VIS-DES-UOD-06048-00..
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1. function HOWFS STARPOS X 32 0 msgSend wvcam vchoiaServer ANASTAR The vchoiaServer process replies with a 256 character long string Most replies contain OK FAILED or the data returned by the command packed into a string In the case of the ANASTAR command the resultant coefficients are not returned They are instead copied to file and to the database Laboratory Astronomy Technology Centre University of Durham Rutherford UK Astronomical Instrumentation Group Appleton cLRc HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description This document defines the interface with vchoia and the HOWES database structure and entries The interface will be based on the EVH toolkit described in RD4 The interface will be implemented by inheriting from the evhSTD COMMANDS class which provides default implementation for the standard commands l z E A Sears Sequencer script Il wvcam environment msgSend wwcam vchoia SETUP function lt params gt nee ere Replies lt id gt Appl_data VIRCAM OS ICS HOWFS status state etc msgSend wwcam vchoia WAIT id lt id gt S status state etc msgSend wwcam vchoia ANASTAR Commands A ee a a ORE vchpan vemefg module k module information HO V VF S Image MN HOWFS test Analysis data Sporer L dicVIRCAM2. 5 4 Coefficient file When the analysis is complete the results are written to the database at fit coeffs and also to a coefficients file The coefficients file name is given by database parameter setup data coeffFileName The VIRCAM software will provide a new filename for each observation The filename will conform to the ESO VLT naming conventions RDO1 and will be the same as that used for the associated observation with COEFFS appended to the filename This file will be used to store data obtained during an analysis It will be processed offline to generate the look up tables required for correcting the shape of the primary mirror in open loop mode The format of the file will be that of a 2 column binary FITS table containing the modulus and angle for each mode Other parameters that are relevant to that HOWFES observation are included as FITS header parameters These are specified in Table 3 A full list of FITS header keywords used by the HOWFS software is given in Tables 6 and 7 Table 3 Headers to the Coefficients FITS File FITS Keyword HOWFS IMGFILE string Name of file containing defocused images Included for reference HOWES ID Unique id for each HOWES observation TEL M1 TMP double Temperature of Mirror in degrees Celsius when image was acquired This can be retrieved from Image File but included here for efficiency TEL double Telescope Altitude in degrees This can be retrieved from Image File but included he
3. Run Simplex 8 Generate Image Pair A A a y a a a a 13 WAIT LS 12 Calculate Fitness ee 15 Save Coeffs to database and file 17 CHECK Figure 8 Exchange of messages between the vchoia classes when doing an analysis University of Durham Rutherford UK Astronomical Instrumentation Group Appleton Laboratory carc Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description 8 amp 8 DEPLOYMENT The HOWFS image analysis software including the vchoiaServer process will be contained within the vchoia module The HOWFS database will be contained within the dbl subdirectory of the vchoia module This vchoia module will be deployed using the pkgin tool RD6 The vchoiaServer process will run on the instrument workstation and on the same VLT environment wvcam AD7 as the observation software The pkgin tool will be responsible for creating the necessary VLT environments and for building the database The HOWES database will be contained within the dbl subdirectory of the vchoia module which is assumed to be included in the wvcam database contained in the vcins module as shown in Figure 3 The configuration file and null aberrations file are stored in the vchoia module 9 TESTING Testing of the software will be done using ESO s tools for automated testing TAT RD8 TAT provides a set of tools that can be used as part of a script to test softwar
4. Spherical AA 8 ez e l2 sin e 1 2 cos 9 asp 5 1 sin e 5 1 cos 10 5 Order Spherical Defocus Z22 o S O e 6 1 sin e 6 1 cos e 3 2 sin e 3 2 cos 12 APPENDIX C LOG FILES The HOWFS will also log the following events to log files using the CCS logging system RD9 Each event will be time stamped Two types of log files will be generated depending on the mode of operation University of Durham gore ford UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description e Operational log file o A record of start up and shutdown times o Each command received from the OS o A description of each measurement made and the wave front coefficients derived e Engineering log file o Command received from the OS including parameters o Informational messages when running in VERBOSE mode o Error messages and fault conditions with diagnostic information 000 University of Durham eon ieee UK Astronomical Instrumentation Group ppleton Laboratory carc Astronomy Technology Centre HOWFSv3 4 doc
5. substate detector badPixelMask detAngle m imageld imgFileName darklmgFile flatlmgFile VIS DES UOD 06048 0002 window NX NY STRX STRY setup startUpCoeffs active m modulus angle startpntModified nullCoeffs nullModified nullSubtract modulus angle coeffFileName altitude mirror Temp data preCentre X Y m postCentre X Y starPos X Y seeing modes type symmetry ____ order name setupF ile fit coeffs active modulus angle simplexDiag relative Tolerance m IterationCount m funEvalsCount m executionTime successFlaq preProcess thresholdActive m maxIntensity m totallntensity threshold badPixels algParameters _ simplex maxRelTolerance m maxlterationCount maxFunEvals raytracer opticalConstants pupilDiameter m focallength defocus m ObsRatio pixelSize obsOffsetX obsOffsetY m ImageSizelnPixels IntensityRatio tracingEngine gridSize m subGridSize preBlur Figure 5 Database structure for module vchoia University of Durham ger ford UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front
6. 2002 AD5 Image Analysis Algorithms for VISTA wavefront sensing VIS TRE UOD 06042 0005 Issue 1 0 12 Nov 2003 University of Durham eon ieee UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description AD6 Operation of VISTA Active Optics VIS TRE VSC 13030 0001 Issue 1 0 22 Aug 2003 AD7 VISTA IR Camera Software User and Maintenance Manual VIS MAN ATC 06080 0020 Issue 1 0 12 November 2003 AD8 High Order Curvature Sensor Sensing Positions VIS ICD UOD 06042 0020 Issue 0 3 12 October 2005 1 4 Reference Documents RD1 Template Instrument Software User and Maintenance Manual VLT MAN ESO 17240 1973 Issue 4 31 March 2003 RD2 VLT Software Active Optics Design Description VLT SPE ESO 17210 1173 20 October 1997 RD3 Base Observation Software Stub BOSS User Manual VLT MAN ESO 17240 2265 Issue 4 5 April 2004 RD4 CCS Event Tool Kit EVH User Manual VLT MAN ESO 17210 07711 Issue 1 8 6 October 2001 RD5 VLT Software TCS Auto Guiding and Field Stabilisation Design Description VLT SPE ESO 17230 0933 Issue 3 0 10 April 2000 RD6 Installation tool for VLT SW packages User and maintenance manual VLT MAN ESO 17240 1913 Issue 4 31 Mar 2003 RD7 Numerical Recipes in C The art of Scientific Computing William H Press et al 2nd ed Cambridge Press 2002 RD
7. E Sensor Software Design IR Camera Description Table 1 Definition of variables stored in the database Variable Name Origin Type Description status Status String Standard state information Statues String Detailed state information Config String Name of file storing bad pixel mask detAngle Config Double Instrument angle with telescope axis in degrees mageld Header Integer Unique Id of this image imgFileName Setup String Name of file containing the images to be analysed darkImgFile Dark image filename FITS flatImgFile Flat image filename FITS detector window Setup double Size of ROI in X dimension in pixels Setup double Size of ROI in Y dimension in pixels STRX Setup double Lower left pixel of ROI in X dimension STRY Setup double Lower left pixel of ROI in Y dimension setup startUpCoeffs active Setup vector of Indicator to show if mode is to be fitted booleans If not true coefficients are used as bias values modulus Setup vector of Amplitude of mode in nm doubles angle Setup vector of Rotation angle of mode in degrees doubles Only applicable to symmetric modes startpntModified Setup Boolean Flag to show that the startup coefficients have been manually modified psetup nullCoeffs Setup Boolean Flag to show that null coefficients have been modified and are not as in the null file Setup Boolean When flag is set null coefficients are subtracted from analysis result Config Vector of Amplitud
8. for total intensity If sum of University of Durham Rutherford UK Astronomical Instrumentation Group Appleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description badPixels Status Integer Number of bad pixels in the two Images two images is below this value and thresholdActive is set an error occurs alg Parameters simplex maxRelTolerance Config double Stopping criteria for simplex algorithm Stop simplex analysis when relative tolerance falls underneath this value maxIterationCount Maximum number of simplex iterations allowed maxFunEvals Config integer Maximum number of function evaluations allowed alg Parameters raytracer opticalConstants pupilDiameter Pupil diameter in metres focalLength Focal length in metres defocus Defocus of WFS CCDs in mm obsRatio Config double Central obscuration ratio with respect to pupil diameter pixelSize Pixel size in microns obsOffset X Setup double Offset of the central obscuration in CCD pixels in the X direction obsOffset Y Setup double Offset of the central obscuration in CCD pixels in the Y direction imgsSizeInPixels Image size in pixels intensityRatio Intensity ratio of two images algParameters raytracer tracingEngine gridSize subGridSize preBlur Config boolean Flag to indicate if images should be blurred by seeing value Normally TRUE 5 2 Start up coefficients for HO
9. in any one of two sub states IDLE and BUSY Depending on the current state some commands may not be accepted The various states may be defined as follows e OFFLINE The vchoiaServer process is not running or is in the OFFLINE state The database should be arranged to show the state of vchoiaServer as OFFLINE when the wvcam environment is first started and the process should have an exit handler that sets the state to OFFLINE when it is shut down or dies The server can be switched to the OFFLINE state by the OFF command e STANDBY The vchoiaServer process is reading its configuration file or has failed to read its configuration file due to an error The vchoiaServer process is up and running but unable to process data The SETUP ANASTAR CHECK and WAIT commands are not accepted in this state In the event of an error the ONLINE command can make the process re read the configuration file and go to the ONLINE state e ONLINE The vchoiaServer process is running and able to process data The STANDBY command will make the process go into the STANDBY state for compatibility with the startup tool Once in the ONLINE state the process can be in one of two sub states o IDLE No processing is taking place The process can accept an ANASTAR or SETUP command The process transfers to the BUSY state on receipt of an ANASTAR command NOTE The SETUP command is likely to be very fast since it only sets parameters so there is no need t
10. modulf I HOWFS dictionary l ee lolo a a l HOWFS setup files Figure 3 Organisation of the vchoia Module and its Interaction with Other Vista Camera vc Modules 3 WINDOWING AND CALIBRATION Unlike the LOWFS the HOWFS image analysis software makes use of a FITS file containing the full set of 16 images from the IR image plane The HOWFS curvature images for this observation are contained in just one of these detector images The relevant image is identified in the VALIDEXT field in the image header The HOWFS software provides its own dark subtraction and flat fielding capability The VIRCAM software will ensure that the relevant calibration frames are taken The names of the relevant files are contained within the database The HOWFS software expects to find dark and flat fielded calibrations in these files The format of these files is identical to that of the curvature image data It also expects to find a bad pixel mask file This also has the same format but with a 1 or 0 for each pixel to represent good and bad pixels University of Durham ge UK Astronomical Instrumentation Group ppieton Laboratory carc Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description 4 OPERATIONAL STATES The vchoiaServer process can be switched into one of the three standard states OFFLINE STANDBY and ONLINE While in the ONLINE state the process can also be
11. of 26 IR Camera Description Nigel Dipper Telescope Instrument Workstation Setup Files Wavefront Coeffs tale OWES Telescope Derotated Null ac ii setup File Info Coefficients Lue Rotated HO HOWFS Wavetron ommands Null 3 Hawes Coelficients Comm Filter tafo eg Info I1 Config Files Observation Lo Header q l HOWFS l Coeffs File KONES Data Store I 10 nd Durham Software IRACE HOWFS j HOWFS Hardware PixeljData l Calibration UKATC Software 7 Data Other VISTA i HOWFS I Software R O Eso VLT Software Figure 2 Context diagram showing the interactions between the HOWFS software and the Observation Software The HOWFS Image Analysis process is known as vchoiaServer and is part of the vchoia module This process and its interaction with various other modules is shown in detail in Figure 3 The HOWFS image analysis is driven from sequencer scripts invoked by the ESO Broker for Observation Blocks BOB It fits more closely with the ESO model of an on line data reduction task than with an instrument sub system The HOWFS database will be contained within the wvcam environment and the database is created when the wvcam environment is started The vchoiaServer process connects to that database when it starts up The sequencer script will communicate with the vchoiaServer process by sending it messages of the form msgSend wvcam vchoiaServer VERSION msgSend wvcam vchoiaServer SETUP
12. will be overridden as necessary Class vchoiaSETUP will handle the SETUP command since a default implementation is not provided vcholaServer will co ordinate the activity of the objects used within the process Class polySearch inherits from class amoeba The latter implements the SIMPLEX algorithm as described in RD7 Class rayTracer is used for raytracing the defocused images Raytracing as used here is described in ADS Class poly Tables will store the first order partial derivatives of the polynomials of the modes that will be fitted during the image analysis The modes are listed in section 11 After the WAIT command has completed the new coefficients may be read from the HOWFS database or from the specified coefficients file Once the VIRCAM software has made an observation using the HOWES filter and saved the resulting image Figure 8 shows the exchange of commands between vchoiaServer the VIRCAM software and the classes implementing the actual image analysis A higher level diagram showing interaction with the Sequencer can be seen in ADO3 Fig 14 The VIRCAM software will send SETUP commands to adjust processing control parameters Image analysis is then triggered by sending command ANASTAR vchoiaServer reads the image file obtains the image size from the database and the seeing value from the image file header The star X Y position in the focal plane and the positions of the pair of images on the d
13. 8 Tools for Automated Testing User Manual VLT MAN ESO 17200 0908 Issue 1 4 15 Feb 2001 RD9 Central Control Software User Manual VLT MAN ESO 17210 0619 Issue 2 4 31 Mar 2004 Data Interface Control Document GEN SPE ESO 19400 0794 Issue 2 0 21 May 2002 La RD10 2 OVERVIEW The HOWES has two main tasks AD6 The first one is to provide measurements used in building lookup tables that predict the shape of the primary mirror with any given altitude University of Durham eon ieee UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description and temperature The second one is to perform a Zero point calibration check once or twice during an observing night The HOWES is based on the curvature sensor principle AD1 AD2 and consequently requires two defocused images of a star The HOWFS will use the science detector arrays to acquire 1ts defocused images The defocused images will be produced by selecting a specially designed filter from the camera filter wheel A layout of the images produced by the HOWFS filter on one of the IR detector is shown in Figure 1 The positions of the HOWES filters in the filter wheel and the consequent positions of the curvature images on the focal plane are defined in AD8 The HOWES software will only be responsible for doing the image analysis The HOWFS softw
14. OWFS DARKFILE SETUP string File containing a dark image HOWFS FLATFILE SETUP string File containing a flat image rewscons eee ee eaan in with additional data A Pe stove les arog o above files are kept rowers A one pixels indicated HDR obscuration in X direction HDR obscuration in Y direction HDR Plane CO ordinates a ar HDR Plane co ordinates HDR defocused Image HDR defocused Image HDR second defocused Image HDR second defocused Image for the simplex algorithm the simplex algorithm CFG have been modified A A dime o analysed images converged A ER le MCP ea by e simplex University of Durham jea ford UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front E Sensor Software Design IR Camera Description CFG be applied YAA PAL were produced Table 7 Keywords needed by HOWFS software but defined by other subsystems KEYWORD_______ PURPOSE Type Units Comments _ _ DETCHIPID SETUP string Detector ID of this image _ __ VALIDEXT SETUP string ID of detector image that contains HOWFS images 11 APPENDIX B COEFFICIENTS TO FIT The following coefficients will be fitted using the simplex algorithm The actual polynomials are listed in AD4 o Tit 22 23 Ignore these modes pL Defocus A G O 2 Coma e 2 1 sin e 2 1 cos e 3 1 sin e 3 1 cos e 4 1 sin e 4 1 cos 6 22 if e 22 sin e 2 2 cos 7
15. WFS The HOWES software normally uses the expected null aberrations at a given point in the focal plane as the starting point for the simplex To do this the HOWFS software requires a file listing the values of null aberrations for each position on the focal plane at which a HOWEFS measurement will be made These positions are specified in ADS The null aberrations relevant to the current HOWFS measurement are sent to vchoiaServer If the values sent are different to those held in the file the nullModified flag see below should also be set When the analysis starts and if the startpntModifed flag see below is not set the null aberrations are copied to the starting point aberrations in the data base These are then the start point for the simplex University of Durham eon ieee UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description Various flags are provided to allow the analysis to be operated in a non standard way for engineering and commissioning applications Firstly the null aberrations may be manually specified In this case a flag nullModified 1s set to indicate that the database values differ from the null aberration file Secondly the starting point aberrations may be manually specified in the database A flag startpntModified is set to indicate that the start point is different to the null aberrat
16. are defined by specifying the centre of the first defocused image in pixels in X and Y and similarly for the second defocused image These positions are specified in the database entries setup data preCentre and setup data postCentre Figure 6 shows the orientation of the HOWES filter in one position The blue lighter shaded square represents the HOWFS filter while the green squares represent four of the IR detectors The image axis is not exactly parallel with the radius of the filter wheel but is set at an angle such that the axis of the centres of the two defocused images falls along the X axis of the selected detector for HOWFS positions where the Y University of Durham Rutherford UK Astronomical Instrumentation Group Appleton Laboratory Astronomy Technology Centre cLRc HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description offset from the centre of the focal plane is a minimum This has been exaggerated in the diagram which is not to scale Part of IR Camera Focal Plane Filte Wheel Radius Filter Wheel Axis First Defocused HOWFS Filter Image IR Camera Full Focal Plane O Figure 6 Orientation of the HOWFS Filter and Images University of Durham Rutherford UK Appleton Astronomical Instrumentation Group Laboratory carc Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description
17. are will be referred to as the VISTA Camera High Order Image Analysis or vchoia module from now on The process derived from this module will be known as vchoiaServer Selection of the appropriate filter and acquisition of the star will be performed by the OS through the ICS TCS and DCS modules Figure 2 shows the context of the HOWFS with respect to the other camera and telescope systems The template sequencer scripts will be responsible for despatching the appropriate commands to the image analysis process The DCS will store the acquired image in the Data Store as a FITS file The OS will then append data specific to the exposure to the header of the FITS file before 1t 1s actually processed by the HOWES software During analysis data will be logged using the CCS logging system RD9 Data produced from the analysis will also be stored in a coefficient file that can be processed offline to produce the lookup table which is used in open loop correction of the primary mirror HOWFS FILTER 2nd Defocus 1st Defocus Image Axis Defocused Images Figure 1 Layout of the images produced by the HOWFS filter on one of the IR detector Not to scale University of Durham Rutherford UK Astronomical Instrumentation Group Appleton Laboratory Astronomy Technology Centre cLRc HOWFSv3 4 doc Dates 12 April 2006 0002 High Order Wave Front VIS DES UOD 06048 0002 5 A Sensor Software Design Page 7
18. ceicoustveincceccossedesze anddessnwieusses avcte Senndcdecbosaddaccensuvett aincdecowmsecedeseveseswuntedes 4 1 3 APPLICABLE DOCUMENTS ica 4 1 4 REFERENCE DOCUMENTS cons 5 2 OVERVIEW iaa 5 3 WINDOWING AND CALIBRATION cccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccccsccoccees 8 4 OPERA TIONAL STA TE DB wissdesvcvccseadecccciscaveccecdncsacedeevscaschusaceassaveawecdacestedda vest seekisdasboneedncacgetss vacuwacedeavecnsaes 9 5 DATA DESCRIPTION isc sscaccaeencacanccacece da caeztacdcacaaesacacoeandeiatancessasdcncasadssucecusdaucaousacseaesudaacacerseussedueeeceeearer 10 5 1 DATABASE DEFINITIONS aa 10 5 2 START UP COEFFICIENTS FOR HOWES ccccccscecceccccccecceccsceccecceceecececcecsscescescessscescescesescuscasceseess 14 5 2 1 Null Abera ons T lO aa belo ace Es aaa eaaa aaa e n aa aiai 15 5 3 DETECTOR SETUP PARAMETERS ca o 15 5 4 COEFICIENTE PIDE EE E 17 6 COMMAND INTERFACE BETWEEN VCHOIA AND OBSERVATION SOFTWARE 18 7 INTERNAL CLASS DIAGRAMS FOR V CHOTA 2 cccccccccccccccccccccccccccccccccccccccccccceccccccccecs 19 8 DEPUOYVMEN Lor nos 22 9 TESTING ia ioia 22 10 APPENDIX A DATA DICTIONARY SPECIFICATIONS ccccccccsccccccccccccccccccccccccccccccccces 22 11 APPENDIX B COEFFICIENTS TO FIT cccccccccccccccccccccccccccccccccccccccccccccccccccccccccceccecces 25 12 APPENDIX C LOG FILES esesesssscscscscseseseseseseseseos
19. e components TAT will also configure temporary VLT environments in which to perform the tests With TAT it is possible to create a battery of tests which can be run each time the software is updated to make sure that any existing functionality is not lost TAT can make bugs identifiable by providing repeatable tests that show the occurrence of a specific error The module will be tested as follows 1 Typical images as observed by the HOWFS during operation will be provided for testing A mixture of simulated and experimental images from the lab will be used 2 Unsuitable images will be provided to see if they can be reliably rejected before starting a time consuming analysis process 3 Test cases for all the implemented commands will be provided 4 Pairs of simulated defocused images with known aberrations will be used to test the algorithm Test data will be saved within the vchoia module in the test subdirectory To save bandwidth during network module transfers this data may need to be compressed It can be uncompressed during a make within the test directory 10 APPENDIX A DATA DICTIONARY SPECIFICATIONS The ESO VLT software standard makes use of keyword dictionaries to define the meaning data type and format of keywords used within the software The relevant HOWES dictionary will be contained within the dicVIRCAM module The keywords listed in Table 6 are used during configuration of the software module CFG and setup p
20. e of mode in nm doubles Config Vector of Rotation angle of mode in degrees doubles Only applicable to symmetric modes setup data SS coeffFileName Name of file to contain fit coefficients Telescope altitude angle in degrees University of Durham ser ford UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front E Sensor Software Design IR Camera Description M1 mirror temperature in degrees C dimension in pixels dimension in pixels dimension in pixels dimension in pixels coordinates in mm coordinates in mm seeing Header double Seeing in arc seconds setup modes Strings integers integers Strings A Rotation angle in degrees Only applicable to symmetric modes fit simplexDiag relativeTolerance Status double Relative tolerance between best and worst solutions on completion iterationCount Number of iterations used funEvalsCount Number of function evaluations used Time taken for fit in seconds successFlag Status Boolean Flag to indicate if simplex analysis was ase fee completed within maximum number of iterations and function evaluations thresholdActive Setup Boolean If flag set to true an error occurs if the total intensity is less than the threshold Status Integer Highest pixel value in both images totalIntensity Status Integer Total intensity of all pixels in both images threshold Setup Integer Threshold
21. etector are taken from the database vchoiaServer then starts the analysis process and returns a unique ID straight away to the Sequencer or an error FAILED on error While analysis is taking place the Observation Software can query vchoiaServer to see if analysis has been completed using the CHECK command Alternatively the Observation Software can issue the WAIT command and a reply will be sent back as soon as the analysis completes University of Durham eon ieee UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description evhSIMPLE_TASK evhDB_TASK amoeba evhSTD_COMMANDS vchoiaSetup vchoiaServer polySearch 1 V vchoiaCMDS polyTables _ rayTracer Figure 7 Class hierachy within the vchoia module Laboratory Astronomy Technology Centre University of Durham Rutherford UK Astronomical Instrumentation Group Appleton cLRc HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description SETUF 2 INITIALISE Image pairs and fitness L IOK calculations will be ee repeated as many times 4 0K as necessary by the ds Simplex algorithrr l l
22. ions The simplex algorithm can be a very slow process To aid convergence this latter facility is provided to allow the simplex algorithm to be started close to the expected results Thirdly the relevant null aberrations will not be subtracted from the result if the nullSubtract flag is reset 5 2 1 Null Aberrations File The null aberrations sent to vchoiaServer are read from a null coefficients file This file lists the values of null aberrations for each position in the focal plane at which a HOWFS measurement may be made The format of the file will be that of an ASCII text table Each row of the table will correspond to a HOWES position The columns of the table are listed in Table 2 The initial version of this file will be populated with values resulting from modelling The table will be updated during commissioning to contain relevant values for the optical systems as built Table 2 Columns in the Null Aberrations file ASCII text table Parameter Type Description Name X coordinate in the focal plane in mm Y coordinate in the focal plane in mm modulusO Modulus of aberration mode 0 in nm Rotation angle of aberration mode 0 in degrees Modulus of aberration mode in nm Rotation angle of aberration mode in degrees modulus n 1 Modulus of aberration mode n 1 in nm angle n 1 Rotation angle of aberration mode n 1 in degrees 5 3 Detector Setup Parameters The position of the images on the science detector
23. lag attribute to confirm CHECK Returns non zero ID if busy else 0 SETUP Set the specified parameters to the specified values The keywords available for configuration are listed in Table 6 function lt keyword gt lt value gt Define a list of keywords lt keyword gt lt value gt and values to be assigned file lt filename gt Define a file containing a list of keywords and values to be interpreted Standard Commands Returns state as lt string gt Returns the status as STATE state substate Returns status as lt string gt Returns OK Returns OK Returns OK Returns OK OFF Switch to OFFLINE state Returns OK Return the vchoia module version Returns version as lt string gt Terminate the process Shutdown the process cleanly VERSION sifa lls Laboratory Astronomy Technology Centre University of Durham Rutherford UK Astronomical Instrumentation Group Appleton cLRc HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description po Returns OK 7 INTERNAL CLASS DIAGRAMS FOR VCHOIA The interface of module vchoia will be developed using the EVH toolkit RD4 Figure 7 shows the hierarchical class structure of the module This design hierarchy is loosely based on that of the TCS auto guider workstation module described in RD5 Class vcho1aCMDS will handle all the VLT standard commands The default implementations provided by the evhSTD COMMANDS
24. o change to the BUSY state during a SETUP o BUSY Processing is taking place The process cannot accept a new ANASTAR or SETUP command and they will return an error The process returns to the IDLE sub state when it has finished processing A STOP or ABORT command can be used to abort the processing and return to the IDLE state immediately Figure 4 shows the state chart of process vcholaServer Laboratory Astronomy Technology Centre University of Durham Rutherford UK Astronomical Instrumentation Group Appleton cLRc HOWFSv3 4 doc VIS DES UOD 06048 0002 0002 High Order Wave Front Sensor Software Design IR Camera Description Startup Start Environment EXIT Start vchoiaServer ABORT STOP ONLINE ANASTAR Finish eS Config file Start vchoiaServer STANDBY ONLINE Figure 4 Operational States of process vchoiaServer 5 DATA DESCRIPTION 5 1 Database Definitions A database that represents the internal state of the vchoiaServer process is setup as shown in Figure 5 The database is loosely based on the VLT software active optics design described in RD2 Table 1 provides additional information on the objects listed in the database Laboratory Astronomy Technology Centre University of Durham Rutherford UK Astronomical Instrumentation Group Appleton cLRc HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description status State
25. ososcscscseseseseseoeosososososesesessososososcseseseseseseseosssseseseseseos 25 University of Durham Rutherford UK Astronomical Instrumentation Group Appleton Laboratory circ Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description 1 INTRODUCTION 1 1 Scope This document describes the design of the HOWFS software This includes the interface of the HOWEFS to the Observation Software OS modules of the VISTA IR Camera software hereafter referred to as the VIRCAM software 1 2 Acronyms and Abbreviations BOSS Base Observation Software Stub CCS Central Control Software DCS Detector Control Software EVH Event Handler Toolkit FITS Flexible Image Transport System HOWFS High Order Wavefront Sensor ICS Instrument Control Software OS Observation Software ROI Region of Interest TAT Tools for Automated Testing TCS Telescope Control System VCHOIA Vista Camera High Order Image Analysis VLT Very Large Telescope 1 3 Applicable Documents AD1 Wavefront Sensors Subsystem Design VIS DES UOD 06042 0001 Issue 3 0 8 Mar 2004 AD2 Wavefront Sensors Subsystem Design Delta PDR VIS TRE UOD 06042 0004 Issue 1 0 22 May 2003 AD3 VISTA IR Camera Observation Software Design Description VIS DES ATC 06082 0001 Issue 3 2 24 Feb 2005 AD4 Actuator Patterns Quasi Zernikes and Vibration Mode on the Primary Mirror VIS TRE ATC 02020 0005 Issue 1 0 15 January
26. re for efficiency a Date and time when analysis was performed The final relative tolerance value produced by the simplex algorithm Number of iterations performed by the simplex algorithm HOWFS SUCCESS Indicator to show whether simplex fit was successful HOWFS ACTIVE Vector of The active modes vector Booleans HOWFS STARPOS X X position of star in focal plane coordinates in mm HOWFS STARPOS Y Y position of star in focal plane coordinates in mm HOWFS DETANGLE Angle of camera with respect to telescope in degrees University of Durham eon ieee UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description 6 COMMAND INTERFACE BETWEEN VCHOIA AND OBSERVATION SOFTWARE The commands listed in Table 4 are those which will be sent from the sequencer scripts to the vcholaServer process Table 4 Commands accepted by the vchoia process Command Optional Parameters Description ANASTAR Start image analysis and return straight away with a string containing a unique ID starting at 1 or FAILED on error Returns ID lt string gt WAIT id lt id gt If lt id gt does not match current ID or on error returns ERROR If BUSY waits for analysis to complete and then returns OK If IDLE returns OK straight away Note OK does not guarantee that the Simplex converged Check the fit simplexDiag successF
27. rior to an analysis SETUP The keywords are designed to meet the requirements of RD10 Some of the SETUP keywords will be embedded in the FITS header of the image file and these have been marked as HDR By logging some of these parameters in the image file University of Durham eon ieee UK Astronomical Instrumentation Group ppleton Laboratory CRE Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front E Sensor Software Design IR Camera Description header the analysis can be run at any time The HDR keywords represent metadata about the image which is produced when the image is acquired and will therefore remain unchanged throughout the existence of the image The keywords used in the ESO FITS file have to comply with ESO s extended hierarchical FITS keywords A straight forward conversion can be performed on the keywords marked as HDR to derive the ESO compliant FITS keywords Two examples are given in Table 5 Table 5 Converting from setup keywords to ESO s Hierarchical FITS keywords SETUP KEYWORD ESO EXTENDED HIERARCHICAL FITS KEYWORD HOWFS OBSOFFX HIERARCH ESO INS HOWFS OBSOFFX HOWFS STRTPNT MODMODE3 HIERARCH ESO INS HOWFS STRTPNT MODMODE3 The SETUP command of vchoia will parse all three types of keywords During configuration the keywords will normally be passed through a file rather than on an individual basis The keywords in the header of the image file will override any previous value sent thro
28. ross referenced DICB table 5 Inserted INS subsystem keyword in conversion table 6 Made all keywords fits compliant table7 Added table to indicate keywords defined by other sub systems but used by HOWFS software section 11 Commands will be logged in engineering log 30 22702005 02 05 Various Major update after Durham ATC meeting of 17 Feb 05 mer 10 03 06 Multiple changes to match actual code 3 3 5 04 06 Figure 5 NullFile no longer held in database Table 1 section 5 2 1 Null Aberrations 3 4 12 04 06 Figure 2 and Corrected figures provided by Steven Beard Figure 3 NOTIFICATION LIST The following people should be notified by email that a new version of this document has been issued and is available on the IR Camera document database RAE M Caldwell K Ward G Dalton ATC S Beard J M Stewart Durham P Clark N Dipper E Younger Laboratory Astronomy Technology Centre University of Durham Rutherford UK Astronomical Instrumentation Group Appleton CLR HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description TABLE OF CONTENTS CHANGE RECORD sesssscsesesesesesesesesessososcscsesoseseseseseoeososososcscseseseseseseseseseoscscseseseseseseseseoeososososeseseseseseseseseseseses 2 NOFIFICATION LIS Teenei EEEa 2 1 INTRODUCTION coincido ENERET EDERE NETA ETETEN EE EDEA A erR 4 1 1 OO N E E A EE E sein she se bre ee EA EA E EE A Go E AN E E Set ak E AE N 4 1 2 ACRONYMS AND ABBREVIATIONS i i
29. ugh the SETUP commands The vchoia module will also make use of keywords defined by other subsystems These are listed in Table 7 Table 6 Keywords used by the HOWFS software PURPOS KEYWORD E Type Comment HOWFS PUPDIA HOWFS DEFOCUS respect to pupil diameter HOWFS IMGSIZE integer pixels O S HOWFS PIXSIZE HOWFS INTRATIO double Intensity Ratio between IS defocused images due to beam splitter raytracer in pixels HOWFS SUBGDSZ PE E ee HOWFS NAMEMODi string Nameofmodetofit HOWFS TYPEMODi i Type of mode Zernike or Elastic cos and sin terms HOWFS ORDMODi integer _ Orderofmode HOWFS NULLFILE ep File containing null values for the aberrations against radius have been modified results HOWFS NULLABER MODMODEi CFG double nm Modulus of null aberration sevup P meget ee Y University of Durham Rutherford UK Astronomical Instrumentation Group Appleton Laboratory circ Astronomy Technology Centre HOWFSv3 4 doc VIS DES UOD 06048 0002 0002 High Order Wave Front Je Sensor Software Design IR Camera Description SETUP i Ae Se Vao Relate Tolereno SETUP POSO A acnievea by me simples achieved by the simplex oee e e e on SETUP simplex algorithm ITR HDR Final iteration count a the er Disco OOO PREBLUR CFG logical T F Flag to indicate whether SETUP observed images must be blurred HOWFS USEMODi SETUP Indicator to fit mode HOWFS IMGFILE SETUP a File containing defocused images H
30. yisth Visible amp Infrared Survey Telescope for Astronomy IR CAMERA Document Title High Order Wave Front Sensor Software Design Description Document Number VIS DES UOD 06048 0002 Issue 3 4 Date 12 April 2006 Document Nigel Dipper Signature Prepared By Software Engineer and Date Document Steven Beard Signature Approved By IR Camera Software Manager and Date Paul Clark WES Work Package Manager Document Kim Ward Signature Released By IR Camera Project Manager and Date The information contained in this document is strictly confidential and is intended for the addressee only The unauthorised use disclosure copying alteration or distribution of this document is strictly prohibited and may be unlawful University of Durham ge erence UK Astronomical Instrumentation Group ppleton Laboratory came Astronomy Technology Centre HOWFSv3 4 doc 0002 High Order Wave Front Sensor Software Design IR Camera Description CHANGE RECORD Section s Description of Change Change Request Affected Reference Remarks om sid Ret T 2 0 04 03 04 section 1 4 Added reference to DICB figure 2 Updated to improve pdf output figure 4 Replaced substates CONFIG and PROCESSING with single state BUSY section 4 3 Corrected typo CCD gt science detector figure 7 Updated class hierarchy diagram section 7 Module vemcfg will store config data section 8 Third party software references removed section 9 C
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