hub menu From this dialog it is currently only possible to send survey tiles not survey areas to Aladin All t
66. tation Tile relative to Survey Area The tile orientation is the angle on the sky between the Height axis of the survey area and the Y shorter axis of VISTA focal plane Figure 1 3 measured increasing Eastward from the Height axis on the sky Tile orientation can be set at either 0 90 180 or 270 deg Because VISTA tiles are rectangular not square a more efficient tiling of a survey area fewer tiles to cover it can result from choosing an appropriate Tile Orientation to best fit the survey area with the minimum number of tiles 3 2 6 5 Backtrack Step In case the guide aO star requirements cannot be met at a tile position SADT moves the Tile position Backtrack Step is the amount in arcseconds by which the SADT s guide aO star search algorithm shifts a tile back along the row of tiles The backtrack step is repeated until guide aO stars are found or the previous tile position is reached In extremis sidetracking can also be enabled in sadt cfg though this 1s not normally recommended After backtracking there will often be more tiles needed and they will be at different positions than would be found with the Find guide aO Stars selection set to Off in the Options menu The X boundaries of tiles in adjacent rows will also not match up VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG In the unlikely event that guide aO stars are not required Backtracking can be suppressed by setting Backtrack Step 0
67. the SADT are a To generate the pointing position for each tile making up a survey b To find the 6 sets of guide stars GS and active optics stars AOS necessary to observe each survey tile c To iteratively adjust the tile positions if insufficient GS and or AOS were found d To enable tiles to be plotted or overlaid on sky images displayed in Aladin or other VO tools communicating via a PLASTIC hub e To output the results in a form that can be used in the Phase2 Preparation Program P2PP to generate the OBs ready to await scheduling for execution Note that this manual doesn t tell the whole story of how VISTA surveys are prepared this is covered in ESO documentation Figure 1 1 and Figure 1 2 diagram the process of producing and executing a survey in two ways excluding matters related to scheduling User OG Survey Plan Standard Activity Flow Specify survey areas first black and red transitions Alternative Activity Flow Create parent OB first gray and red transitions gt Specify survey areas Select guide aO star catalog Generate tiles with guide aO stars Save results gt Copy parent OB to each tile N P2PP _S Create parent OB Y Import OBs N position and export as OBX PAF d Figure 1 1 Use of SADT with P2PP Check OBs into ESO OB repository OB Repository at ESO OBs in repositor
68. tile to at least 2 camera pixels Sec 8 1 e Pawprint A pawprint is the image formed by the 16 non contiguous images of the sky produced by VISTA with its 16 non contiguous chips The four definitions above also determine the hierarchical structure of the xml files that SADT outputs and that are read by P2PP Sec 8 6 e Angle Survey Area relative to Sky The position angle degrees on the sky between North in the selected coordinate system and the Height axis of the survey area Angle is measured increasing Eastward from North on the sky e Orientation Tile relative to Survey Area The angle on the sky between the Height axis of the survey area and the Y shorter axis of VISTA focal plane Figure 1 3 measured increasing Eastward from the Height axis on the sky 1 5 Introduction A survey with the wide field survey telescope VISTA involves observing predefined areas of sky typically with the same basic observing parameters Observation Block OB except for position on the sky repeated at many sky positions and perhaps at several times or with different filters The SADT is intended to automate the process of producing sky position dependent data needed to execute the many OBs required for large area surveys SADT provides editing and graphical display facilities for Survey Areas creates Tiles and Pawprints selects guide and active optics stars for these areas and saves the output in a form understood by the phase 2 p
69. tion on a survey as an object in memory and consequently the more tiles there are and the more GS AOS have been found the more memory is required VISTA Survey Area Definition Tool User Manual for VISTA a This can lead to progress being uncomfortably slow with large survey areas One way to mitigate this is have more memory available which gives better performance The SADT start up script attempts to set a maximum heap size appropriate to the memory available on the machine it is run on a VIS MAN QMU 0001 0003 i ail Visible amp de Astronomy Given the finite memory available on any particular machine the alternate mitigation is to split the survey up into a number of sub areas and run SADT separately for each sub area The output xml files could subsequently be edited and merged into a single file if required Though on any reload SADT operations on this file would probably run very slowly 2 1 2 Network speed Another the speed limitation which can arise is a result of the remote network access to search for guide aO stars as when selecting a guide star catalogue that its location on the internet and the speed of the internet connection can have a strong effect on the time it takes hours for large numbers of tiles 2 2 SADT Installation 2 2 1 Install P2PP first P2PP should be installed according to instructions from ESO before installing SADT During installation P2PP will download and install the current version of
70. tion there must be at least two AOS one on each of the two Low Order Wavefront Sensor CCDs LOWFS PY AOSA and LOWES NY AOSB see Figure 1 3 The major functions of the Survey Area Definition Tool SADT are a To generate the pointing position for each tile making up a survey b To find the 6 sets of guide stars GS and active optics stars AOS necessary for each survey tile c To iteratively adjust the tile positions 1f insufficient GS and or AOS were found d To enable tiles to be plotted or overlaid on sky images displayed in Aladin or other VO tools communicating via a PLASTIC hub e To output the results in a form that can be used in the Phase2 Preparation Program P2PP to generate the OBs ready to await scheduling for execution 1 6 Ways of Defining Survey Areas SADT must calculate or be given the positions of the component tiles of each Survey Area in the chosen coordinate system SADT deduces the component pawprints and their GS and AOS stars from the tile positions once the tiling begins The survey areas and tiles are first defined in the chosen input coordinate system Note that regardless of the input coordinate system used the tiles in the output xml files are specified in RA Dec J2000 for use at the telescope SADT has three distinct ways of producing the tiles There may be multiple instances of each type in any Survey 1 6 1 Rectangular Geodetic areas via GUI in a choice of systems In a Geo
71. to make a tile ABCDEF as in the table below VISTA Survey Area Definition a LL Tool User Manual for VISTA EG For example VISTA Tile6n corresponds to ABCDEF up right down forming an n etc as detailed below for each available sequence of pawprint positions 8 2 1 1 Tile6n VISTA Tile6n corresponds to ABCDEF up right down forming an n SEQ TILE NAME 6 step n pattern SEQ TILE OFFSETX 0 475 0 475 0 475 0 475 0 475 0 475 SEQ TILE OFFSETY 0 475 0 0 0 475 0 475 0 0 0 475 SEQ TILE OFFSETROT 0 0 00 00 00 00 0 0 Tile6n Figure 8 3 Tile6n 8 2 1 2 Tile6u VISTA Tile6u corresponds to CBAFED down right up forming an u SEQ TILE NAME 6 step u pattern SEQ TILE OFFSETX 0 475 0 475 0 475 0 475 0 475 0 475 SEQ TILE OFFSETY 0 475 0 0 0 475 0 475 0 0 0 475 SEQ TILE OFFSETROT 0 0 0 0 0 0 0 0 0 0 0 0 Tile6u Figure 8 4 Tile6u VISTA Survey Area Definition e ai Kl Tool User Manual for VISTA EG 8 2 1 3 Tile6z VISTA Tile6z corresponds to CDEBAF right down left down right forming an z SEQ TILE NAME 6 step large Z pattern SEQ TILE OFFSETX 0 475 0 475 0 475 0 475 0 475 0 475 SEQ TILE OFFSETY 0 475 0 475 0 0 0 0 0 475 0 475 SEQ TILE OFFSETROT 0 0 0 0 0 0 0 0 00 0 0 Figure 8 5 Tile 6z 8 2 1 4 Tile6s VISTA Tile6s corresponds to DCBEFA left down right down left forming an s SEQ TILE NAME 6 step large S pattern SEQ TILE OFFSETX 0
72. tting priority to 999 e Restore Selected Tile s Left click on the residual group of pawprint centres for a tile selects it and right click gives the Restore Tile option Selecting it restores the pawprints making up the tile A priority can also be assigned when doing this e Set Tile Priorities Right Clicking inside a selected tile or group of tiles gives the Set tile priority option on the popup menu The internal 4 step priority can be set in the integer range 0 3 with each priority associated with a different colour 0 red default 1 purple 2 light blue 3 dark blue N B Currently Tile priorities are not used externally to SADT Any priorities needed are currently set outside SADT after OB creation for example in scheduling containers see P2PP manual The tiles in Figure 6 2 are shown in Figure 6 5 after deleting several tiles which were generated due to the Tile to Tile Overlap settings 3 2 6 1 and assigning different priorities to one tile in each of the 3 remaining Tile pairs VISTA Survey Area Definition Tool User Manual for VISTA my VIS MAN QMU 0001 0003 Visible amp Nornen Astronomy ae bn 01 00 00 00 00 00 01 00 00 02 00 00 03 00 00 04 00 00 05 00 00 19 20 00 19 16 00 19 12 00 19 08 00 19 04 00 19 00 00 18 56 00 18 52 00 18 48 00 Figure 6 5 Tiles in Figure 6 2 with some deleted and various priorities note colours set Note the dots at the centres of each pawprint of the
73. uble coverage to both double covered tiles e TILE OVERLAP Y 0 just completely overlaps the singly exposed edge strips of adjacent tiles in Y giving doubly exposed edge as elsewhere in the tile e TILE OVERLAP Y 330 just butts no overlap the singly exposed strips not recommended 3 2 6 3 Maximum Jitter Amplitude The maximum amplitude in arcseconds of the Jitter pattern to be used in the OBs must be set from the GUI under Options gt Configure gt Maximum Jitter Amplitude This is determined by looking at the defined Jitter patterns 8 3 taking the modulus of all the values finding the largest modulus in OFFSETX and OFFSETY and then rounding up The values for Maximum Jitter Amplitude for each available Jitter pattern are given in Table 3 1 As during OB definition in P2PP the jitter offsets in a pattern may be scaled by the multiplicative factor so the Maximum Jitter Amplitude value in Table 3 1 include allowance for this factor The default value of Jitter Scale Multiplier of 15 0 set in sadt cfg is large enough to accommodate all the values in Table 3 1 only if Jitter Scale Multiplier remains at its default value of 1 0 The Random Jitter available in P2PP is not a fixed pattern like the others but is generated with a given amplitude when the OBs are created For Maximum Jitter Amplitude use the amplitude 0 peak of this Random jitter as to be set in P2PP Together the position and dimensions of the four guide a
74. y H Visible amp Infrared Survey Telescope for Astronomy Data Flow System Star Catalogue Black text common to all ESO VLT instruments Blue text additions for VISTA Instrument Summary VIS MAN QMU 0001 0003 11 September 2009 VISTA Survey Area Definition Tool User Manual for VISTA e VIRCAM executes the templates and interprets PAF fil bedded inside the OB ekke ed kle SS the contents of the PAF files parameters of type paramFile e Each OB contains a VIRCAM_img_acq template followed by a VIRCAM_img_tile template Survey description e BOB interprets the OB and recreates the PAF files Guide star info PAF files Observation Blocks empeddaed PAF files Template parameters Template Signatures Template Instrument Signatures Sunhmary Template S ripts Tile Patterns Instrument Summary Instrument Package VERSION Plate scale Detector size Field of view Available Filters Available Tile Patterns etc Figure 1 2 Survey process 1 2 Abbreviations and Acronyms AOS aO GS LOWES OB P2PP PAF PLASTIC SADT VIRCAM VISTA Active Optics Star Active optics NOT Adaptive optics Guise Star Low Order Wave Front Sensor Observing Block Phase 2 Preparation Program PArameter File PLatform for AStronomical Tool InterConnection Survey Area Definition Tool VISTA InfraRed CAMera

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