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Data Flow System

Document Title: Document Number: Issue: Date:
Document Prepared by: Document Approved by: Document Reviewed by: Document Released by: Peter Bunclark & Simon Hodgkin (CASU) Mike Irwin (CASU Manager) William Sutherland (VISTA Project Scientist) Jim Emerson (VDFS Project leader)

VISTA Infra Red Camera Calibration Plan VIS-SPE-IOA-20000-0002 1.4 pre 1 2006-11-13
Signature And date: Signature And date: Signature And date: Signature And date:


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Change Record
Issue 0.5 1.0 1.1 1.2 1.3 Date 2004-04-08 2004-12-15 2005-05-03 2005-05-11 2006-09-28 Sections All All All All All Remarks New Document FDR release post-FDR revision Final FDR fixes Rework of photometry reflecting WFCAM experience, procedure changes following pipeline prototyping, hardware references following actual build details. QC table

1.4pre 1

2006-11-13

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Notification List
The following people should be notified by email that a new issue of this document is available. IoA: RAL: QMUL ATC W Sutherland G Dalton J Emerson Malcolm Stewart Steven Beard


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Table of Contents
Change Record ............................................................................................................... 2 Notification List ............................................................................................................. 3 Table of Figures ............................................................................................................. 6 1 Introduction ............................................................................................................ 7 1.1 Purpose ........................................................................................................... 7 1.2 Scope .............................................................................................................. 7 1.3 Applicable Documents ................................................................................... 7 1.4 Reference Documents .................................................................................... 8 1.5 Abbreviations and Acronyms ........................................................................ 8 1.6 Glossary ......................................................................................................... 9 2 Overview .............................................................................................................. 11 2.1 Hardware ...................................................................................................... 11 2.2 Observing Modes ......................................................................................... 14 2.2.1 Imaging Mode Description .................................................................. 14 2.2.2 Calibrations .......................................................................................... 14 2.2.3 High Order Wave Front Sensor (HOWFS) Mode ............................... 14 2.2.4 Calibrations .......................................................................................... 15 2.3 Pipeline ........................................................................................................ 15 2.4 Operation...................................................................................................... 15 3 Calibration Accuracy ........................................................................................... 17 3.1 Overview ...................................................................................................... 17 3.2 Astrometric Error ......................................................................................... 17 3.3 Photometric Error......................................................................................... 17 3.3.1 RMS ......................................................................................................... 18 3.3.2 Additive systematics ................................................................................ 18 3.3.3 Multiplicative systematics ....................................................................... 18 3.3.4 Extinction monitoring .............................................................................. 19 4 Calibration Data for Instrumental Signature Removal ........................................ 20 4.1 Purpose ......................................................................................................... 20 4.2 Reset Frames ................................................................................................ 22 4.3 Dark Frames ................................................................................................. 22 4.4 Dome flats .................................................................................................... 23 4.5 Detector Noise ............................................................................................. 24 4.6 Linearization Measurements ........................................................................ 24 4.7 Twilight Flats ............................................................................................... 25 4.8 Illumination Correction Measurement ......................................................... 26 4.9 Image Persistence Measurements ................................................................ 27 4.10 Electrical Cross-Talk Measurements ........................................................... 27 5 Data for Photometric Calibration ......................................................................... 29 5.1 Introduction .................................................................................................. 29 5.2 Calibration from 2MASS ............................................................................. 29 5.3 Calibration from Standard Star Fields ......................................................... 29 5.4 Standard Fields............................................................................................. 31 6 Calibration Data Derived from Science Data ...................................................... 32 6.1 For Instrument Signature Removal .............................................................. 32


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6.1.1 Night-Sky Maps ................................................................................... 6.1.2 Sky Subtraction and Fringe Removal .................................................. 6.1.3 Jittering ................................................................................................ 6.1.4 Microstepping ...................................................................................... 6.2 For Astrometric Calibration ......................................................................... 6.2.1 Optical Distortion Effects .................................................................... 6.2.2 Final WCS Fit ...................................................................................... 7 Quality Control .................................................................................................... 7.1 Further Quality Control Data Derived from Science Frames ...................... 7.1.1 Object Extraction ................................................................................. 7.2 On line quality control (QC-0) ..................................................................... 7.3 Quality Control Parameters.......................................................................... 8 Templates ............................................................................................................. 8.1 Imaging Calibration Templates.................................................................... 8.1.1 Reset ..................................................................................................... 8.1.2 Dark...................................................................................................... 8.1.3 Dark Current ........................................................................................ 8.1.4 Acquire Dome Screen .......................................................................... 8.1.5 Dome Flat............................................................................................. 8.1.6 Detector Linearity ................................................................................ 8.1.7 Noise and Gain ..................................................................................... 8.1.8 Acquire Twilight Field ......................................................................... 8.1.9 Twilight Flat......................................................................................... 8.1.10 Persistence............................................................................................ 8.1.11 Astrometric Calibration ....................................................................... 8.1.12 Photometric Calibration Standard Fields ............................................. 8.1.13 Quick look ............................................................................................ 8.1.14 Cross-talk ............................................................................................. 8.1.15 Illumination .......................................................................................... 8.2 HOWFS mode calibration............................................................................ 8.2.1 HOWFS Acquire Dome Screen ........................................................... 8.2.2 HOWFS Reset ...................................................................................... 8.2.3 HOWFS Dark....................................................................................... 8.2.4 HOWFS Dome Flat.............................................................................. 8.3 Imaging Mode Science Templates ............................................................... 8.3.1 Acquire ................................................................................................. 8.3.2 Observe Paw ........................................................................................ 8.3.3 Observe Tile ......................................................................................... 8.3.4 Observe Offsets .................................................................................... 8.3.5 Observing a set of Tiles ....................................................................... 8.4 HOWFS mode data ...................................................................................... 8.4.1 HOWFS Acquire .................................................................................. 8.4.2 HOWFS Wave front ............................................................................ 8.4.3 HOWFS Expose ................................................................................... 8.5 Instrument Health Templates ....................................................................... 9 Technical Programs ............................................................................................. 9.1 TP-VIS1: Establishment of Secondary Standard Fields .............................. 10 Format of Data Frames ....................................................................................

32 32 33 34 34 34 35 37 37 37 37 38 43 47 47 47 47 47 47 48 48 48 49 49 50 50 50 50 51 51 51 51 52 52 52 52 53 54 55 55 56 56 56 56 57 58 58 60


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10.1 Principle ....................................................................................................... 10.2 Model FITS header ...................................................................................... Appendix A. 2MASS calibration Fields ................................................................ 11 Index ................................................................................................................

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Table of Figures
Figure 2-1 VISTA Focal plane: Each of the 4 groups of detectors in the Y direction (e.g. #s 1-4, 5-8, 9-12, 13-16) is read out by a separate IRACE controller. ........ Figure 2-2 VISTA Engineering Pawprint. ................................................................... Figure 2-3 Filter Transmission Curves for Reference Samples of Y, J, H, and Ks bands. ................................................................................................................... Figure 4-1 Cascade Diagram for producing Calibration Frames ................................. Figure 8-1 Hierarchy of VISTA IR Camera Templates............................................... Figure 8-3 Pre-selected twilight fields ......................................................................... Figure 9-1 Distribution of the 2MASS touchstone fields on the sky ........................... Table 10-1 FITS Example Header ............................................................................... 11 12 13 21 43 49 58 70


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1 Introduction
1.1 Purpose
This document forms part of the package of documents describing the Data Flow System for VISTA, the Visible and Infrared Telescope for Astronomy. As stated in [AD1] "The Calibration Plan is the prime document which describes the different instrument-specific components of the Data Flow System".

1.2 Scope
This document describes the VISTA DFS calibration plan for the output from the 16 Raytheon VIRGO IR detectors in the (Infra Red) camera for VISTA. The baseline requirements for calibration are included in the VISTA DFS Impact Document [AD2]. The major reduction recipes and algorithms to be applied to the data are described in the VISTA DFS Data Reduction Library Design [RD1]. Each camera exposure will produce a `pawprint' consisting of 16 non-contiguous images of the sky, one from each detector. The VISTA pipeline will remove instrumental artefacts, combine the pawprint component exposures offset by small jitters, and photometrically and astrometrically calibrate each pawprint. It will also provide Quality Control measures. It will not combine multiple adjacent pawprints into contiguous filled images, nor stack multiple pawprints at the same sky position. This document does not describe any calibrations or procedures relating to the CCD detectors that are also located within the camera and which interact with the Telescope Control System. This document covers only the Routine Phase of operations of VISTA's IR Camera. In particular it does not describe any calibrations or procedures that form part of the Commissioning Plan for VISTA, nor any procedures needed during routine Engineering Maintenance. [Except for HOWFS observations, which are made using the science detectors, and passed to the science archive.] Arrangements for processing any calibrations or procedures carried out under such categories are the responsibility of the VISTA Project Office.

1.3 Applicable Documents
The following documents, of the exact issue shown, form part of this document to the extent specified herein. In the event of conflict between the documents referenced herein and the contents of this document, the contents of this document shall be considered as a superseding requirement. [AD1] Data Flow for the VLT/VLTI Instruments Deliverables Specification, VLTSPE-ESO-19000-1618, issue 2.0, 2004-05-22. [AD2] VISTA Infra Red Camera DFS Impact, VIS-SPE-IOA-20000-00001, issue 1.3, 2005-12-25. [AD3] VISTA Infrared Camera Data Flow System PDR RID Responses with PDR Panel Disposition, VIS-TRE-IOA-20000-0006 issue 1.0


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[AD4] VISTA Infrared Camera Data Flow System FDR RID Responses VIS-TREIOA-20000-0013 issue 1.0 2005-12-25

1.4 Reference Documents
The following documents are referenced in this document. [RD1] VISTA Infra Red Camera Data Reduction Library Design, VIS-SPE-IOA20000-0010, issue 1.3, 2006-01-31. [RD2] Data Interface Control Document, GEN-SPE-ESO-19940-794, issue 3, 200502-01. [RD3] VISTA Operational Concept Definition Document, VIS-SPE-VSC-00000-0002 issue 1.0, 2001-03-28 [RD4] VISTA Infrared Camera Technical Specification, VIS-SPE-ATC-06000-0004, issue 2.0, 2003-11-20 [RD5] VISTA IR Camera Software Functional Specification, VIS-DES-ATC-0608100001, issue 2.0, 2003-11-12. [RD6] IR Camera Observation Software Design Description, VIS-DES-ATC-060840001, issue 3.2, 2005-02-24. [RD7] VISTA Science Requirements Document, VIS-SPE-VSC-00000-0001, issue 2.0, 2000-10-26 [RD8] A Global Photometric Analysis of 2MASS Calibration Data, Nikolaev et al., Astron. J. 120, 3340-3350, 2000 [RD9] 2MASS Calibration Scan Working Databases and Atlas Images, http://www.ipac.caltech.edu/2mass/releases/allsky/doc/seca4_1.html [RD10] A New System of Faint Near-Infrared Standard Stars, Persson et al., Astrophys. J. 116, 2475-2488, 1998 [RD11] JH standard stars for large telescopes: the UIRT Fundamental and Extended lists, Hawarden et al., Mon.Not.R.Soc. 325, 563-574,2001 [RD12] The FITS image extension, Ponz et al, Astron. Astrophys. Suppl. Ser. 105, 53-55, 1994 [RD13] Representations of world coordinates in FITS, Griesen, & Calabretta, A&A, 395, 1061.2002 [RD14] Representations of celestial coordinates in FITS, Calabretta & Griesen, A&A, 395, 1077, 2002 [RD15] Overview of VISTA IR Camera Data Interface Dictionaries, VIS-SPEIOA-20000-0004, 0.1, 2003-11-13 [RD16] Northern JH Standard Stars fro Array Detectors, Hunt et al Astr.J 115, 2594, 1998

1.5 Abbreviations and Acronyms
2MASS CDS DAS DFS FITS HOWFS ICRF 2 Micron All Sky Survey Correlated Double Sampling Data Acquisition System Data Flow System Flexible Image Transport System High Order Wave-Front Sensor International Coordinate Reference Frame


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IMPEX IR IWS LOWFS OB OS OT PI QC-0 QC-1 SDT TCS URD VDFS VIRCAM VISTA VPO WCS WFCAM ZPN

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Import Export (P2PP ASCII files) Infra Red Instrument Workstation Low Order Wave-Front Sensor Observation Block Observing System Observing Tool Principal Investigator Quality Control, level zero Quality Control, level one Survey Definition Tool Telescope Control System User Requirements Document VISTA Data Flow System VISTA Infra Red Camera Visible and Infrared Survey Telescope for Astronomy VISTA Project Office World Coordinate System Wide Field Camera (on UIRT) Zenithal Polynomial

1.6 Glossary
Confidence Map An integer array, normalized to a median of 100% which is associated with an image. Combined with an estimate of the sky background variance of the image it assigns a relative weight to each pixel in the image and automatically factors in an exposure map. Bad pixels are assigned a value of 0, 100% has the value 100, and the maximum possible is 32767 (negative values are reserved for future upgrades). The background variance value is stored in the FITS header. It is especially important in image filtering, mosaicing and stacking. DIT Digital Integration Time. Separate readouts are summed digitally. Exposure The stored product of many individual integrations that have been co-added in the DAS. Each exposure is associated with an exposure time. Integration A simple snapshot, within the DAS, of a specified elapsed time DIT seconds. This elapsed time is known as the integration time. Jitter (pattern) A pattern of exposures at positions each shifted by a small movement (<30 arcsec) from the reference position. Unlike a microstep the non-integral part of the shifts is any fractional number of pixels. Each position of a jitter pattern can contain a microstep pattern.


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Mesostep A sequence of exposures designed to completely sample across the face of the detectors in medium-sized steps to monitor residual systematics in the photometry. Microstep (pattern) A pattern of exposures at positions each shifted by a very small movement (<3 arcsec) from the reference position. Unlike a jitter the non-integral part of the shifts are specified as 0.5 of a pixel, which allows the pixels in the series to be interleaved in an effort to increase sampling. A microstep pattern can be contained within each position of a jitter pattern. Movement A change of position of the telescope that is not large enough to require a new guide star. Offset A change of position of the telescope that is not large enough to require a telescope preset, but is large enough to require a new guide star. Pawprint The 16 non-contiguous images of the sky produced by the VISTA IR camera, with its 16 non-contiguous chips (see Figure 2-2). The name is from the similarity to the prints made by the padded paw of an animal (the analogy suits earlier 4chip cameras better). Preset A telescope slew to a new position involving a reconfiguration of the telescope control system and extra housekeeping operations that are not necessary for a movement or an offset. Tile A filled area of sky fully sampled (filling in the gaps in a pawprint) 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 would expose each piece of sky, away from the edges of the tile, to at least 2 camera pixels. The pipeline does not combine pawprints into tiles.


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2 Overview
2.1 Hardware
VISTA is a wide field alt-az telescope designed for a single purpose, surveys, and which does not have a conventional focus. It can only be used with a purpose built camera, and is delivered with an IR camera. Thus it is the performance and pointing of the telescope-camera system that is important. The telescope by itself front sensing. The IR Autoguider CCDs and two CCDs, operating in has no capability to lock onto a guide star or carry out wave Camera therefore contains, as well as 16 IR detectors, two two low order wave front sensor (LOWFS) units, each with the I band, as shown in Fig 2-1. Two autoguiders, on opposite

+Y

+X

Figure 2-1 VISTA Focal plane: Each of the 4 groups of detectors in the Y direction (e.g. #s 1-4, 58, 9-12, 13-16) is read out by a separate IRACE controller.


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edges of the focal plane, are used in order to meet the sky coverage requirements, although only one is allowed to apply corrections to the telescope axes at any given time. The LOWFSs measure aberrations that are used by the external active optics control process to adjust the position of the 5 axis (x, y, z, tip, tilt) secondary mirror support system and some aspects of the M1 surface to maintain image quality. The LOWFS operates roughly every 1 minute during tracking and needs exposures of ~40 sec to average out seeing effects. Although the Autoguiders and LOWFSs are physically located within the IR camera, both are considered part of the TCS from a software point of view. This is primarily to maintain consistency with existing VLT software and standards. The VISTA pipeline receives no data from these CCDs. The

Figure 2-2 VISTA Engineering Pawprint.


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CCDs therefore do not impact on the VISTA pipeline, except in so far as the pointing and image quality of the camera are dependent on their proper operation. A high order wave front (curvature) sensor (HOWFS) uses some of the science detectors to determine occasional adjustments to the primary mirror support system. (This is done perhaps once at the start of the night and once around midnight.) Processing the signals from the HOWFS is done within the Instrument Workstation, and so the pipeline will not have to deal with the HOWFS at all. However all data from the IR detectors, including HOWFS data, is passed to the science archive, so the necessary calibration templates for the HOWFS are covered here. Within the IR Camera are 16 Raytheon 2048x2048 VIRGO detectors arranged in a sparse array. Each camera exposure produces a pawprint consisting of 16 noncontiguous images of the sky. An example display of a complete FITS file consisting of a VISTA "pawprint" is shown in Figure 2-2. The VISTA IR camera has only one moving part, the filter wheel which has 8 filter holders, each filter holder containing 16 filters, one for each IR detector. There are further auxiliary (beam splitting) filters for use with the high order wave front sensor.

Figure 2-3 Filter Transmission Curves for Reference Samples of Y, J, H, and Ks bands.

One of the filter holders contains a set of completely block the detectors from incoming thermal emission) which are used for taking delivered with 6 filter sets (Z, Y, J, H, s and

16 cold blanks (metal units which sky radiation, and produce negligible dark frames. The instrument will be a narrow-band at 1.185 - Figure 2-3)


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and a further set of cold blanks, which can be replaced with other filters in due course. The position angle of the camera axis can be controlled by the instrument rotator. Single integrations are taken by a Reset-Read-Read procedure with the difference of the two Reads being performed within the DAS.

2.2 Observing Modes
IMAGING is the only mode in which science data will be acquired, but the science array is used to acquire data for internal wave-front analysis.

2.2.1 Imaging Mode Description
The sky target position is acquired and tracked and in parallel (for observing efficiency) the required filter set is placed in the beam. The LOWFS provides the necessary updates to the M2 and M1 support units. A set of exposures, each of which may consist of a number of integrations, are taken and are usually jittered by small offsets, to remove bad pixels and determine sky background. The set of exposures produced is combined in the pipeline to create a single pawprint, in which the jitters from all detectors are included.

Six such pawprints, taken at appropriate offsets, can be combined to produce an almost uniformly sampled image of a contiguous region, each bit of sky, except at the edges, having been observed by at least two pixels. The individual exposures making up each pawprint may be made on a jitter or a microstep pattern. Microstep patterns are interleaved rather than combined, so the calibration procedures are unchanged, though the data volume increases.

2.2.2 Calibrations
The calibrations are of four sorts: i. those that characterize the properties of the transfer function (image in, electrons out) of the end-to-end system (telescope, camera, IR detector system including associated controllers, etc.) so that instrumental effects can be removed from the data. As VISTA has a wide field of view, particular attention must be paid to variations across the field; ii. those that characterize the astrometric distortions of the images; iii. those that characterize the photometric zero points and extinction coefficients corresponding to the images; iv. those that generate Quality-Control measures.

2.2.3 High Order Wave Front Sensor (HOWFS) Mode
The HOWFS mode is processed in the Instrument Workstation and is logically part of the TCS. However, as it uses the IR detectors, all of whose data are passed to the archive, it is considered as a separate observing mode for VISTA pipeline purposes.


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In HOWFS mode a special beam-splitting filter is used to make a curvature sensor in which two images (above and below focus) of a reference star are formed and used to generate corrections to the forces in the M1 support unit, ensuring the mirror figure is maintained. This mode will typically be used of order twice a night (start and around midnight), or less often if the repeatability of the lookup table is good.

2.2.4 Calibrations
The HOWFS uses some of the science mode IR detectors, but has a special beam splitting filter whose unique signature needs to be removed from the HOWFS data before it can be analysed. However, this flat-fielding is carried out within the HOWFS image-analysis software (which is part of the Camera Software) and not by the pipeline, and is noted here for completeness.

2.3 Pipeline
The VISTA pipeline will produce photometrically and astrometrically calibrated pawprints, with instrumental artefacts removed. In order to achieve almost uniform coverage of a full contiguous area of sky, a six point offset pattern is used by default. A template that implements this pattern is defined and the pipeline will calibrate the resulting six pawprints individually. The further step of combining these into a contiguous map is left to the science user. For certain science programs the OS will allow distinct OBs for eventual "PI" processing; the main example of this would be observing offset sky frames to calibrate the sky in extended-object science frames. The QC pipeline is not required to associate such observations, but will perform routine reductions on such data. Other processes which are not calibration issues, but which may nevertheless relate to achievable data quality, are not discussed here. Such (excluded) processes include: · co-addition of individual integrations of a pawprint into a single exposure within the data-acquisition system; · combination of many pawprints to cover contiguous areas of sky; · co-addition of many pawprints to go deeper.

2.4 Operation
This section defines the observing modes, Section 3 contains an error discussion, Section 4 describes the calibration data required for instrumental signature removal, Section 5 describes the calibration data required for photometric calibration. Section 6 describes the calibration data to be derived from science data, including astrometric calibration. Section 7 discusses Quality Control measures based on regularly measured selected sets of calibrations for the purpose of instrument "health checks". Section 8 describes all templates and Section 9 the Technical Programs. Finally Section 10 details the Format of Data Frames. The philosophy throughout is that the VISTA pipeline will be triggered by the completion of each template. In the case of a template aborting, the pipeline will process as far as possible with the available data. The content of the FITS headers


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allow the VISTA pipeline to handle the set of observed files as an ensemble and to choose appropriate processing based on the header information.


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3 Calibration Accuracy
3.1 Overview
The error budgets for the astrometric, photometric and flat-fielding requirements have two generic components, systematic and random, that contribute to the overall errors. We discuss each in turn and indicate how the requirements will be met by the strategy adopted.

3.2 Astrometric Error
The astrometric calibration will be based on the 2MASS PSC. 2MASS astrometry is derived from direct calibration to TYCHO 2 and is in the ICRS system. [Note that this requires RADECSYS = 'ICRS' in the FITS headers]. It is known to have average systematic errors better than ~100mas and RMS errors better than ~100mas, for all point sources with S:N > ~10:1 [AD2]. We will be using 2MASS as the primary astrometry calibrator and in tests on similar mosaic instruments we have shown that our suggested ZPN distortion model, combined with a linear plate solution for each detector, achieves astrometric calibration at the 100mas or better level. The initial WCS will be based on the known detector characteristics (scale, orientation, focal plane position) and telescope pointing information (tangent point of optical axis on sky). The astrometric refinement algorithm will be based on a standard proven method we have developed for optical mosaic cameras and as such will be capable of automatically converging from starting points as far off as an arcmin. However, after commissioning updates we do not anticipate the initial WCS to be this inaccurate, since this level of accuracy is significantly larger than the combined error budget for the alignment of the various system components [RD4]. Further reduction in the internal astrometric systematics beyond 100mas may be possible by monitoring generic trends in the astrometric solution residuals, but this is out-with the scope of this document.

3.3 Photometric Error
The photometric calibration for VISTA will be measured in two ways: · The initial photometric calibration for all filters will be based on the 2MASS PSC. The 2MASS photometric system is globally consistent to ~1% (Nikolaev et al. 2000). This approach will enable each detector image to be calibrated directly from the 2MASS stars that fall within the field of view. Experience with WFCAM indicates that this approach will result in a photometric calibration to better than 2% for VIRCAM. A network of standard star fields will be observed periodically throughout each night (approximately every 2 hours). These data will enable an independent calibration to be made on a nightly basis. These touchstone fields will provide important information on the stability of VIRCAM, and will be used to measure any intra-detector spatial systematics.

·


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3.3.1 RMS
The error budget for photometry of astronomical sources requires photon noise to be the dominant noise source. For this to be the case, integration times should be chosen such that observations are general sky noise limited, i.e. sky noise should be much greater than RMS readout noise and dark current contributions. Clearly, this places a comparable requirement on the RMS contribution from flat fielding. However, providing the master flats used for this are combined from multiple observations with at least a total of 100,000 detected electrons this is easily achievable. In practice a goal of 0.1% RMS flat field noise due to photon noise contribution is the aim.

3.3.2 Additive systematics
More difficult problems to quantify are the systematics present in the various correction stages due to, for example, changing flat-field characteristics, reset anomalies, unexpected background variation and so on. The additive components of these systematics can be dealt with using a background tracking algorithm which effectively monitors and removes background variations to the level of 0.1% of sky, prior to performing object photometry. This will be part of the catalogue generation software. Subsequent derived object catalogues are therefore relatively insensitive to variations in any additive component provided such variations smoothly change over the image with typical scale length ~ 20 arcsec or greater. Abrupt jumps in background level within a single detector frame usually indicate either a processing problem (e.g. the sector non-linearity correction is incorrect) or a hardware problem. Experience with other systematic contributions level (~ 1% of sky) and 0.1% of sky) where their NIR mosaics (e.g. WFCAM) suggest that other additive such as fringing, will probably only occur at a relatively low the current defringing scheme will reduce these to a level (~ impact is negligible.

The main unknown here is the stability of the reset anomaly. This will be characterised through laboratory tests during camera assembly and acceptance and further quantified during commissioning.

3.3.3 Multiplicative systematics
External differences between the detectors, the differential detector gains, will be calibrated from master twilight flat fields for each passband. In practice the main limitations here are those due to colour equation differences between the detectors, and to residual errors in the nonlinearity corrections rather than the properties of master flat field frames. Intra-detector systematics are taken care of by conventional flat fielding. However, both types of global multiplicative systematics typically can be controlled at the 1-2% level and can be externally monitored and further corrected by the "illumination" measurement correction stage described next. The final photometry correction stage is to use the illumination correction measurements to reduce the effects of uneven illumination e.g. scattered light in the flat fielding, residual detector differences and so on, to below the 2% level. This is a master calibration processing task that is probably best done as either a post main pipeline processing stage or at the science database extraction point.


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The 2MASS-based calibration provides an instantaneous measurement of the throughput of the system, incorporating extinction. Even on cloudy nights, when the transmission is variable, this will provide a significantly better calibration than can be achieved with routine observations of standard star fields. Offline, nightly trend analysis of the extinction derived from 2MASS, combined with regular observations of secondary photometric standard fields, set up in the VISTA instrumental system, will enable an independent calibration of most nights to the level of 1% to 2% global.


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4 Calibration Data for Instrumental Signature Removal
4.1 Purpose
Section 4 describes what calibration data has to be collected with what frequency to allow one to remove instrumental signatures. For each piece of calibration data required this section defines: · Responsible: responsibility for obtaining the calibration data · Phase: when the calibration data has to be acquired (day or night time) · Frequency: how often calibration data need to be acquired. · Purpose: reason for needing the calibration data · Procedure: the procedure for acquiring the calibration data · Raw Outputs: the output of the procedure · Prepared OBs/Templates: the pre-prepared observation blocks or templates to acquire the calibration data · OT queue: the corresponding Observing Tool queue for the Observation Blocks. · Pipeline Recipe: The name (if any) of the processing recipe applied by the data flow system pipeline. Recipes may contain algorithms and procedures as subcomponents. Each such recipe corresponds to one listed in [RD1]. · Pipeline Output: the Pipeline output products, appended with (QC) for those also used as Quality Control parameters · Duration: an estimate of the required time to execute the calibration procedure including overheads. · Prerequisites: possible dependencies on instrumental or sky conditions or other calibration procedures are given · See also: any further information. The calibration data is used for instrumental signature removal. The aim is to provide pawprints as though taken with a perfect camera, which produces a photometrically linear, defect-free, evenly-illuminated, though sparsely sampled, reproduction of the sky. This will have no additional systematic, random noise or other artefacts, and will be on an arbitrary photometric and astrometric scale. Off-sky calibrations and quality control measures will be made routinely, before and after observing, using the in-dome illuminated screen.


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Dark combine

Persistence analyse

Crosstalk analyse

Detector noise

Linearity analyse

Twilight combine

Illumination analyse

Jitter microstep analyse

Master dark frame

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Decay constant Crosstalk matrix Readout noise, gain Linearity curves Master flat field frame Illumination map Reduced paw print

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Figure 4-1 Cascade Diagram for producing Calibration Frames

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Procedure: Raw Outputs: Template: OT queue: Pipeline Recipe: Pipeline Outputs: Duration: Prerequisites: See Also:

Science Operations Daytime Daily A Reset frame is a Reset-Read sequence with minimum exposure taken with the cold blank in (1 sec is the minimum VISTA can produce, but 10s would be a more realistic estimate for the duration for a single exposure including overheads as the IRACE system is specified to process an exposure within 5s and to allow the next exposure to start within 10s). It differs from a dark frame, which consists of a Reset-Read-Read sequence where the output is the difference of the two reads. The aim is to map the effect of the reset. Sequences of Reset frames will be taken offsky and analysed to estimate the stability of the reset pedestal and pixel to pixel variation. Read out frame, compare with library reset frame. FITS files VIRCAM_img_cal_reset.tsf VIRCAM.Daytime.Calibration vircam_reset_combine Variance with respect to standard frame (QC) 10 s

4.3 Dark Frames
Responsible: Phase: Frequency: Purpose: Science Operations Daytime Daily Dark Frames are used to calibrate out and measure two separate additive effects. · the accumulated counts that result from thermal noise (dark current). This is generally a small, but not negligible effect. · an effect, here called `reset anomaly', in which a significant residual structure is left in the image after the reset is removed in the DAS, when it does a correlated double sample (CDS, Reset-Read-Read). Both dark current and reset anomaly are additive and can be removed together, using dark frames (exposures with cold blank filters completely blocking the detectors from incoming radiation) taken with the same integration time as the target observation. In order to minimize contamination from transient events, a dark frame would be a combination of many frames with rejection. If the spatial structure of the reset anomaly is not stable with time


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Procedure:

Raw Outputs: Templates: OT queue: Pipeline Recipes: Duration: Pipeline Outputs:

it could leave a challenging background variation over the detector, which may need to be removed with a background filter. This latter scenario is best avoided as real astronomical signal will inevitably be removed. (In general, for other instruments examined where the reset anomaly structure is repeatable and stable, the integration time seems to determine the spatial structure of the residuals, while the ambient flux seems to determine its intensity.) A series of dark frames will be taken with each integration and exposure time combination used for target observations so that the structure of the reset anomaly can be modelled correctly and the dark correction is consistent. The Dark template, which does not require the telescope, will insert the cold blank and perform a timed exposure. If the requested time is less than the array minimum read-out cycle time of ~1s (e.g. zero) the controller will deliver, and report, the minimum detector integration time of ~1s. FITS Files VIRCAM_img_cal_dark.tsf; vircam_img_cal_darkcurrent.tsf VIRCAM.Daytime.Calibration vircam_dark_combine; vircam_dark_current One set of observations for each integration and exposure setting for the science observations made on the same night Mean Dark Dark + reset anomaly stability measure (QC) Detector dark current (QC) Detector Particle Event rate (QC)

Prerequisites: See Also:

4.4 Dome flats
Science Operations Daytime or non-observing nights. Daily Monitoring instrument performance, image structure, and confidence maps. They will not be used for gain correction (flatfielding) due to non-uniform illumination over the whole of the focal plane and the different colour of the illumination compared to the night sky. Note that dome flats may have a spectral energy distribution closer to that of some objects of interest and thus be more adequate for gain correction, but for pipeline processing whole fields in a consistent way an average gain/flat-field correction for typical objects is the usual method. Procedure: The Dome template will acquire the dome screen (constant illumination); a series of timed exposures are made through a given filter. Raw Outputs: FITS files Prepared OBs: VIRCAM_img_cal_domeflat.obx Responsible: Phase: Frequency: Purpose:


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OT queue: VIRCAM.Daytime.Calibration Pipeline Recipe: vircam_dome_flat_combine Pipeline Outputs Updated Master dome flats Updated confidence maps Bad pixel statistics (QC) Number of saturated pixels Lamp efficiency Duration: 10 min Prerequisites: The need for constant illumination of the dome screen implies that the dome flats cannot be taken in conditions of variable or excessive ambient light. See Also: Dome flat observations are also employed in linearization measurements described in 4.6 and in generating bad pixel maps.

4.5 Detector Noise
Responsible: Phase: Frequency: Purpose: Science Operations Daytime Daily In order to understand the noise properties of the detectors, it is important to measure the readout noise and gain of each chip. This is a vital piece of information, not only as large changes in either property could signal a detector health issue, but also as further down the pipeline the issue of pixel rejection algorithms becomes important (for example, during jittering). Both of these properties can be measured from a pair of dark exposure frames and a pair of dome flat frames. The dark exposures should have matching integration and exposure times to the dome flats, and both dome flat frames should be observed with the same dome illumination. Care should be taken to ensure that the flats are exposed in a region of the response curve where the detectors are reasonably linear. FITS files VIRCAM_img_cal_noisegain.tsf VIRCAM.Daytime.Calibration vircam_detector_noise Readout noise and gain estimate for each read-out channel of each detector (QC) 1 minute

Procedure:

Raw Outputs: Template: OT queue: Pipeline Recipe: Pipeline Outputs: Duration: Prerequisites: See Also:

4.6 Linearization Measurements
Responsible: Science Operations Phase: Daytime or cloudy nights (better) Frequency: Monthly


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Purpose: Infrared detectors can be strongly non-linear. The linearity curve of each detector can be determined through a series of differently timed dome screen observations under constant illumination. These curves are used in conjunction with the pixel timing information to obtain a true linear value for each pixel and to generate high-accuracy bad-pixel maps (linearization in the DAS would be an alternative but is not included in the Technical Specification). Procedure: On a series of specified dates (monthly) take series of dome flats under constant illumination at varying exposures up to full counts. Raw Outputs: FITS files Prepared OBs: VIRCAM_img_cal_linearity.obx OT queue: VIRCAM.Daytime.Calibration Pipeline Recipe: vircam_linearity_analyse Pipeline Output: Linearization curve and lookup tables updated bad-pixel maps Measure of non-linearity function (QC) Bad pixel statistics (QC) Duration: [30] min Prerequisites: The need for constant illumination of the dome screen implies that the dome flats cannot be taken in conditions of variable or excessive ambient light. See Also: Dome flat measures in 4.4

4.7 Twilight Flats
Responsible: Phase: Frequency: Purpose: Science Operations Twilight Evening/Morning Flat-fielding removes multiplicative instrumental signatures from the data. This includes pixel-to-pixel gain variations and the instrumental vignetting profile. It also provides a global gain correction between detectors and individual read out channels within each detector. (Each of the 16 detectors has 16 read out channels, giving a total of 256.) Mean flat-fields also are the data source for the science-level confidence map for each detector and filter combination. This is similar to a weight/bad-pixel map where the mean level is normalized to a value of 100% and bad pixels are flagged with a value of zero. It is used in conjunction with an estimate of the sky background variance in each frame to propagate the weight of each individual pixel. Although this is especially important for later manipulation of the pawprints outside the VISTA pipeline for doing deep stacking and tiling, it is also vital for the object detection part of the pipeline which is used, inter alia, in astrometric and photometric corrections.


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Procedure:

Raw Outputs: Prepared OBs: OT queue: Pipeline Recipe: Pipeline Output:

Duration: Prerequisites: See Also:

Mean flat-fields can be derived from a variety of sources (each with their own advantages and disadvantages). Sky flats taken at twilight have a good (but not perfect) colour match to the night sky observations we wish to correct, and can be taken under conditions where the contribution from night sky fringing, emission from dust (on the optical surfaces) and other spatial effects are most negligible. The slightly imperfect colour match between the twilight and night sky will cause a very small residual error in the gain correction. Dusk and dawn twilight flats can be combined (outside of the pipeline), to update the master flats, and thereby moderate effects caused by the significant variation in the illumination caused by the reset and read times. The sky level must be such that any emission from fringing or dust on the optical surface will be negligible in comparison, and this means that there is only a short time in which to acquire the twilight flats. It will not always be possible to get a complete set of twilight flats every night for schedules involving many filters or on nights with changeable weather. If, however, the detector flat-fields are sufficiently stable, then it is possible to use master flats taken over several nights, which is the method of choice. FITS Files VIRCAM_img_cal_twiflat.obx VIRCAM.Daytime.Calibration vircam_twilight_combine Mean twilight flats Confidence maps Change (vs calibDb) in mean gain correction coefficients between detectors and channels (QC) 10 min evening twilight, 10 min morning twilight.

4.8 Illumination Correction Measurement
Responsible: Phase: Frequency: Purpose: Science Operations Night Monthly The gain correction as modelled by the flat-field should remove all pixel-to-pixel gain differences as well as any large-scale variations due (generally) to vignetting within the focal plane. However, scattered light within the camera may lead to largescale background variations which cannot be modelled and removed, as its level depends critically on the ambient flux. Dividing a target frame by a flat-field frame that is affected by this will cause systematic errors in the photometry across the detector. It is necessary to map out the spatial systematic effects across each detector so that a correction map can be factored into


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the final photometry measured from each detector. Procedure: The illumination correction can be measured in two ways. In the event that observations of a secondary photometric standard field with a density of 100-200 objects per detector are available, then the illumination correction can be measured by looking at the spatial variation of the photometric zero-point across each detector. If such a field is not available, then a mesostep sequence is taken consisting of a series of exposures of a sparse field of relatively bright stars on a regular grid of offsets that cover one detector. Measuring a flux on each exposure allows the definition of a position-dependent scale factor (this must be done for each filter and each detector). Raw Outputs: FITS files Prepared OBs: VIRCAM_img_cal_illumination.obx OT queue: VIRCAM.Nighttime.Calibration Pipeline Recipe: vircam_mesostep_analyse Pipeline Output: Correction map Duration: 30 min Prerequisites: Photometric conditions See Also:

4.9 Image Persistence Measurements
Responsible: Phase: Frequency: Purpose: Procedure: Science operations Night Monthly and on detector/controller change Image persistence (sometimes also called `remanence') is the effect where residual impressions of images from a preceding exposure are visible on the current image. On a sequence of (monthly) dates choose a fairly empty field with a nearly saturated star. Take an exposure and then a sequence of dark frames to measure the characteristic decay time. This must be done for each detector. FITS files VIRCAM_img_cal_persistence.obx VIRCAM.Nighttime.Calibration vircam_persistence_analyse Persistence constants 10 min (although if the decay time constant turns out to be significantly more than about half a minute, then this may be something of an underestimate).

Raw Outputs: Prepared OBs: OT queue: Pipeline Recipe: Pipeline Output: Duration: Prerequisites: See Also:

4.10 Electrical Cross-Talk Measurements
Responsible: Science operations


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Phase: Night Frequency: Monthly Purpose: Electrical cross-talk will be measured in the laboratory and during commissioning, and is expected to be negligible. As crosstalk might change with any alterations to the electrical environment, a routine procedure to check it is planned. Procedure: The 16 detectors are read out in 16 channels, making a total of 256 channels in the camera. Cross-talk calibration consists of placing a saturated star on a channel and measuring any effect on the other 255 channels. This results in a 256x256 matrix, the majority of whose elements will hopefully be zero. Any electrical cross talk between different detectors is anticipated to be smaller than between channels within a detector. Raw Outputs: FITS Files Templates: VIRCAM_img_acq_crosstalk, VIRCAM_img_cal_crosstalk OT queue: VIRCAM.Nighttime.Calibration Pipeline Recipe: vircam_crosstalk_analyse Pipeline Output: Cross-talk matrix. Average measure of off-diagonal components (QC) Duration: 10 min for all detectors, assuming a decay time-constant < 30s Prerequisites: See Also:


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5 Data for Photometric Calibration
5.1 Introduction
The camera will be on the telescope semi-permanently, in a survey mode, providing a stable configuration which enables a long-term approach to photometric calibration to be taken. The strategy is to define routine calibration procedures, so that the accuracy, and hence the scientific value, of the archive, will be maximized. Magnitudes will be calibrated on the Vega scale. As briefly mentioned in Section 3.3, VIRCAM observations will enable two independent calibrations: 1. from the 2MASS all-sky point source catalogue and 2. from routine observations of standard star fields We discus the details of the two methods below

5.2 Calibration from 2MASS
The photometric zeropoint is derived for each image from measurements of stars in the 2MASS point source catalogue (PSC) by solving
ZPVIRCAM + m
inst

-m

2 MASS

= CT ( J - H )

2 MASS

+ const

for all stars in common with VIRCAM (above a threshold signal-to-noise in the PSC and unsaturated in CIRCAM), where: · · · · · ·
ZPVIRCAM is the zeropoint for the filter and detector minst is the VIRCAM instrumental magnitude for the filter (=2.5log(counts/sec) m2 MASS is the 2MASS PSC magnitude CT is the colour term and is derived from a large number of observations ( J - H ) 2MASS is the 2MASS PSC colour of the star const is an offset which may be required in some passbands to ensure the magnitude is on the Vega system.

Subsequent inter-detector comparisons will enable residual errors in the gain correction to be detected and calibrated. Offline analysis would provide a measure of the median zeropoint for the night, and an associated error (and scatter), indicative of photometric quality of the night.

5.3 Calibration from Standard Star Fields
At any time (t) on any night (n) for any star (i) in any filter waveband (b),


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m
cal ib

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=

m

inst

ibtn

+ ZPbtn - btn ( X - 1)

where ZP is the Zero Point (i.e. the magnitude at airmass unity which gives 1 count/second at the detector), mcal is the calibrated instrumental magnitude, minst is the measured instrumental magnitude (-2.5 â log10[counts/sec]), is the extinction coefficient and X is the airmass of the observation. This assumes that the secondorder extinction term and colour-dependency of are both negligible. Typically, the Zero Point of the instrument + telescope system should be stable throughout the night. Long-term decreases in the sensitivity of the instrument, and hence a decreasing ZP, could be caused by for example the accumulation of dust on the primary mirror. On photometric nights the extinction coefficient should be constant in each filter. The extinction will be monitored through each night assuming a fixed zero point and making measurements over a range of airmass. Although 2MASS found their extinction coefficients to vary seasonally any effect should be much less for VISTA since it has narrower filter profiles especially at J, and is at a much drier site. A network of Secondary Standard photometric fields will be set up so that routine photometric standard observations can be made with the telescope in focus every two hours. The standard fields are selected to be 2MASS touchstone fields and or UKIRT faint standard fields, and many will have been observed and calibrated in advance by WFCAM. The secondary fields meet the following criteria: · Extend over the area of the IR camera pawprint · Span 24 hours in RA, with a target spacing of 2 hours. · Enable observations over a range of airmass. Some must be chosen to pass close to the zenith of VISTA (for airmass unity). Some fields will be available to the North and South of the zenith to optimize telescope azimuth slewing. The remainder will be near-equatorial. · Have a density of sources sufficient to characterize the systematic positiondependent photometric effects in VISTA, but not be too crowded. The target is of order 100 stars per detector with magnitudes no fainter than J=18, s=16 to avoid prohibitively long exposures. · They should encompass as broad a spread as possible in colour in order to derive colour terms robustly and facilitate transformations from and to other filter systems and e.g. the AB magnitude system. i.e.
M
std

=m

cal b

+ C (M

std x

-M

std y

)

Equation 2

cal where M std is the magnitude in a defined standard system, mb is the calibrated magnitude in the instrumental system, and C is the colour term for std the appropriate standard colour index ( M xstd - M y ) .


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Technical Program TP-VIS1 describes the observations needed to set up the secondary standard fields.

5.4 Observe Standard Fields
Responsible: Phase: Frequency: Purpose: Science Operations Night 2-Hourly Determine ZP and to allow application of m cal ib = m inst ibtn + ZPbtn - btn ( X - 1) to photometrically calibrate all objects seen. In the event that observations of a secondary photometric standard field with a density of 100-200 objects per detector are available, then the illumination correction can be measured by looking at the spatial variation of the photometric zero-point across each detector. Suitable fields from this network will be observed over a range of airmass each night to determine the Zero Points (ZP) to monitor the extinction coefficients () for all broad-band filters, and if sufficiently high density of standards, to measure the illumination correction. FITS files VIRCAM_img_cal_std.tsf Science vircam_standard_process Zero Point (ZP) Extinction coefficient () Illumination correction map Colour terms (C) Illumination correction Global gain correction (check) 5 min 10 times per night

Procedure:

Outputs: Template: OT queue: Pipeline Recipe: Pipeline Output:

Duration: Prerequisites: See Also:


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6 Calibration Data Derived from Science Data
6.1 For Instrument Signature Removal
6.1.1 Night-Sky Maps
Responsible: Phase: Frequency: Purpose: Science Operations Night Throughout night If experience shows that the detector flats are not reliably stable over the timescale of a night, then night-sky flats will have to be used instead. These are formed either from the target frames or from any special offset sky frames that might have been taken (for example where there is a large extended object in the field). All such frames over an appropriate time range are combined with rejection to form a normalized night sky flat-field. The advantage of dark flats over twilight flats is the better colour match to the average astronomical object. This minimises the sensitivity of the gain and flat-field correction to differential colour terms with respect to astronomical objects. However, fringing and thermal emission from dust particles on the optical surfaces can be high enough to affect the background significantly in some passbands. Dividing the target frames by a sky flat without correcting for these two additive effects could lead to significant systematic errors in photometry. In the Garching pipeline, master flats will be determined from as many observations as possible, but if it is determined that the flats vary rapidly, then only flats taken close in time may be useable. Use normal science exposures. FITS Files None science vircam_jitter_microstep_process Night sky maps Occurs in parallel with all night observing Determine the characteristics of fringing and thermal emission from dust on the optical surfaces during commissioning. 6.1.2

Procedure: Raw Outputs: Prepared OBs: OT queue: Pipeline Recipe: Pipeline Output: Duration: Prerequisites: See Also:

6.1.2 Sky Subtraction and Fringe Removal
Responsible: Phase: Frequency: Purpose: Science operations Night Throughout night The sky background varies over large scales in the infrared. In some wavebands, fringing and thermal emission from any local dust (on optical surfaces) will also be present. All of these


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Procedure: Raw Outputs: Prepared OBs: OT queue: Pipeline Recipe: Pipeline Output: Duration: Prerequisites: See Also:

effects can be removed using the sky-subtraction algorithm. The source of the sky background estimate is usually the science data frames themselves. In cases where large extended or very bright objects might be present, it may be necessary to use `offset sky' exposures in the observation template. Preset or offset to, uncrowded, regions taken near or adjacent to the region of interest. Observe in the same way as the corresponding science field. FITS Files None science vircam_jitter_microstep_process Local sky estimate Fringe and dust maps Same as science field.

6.1.3 Jittering
Responsible: Phase: Frequency: Purpose: Science Operations Night Nearly all the time Removal of bad pixels and other cosmetic effects, as well as cosmic rays, and determining the sky background. Typically a long exposure is split into several shorter exposures, which, rather than being repeated with each pixel looking at exactly the same sky position, are carried out at a series of different (jittered) positions. This is similar to microstepping (same template), but with less fine sampling, and the pipeline combines the jittered exposures using a rejection algorithm. Perform a specified pattern of exposures at each position of a jitter pattern. Predefined patterns and movement size in pixels may be selected. Microsteps can be nested within each jitter position by setting the number of microsteps appropriately in the template. FITS Files VIRCAM_img_obs_tile.tsf, VIRCAM_img_obs_paw.tsf, VIRCAM_img_obs_offsets.tsf Science vircam_jitter_microstep_process Combined frames of pawprint Confidence map for pawprint Variable

Procedure:

Raw Outputs: Template: OT queue: Pipeline Recipe: Pipeline Output:

Duration: Prerequisites: See Also: 6.1.4


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6.1.4 Microstepping
Responsible: Phase: Frequency: Purpose:

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Procedure:

Raw Outputs: Template: OT queue: Pipeline Recipe: Pipeline Output: Duration: Prerequisites: See Also: 6.1.3

Science operations Night As required Improved sampling. This is most likely to be employed in times of excellent seeing, when the point-spread function is undersampled. It can also be used if there are strong intra-pixel sensitivity (QE) variations. It may not be commonly used. It is similar to jittering (same template) but with improved sampling through finer pattern spacing, and the pipeline interleaves the exposures without further rejection. Perform a specified pattern of exposures at each position of a microstep pattern. Predefined patterns and movement size in pixels may be selected, and there is a default pattern/size [2â2 pattern, modulo a 0.5 pixel shift]. By setting the number of microsteps appropriately in the template, microsteps can be nested within each jitter position. FITS Files VIRCAM_img_obs_paw.tsf Science vircam_jitter_microstep_process Interleaved science frames with corresponding confidence maps Variable

6.2 For Astrometric Calibration
Astrometric calibration will take the instrument signature free pawprints and provide the transformation between pixel coordinates and celestial coordinates for each of the 16 constituent images, though still leaving the pawprints on an arbitrary photometric scale. The transformations are manifested in a Flexible-Image Transport System (FITS) [RD12] World-Coordinate System (WCS) [RD14]. The projection used will be Zenithal Polynomial (ZPN), based on the predicted properties from the optical design. Quantifying the distortion terms used in the WCS will be done from on-sky observations. An initial astrometric distortion is available from the optical design, and an updated early empirical value will be derived from commissioning data. Following that, an increasingly accurate value will be derived from the astrometry of all target frames.

6.2.1 Optical Distortion Effects
Responsible: Phase: Frequency: Purpose: Science Operations Night All science frames The strongest term in the optical-distortion model is the cubic radial term, but this and all distortions will be slightly colour (i.e. filter) dependent and must be determined on sky. The expected


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Procedure: Raw Outputs: Prepared OBs: OT queue: Pipeline Recipe: Pipeline Output: Duration: Prerequisites: See Also:

power of the distortion means that no practically useful jitter is possible without non-linear resampling. The radial scale distortion also has an impact on photometric measurements, inducing an error up to 3.5% in the corners of the field, compared to the centre, if uncorrected. It is thus crucial to determine it accurately. Astrometric stars in the science fields are used to map the distortion, an increasingly accurate description of which builds up from the astrometry of all target frames. FITS files None Science This is not part of the pipeline. Refined optical distortion model No overhead Initial value from optical design, an early empirical value from commissioning data,

6.2.2 Final WCS Fit
Responsible: Phase: Frequency: Purpose: DFS calibration pipeline Night All imaging frames on sky The camera software writes an initial WCS based on the given position of the guide star into the FITS headers of each data frame. The accuracy will be better than 2, dependent on the guide star accuracy, and the determined geometry of the camera. This provides a close starting point for orientation of the data frames and location of astrometric stars for a full WCS solution that will provide refined scientific quality astrometry. After instrumental-signature removal astrometric stars are centroided in the data frames to typically 0.1 pixels accuracy. An astrometric solution is carried out using reference catalogues based on the International Coordinate Reference Frame (ICRF) [e.g. 2MASS catalogue]. Accuracy is dependent on the reference catalogue accuracy, but the final uncertainty estimate comes from the RMS of the fit and the known systematics of the reference catalogue. None None None vircam_jitter_microstep_process Refined WCS FITS header for all frames Pointing accuracy (QC) [Calculated from equatorial coordinates computed at particular location using the fitted WCS and the initial WCS that was written to the raw header] Zero overhead

Procedure: Raw Outputs: Prepared OBs: OT queue: Pipeline Recipe: Pipeline Output:

Duration:


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Prerequisites: Commissioning to determine initial WCS See Also:


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7 Quality Control
7.1 Further Quality Control Data Derived from Science Frames
7.1.1 Object Extraction
Responsible: Phase: Frequency: Purpose: Science Operations Night Nearly all the time Object extraction is vital for various steps in the pipeline, including astrometric and photometric calibration, where the position and/or photometric measures of real objects are required. It is also needed in order to assess the quality of the data in terms of the observing conditions and the depth of exposure. Extract objects from each frame using the object extraction algorithm. Classify objects as stellar, non-stellar and noise using the classification scheme. Use the stellar objects to work out the average properties of the images on the frame. FITS Files Science vircam_jitter_microstep_process Mean sky background (QC) Mean sky noise (QC) Number of noise objects (QC) Mean seeing (QC) Mean stellar ellipticity (QC) Variable

Procedure:

Raw Outputs: Template: OT queue: Pipeline Recipe: Pipeline Output:

Duration: Prerequisites: See Also:

7.2 On line quality control (QC-0)
QC-0 is generic for all VLT-compliant instruments and is provided by the Data-Flow Operations group. All image-mode data produced by the instrument is fed into the pipeline to produce QC-1 parameters.


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7.3 Quality Control Parameters
Quality-control parameters are generated during pipeline processing. These may be used at a later time for trend analysis.
Parameter QC.APERTURE_CORR 2 arcsec [mag] diam aperture flux correction. Description the aperture flux correction for stellar images due to flux falling outside the aperture. Determined using a curve-of-growth of a series of fixed-size apertures. Alternative simple measure of image profile properties, particularly the presence of extended PSF wings, as such monitors optical properties of system; also required for limiting magnitude computations. determined from the statistics of the pixel distribution from the ratio of two flatfield sequences of significantly different average count levels. The fraction of bad pixels per detector (either hot or cold) should not change determined from presence of +ve or -ve ghost images on other channels/detectors using exposures in bright star fields. Potentially a fully populated 256x256 matrix but likely to be sparsely populated with a small number of non-zero values of band-diagonal form. This QC summary parameter is the average value of the modulus of the off-diagonal terms. Values for the cross-talk matrix should be very stable with time, hardware modifications notwithstanding. measured using the median of the pixel values, can later be compared similar darks for trends

QC.BAD_PIXEL_STAT fraction of bad pixels/detector [scalar]. QC.CROSS_TALK average values for cross-talk component matrix [scalar].

QC.DARKCURRENT average dark current on frame [adu/sec]. QC.DARKDIFF_MED Median new-library dark frame [adu]. QC.DARKDIFF_RMS [adu] RMS new-library dark frame QC.DARKMED median dark counts QC.DARKRMS RMS noise of combined dark frame [adu]. QC.ELLIPTICITY mean stellar ellipticity [scalar].

Measure the median of the difference of a new mean dark frame and a library reset frame. measure the RMS of the difference of a new mean dark frame and a library dark frame. median counts in dark frames. RMS is defined here as the Gaussian equivalent MAD ie. 1.48*median-of-absolute-deviation from median The RMS can later be compared with library values for darks of the same integration and exposure times. the detected image intensity-weighted second moments will be used to compute the average ellipticity of


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QC.FLATRATIO_MED Median new/library flat frame [scalar]. QC.FLATRATIO_RMS RMS new/library flat frame [scalar]. QC.FLATRMS RMS flatfield pixel sens per detector [fraction].

suitable signal:to:noise stellar images. Shot-noise causes even perfectly circular stellar images to have non-zero ellipticity but more significant values are indicative of one of: optical, tracking and autoguiding, or detector hardware problems. Measure the median of the ratio of a new mean flat frame and a library flat frame. Measure the RMS of the ratio of a new mean flat frame and a library flat frame. RMS is defined here as the Gaussian equivalent MAD ie. 1.48*median-of-absolute-deviation from unity after normalising by median level ie. measuring the RMS sensitivity variation. The RMS can later be compared with library values for troubleshooting problems. significantly with time. A robust estimate of the background noise is done before the first fringe fitting pass. Once the last fringe fit is done a final background noise estimate is done. This parameter is the ratio of the value before fringe fitting to the final value after defringing. determined from pairs of darks and flatfields of the same exposure/integration time and illumination by comparing the measured noise properties with the expected photon noise contribution. The gain of each detector should remain stable so long as the electronics/micro-code have not been modified. the ratio of median counts in a mean flat exposure for a given detector relative to the ensemble defines the internal gain correction for the detector These internal relative detector gain corrections should be stable with time. The RMS of the illumination correction over all the frame. measured from the average FHWM of stellar-classified images of suitable signal:to:noise. The seeing will obviously vary over the night with time, wavelength (filter) and as airmass^0.6. This variation should be predictable given local site seeing measures. A comparison with the expected value can be used as an indication of poor guiding, poor focus or instrument malfunction. estimate of 5-sigma limiting mag for stellar-like objects for each science observation, derived from QCs ZPT_2MASS, SKY_NOISE, APERTURE_CORR. Can later be compared with a target value to see if

QC.FRINGE_RATIO [scalar] Ratio of sky noise before/after fringe fit QC.GAIN gain [e/ADU].

QC.GAIN_CORRECTION detector median flatfield/global median [scalar]. QC.ILLUMCOR_RMS QC.IMAGE_SIZE mean stellar image FWHM [arcsec].

QC.LIMITING_MAG limiting mag ie. depth of exposure [mag].


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QC.LINEARITY percentage average nonlinearity [percentage].

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QC.LINFITQUAL RMS fractional error in linearity fit QC.MAGNZPT Number of stars in zero point calc. QC.MAGZERR Photometric zero point error [mag]. QC.MAGZPT Photometric zero point [mag]. QC.MEAN_SKY mean sky level [ADU]. QC.NOISE_OBJ number of classified noise objects per frame [number]. QC.PARTICLE_RATE cosmic ray/spurion rate [count/s/detector]. QC.PERSIST_DECAY mean exponential time decay constant [s]. QC.PERSIST_ZERO fractional persistence at T0 (extrapolated). QC.READNOISE readnoise [electron].

main survey requirements (ie. usually depth) are met. derived from measured non-linearity curves for each detector interpolated to 10k counts (ADUs) level. Although all infrared systems are non-linear to some degree, the shape and scale of the linearity curve for each detector should remain constant. A single measure at 20k counts can be used to monitor this although the full linearity curves will need to be examined quarterly [TBC] to look for more subtle changes. Derived by applying the linearity coefficients to the image data that were used to measure them. This is the RMS of the residuals of the linearised data normalised by the expected linear value The number of stars on this image used to calculate the photometric zeropoint. A measure of the RMS photometric zero point error using an aperture of 1* the core radius. A measure of the photometric zero point using an aperture of 1* the core radius. computed using a clipped median for each detector Sky levels (perhaps not at Ks) should vary smoothly over the night. Strange changes in values may indicate a hardware fault. measured using an object cataloguer combined with a morphological classifier. The number of objects classified as noise from frame-to-frame should be reasonably constant; excessive numbers indicate a problem. average no. of pixels rejected during combination of dark frames, used to give an estimate of the rate of cosmic ray hits for each detector. This can later be compared with previous estimates and monitored. the decay rate of the persistence of bright images on subsequent exposures will be modelled using an exponential decay function with time constant tau. Requires an exposure on a bright star field followed a series of darks. determined from the persistence decay behaviour from exponential model fitting. Requires an exposure on a bright star field followed a series of darks (as above) measured from the noise properties of the difference in two consecutive dark frames, using a MAD estimator as above for robustness against spurions. The noise properties of each detector should remain stable so long as the electronics/micro-code have not been


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QC.RESETDIFF_MED Median new-library reset frame [adu]. QC.RESETDIFF_RMS [adu] RMS new-library reset frame QC.RESETMED median reset level QC.RESETRMS RMS noise in combined reset frame.

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modified. Measure the median of the difference of a new mean reset frame and a library reset frame. measure the RMS of the difference of a new mean reset frame and a library reset frame. median reset level

variation is defined here as the Gaussian equivalent MAD ie. 1.48*median-of-absolute-deviation from unity after normalising by median level ie. measuring the RMS reset level variation. The RMS can later be compared with library values for troubleshooting problems. QC.SATURATION determined from maximum peak flux of detected stars saturation level of bright from exposures in a standard bright star field. The stars [ADU]. saturation level*gain is a check on the full-well characteristics of each detector. QC.SKY_NOISE RMS sky computed using a MAD estimator with respect to noise [ADU]. median sky after removing large scale gradients. The sky noise should be a combination of readout-noise, photon-noise and detector quirks. Monitoring the ratio of expected noise to measured provides a system diagnostic at the detector level. QC.WCS_DCRVAL1 measure of difference between dead-reckoning actual WCS zero point X pointing and true position of the detector on sky. raw header value [deg]. Derived from current polynomial distortion model and 6-constant detector model offset. QC.WCS_DCRVAL2 measure of difference between dead-reckoning actual WCS zero point Y pointing and true position of the detector on sky. raw header value [deg]. Derived from current polynomial distortion model and 6-constant detector model offset. QC.WCS_DTHETA actual measure of difference between dead-reckoning PA and WCS rotation PA - raw PA true position angle of the detector. Derived from header value [deg]. current polynomial distortion model and 6-constant detector model effective rotation term. QC.WCS_RMS robust RMS robust average of residuals from WCS solution for of WCS solution for each each detector. Measure of integrity of WCS solution. detector [arcsec]. QC.WCS_SCALE measure of the average on-sky pixel scale of detector measured WCS plate scale after correcting using current polynomial distortion per detector [deg/pixel]. model QC.WCS_SHEAR power of measure of WCS shear after normalising by plate scale cross-terms in WCS solution and rotation, expressed as an equivalent distortion [deg]. angle. Gives a simple measure of distortion problems in WCS solution.


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QC.ZPT_2MASS 1st-pass photometric zeropoint [mag].

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the magnitude of a star that gives 1 detected ADU/s (or e-/s) for each detector, derived using 2MASS comparison stars for every science observation. This is a first pass zero-point to monitor gross changes in throughput. Extinction will vary over a night, but detector to detector variations are an indication of a fault. QC.ZPT_STDS photometric the magnitude of a star that gives 1 detected ADU/s (or zeropoint [mag]. e-/s) for each detector, derived from observations of VISTA standard star fields. Combined with the trend in long-term system zero-point properties, the ensemble "average" zero-point directly monitors extinction variations (faults/mods in the system notwithstanding) The photometric zeropoints will undoutbedly vary (slowly) over time as a result of the cleaning of optical surfaces etc.


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8 Templates
The hierarchy of the templates defined for VIRCAM are shown in Figure 8-1 below. There are a series of templates for each of the operating modes described in section 3. Note: the template definitions are refined from those presented in early drafts of this document to reflect enhancements in the final design of the camera observation software [RD6]. Acquisition templates (shown in blue italic), which define the operating · mode and telescope target parameters. Each Observation Block begins with an acquisition template defining the primary target to which that Observation Block refers. Acquisition templates do not generate exposures. · Calibration templates (shown in red), which obtain exposures necessary for calibrating observations in a particular instrument mode. A calibration template can result in one or more exposures being made. · Observation templates (shown in black), which obtain the exposures necessary to make science observations. An observation template can result in one or more exposures being made.
HOWFS mode VIRCAM_howfs_acq VIRCAM_howfs_acq_domescreen VIRCAM_howfs_cal_reset VIRCAM_howfs_cal_dark VIRCAM_howfs_cal_domeflat VIRCAM_howfs_obs_exp VIRCAM_howfs_obs_wfront IMAGING mode VIRCAM_img_acq VIRCAM_img_acq_twighlight VIRCAM_img_acq_domescreen VIRCAM_img_cal_reset VIRCAM_img_cal_dark VIRCAM_img_cal_darkcurrent VIRCAM_img_cal_domeflat VIRCAM_img_cal_linearity VIRCAM_img_cal_noisegain VIRCAM_img_cal_twiflat VIRCAM_img_cal_persistence VIRCAM_img_obs_paw VIRCAM_img_cal_std VIRCAM_img_obs_exp VIRCAM_img_obs_tile VIRCAM_img_cal_crosstalk VIRCAM_img_obs_offsets VIRCAM_img_cal_illumination

Figure 8-1 Hierarchy of VISTA IR Camera Templates

The relationship between the templates, the data they produce and the pipeline recipes which will be used is displayed in Table 8-1.


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DATA FILE HOWFS reset frame HOWFS Dark Frame HOWFS dome flat HOWFS wavefront HOWFS wavefont Test observation Reset Frame Dark Frame Dark Current Persistence sky measure Persistence dark measure Dome Flat Linearity Measure VIRCAM_ TEMPLATE howfs_cal_reset howfs_cal_dark howfs_cal_domeflat howfs_obs_exp howfs_obs_wfront img_obs_exp img_cal_reset img_cal_dark img_cal_darkcurrent

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VIS-SPE-IOA-20000-0002 2006-09-28 1.3 44 of 72 DPR TECH IMAGE IMAGE IMAGE IMAGE IMAGE IMAGE IMAGE IMAGE IMAGE IMAGE persistence_analyse IMAGE Test not processed reset_combine dark_combine dark_current Exposure parameters Exposure parameters Exposure parameters Exposure parameters WCS set Exposure parameters dome_flat_combine Exposure parameters Exposure parameters library reset frame library dark frame None Mean reset Mean dark Dark Current map linearity channel table library dark frame library flat field library bad-pixel map library dark frame linearity channel table library dark frame channel map Persistence constants Mean Dome Flat Dome confidence map Linearity channel table Bad pixel map HOWFS data is processed on the instrument workstation RECIPE HEADER INPUTS CALIB DB PRODUCTS

DRP CATG
TECHNICAL TECHNICAL TECHNICAL ACQUISITION ACQUISITION

DRP TYPE BIAS DARK FLAT,LAMP OBJECT, PSF-CALIBRATOR OBJECT, PSF-CALIBRATOR OBJECT BIAS DARK DARK, DARKCURRENT OBJECT, PERSISTENCE DARK, PERSISTENCE FLAT, LAMP FLAT, LAMP, LINEARITY

TEST CALIB CALIB CALIB CALIB

img_cal_persistence CALIB

img_cal_domeflat

CALIB

IMAGE

img_cal_linearity

CALIB

IMAGE

linearity_analyse


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DATA FILE Noise & Gain Twilight Flat VIRCAM_ TEMPLATE img_cal_noisegain

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VIS-SPE-IOA-20000-0002 2006-09-28 1.3 45 of 72 DPR TECH IMAGE RECIPE detector_noise HEADER INPUTS Exposure parameters Exposure parameters CALIB DB linearity channel table library bad-pixel map library dark frame linearity channel table library dark frame linearity channel table library flat field library confidence map persistence constants library dark frame linearity channel table library flat field library confidence map persistence constant crosstalk matrix library fringe map photometric catalogue library dark frame linearity channel table library flat field library confidence map persistence constants crosstalk matrix library fringe map photometric catalogue PRODUCTS Noise and gain values Mean twilight flat Sky confidence map Gain correction cross-talk matrix

DRP CATG CALIB

DRP TYPE FLAT, LAMP, GAIN DARK, GAIN FLAT, TWILIGHT DARK,TWILIGHT

img_cal_twiflat

CALIB

IMAGE

twilight_combine

Cross-Talk obs

img_cal_crosstalk

CALIB

OBJECT, CROSSTALK

IMAGE

crosstalk_analyse

Exposure parameters

Mesostep sequence

img_cal_illumination

CALIB

STD, ILLUMINATION

IMAGE

mesostep_analyse

Exposure parameters WCS set

illumination map

Standard star field

img_cal_std

CALIB

STD, FLUX

IMAGE, JITTER

standard_process

Exposure parameters WCS set

photometric coefficients


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DATA FILE Pawprint Pawprint Extd object Tile Tile extended nonstandard tile pattern nonstandard tile of extended source img_obs_tile SCIENCE SCIENCE img_obs_offsets SCIENCE img_obs_paw SCIENCE SCIENCE VIRCAM_ TEMPLATE

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VIS-SPE-IOA-20000-0002 2006-09-28 1.3 46 of 72 DPR TECH IMAGE, JITTER IMAGE, JITTER IMAGE, JITTER IMAGE, JITTER IMAGE, JITTER jitter_microstep_process IMAGE, JITTER RECIPE jitter_microstep_process library dark frame linearity channel table library flat field library confidence map persistence constants library fringe map crosstalk matrix photometric catalogue Reduced Paw Prints Associated confidence maps Object catalogues Sky map (e.g. for de-fringing, when input criteria met) HEADER INPUTS CALIB DB PRODUCTS

DRP CATG SCIENCE

DRP TYPE OBJECT OBJECT, EXTENDED OBJECT OBJECT, EXTENDED OBJECT

jitter_microstep_process Exposure parameters WCS set

OBJECT, EXTENDED

Table 8-1 Relationship between Data Types, Observation Templates and Pipeline Recipes


8.1 Imaging Calibration Templates
8.1.1 Reset
Name: Identifier: Description: Parameters: Raw Frames: Pipeline recipes: Reset VIRCAM_img_cal_reset.tsf Make a number of reset frames (reset-read only) with cold blank (a single reset/read sequence). Used with HOWFS and IMAGING mode. number of reset frames FITS vircam_reset_combine

8.1.2 Dark
Name: Identifier: Description: Parameters: Raw Frames: Pipeline recipes: Dark VIRCAM_img_cal_dark.tsf Make a number of dark exposures (reset-read-read) with cold blank integration time, number of integrations, number of frames FITS vircam_dark_combine

8.1.3 Dark Current
Name: Identifier: Description: Parameters: Raw Frames: Pipeline recipes: Dark Current VIRCAM_img_cal_darkcurrent.tsf Make a series of dark exposures at a variety of different exposure times List of integration times, and corresponding numbers of integrations for determination of detector dark current. Sequence of FITS files vircam_dark_combine

8.1.4 Acquire Dome Screen
Name: Identifier: Description: Parameters: Raw Frames: Pipeline recipes: Dome Screen VIRCAM_img_acq_domescreen.tsf Set instrument into IMAGING mode and select science filter. Move telescope to point at illuminated screen and switch on lamps. Filter, illumination combination None None

8.1.5 Dome Flat
Name: Identifier: Dome Flat VIRCAM_img_cal_domeflat.tsf


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Description:

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Parameters: Raw Frames: Pipeline recipes:

Make a dome flat exposure (or sequence of exposures) suitable for calibrating IMAGING mode observations. The flat-field lamps may be switched off when exposure is complete. Filter, list of integration times and corresponding numbers of integrations, switch calibration source off flag, lamp setting. FITS files vircam_dome_flat_combine

8.1.6 Detector Linearity
Name: Identifier: Description: Parameters: Raw Frames: Pipeline recipes: Linearity VIRCAM_img_cal_linearity.tsf Make series of dome flat exposures and corresponding darks at a list of exposure times. Filter, List of integration times and corresponding numbers of integrations FITS files vircam_linearity_analyse

8.1.7 Noise and Gain
Name: Identifier: Description: Parameters: Raw Frames: Pipeline recipes: Noisegain VIRCAM_img_cal_noisegain.tsf Make two dark exposures followed by the same number of dome screen flat-field exposures with matched integration times and number of integrations. filter, optional: detector controller mode, list of integration times and corresponding number of integrations, lamp level, optional "switch off calibration source when finished". FITS Files vircam_detector_noise

8.1.8 Acquire Twilight Field
Name: Identifier: Description: Parameters: Raw Frames: Pipeline recipes: Twilight VIRCAM_img_acq_twilight.tsf Select a dusk or dawn twilight field (Figure 2-1). Track (no autoguiding). filter, acceptable Azimuth, Altitude range for search, moon avoidance distance, optional: Azimuth, Altitude, rotator position angle. None None


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Figure 8-2 Pre-selected twilight fields

8.1.9 Twilight Flat
Name: Identifier: Description: Twilight Flat VIRCAM_img_cal_twiflat.tsf Take a series of exposures sufficient to make a twilight sky flat-field, automatically determining exposure values. Move telescope in small offsets between integrations to reject bright stars. List of integration times and corresponding numbers of integrations, or illumination level, depending on level of automation. Includes procedure to wait until sky brightness is appropriate, or abort if the time is too late (dusk and dawn). FITS files vircam_twilight_combine

Parameters:

Raw Frames: Pipeline recipes:

8.1.10
Name: Identifier: Description:

Persistence
Persistence VIRCAM_img_cal_persistence.tsf Take one exposure with a selected science filter, followed by a series of dark exposures. All exposures have the same integration time and number of integrations. The field should contain a nearly-saturated star. science filter, number of dark exposures, number of

Parameters:


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Raw Frames: Pipeline recipes:

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exposures, integration time, number of integrations. FITS files vircam_persistence_analyse

8.1.11

Astrometric Calibration

No specific astrometric calibration templates are required as all science frames will be calibrated according to the procedure described in 6.2.2.

8.1.12
Name: Identifier: Description:

Photometric Calibration Standard Fields
Calibrate VIRCAM_img_cal_std.tsf This template is identical to VIRCAM_img_obs_paw.tsf (see 8.3.2 for full operational description) except for the insertion of FITS information indicating a photometric standard field (STANDARD = T). It is only necessary to observe a pawprint for calibration, a full tile is unnecessary. Number of filter positions F, and (if F>1) filter IDs; Number of jitter positions J, Number of microstep positions M nested at each jitter position; (if J >1) jitter pattern ID, jitter scale factor, and (if M=1) at each jitter position integration time, number of integrations; (if M>1) microstep pattern ID, microstep scale factor, and at each microstep position the integration time, number of integrations. As many FITS files as there are exposures vircam_standard_process

Parameters:

Raw Frames: Pipeline recipes:

8.1.13
Name: Identifier: Description: Parameters:

Quick look
quick look VIRCAM_img_obs_exp.tsf Make a series of exposures at the same target position with a single filter, with no jittering or microstepping. science filter, number of exposures, integration time, number of integrations. FITS files None.

Raw Frames: Pipeline recipes:

8.1.14
Name: Identifier: Description:

Cross-talk
Cross-talk VIRCAM_img_cal_crosstalk.tsf Make a series of exposures, with each exposure offset from the previous one by a sequence of meso-steps designed to place a bright star on each of the 16 readout channels on each detector. science filter, optional list of meso-step offsets, optional

Parameters:


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Raw Frames: Pipeline recipes:

detector mode, number of exposures, integration time, number of integrations. FITS files vircam_crosstalk_analyse

8.1.15
Name: Identifier: Description:

Illumination
Illumination VIRCAM_img_cal_illumination.tsf make a series of exposures, with each exposure offset from the previous one by a sequence of meso-steps designed to place a bright star at a regular grid of offset positions across each detector. List of science filters, list of mesostep offsets, list of [guide star plus two aO stars] for each mesostep in the sequence, optional detector mode, number of exposures, integration time, number of integrations. FITS files vircam_mesosteop_analyse

Parameters:

Raw Frames: Pipeline recipes:

8.2 HOWFS mode calibration
HOWFS processing is carried out on the Instrument Workstation, and data is not passed on to the pipeline.

8.2.1 HOWFS Acquire Dome Screen
Name: Identifier: Description: Parameters: Raw Frames: IWS Procedures: Pipeline recipes: HOWFS Acquire Dome Screen VIRCAM_howfs_acq_domescreen.tsf Set camera into HOWFS mode and select HOWFS intermediate filter. Move telescope to dome illuminated screen, set tracking off and set illumination level. Filter, screen illumination lamp combination. None No None

8.2.2 HOWFS Reset
Name: Identifier: Description: Parameters: Raw Frames: IWS Procedures: Pipeline recipes: HOWFS Reset VIRCAM_howfs_cal_reset.tsf Make a series of reset exposures suitable for calibrating HOWFS observations. Filter (Dark), number of frames. FITS Yes None


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8.2.3 HOWFS Dark
Name: Identifier: Description: Parameters: Raw Frames: IWS Procedures: Pipeline recipes: HOWFS Dark VIRCAM_howfs_cal_dark.tsf Make several dark exposures suitable for calibrating HOWFS observations. Filter, integration time, number of integrations. FITS Yes None

8.2.4 HOWFS Dome Flat
Name: Identifier: Description: Parameters: Raw Frames: IWS Procedures: Pipeline recipes: HOWFS Dome Flat VIRCAM_howfs_cal_domeflat.tsf Make a flat-field exposure (or exposures) suitable for calibrating HOWFS observations. Filter & illumination combination, integration time, number of integrations, focal plane X, Y, and detector window size. FITS Yes None

8.3 Imaging Mode Science Templates
The nesting of the observing loops is described in the same way as in the URD [AD2] using a shorthand based on the order of nesting of the loops for the 6 components, (F for filter, T for tile, P for pawprint, J for jitter, M for microstep, E for exposure), with the order of the letters indicating increasing nesting of the loop as one reads to the right.

8.3.1 Acquire
Name: Identifier: Description:
Acquire VIRCAM_img_acq.tsf Acquire single target. Check/Set camera to IMAGING mode, check/set camera position angle, check/select first science filter, all in parallel with a preset of telescope to new target, optionally (and usually) guide, optionally (and usually) activate LOWFS. The flat-field lamp is checked and automatically switched off when the telescope presets to a new celestial target.

i.e. nest Preset to defined position Check/Set IMAGING mode in parallel Check/Set camera PA in parallel [default +X axis to +RA] Check/Set first filter in parallel If guiding required


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Parameters:

Raw Frames: Pipeline recipes:

Acquire guide star LOWFS on two stars in parallel Target coordinates, focal plane position to be at target position [e.g. centre of camera (default), or specified offset from centre of camera, or centre of a specified detector], camera position angle (E of N on sky, defaults to give +X to +RA), first filter, autoguiding required flag, if set (default) coordinates for 1 guide star from the SDT, LOWFS required flag, if set (default) 1 pair LOWFS stars found by the SDT. None None

8.3.2 Observe Paw
Name: Identifier: Description: Observe VIRCAM_img_obs_paw.tsf This template makes one "pawprint" observation using a selection of filter changes, jittering and microstep movements. It is assumed the telescope has already been positioned at the target using the acquisition template. The detector controller is configured with the required readout and exposure times and the following sequence executed: FJME -- step through science filters in outer loop. At each science filter execute a jitter pattern (if specified), and within each jitter pattern execute a microstep pattern (if specified) List of science filters Number of jitter positions, [optional: jitter pattern ID, jitter scale factor] Number of microstep patterns, [optional: microstep pattern ID, microstep scale factor] Number of exposures Integration time Number of integrations [optional: New camera-position angle] As many FITS files as there are exposures vircam_jitter_microstep_process The pipeline handles microstepped and jittered exposures differently. To just perform exposures at a fixed position set J=1 and M=1 To just perform a jitter pattern with no microsteps set M=1 To just perform a microstep pattern with no jitters set J=1

Parameters:

Raw Frames: Pipeline recipes: Note:


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8.3.3 Observe Tile
Name: Identifier: Description:

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Observe Tile VIRCAM_img_obs_tile.tsf This template makes sufficient observations to generate a contiguous "tile", using a selection of pawprints, filter changes, jittering and microstep movements. It is assumed the telescope has already been pointed to the null target with the acquisition template. The detector controller is configured with the required readout and exposure time parameters and one of the following sequences executed: FPJME ­ Construct the tile from a series of pawprints, repeating each pawprint with a different science filter. Within each pawprint execute a jitter pattern (if specified), and within each jitter pattern execute a microstep pattern (if specified). PFJME ­ Construct the tile from a series of pawprints. Within each pawprint execute a jitter pattern, except, this time repeat each jitter with a different science filter before moving on to the next. Within each jitter, execute a microstep pattern (if specified). FJPME ­ Construct the tile from a pawprint and jitter pattern such that one jitter observation is made from each pawprint in turn. Within each jitter pattern there can be a microstep pattern. The whole sequence may be repeated with different science filters. Each time a new pawprint is selected, the TCS is provided with a new guide star and a new pair of LOWFS stars, taken from the list provided by the template. i.e. nest FPJME For each Filter For each pawprint position (1 to P) Check/offset telescope (steps 5-10) Acquire new guide and LOWFS stars For each jitter position (1 to J) Check/Move telescope (steps <30, same guide star) For each microstep (1 to M) Check/Move telescope (steps <3, same guide star) For each exposure (1 to E) Make exposure Next exposure Next microstep Next jitter Next pawprint Next Filter

Parameters:

Nesting pattern (FPJME, PFJME or FJPME as above) List of science filters Tile pattern ID, tile scale factor


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Raw Frames: Pipeline Recipes: Note

List of [guide star plus two HOWFS stars] for each pawprint in the tile pattern Number of jitter positions, [optional: jitter pattern ID, jitter scale factor], Number of microstep positions, [optional: microstep pattern ID, microstep scale factor] Number of exposures Integration time Number of integrations As many FITS files as there are exposures vircam_jitter_microstep_process The pipeline handles microstepped and jittered exposures in a different way.

8.3.4 Observe Offsets
Name: Identifier: Description:
Observe Offsets VIRCAM_img_obs_offsets.tsf Similar to Observe Tile except the offsets are not limited to a set of pre-defined offset patterns. The purpose is to allow the versatility of more general sets of offsets, rather than those offset pattern that have been predefined for produce a simple tile. List of science filters Tile pattern ID Tile scale factor List of [guide star plus two LOWFS stars] for each offset List of RA, Dec offsets Number of exposures Integration time Number of integrations [optional: list of position-angle offsets] (Number of pawprint locations â number of exposure in each pawprint) FITS files vircam_jitter_microstep_process Pipeline produces pawprints, these are not merged.

Parameters:

Raw Frames: Pipeline recipes: Note

8.3.5 Observing a set of Tiles
Three templates (FTPJME, TFPJME and TPFJME) that observe more than one tile were outlined in the URD [AD2]. The template design has now been considerably streamlined such that the required behaviour can be realised with the observe-tile template, or with multiple templates within an OB.


DATA FLOW Calibration Plan SYSTEM 8.4 HOWFS mode data

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HOWFS processing is carried out on the Instrument Workstation, and data is not passed on to the pipeline.

8.4.1 HOWFS Acquire
Name: Identifier: Description: HOWFS Acquire VIRCAM_howfs_acq.tsf Acquire a HOWFS (High-Order Wave Front Sensor) source. Set instrument into HOWFS mode which selects HOWFS intermediate filter. If guiding and LOWFS are required, set guide star and two LOWFS coordinate sets. HOWFS filter Target coordinates and camera position angle [optionally: guide star, two LOWFS stars] focal plane X,Y None None None

Parameters:

Raw frames: IWS Procedures: Pipeline recipes:

8.4.2 HOWFS Wave front
Name: Identifier: Description: HOWFS wave front VIRCAM_howfs_obs_wfront.tsf Make a HOWFS wave front measurement for measuring the current residual from the active optics lookup table. This will typically be done only ~ twice per night, once at the start of the night, and once around midnight if necessary. HOWFS filter focal plane X,Y and detector window size integration time number of integrations [optional: max iterations, number of coefficients, name of file] FITS Trigger HOWFS analysis system, forward coefficient residuals to TCS None

Parameters:

Raw Frames: IWS Procedures: Pipeline recipes:

8.4.3 HOWFS Expose
Name: Identifier: HOWFS Expose VIRCAM_howfs_obs_exp.tsf


DATA FLOW Calibration Plan SYSTEM
Description:

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Parameters:

Raw Frames: IWS Procedures: Pipeline recipes:

Make a HOWFS wave front measurement suitable for populating the active optics lookup tables in the TCS. This will be done only very occasionally [~quarterly] in engineering time and does not form part of the routine operations. HOWFS filter focal plane X,Y and detector window size integration time number of integrations [optional: max iterations, number of coefficients, name of file] FITS Trigger HOWFS analysis system, produce look up table. None

8.5 Instrument Health Templates
Instrument health monitoring templates are defined in [RD5] and are run on a regular basis. For example the instrument filter wheel is tested regularly for position repeatability, and this may determine how often to repeat a flat-field calibration with a particular science filter. The templates in [RD5] are not repeated here, since these monitoring outputs are not processed by the VISTA pipeline and hence are not described in this Calibration Plan.


DATA FLOW Calibration Plan SYSTEM

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9 Technical Programs
9.1 TP-VIS1: Establishment of Secondary Standard Fields
This section outlines the procedures required to establish a network of secondary standard fields early in the operation of VIRCAM.

Figure 9-1 Distribution of the 2MASS touchstone fields on the sky

Name: Secondary Standard Fields Program Identifier: TP-VIS1-IMA-PHO-0001 Purpose: Provide secondary standards for VISTA for routine calibrations (see Section 5) Description: A programme of observations around the primary standards is required to make direct measurements of all the secondary standards in the VIRCAM filter system. These observations will be repeated throughout the year to minimize the errors in the secondary star measurements, to identify variables, and to provide full coverage in Right Ascension. These fields are chosen to ensure photometric pedigree and are drawn from the list of 2MASS touchstone fields [RD9] and from published lists of photometric standards ([RD10], [RD11], [RD16]). Many of these fields are also WFCAM calibration fields. The secondary standard fields are tabulated in Appendix A. Observing Conditions: Photometric Frequency: Complete night at quarterly intervals over first 2 years of VIRCAM operations to ensure the photometric pedigree and accuracy of the standard fields Special Conditions: None Analysis procedure: A master catalogue of standard stars will be derived for each field with photometry in each of the VIRCAM filters.


DATA FLOW Calibration Plan SYSTEM

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Photometry will be measured using standard VFDS pipeline procedures [RD1]. Products: Z, Y, J, H, S magnitudes of ~1500 secondary standards in each field Accuracies: The target is 0.005 magnitude rms for secondary standards in each waveband after two years of repeated observations. Responsible Person: JPE


DATA FLOW Calibration Plan SYSTEM

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10

Format of Data Frames

10.1 Principle
There is only one data format, used in both IMAGING and HOWFS modes. Data frames will be in ESO modified standard FITS format [RD12], the ESO modifications being limited to the hierarchical header proposal. The headers are compliant with the final World Coordinate System (WCS) specification [RD13]. Data from the full set of chips is stored in Multi Extension Format (MEF) as 32-bit signed integers [RD12], each extension corresponding to a particular detector. Offset 16-bit format is not used because data will be co-added in the data acquisition system before output. Though not a requirement, the integer format enables the use of highly efficient lossless compression.

10.2 Model FITS header
A model FITS header for raw data is presented in Table 10-1. In addition to the header shown in the model, standard pipelineprocessing keywords will be inserted into the data products.
SIMPLE = T / Standard FITS format (NOST-100.0) BITPIX = 8 / # of bits storing pix values NAXIS = 0 / # of axes in frame EXTEND = T / Extension may be present ORIGIN = 'ESO ' / European Southern Observatory DATE = '2006-03-21T15:06:48' / Date this file was written TELESCOP= 'VISTA ' / ESO Telescope Name INSTRUME= 'VIRCAM ' / Instrument used. OBJECT = 'OBJECT ' / Original target. RA = 318.346792 / 21:13:23.2 RA (J2000) pointing (deg) DEC = -88.93761 / -88:56:15.3 DEC (J2000) pointing (deg) EQUINOX = 2000. / Standard FK5 (years) RADECSYS= 'FK5 ' / Coordinate reference frame EXPTIME = 10.0000000 / Integration time MJD-OBS = 53815.62973579 / Obs start DATE-OBS= '2006-03-21T15:06:49.1726' / Observing date UTC = 54270.829 / 15:04:30.829 UTC at start (sec) LST = 80333.420 / 22:18:53.420 LST at start (sec) PI-COI = 'J.Lewis-P.Bunclark' / PI-COI name. OBSERVER= 'Peter Bunclark' / Name of observer. ORIGFILE= 'VIRCAM_IMG_OBS080_0001.fits' / Original File Name COMMENT VISTA IR Camera OS $Revision: 0.21 $ HIERARCH ESO ADA ABSROT END = 0.00000 / Abs rot angle at exp end (deg) HIERARCH ESO DPR CATG = 'TEST ' / Observation category HIERARCH ESO DPR TECH = 'IMAGE,FILTOFFSET' / Observation technique HIERARCH ESO DPR TYPE = 'STD,STRAYLIGHT' / Observation type HIERARCH ESO INS DATE = '2005-12-14' / Instrument release date (yyyy-mm-d HIERARCH ESO INS FILT1 DATE = '2006-01-27T10:02:27' / Filter index time HIERARCH ESO INS FILT1 FOCUS = 0.000 / Filter focus offset [mm] HIERARCH ESO INS FILT1 ID = 'SLOT8 ' / Filter unique id HIERARCH ESO INS FILT1 NAME = 'Y ' / Filter name HIERARCH ESO INS FILT1 NO = 25 / Filter wheel position index HIERARCH ESO INS FILT1 WLEN = 0.000 / Filter effective wavelength [nm] HIERARCH ESO INS HB1 SWSIM = F / If T, heart beat device simulated HIERARCH ESO INS ID = 'VIRCAM/1.56' / Instrument ID HIERARCH ESO INS LSC1 OK = T / If T, controller is operational HIERARCH ESO INS LSC1 SWSIM = F / If T, lakeshore ctrllr simulated HIERARCH ESO INS LSM1 OK = T / If T, controller is operational HIERARCH ESO INS LSM1 SWSIM = F / If T, lakeshore monitor simulated HIERARCH ESO INS LSM2 OK = T / If T, controller is operational HIERARCH ESO INS LSM2 SWSIM = F / If T, lakeshore monitor simulated


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS LSM3 OK LSM3 SWSIM PRES1 ID PRES1 NAME PRES1 UNIT PRES1 VAL SW1 ID SW1 NAME SW1 STATUS SW2 ID SW2 NAME SW2 STATUS SW3 ID SW3 NAME SW3 STATUS TEMP1 ID TEMP1 NAME TEMP1 UNIT TEMP1 VAL TEMP10 ID TEMP10 NAME TEMP10 UNIT TEMP10 VAL TEMP12 ID TEMP12 NAME TEMP12 UNIT TEMP12 VAL TEMP14 ID TEMP14 NAME TEMP14 UNIT TEMP14 VAL TEMP15 ID TEMP15 NAME TEMP15 UNIT TEMP15 VAL TEMP16 ID TEMP16 NAME TEMP16 UNIT TEMP16 VAL TEMP17 ID TEMP17 NAME TEMP17 UNIT TEMP17 VAL TEMP18 ID TEMP18 NAME TEMP18 UNIT TEMP18 VAL TEMP19 ID TEMP19 NAME TEMP19 UNIT TEMP19 VAL TEMP2 ID TEMP2 NAME TEMP2 UNIT TEMP2 VAL TEMP20 ID TEMP20 NAME TEMP20 UNIT TEMP20 VAL TEMP21 ID TEMP21 NAME TEMP21 UNIT TEMP21 VAL TEMP22 ID TEMP22 NAME TEMP22 UNIT TEMP22 VAL TEMP23 ID TEMP23 NAME TEMP23 UNIT TEMP23 VAL TEMP24 ID TEMP24 NAME = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = = =

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T / If T, controller is operational F / If T, lakeshore monitor simulated 'Vac1 ' / Pressure sensor type 'Vacuum gauge 1' / Pressure sensor name 'mbar ' / Pressure unit 0.000 / Pressure [mbar] 'INPOS ' / Switch ID 'Filter In-position Switch' / Switch name 'INACTIVE' / Switch status 'REFSW ' / Switch ID 'Filter Reference Select' / Switch name 'PRIMARY ' / Switch status 'HOME ' / Switch ID 'Filter Reference Switch' / Switch name 'INACTIVE' / Switch status 'Amb ' / Temperature sensor type 'Ambient temperature' / Temperature sensor name 'K ' / Temperature unit 302.580 / Temperature [K] 'CC1_2 ' / Temperature sensor type 'Cryo cooler 1 2nd' / Temperature sensor name 'K ' / Temperature unit 24.105 / Temperature [K] 'CC2_2 ' / Temperature sensor type 'Cryo cooler 2 2nd' / Temperature sensor name 'K ' / Temperature unit 27.791 / Temperature [K] 'CC3_2 ' / Temperature sensor type 'Cryo cooler 3 2nd' / Temperature sensor name 'K ' / Temperature unit 22.735 / Temperature [K] 'WFSN ' / Temperature sensor type 'WFS CCD assembly PY' / Temperature sensor name 'K ' / Temperature unit 1.000 / Temperature [K] 'WFSS ' / Temperature sensor type 'WFS CCD assembly NY' / Temperature sensor name 'K ' / Temperature unit 123.550 / Temperature [K] 'Dt1AB ' / Temperature sensor type 'Science detector 1AB' / Temperature sensor name 'K ' / Temperature unit 73.583 / Temperature [K] 'Dt1CD ' / Temperature sensor type 'Science detector 1CD' / Temperature sensor name 'K ' / Temperature unit 73.002 / Temperature [K] 'Dt2BA ' / Temperature sensor type 'Science detector 2BA' / Temperature sensor name 'K ' / Temperature unit 74.668 / Temperature [K] 'Win ' / Temperature sensor type 'Cryostat window cell' / Temperature sensor name 'K ' / Temperature unit 176.710 / Temperature [K] 'Dt2DC ' / Temperature sensor type 'Science detector 2DC' / Temperature sensor name 'K ' / Temperature unit 74.106 / Temperature [K] 'Dt3AB ' / Temperature sensor type 'Science detector 3AB' / Temperature sensor name 'K ' / Temperature unit 74.677 / Temperature [K] 'Dt3CD ' / Temperature sensor type 'Science detector 3CD' / Temperature sensor name 'K ' / Temperature unit 75.485 / Temperature [K] 'Dt4BA ' / Temperature sensor type 'Science detector 4BA' / Temperature sensor name 'K ' / Temperature unit 74.778 / Temperature [K] 'Dt4DC ' / Temperature sensor type 'Science detector 4DC' / Temperature sensor name


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS INS OBS OBS OBS OBS OBS OBS OBS OBS OBS OCS OCS OCS TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL

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TEMP24 UNIT = 'K ' / Temperature unit TEMP24 VAL = 74.544 / Temperature [K] TEMP25 ID = 'FPA ' / Temperature sensor type TEMP25 NAME = 'FPA thermal plate' / Temperature sensor name TEMP25 UNIT = 'K ' / Temperature unit TEMP25 VAL = 69.997 / Temperature [K] TEMP26 ID = 'WFSpl ' / Temperature sensor type TEMP26 NAME = 'WFS plate' / Temperature sensor name TEMP26 UNIT = 'K ' / Temperature unit TEMP26 VAL = 108.360 / Temperature [K] TEMP3 ID = 'Tube ' / Temperature sensor type TEMP3 NAME = 'Cryostat tube' / Temperature sensor name TEMP3 UNIT = 'K ' / Temperature unit TEMP3 VAL = 33.256 / Temperature [K] TEMP4 ID = 'LNtnk ' / Temperature sensor type TEMP4 NAME = 'Liquid nitrogen tank' / Temperature sensor name TEMP4 UNIT = 'K ' / Temperature unit TEMP4 VAL = 103.180 / Temperature [K] TEMP5 ID = 'Baff ' / Temperature sensor type TEMP5 NAME = 'Baffle ' / Temperature sensor name TEMP5 UNIT = 'K ' / Temperature unit TEMP5 VAL = 21.332 / Temperature [K] TEMP6 ID = 'Lens ' / Temperature sensor type TEMP6 NAME = 'Lens barrel' / Temperature sensor name TEMP6 UNIT = 'K ' / Temperature unit TEMP6 VAL = 100.570 / Temperature [K] TEMP7 ID = 'FwShd ' / Temperature sensor type TEMP7 NAME = 'Filter wheel shield' / Temperature sensor name TEMP7 UNIT = 'K ' / Temperature unit TEMP7 VAL = 124.420 / Temperature [K] TEMP8 ID = 'FwHub ' / Temperature sensor type TEMP8 NAME = 'Filter wheel hub' / Temperature sensor name TEMP8 UNIT = 'K ' / Temperature unit TEMP8 VAL = 109.570 / Temperature [K] THERMAL DET MEAN= 0.00 / Detector mean temperature [K] THERMAL DET TARGET= 70.00 / Detector target temperature [K] THERMAL ENABLE= F / If T, enable thermal control VAC1 OK = T / If T, controller is operational VAC1 SWSIM = F / If T, vacuum sensor simulated DID = 'ESO-VLT-DIC.OBS-1.11' / OBS Dictionary GRP = '0 ' / linked blocks ID = -1 / Observation block ID NAME = 'Maintenance' / OB name PI-COI ID = 0 / ESO internal PI-COI ID PI-COI NAME = 'M.Caldwell-A.Born' / PI-COI name PROG ID = 'Maintenance' / ESO program identification START = '2006-01-30T13:54:10' / OB start time TPLNO = 1 / Template number within OB DET1 IMGNAME= 'VIRCAM_GEN_STD' / Data File Name. RECIPE = 'DEFAULT ' / Data reduction recipe to be used REQTIME = 10.000 / Requested integration time [s] ABSROT START= 0.000 / Abs rotator angle at start AIRM END = 0.000 / Airmass at end AIRM START = 0.000 / Airmass at start ALT = 25.691 / Alt angle at start (deg) AMBI FWHM END= -1.00 / Observatory Seeing queried from AS AMBI FWHM START= -1.00 / Observatory Seeing queried from AS AMBI PRES END= 750.00 / Observatory ambient air pressure q AMBI PRES START= 750.00 / Observatory ambient air pressure q AMBI RHUM = 12. / Observatory ambient relative humi AMBI TAU0 = 0.000000 / Average coherence time AMBI TEMP = 10.00 / Observatory ambient temperature qu AMBI WINDDIR= 0. / Observatory ambient wind directio AMBI WINDSP = 10.00 / Observatory ambient wind speed que AO ALT = 0.000000 / Altitude of last closed loop aO AO DATE =' ' / Last closed loop aO AO M1 DATE = '2006-03-21T15:06:47' / Last M1 update AO M2 DATE = '2006-03-21T15:06:46' / Last M2 update AO MODES = 0 / Which aO modes corrected closed lo AZ = 0.317 / Az angle at start (deg) S=0,W=90 DATE = 'not set ' / TCS installation date DID = 'ESO-VLT-DIC.TCS-01.00' / Data dictionary for TEL DID1 = 'ESO-VLT-DIC.VTCS-0.2' / Additional data dict. fo


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH NJITTER = NOFFSETS= NUSTEP = OBSNUM = REQTIME = END XTENSION= BITPIX = NAXIS = NAXIS1 = NAXIS2 = PCOUNT = GCOUNT = EXTNAME = EXTVER = ORIGIN = DATE = EXPTIME = MJD-OBS = DATE-OBS= CTYPE1 = CTYPE2 = CRVAL1 = CRVAL2 = CRPIX1 = ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TEL TPL TPL TPL TPL TPL TPL TPL TPL

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DOME STATUS = 'FULLY-OPEN' / Dome status ECS FLATFIELD= 0 / Flat field level ECS MOONSCR = 0.00 / Moon screen position ECS VENT1 = 0.00 / State of vent i ECS VENT2 = 0.00 / State of vent i ECS VENT3 = 0.00 / State of vent i ECS WINDSCR = 0.00 / Wind screen position FOCU ID = 'CA ' / Telescope focus station ID FOCU VALUE = 0.000 / M2 setting (mm) GEOELEV = 2530. / Elevation above sea level (m) GEOLAT = -24.6157 / Tel geo latitute (+=North) (deg) GEOLON = -70.3976 / Tel geo longitude (+=East) (deg) GUID FWHM = 0.00 / Seeing measured by autoguider GUID STATUS = 'OFF ' / Status of autoguider ID = 'v 0.44 ' / TCS version number M2 ACENTRE = 0.00 / M2 centring alpha M2 ATILT = 0.00 / M2 tilt alpha M2 BCENTRE = 0.00 / M2 centring beta M2 BTILT = 0.00 / M2 tilt beta M2 Z = 0.00000 / Focussing position of M2 in Z coor MOON DEC = -27.46744 / -27:28:02.7 DEC (J2000) (deg) MOON RA = 253.667459 / 16:54:40.1 RA (J2000) (deg) OPER = 'Operator name not set' / Telescope Operator PARANG END = 0.000 / Parallactic angle at end (deg) PARANG START= 0.000 / Parallactic angle at start (deg) POSANG = 0.000 / Rot position angle at start TARG ALPHA = 211323.230 / Alpha coordinate for the target TARG COORDTYPE= 'M ' / Coordinate type (M=mean A=apparent TARG DELTA = -885615.400 / Delta coordinate for the target TARG EPOCH = 2000.000 / Epoch TARG EPOCHSYSTEM= 'J ' / Epoch system (default J=Julian) TARG EQUINOX= 2000.000 / Equinox TARG PARALLAX= 0.000 / Parallax TARG PMA = 0.000000 / Proper Motion Alpha TARG PMD = 0.000000 / Proper motion Delta TARG RADVEL = 0.000 / Radial velocity TH M1 TEMP = 0.00 / M1 superficial temperature TH STR TEMP = 0.00 / Telescope structure temperature TRAK STATUS = 'NORMAL ' / Tracking status DID = 'ESO-VLT-DIC.TPL-1.9' / Data dictionary for TPL EXPNO = 1 / Exposure number within template ID = 'VIRCAM_gen_tec_StrayLight' / Template signature NAME = 'VIRCAM stray light investigation' / Template nam NEXP = 6 / Number of exposures within templat PRESEQ = 'VIRCAM_gen_tec_StrayLight.seq' / Sequencer scrip START = '2006-01-30T13:54:10' / TPL start time VERSION = '$Revision: 0.13 $' / Version of the template 0 / Number of jitter positions 0 / Number of offset positions 0 / Number of microstep positions 1 / Observation number 10.000 / Requested integration time [s] ' 32 2 2048 2048 0 1 / / / / / / / / IMAGE extension # of bits per pix value # of axes in data array # of pixels in axis1 # of pixels in axis2 number of random group parameters number of random groups Extension name

'IMAGE

'DET1.CHIP9' 1 / Extension version 'ESO ' / European Southern Observatory '2006-01-30T13:54:47.7333' / Date the file was written 10.0000000 / Integration time 53765.57956362 / Obs start 2006-01-30T13:54:34.297 '2006-01-30T13:54:34.2967' / Observing date 'RA---ZPN' / Coord type of celestial axis 1 'DEC--ZPN' / Coord type of celestial axis 2 318.346791667 / RA at reference pixel -88.9376111111 / Dec at reference pixel 5401.6 / Pixel coordinate at ref point


DATA FLOW Calibration Plan SYSTEM
CRPIX2 CDELT1 CDELT2 CD1_1 CD1_2 CD2_1 CD2_2 HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH = = = = = = =

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6860.8 / Pixel coordinate at ref point 9.49444444444444E-05 / Coordinate increment -9.49444444444444E-05 / Coordinate increment 5.81347849634012E-21 / WCS transform matrix element 9.49444444444444E-05 / WCS transform matrix element -9.49444444444444E-05 / WCS transform matrix element -5.81347849634012E-21 / WCS transform matrix element ESO DET CHIP ID = 'ESO-Virgo45' / Detector ID ESO DET CHIP LIVE = T / Detector live or broken ESO DET CHIP NAME = 'Virgo' / Detector name ESO DET CHIP NO = 9 / Unique Detector Number ESO DET CHIP NX = 2048 / Pixels in X ESO DET CHIP NY = 2048 / Pixels in Y ESO DET CHIP PXSPACE= 2.000e-05 / Pixel-Pixel Spacing ESO DET CHIP TYPE = 'IR' / The Type of Det Chip ESO DET CHIP VIGNETD = F / Detector chip vignetted? ESO DET CHIP X = 3 / Detector position x-axis ESO DET CHIP Y = 4 / Detector position y-axis ESO DET CHOP FREQ = 0 / Chopping Frequency ESO DET CON OPMODE = 'NORMAL' / Operational Mode ESO DET DID = 'ESO-VLT-DIC.IRACE-1.34' / Dictionary Name and Re ESO DET DIT = 10.0000000 / Integration Time ESO DET DITDELAY = 0.000 / Pause Between DITs ESO DET EXP NAME = 'VIRCAM_GEN_STD030_0001' / Exposure Name ESO DET EXP NO = 3 / Exposure number ESO DET EXP UTC = '2006-01-30T13:54:47.7333' / File Creation Time ESO DET FRAM NO = 1 / Frame number ESO DET FRAM TYPE = 'INT' / Frame type ESO DET FRAM UTC = '2006-01-30T13:54:46.7037' / Time Recv Frame ESO DET IRACE ADC1 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC1 ENABLE= 1 / Enable ADC Board (0/1) ESO DET IRACE ADC1 FILTER1= 0 / ADC Filter1 Adjustment ESO DET IRACE ADC1 FILTER2= 0 / ADC Filter2 Adjustment ESO DET IRACE ADC1 HEADER= 1 / Header of ADC Board ESO DET IRACE ADC1 NAME= 'VISTA-AQ-GRP' / Name for ADC Board ESO DET IRACE ADC10 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC10 ENABLE= 1 / Enable ADC Board (0/1) ESO DET IRACE ADC10 FILTER1= 0 / ADC Filter1 Adjustment ESO DET IRACE ADC10 FILTER2= 0 / ADC Filter2 Adjustment ESO DET IRACE ADC10 HEADER= 1 / Header of ADC Board ESO DET IRACE ADC10 NAME= 'VISTA-AQ-GRP' / Name for ADC Board ESO DET IRACE ADC11 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC11 ENABLE= 1 / Enable ADC Board (0/1) ESO DET IRACE ADC11 FILTER1= 0 / ADC Filter1 Adjustment ESO DET IRACE ADC11 FILTER2= 0 / ADC Filter2 Adjustment ESO DET IRACE ADC11 HEADER= 1 / Header of ADC Board ESO DET IRACE ADC11 NAME= 'VISTA-AQ-GRP' / Name for ADC Board ESO DET IRACE ADC12 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC12 ENABLE= 1 / Enable ADC Board (0/1) ESO DET IRACE ADC12 FILTER1= 0 / ADC Filter1 Adjustment ESO DET IRACE ADC12 FILTER2= 0 / ADC Filter2 Adjustment ESO DET IRACE ADC12 HEADER= 1 / Header of ADC Board ESO DET IRACE ADC12 NAME= 'VISTA-AQ-GRP' / Name for ADC Board ESO DET IRACE ADC13 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC13 ENABLE= 1 / Enable ADC Board (0/1) ESO DET IRACE ADC13 FILTER1= 0 / ADC Filter1 Adjustment ESO DET IRACE ADC13 FILTER2= 0 / ADC Filter2 Adjustment ESO DET IRACE ADC13 HEADER= 1 / Header of ADC Board ESO DET IRACE ADC13 NAME= 'VISTA-AQ-GRP' / Name for ADC Board ESO DET IRACE ADC14 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC14 ENABLE= 1 / Enable ADC Board (0/1) ESO DET IRACE ADC14 FILTER1= 0 / ADC Filter1 Adjustment ESO DET IRACE ADC14 FILTER2= 0 / ADC Filter2 Adjustment ESO DET IRACE ADC14 HEADER= 1 / Header of ADC Board ESO DET IRACE ADC14 NAME= 'VISTA-AQ-GRP' / Name for ADC Board ESO DET IRACE ADC15 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC15 ENABLE= 1 / Enable ADC Board (0/1) ESO DET IRACE ADC15 FILTER1= 0 / ADC Filter1 Adjustment ESO DET IRACE ADC15 FILTER2= 0 / ADC Filter2 Adjustment ESO DET IRACE ADC15 HEADER= 1 / Header of ADC Board ESO DET IRACE ADC15 NAME= 'VISTA-AQ-GRP' / Name for ADC Board ESO DET IRACE ADC16 DELAY= 7 / ADC Delay Adjustment ESO DET IRACE ADC16 ENABLE= 1 / Enable ADC Board (0/1)


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET

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IRACE ADC16 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC16 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC16 HEADER= 1 / Header of ADC Board IRACE ADC16 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC2 DELAY= 7 / ADC Delay Adjustment IRACE ADC2 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC2 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC2 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC2 HEADER= 1 / Header of ADC Board IRACE ADC2 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC3 DELAY= 7 / ADC Delay Adjustment IRACE ADC3 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC3 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC3 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC3 HEADER= 1 / Header of ADC Board IRACE ADC3 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC4 DELAY= 7 / ADC Delay Adjustment IRACE ADC4 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC4 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC4 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC4 HEADER= 1 / Header of ADC Board IRACE ADC4 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC5 DELAY= 7 / ADC Delay Adjustment IRACE ADC5 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC5 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC5 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC5 HEADER= 1 / Header of ADC Board IRACE ADC5 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC6 DELAY= 7 / ADC Delay Adjustment IRACE ADC6 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC6 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC6 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC6 HEADER= 1 / Header of ADC Board IRACE ADC6 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC7 DELAY= 7 / ADC Delay Adjustment IRACE ADC7 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC7 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC7 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC7 HEADER= 1 / Header of ADC Board IRACE ADC7 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC8 DELAY= 7 / ADC Delay Adjustment IRACE ADC8 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC8 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC8 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC8 HEADER= 1 / Header of ADC Board IRACE ADC8 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE ADC9 DELAY= 7 / ADC Delay Adjustment IRACE ADC9 ENABLE= 1 / Enable ADC Board (0/1) IRACE ADC9 FILTER1= 0 / ADC Filter1 Adjustment IRACE ADC9 FILTER2= 0 / ADC Filter2 Adjustment IRACE ADC9 HEADER= 1 / Header of ADC Board IRACE ADC9 NAME= 'VISTA-AQ-GRP' / Name for ADC IRACE SEQCONT= 'F' / Sequencer Continuous Mode MINDIT = 1.0011000 / Minimum DIT MODE NAME = '' / DCS Detector Mode NCORRS = 2 / Read-Out Mode NCORRS NAME = 'Double' / Read-Out Mode Name NDIT = 1 / # of Sub-Integrations NDITSKIP = 0 / DITs skipped at 1st.INT RSPEED = 1 / Read-Speed Factor RSPEEDADD = 0 / Read-Speed Add VOLT1 CLKHI1= 4.0000 / Set Value High-Clock VOLT1 CLKHI10= 4.0000 / Set Value High-Clock VOLT1 CLKHI11= 4.0000 / Set Value High-Clock VOLT1 CLKHI12= 5.0000 / Set Value High-Clock VOLT1 CLKHI13= 1.0000 / Set Value High-Clock VOLT1 CLKHI14= 4.0000 / Set Value High-Clock VOLT1 CLKHI15= 0.0000 / Set Value High-Clock VOLT1 CLKHI16= 2.5000 / Set Value High-Clock VOLT1 CLKHI2= 4.0000 / Set Value High-Clock VOLT1 CLKHI3= 4.0000 / Set Value High-Clock VOLT1 CLKHI4= 5.0000 / Set Value High-Clock VOLT1 CLKHI5= 1.0000 / Set Value High-Clock

Board

Board

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Board


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1

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CLKHI6= 4.0000 / Set Value High-Clock CLKHI7= 0.0000 / Set Value High-Clock CLKHI8= 2.5000 / Set Value High-Clock CLKHI9= 4.0000 / Set Value High-Clock CLKHINM1= 'clk1Hi pmc' / Name of High-Clock CLKHINM10= 'clk10Hi FrameStart' / Name of High-Clock CLKHINM11= 'clk11Hi UcResetEnable' / Name of High-Clock CLKHINM12= 'clk12Hi VHiRowEnable' / Name of High-Clock CLKHINM13= 'clk13Hi VLoRowEnable' / Name of High-Clock CLKHINM14= 'clk14Hi VHiReset' / Name of High-Clock CLKHINM15= 'clk15Hi VLoReset' / Name of High-Clock CLKHINM16= 'clk16Hi VpOut' / Name of High-Clock CLKHINM2= 'clk2Hi FrameStart' / Name of High-Clock CLKHINM3= 'clk3Hi UcResetEnable' / Name of High-Clock CLKHINM4= 'clk4Hi VHiRowEnable' / Name of High-Clock CLKHINM5= 'clk5Hi VLoRowEnable' / Name of High-Clock CLKHINM6= 'clk6Hi VHiReset' / Name of High-Clock CLKHINM7= 'clk7Hi VLoReset' / Name of High-Clock CLKHINM8= 'clk8Hi VpOut' / Name of High-Clock CLKHINM9= 'clk9Hi pmc' / Name of High-Clock CLKHIT1= 4.0283 / Tel Value High-Clock CLKHIT10= 4.0234 / Tel Value High-Clock CLKHIT11= 4.0234 / Tel Value High-Clock CLKHIT12= 5.0244 / Tel Value High-Clock CLKHIT13= 1.0352 / Tel Value High-Clock CLKHIT14= 4.0283 / Tel Value High-Clock CLKHIT15= 0.0439 / Tel Value High-Clock CLKHIT16= 2.5293 / Tel Value High-Clock CLKHIT2= 4.0283 / Tel Value High-Clock CLKHIT3= 4.0283 / Tel Value High-Clock CLKHIT4= 5.0195 / Tel Value High-Clock CLKHIT5= 1.0352 / Tel Value High-Clock CLKHIT6= 4.0332 / Tel Value High-Clock CLKHIT7= 0.0439 / Tel Value High-Clock CLKHIT8= 2.5293 / Tel Value High-Clock CLKHIT9= 4.0430 / Tel Value High-Clock CLKLO1= 0.0000 / Set value Low-Clock CLKLO10= 0.0000 / Set value Low-Clock CLKLO11= 0.0000 / Set value Low-Clock CLKLO12= 5.0000 / Set value Low-Clock CLKLO13= 1.0000 / Set value Low-Clock CLKLO14= 4.0000 / Set value Low-Clock CLKLO15= 0.0000 / Set value Low-Clock CLKLO16= 9.7500 / Set value Low-Clock CLKLO2= 0.0000 / Set value Low-Clock CLKLO3= 0.0000 / Set value Low-Clock CLKLO4= 5.0000 / Set value Low-Clock CLKLO5= 1.0000 / Set value Low-Clock CLKLO6= 4.0000 / Set value Low-Clock CLKLO7= 0.0000 / Set value Low-Clock CLKLO8= 9.7500 / Set value Low-Clock CLKLO9= 0.0000 / Set value Low-Clock CLKLONM1= 'clk1Lo pmc' / Name of Low-Clock CLKLONM10= 'clk10Lo FrameStart' / Name of Low-Clock CLKLONM11= 'clk11Lo UcResetEnable' / Name of Low-Clock CLKLONM12= 'clk12Lo VHiRowEnable' / Name of Low-Clock CLKLONM13= 'clk13Lo VLoRowEnable' / Name of Low-Clock CLKLONM14= 'clk14Lo VHiReset' / Name of Low-Clock CLKLONM15= 'clk15Lo VLoReset' / Name of Low-Clock CLKLONM16= 'clk16Lo VpOut' / Name of Low-Clock CLKLONM2= 'clk2Lo FrameStart' / Name of Low-Clock CLKLONM3= 'clk3Lo UcResetEnable' / Name of Low-Clock CLKLONM4= 'clk4Lo VHiRowEnable' / Name of Low-Clock CLKLONM5= 'clk5Lo VLoRowEnable' / Name of Low-Clock CLKLONM6= 'clk6Lo VHiReset' / Name of Low-Clock CLKLONM7= 'clk7Lo VLoReset' / Name of Low-Clock CLKLONM8= 'clk8Lo VpOut' / Name of Low-Clock CLKLONM9= 'clk9Lo pmc' / Name of Low-Clock CLKLOT1= 0.0391 / Tel Value Low-Clock CLKLOT10= 0.0391 / Tel Value Low-Clock CLKLOT11= 0.0439 / Tel Value Low-Clock CLKLOT12= 4.9609 / Tel Value Low-Clock CLKLOT13= 1.0254 / Tel Value Low-Clock


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1 VOLT1

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CLKLOT14= 4.0283 / Tel Value Low-Clock CLKLOT15= 0.0342 / Tel Value Low-Clock CLKLOT16= 9.4824 / Tel Value Low-Clock CLKLOT2= 0.0391 / Tel Value Low-Clock CLKLOT3= 0.0293 / Tel Value Low-Clock CLKLOT4= 4.9609 / Tel Value Low-Clock CLKLOT5= 1.0303 / Tel Value Low-Clock CLKLOT6= 4.0234 / Tel Value Low-Clock CLKLOT7= 0.0342 / Tel Value Low-Clock CLKLOT8= 9.4775 / Tel Value Low-Clock CLKLOT9= 0.0439 / Tel Value Low-Clock DC1 = -2.3600 / Set value DC-Voltage DC10 = -3.3500 / Set value DC-Voltage DC11 = 0.0000 / Set value DC-Voltage DC12 = 0.7000 / Set value DC-Voltage DC13 = 0.7000 / Set value DC-Voltage DC14 = 3.5000 / Set value DC-Voltage DC15 = 2.2000 / Set value DC-Voltage DC16 = 3.3000 / Set value DC-Voltage DC2 = -3.3500 / Set value DC-Voltage DC3 = 0.0000 / Set value DC-Voltage DC4 = 0.7000 / Set value DC-Voltage DC5 = 0.7000 / Set value DC-Voltage DC6 = 3.5000 / Set value DC-Voltage DC7 = 2.2000 / Set value DC-Voltage DC8 = 3.3000 / Set value DC-Voltage DC9 = -2.3600 / Set value DC-Voltage DCNM1 = 'DC1 VIdle' / Name of DC-voltage DCNM10= 'DC10 VSlew' / Name of DC-voltage DCNM11= 'DC11 VRstUc' / Name of DC-voltage DCNM12= 'DC12 VDetCom' / Name of DC-voltage DCNM13= 'DC13 VnUc' / Name of DC-voltage DCNM14= 'DC14 VpUc' / Name of DC-voltage DCNM15= 'DC15 VnOut' / Name of DC-voltage DCNM16= 'DC16 RefBias' / Name of DC-voltage DCNM2 = 'DC2 VSlew' / Name of DC-voltage DCNM3 = 'DC3 VRstUc' / Name of DC-voltage DCNM4 = 'DC4 VDetCom' / Name of DC-voltage DCNM5 = 'DC5 VnUc' / Name of DC-voltage DCNM6 = 'DC6 VpUc' / Name of DC-voltage DCNM7 = 'DC7 VnOut' / Name of DC-voltage DCNM8 = 'DC8 RefBias' / Name of DC-voltage DCNM9 = 'DC9 VIdle' / Name of DC-voltage DCTA1 = -2.3633 / Tel Value 1 for DC DCTA10= -3.3594 / Tel Value 1 for DC DCTA11= 0.0000 / Tel Value 1 for DC DCTA12= 0.7031 / Tel Value 1 for DC DCTA13= 0.7031 / Tel Value 1 for DC DCTA14= 3.5010 / Tel Value 1 for DC DCTA15= 2.1973 / Tel Value 1 for DC DCTA16= 3.3008 / Tel Value 1 for DC DCTA2 = -3.3545 / Tel Value 1 for DC DCTA3 = 0.0049 / Tel Value 1 for DC DCTA4 = 0.6982 / Tel Value 1 for DC DCTA5 = 0.6982 / Tel Value 1 for DC DCTA6 = 3.5010 / Tel Value 1 for DC DCTA7 = 2.1973 / Tel Value 1 for DC DCTA8 = 3.2959 / Tel Value 1 for DC DCTA9 = -2.3682 / Tel Value 1 for DC DCTB1 = -2.3535 / Tel Value 2 for DC DCTB10= -3.3203 / Tel Value 2 for DC DCTB11= 0.0000 / Tel Value 2 for DC DCTB12= 0.6982 / Tel Value 2 for DC DCTB13= 0.7031 / Tel Value 2 for DC DCTB14= 3.5010 / Tel Value 2 for DC DCTB15= 2.1826 / Tel Value 2 for DC DCTB16= 3.2959 / Tel Value 2 for DC DCTB2 = -3.3154 / Tel Value 2 for DC DCTB3 = 0.0000 / Tel Value 2 for DC DCTB4 = 0.6982 / Tel Value 2 for DC DCTB5 = 0.6982 / Tel Value 2 for DC DCTB6 = 3.4961 / Tel Value 2 for DC DCTB7 = 2.1826 / Tel Value 2 for DC


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET VOLT1 VOLT1 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2

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DCTB8 = 3.2959 / Tel Value 2 for DC DCTB9 = -2.3584 / Tel Value 2 for DC CLKHI1= 4.0000 / Set Value High-Clock CLKHI10= 4.0000 / Set Value High-Clock CLKHI11= 4.0000 / Set Value High-Clock CLKHI12= 5.0000 / Set Value High-Clock CLKHI13= 1.0000 / Set Value High-Clock CLKHI14= 4.0000 / Set Value High-Clock CLKHI15= 0.0000 / Set Value High-Clock CLKHI16= 2.5000 / Set Value High-Clock CLKHI2= 4.0000 / Set Value High-Clock CLKHI3= 4.0000 / Set Value High-Clock CLKHI4= 5.0000 / Set Value High-Clock CLKHI5= 1.0000 / Set Value High-Clock CLKHI6= 4.0000 / Set Value High-Clock CLKHI7= 0.0000 / Set Value High-Clock CLKHI8= 2.5000 / Set Value High-Clock CLKHI9= 4.0000 / Set Value High-Clock CLKHINM1= 'clk1Hi pmc' / Name of High-Clock CLKHINM10= 'clk10Hi FrameStart' / Name of High-Clock CLKHINM11= 'clk11Hi UcResetEnable' / Name of High-Clock CLKHINM12= 'clk12Hi VHiRowEnable' / Name of High-Clock CLKHINM13= 'clk13Hi VLoRowEnable' / Name of High-Clock CLKHINM14= 'clk14Hi VHiReset' / Name of High-Clock CLKHINM15= 'clk15Hi VLoReset' / Name of High-Clock CLKHINM16= 'clk16Hi VpOut' / Name of High-Clock CLKHINM2= 'clk2Hi FrameStart' / Name of High-Clock CLKHINM3= 'clk3Hi UcResetEnable' / Name of High-Clock CLKHINM4= 'clk4Hi VHiRowEnable' / Name of High-Clock CLKHINM5= 'clk5Hi VLoRowEnable' / Name of High-Clock CLKHINM6= 'clk6Hi VHiReset' / Name of High-Clock CLKHINM7= 'clk7Hi VLoReset' / Name of High-Clock CLKHINM8= 'clk8Hi VpOut' / Name of High-Clock CLKHINM9= 'clk9Hi pmc' / Name of High-Clock CLKHIT1= 4.0283 / Tel Value High-Clock CLKHIT10= 4.0234 / Tel Value High-Clock CLKHIT11= 4.0186 / Tel Value High-Clock CLKHIT12= 5.0098 / Tel Value High-Clock CLKHIT13= 1.0400 / Tel Value High-Clock CLKHIT14= 4.0283 / Tel Value High-Clock CLKHIT15= 0.0488 / Tel Value High-Clock CLKHIT16= 2.5342 / Tel Value High-Clock CLKHIT2= 4.0234 / Tel Value High-Clock CLKHIT3= 4.0283 / Tel Value High-Clock CLKHIT4= 5.0195 / Tel Value High-Clock CLKHIT5= 1.0352 / Tel Value High-Clock CLKHIT6= 4.0283 / Tel Value High-Clock CLKHIT7= 0.0488 / Tel Value High-Clock CLKHIT8= 2.5342 / Tel Value High-Clock CLKHIT9= 4.0430 / Tel Value High-Clock CLKLO1= 0.0000 / Set value Low-Clock CLKLO10= 0.0000 / Set value Low-Clock CLKLO11= 0.0000 / Set value Low-Clock CLKLO12= 5.0000 / Set value Low-Clock CLKLO13= 1.0000 / Set value Low-Clock CLKLO14= 4.0000 / Set value Low-Clock CLKLO15= 0.0000 / Set value Low-Clock CLKLO16= 9.7500 / Set value Low-Clock CLKLO2= 0.0000 / Set value Low-Clock CLKLO3= 0.0000 / Set value Low-Clock CLKLO4= 5.0000 / Set value Low-Clock CLKLO5= 1.0000 / Set value Low-Clock CLKLO6= 4.0000 / Set value Low-Clock CLKLO7= 0.0000 / Set value Low-Clock CLKLO8= 9.7500 / Set value Low-Clock CLKLO9= 0.0000 / Set value Low-Clock CLKLONM1= 'clk1Lo pmc' / Name of Low-Clock CLKLONM10= 'clk10Lo FrameStart' / Name of Low-Clock CLKLONM11= 'clk11Lo UcResetEnable' / Name of Low-Clock CLKLONM12= 'clk12Lo VHiRowEnable' / Name of Low-Clock CLKLONM13= 'clk13Lo VLoRowEnable' / Name of Low-Clock CLKLONM14= 'clk14Lo VHiReset' / Name of Low-Clock CLKLONM15= 'clk15Lo VLoReset' / Name of Low-Clock


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET DET VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2 VOLT2

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CLKLONM16= 'clk16Lo VpOut' / Name of Low-Clock CLKLONM2= 'clk2Lo FrameStart' / Name of Low-Clock CLKLONM3= 'clk3Lo UcResetEnable' / Name of Low-Clock CLKLONM4= 'clk4Lo VHiRowEnable' / Name of Low-Clock CLKLONM5= 'clk5Lo VLoRowEnable' / Name of Low-Clock CLKLONM6= 'clk6Lo VHiReset' / Name of Low-Clock CLKLONM7= 'clk7Lo VLoReset' / Name of Low-Clock CLKLONM8= 'clk8Lo VpOut' / Name of Low-Clock CLKLONM9= 'clk9Lo pmc' / Name of Low-Clock CLKLOT1= 0.0537 / Tel Value Low-Clock CLKLOT10= 0.0488 / Tel Value Low-Clock CLKLOT11= 0.0439 / Tel Value Low-Clock CLKLOT12= 4.9512 / Tel Value Low-Clock CLKLOT13= 1.0352 / Tel Value Low-Clock CLKLOT14= 4.0234 / Tel Value Low-Clock CLKLOT15= 0.0439 / Tel Value Low-Clock CLKLOT16= 9.4678 / Tel Value Low-Clock CLKLOT2= 0.0488 / Tel Value Low-Clock CLKLOT3= 0.0488 / Tel Value Low-Clock CLKLOT4= 4.9609 / Tel Value Low-Clock CLKLOT5= 1.0449 / Tel Value Low-Clock CLKLOT6= 4.0283 / Tel Value Low-Clock CLKLOT7= 0.0488 / Tel Value Low-Clock CLKLOT8= 9.4678 / Tel Value Low-Clock CLKLOT9= 0.0586 / Tel Value Low-Clock DC1 = -2.3600 / Set value DC-Voltage DC10 = -3.3500 / Set value DC-Voltage DC11 = 0.0000 / Set value DC-Voltage DC12 = 0.7000 / Set value DC-Voltage DC13 = 0.7000 / Set value DC-Voltage DC14 = 3.5000 / Set value DC-Voltage DC15 = 2.2000 / Set value DC-Voltage DC16 = 3.3000 / Set value DC-Voltage DC2 = -3.3500 / Set value DC-Voltage DC3 = 0.0000 / Set value DC-Voltage DC4 = 0.7000 / Set value DC-Voltage DC5 = 0.7000 / Set value DC-Voltage DC6 = 3.5000 / Set value DC-Voltage DC7 = 2.2000 / Set value DC-Voltage DC8 = 3.3000 / Set value DC-Voltage DC9 = -2.3600 / Set value DC-Voltage DCNM1 = 'DC1 VIdle' / Name of DC-voltage DCNM10= 'DC10 VSlew' / Name of DC-voltage DCNM11= 'DC11 VRstUc' / Name of DC-voltage DCNM12= 'DC12 VDetCom' / Name of DC-voltage DCNM13= 'DC13 VnUc' / Name of DC-voltage DCNM14= 'DC14 VpUc' / Name of DC-voltage DCNM15= 'DC15 VnOut' / Name of DC-voltage DCNM16= 'DC16 RefBias' / Name of DC-voltage DCNM2 = 'DC2 VSlew' / Name of DC-voltage DCNM3 = 'DC3 VRstUc' / Name of DC-voltage DCNM4 = 'DC4 VDetCom' / Name of DC-voltage DCNM5 = 'DC5 VnUc' / Name of DC-voltage DCNM6 = 'DC6 VpUc' / Name of DC-voltage DCNM7 = 'DC7 VnOut' / Name of DC-voltage DCNM8 = 'DC8 RefBias' / Name of DC-voltage DCNM9 = 'DC9 VIdle' / Name of DC-voltage DCTA1 = -2.3535 / Tel Value 1 for DC DCTA10= -3.3447 / Tel Value 1 for DC DCTA11= 0.0049 / Tel Value 1 for DC DCTA12= 0.7031 / Tel Value 1 for DC DCTA13= 0.7031 / Tel Value 1 for DC DCTA14= 3.4961 / Tel Value 1 for DC DCTA15= 2.1973 / Tel Value 1 for DC DCTA16= 3.2959 / Tel Value 1 for DC DCTA2 = -3.3447 / Tel Value 1 for DC DCTA3 = 0.0049 / Tel Value 1 for DC DCTA4 = 0.6982 / Tel Value 1 for DC DCTA5 = 0.6982 / Tel Value 1 for DC DCTA6 = 3.4961 / Tel Value 1 for DC DCTA7 = 2.1973 / Tel Value 1 for DC DCTA8 = 3.2959 / Tel Value 1 for DC DCTA9 = -2.3535 / Tel Value 1 for DC


DATA FLOW Calibration Plan SYSTEM
HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH HIERARCH INHERIT PV2_1 PV2_2 PV2_3 PV2_4 PV2_5 END ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO ESO =T = = = = =

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DET VOLT2 DCTB1 = -2.3438 / Tel Value 2 for DC DET VOLT2 DCTB10= -3.3057 / Tel Value 2 for DC DET VOLT2 DCTB11= 0.0049 / Tel Value 2 for DC DET VOLT2 DCTB12= 0.6982 / Tel Value 2 for DC DET VOLT2 DCTB13= 0.7031 / Tel Value 2 for DC DET VOLT2 DCTB14= 3.4912 / Tel Value 2 for DC DET VOLT2 DCTB15= 2.1826 / Tel Value 2 for DC DET VOLT2 DCTB16= 3.2910 / Tel Value 2 for DC DET VOLT2 DCTB2 = -3.3057 / Tel Value 2 for DC DET VOLT2 DCTB3 = 0.0049 / Tel Value 2 for DC DET VOLT2 DCTB4 = 0.6982 / Tel Value 2 for DC DET VOLT2 DCTB5 = 0.6982 / Tel Value 2 for DC DET VOLT2 DCTB6 = 3.4912 / Tel Value 2 for DC DET VOLT2 DCTB7 = 2.1777 / Tel Value 2 for DC DET VOLT2 DCTB8 = 3.2910 / Tel Value 2 for DC DET VOLT2 DCTB9 = -2.3438 / Tel Value 2 for DC DET WIN NX = 2048 / # of Pixels in X DET WIN NY = 2048 / # of Pixels in Y DET WIN STARTX = 1 / Lower left X ref DET WIN STARTY = 1 / Lower left Y ref DET WIN TYPE = 0 / Win-Type: 0=SW/1=HW / Extension inherits primary header 1. / WCS parameter value term 0. / WCS parameter value term 42. / WCS parameter value term 0. / WCS parameter value term 0. / WCS parameter value term

The section between the two ENDs repeating as appropriate for the next 15 extensions. Table 10-1 FITS Example Header


DATA FLOW Calibration Plan SYSTEM Appendix A.
2MASS Tile 90021 90294 90299 90004 90301 90533 90191 90400 90401 90013 90402 90121 90312 92026 90067 90860 90867 90273 90868 90565 90009 90330 90279 90547 90808 90234 90813 92409 92202 90893 90298 90021 90294 90299 90004 90301 90533 90191 90400 90401 90013 90402 90121 90312 92026 90067 92397 90217 90860 90867 90273 90868 90565 90009 90330 90279 90547 90808 90234 90813 92409 92202 90893 90298

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2MASS calibration Fields
DEC(J2000) -1.97294 -39.40154 -70.58353 +0.71693 -39.84268 +6.93647 +3.62342 -65.73341 -71.00065 +0.01890 -69.66665 -59.65713 -39.09847 -1.57084 +11.84773 -0.12034 -0.45767 -44.81900 -0.65787 +5.87185 -24.68901 +30.14552 -45.42783 -4.27488 -4.48794 -49.64775 -5.06339 +20.84962 -11.07477 +0.54857 -74.50079 -1.97294 -39.40154 -70.58353 +0.71693 -39.84268 +6.93647 +3.62342 -65.73341 -71.00065 +0.01890 -69.66665 -59.65713 -39.09847 -1.57084 +11.84773 -13.22047 -50.05148 -0.12034 -0.45767 -44.81900 -0.65787 +5.87185 -24.68901 +30.14552 -45.42783 -4.27488 -4.48794 -49.64775 -5.06339 +20.84962 -11.07477 +0.54857 -74.50079 glon 107.367 318.916 303.708 154.117 244.635 179.513 190.909 276.286 282.110 206.632 279.959 268.951 257.574 226.548 215.639 287.009 351.082 325.155 356.367 20.521 352.970 50.250 346.065 29.111 30.125 349.607 41.333 77.728 47.133 80.124 308.690 107.367 318.916 303.708 154.117 244.635 179.513 190.909 276.286 282.110 206.632 279.959 268.951 257.574 226.548 215.639 271.788 294.815 287.009 351.082 325.155 356.367 20.521 352.970 50.250 346.065 29.111 30.125 349.607 41.333 77.728 47.133 80.124 308.690 glat· -64.025· -77.157· -46.535· -58.275· -55.506· -36.676· -29.778· -35.956· -33.373· -12.049· -28.523· -25.881· -0.669· 21.547· 31.905· 61.828· 51.867· 12.572· 48.363· 34.698· 16.585· 42.071· -8.926· -1.920· -4.377· -36.216· -26.643· -26.651· -47.917· -54.382· -41.894· -64.025· -77.157· -46.535· -58.275· -55.506· -36.676 -29.778· -35.956· -33.373· -12.049· -28.523· -25.881· -0.669· 21.547· 31.905· 44.166· 12.036· 61.828· 51.867· 12.572· 48.363· 34.698· 16.585· 42.071· -8.926· -1.920· -4.377· -36.216· -26.643· -26.651· -47.917· -54.382· -41.894

RA(J2000) 6.10619 8.31622 11.25260 28.66074 51.72678 55.26392 66.58918 74.90247 78.62001 89.28447 93.56589 97.37444 126.40319 128.12790 132.81203 185.41757 220.24529 224.21932 225.11368 246.68168 246.80780 247.89420 267.09736 282.82780 285.48438 307.83812 310.27504 330.11998 331.40247 349.54575 356.63061 6.10619 8.31622 11.25260 28.66074 51.72678 55.26392 66.58918 74.90247 78.62001 89.28447 93.56589 97.37444 126.40319 128.12790 132.81203 170.45775 180.44070 185.41757 220.24529 224.21932 225.11368 246.68168 246.80780 247.89420 267.09736 282.82780 285.48438 307.83812 310.27504 330.11998 331.40247 349.54575 356.63061


DATA FLOW Calibration Plan SYSTEM

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11

Index
Linearization ............................... 24, 25 Low Order Wave-Front Sensor ... 9, 11, 14, 51, 52, 53, 54, 55 mesostep ........................................... 27 Mesostep ........................................... 27 Microstep .. 9, 10, 14, 34, 49, 51, 52, 53 Movement ......................... 9, 10, 33, 34 noise ................................ 20, 22, 24, 37 Noise ............................... 20, 22, 24, 37 Observing block ............................ 9, 54 Observing Tool .... 9, 20, 22, 23, 24, 25, 26, 27, 28, 31, 32, 33, 34, 35, 37 Offset .. 7, 10, 15, 32, 33, 52, 53, 54, 59 Pawprint ... 7, 10, 13, 14, 15, 30, 33, 49, 51, 52, 53, 54 Persistence ........................................ 27 Photometric .. 14, 15, 20, 25, 27, 29, 30, 31, 34, 37, 49, 57 Pipeline .. 10, 13, 15, 20, 22, 23, 24, 25, 26, 27, 28, 31, 32, 33, 34, 35, 37, 38, 46, 47, 48, 49, 50, 51, 52, 54, 55, 56, 57, 59 Preset..................................... 10, 33, 51 QC-0 ............................................. 9, 37 QC-1 ................................................... 9 rotator................................................ 14 Rotator .............................................. 14 Sampling ........................... 8, 30, 33, 34 Science Requirements......................... 8 Sensitivity ................................... 30, 34 Survey ..................................... 9, 29, 70 Survey Definition Tool ................. 9, 52 Telescope Control System9, 12, 14, 53, 55, 56 Templates..... 13, 15, 20, 42, 46, 49, 51, 54, 56 Tile ............................ 42, 49, 51, 53, 54 twilight ............................ 25, 26, 47, 48 Twilight........................... 25, 26, 47, 48 WFCAM ................................. 9, 30, 57 World-Coordinate System9, 34, 35, 36, 59 _oo_

2MASS ....................................8, 30, 35 Active optics .........................12, 55, 56 Astrometric ..14, 15, 20, 25, 34, 35, 37, 49 Autoguider ........................................11 Background ....9, 14, 22, 25, 26, 32, 33, 37 Bad pixels..........................9, 14, 25, 33 Chips ...........................................10, 59 Confidence map ..............25, 26, 33, 34 Correlated Double Sampling.........8, 22 Crosstalk ...........................................28 Dark...............13, 22, 23, 24, 27, 42, 46 data flow............................................20 Data flow ...........................................20 Data Flow System ..7, 8, 12, 14, 15, 35, 56 Detectors ....7, 8, 10, 11, 13, 14, 15, 22, 24, 25, 26, 28 Distortion ....................................34, 35 Efficiency ....................................14, 24 Exposure ....7, 9, 13, 15, 22, 23, 24, 27, 31, 33, 37, 46, 47, 51, 52, 53, 54 Filter .13, 14, 15, 22, 25, 27, 29, 30, 34, 46, 47, 49, 50, 51, 52, 53, 55, 56, 57 Filter wheel .................................13, 56 FITS8, 9, 13, 15, 22, 23, 24, 25, 26, 27, 28, 31, 32, 33, 34, 35, 37, 46, 47, 48, 49, 50, 51, 52, 54, 55, 56, 59, 69 flat ...........23, 24, 25, 26, 47, 48, 51, 56 Flat ....23, 24, 25, 26, 32, 47, 48, 51, 56 Focal plane ...11, 12, 23, 26, 51, 52, 55, 56 Gain ...........................23, 24, 25, 26, 31 illumination ..23, 24, 25, 27, 46, 48, 50, 51 Illumination ..23, 24, 25, 26, 27, 31, 46, 48, 50, 51 Instrumental signature ...........15, 20, 25 Integration .............................52, 53, 54 Jitter....9, 10, 14, 33, 34, 49, 51, 52, 53, 54