Kaufer / Kerber The 2007 ESO Instrument Calibration Workshop

Proceedings of the ESO Workshop held in Garching, Germany, 23-26 January 2007
1. Auflage 2008
ISBN: 978-3-540-76963-7
Verlag: Springer Berlin Heidelberg
Format: PDF
Kopierschutz: 1 - PDF Watermark

E-Book, Englisch, 616 Seiten

Reihe: ESO Astrophysics Symposia

The 2007 ESO Instrument Calibration workshop brought together more than 120 participants with the objective to a) foster the sharing of information, experience and techniques between observers, instrument developers and instrument operation teams, b) review the actual precision and limitations of the applied instrument calibration plans, and c) collect the current and future requirements by the ESO users. These present proceedings include the majority of the workshop's contributions and document the status quo of instrument calibration at ESO in large detail. Topics covered are: Optical Spectro-Imagers, Optical Multi-Object Spectrographs, NIR and MIR Spectro-Imagers, High-Resolution Spectrographs, Integral Field Spectrographs, Adaptive Optics Instruments, Polarimetric Instruments, Wide Field Imagers, Interferometric Instruments as well as other crucial aspects such as data flow, quality control, data reduction software and atmospheric effects. It was stated in the workshop that 'calibration is a life-long learning process''. In this sense, this book will be a reference point for all future efforts to improve instrument calibration procedures in astronomy.

Autoren/Hrsg.

Kaufer, Andreas

Kerber, Florian

Inhaltsverzeichnis

1;Preface;5
2;Contents;7
3;List of Contributors;15
4;Part I Introduction;27
4.1;Instruments Calibration at the La Silla Paranal Observatory;28
4.1.1;1 La Silla Paranal Observatory;28
4.1.1.1;1.1 Scientific Operations: Statistic;28
4.1.2;2 From the Theory (VLT White Book) to the Practice (Operations);31
4.1.2.1;2.1 The Calibration Plan;31
4.1.2.2;2.2 The Quality Control (QC);32
4.1.2.3;2.3 The Instrument Operation Team (IOT);33
4.1.3;References;34
4.1.4;Discussion;34
4.2;The Detector Monitoring Project;35
4.2.1;1 Introduction;35
4.2.2;2 Status at the La Silla Observatory;36
4.2.3;3 Status at the Paranal Observatory;38
4.2.4;4 The Detector Monitoring Plan;40
4.2.5;5 The Common Pipeline Library;43
4.2.6;References;44
4.2.7;Discussion;45
5;Part II Session 1: Optical Spectro-Imagers;46
5.1;IOT Overview: Optical Spectro-Imagers;47
5.1.1;1 The Long Tradition of Optical Spectro-Imagers at ESO;47
5.1.2;2 Open Issues;49
5.1.3;3 Instrument Operations Team (IOT) Parallel Activities;51
5.1.4;References;54
5.1.5;Discussion;54
5.2;Photometry with FORS;56
5.2.1;1 Introduction;56
5.2.2;2 Data;56
5.2.3;3 Results;57
5.2.4;Summary and Outlook;61
5.2.5;References;61
5.3;Radial Velocity Measurements Based on FORS2 and FLAMES Spectra;62
5.3.1;1 Introduction;62
5.3.2;2 Data Samples;63
5.3.3;3 Conclusions;66
5.3.4;References;67
5.3.5;Discussion;68
5.4;The VLT-FLAMES Survey of Massive Stars: Instrumental Stability and Detection of Massive Binaries;69
5.4.1;1 Introduction;69
5.4.2;2 Binary Parameters;70
5.4.3;3 Instrumental Stability;70
5.4.4;References;71
5.5;VIMOS Total Transmission Pro.les for Broad-Band Filters;72
5.5.1;1 Transmission Profiles of Telescope + Instrument;72
5.5.2;2 Transmission Pro.les of Broad-Band Filters;74
5.5.3;3 Conclusions;74
5.6;Laboratory Measurements of Calibration Sources for X-Shooter;76
5.6.1;1 Introduction – X-Shooter;76
5.6.2;2 Wavelength Calibration for X-Shooter;76
5.6.3;3 First Results and Next Steps;79
5.6.4;References;79
5.7;Modelling the Fringing of the FORS2 CCD;81
5.7.1;1 Observational Setup;81
5.7.2;2 Reduction;82
5.7.3;3 Results;82
5.7.4;4 Prospects;84
5.7.5;References;85
5.8;Master Response Curves for Flux Calibration of VIMOS Spectroscopy;86
5.8.1;1 VIMOS Spectroscopic Modes;86
5.8.2;2 Master Response Curves;86
5.8.3;3 Veri.cation;87
5.8.4;4 Limitations and Availability;89
5.8.5;Reference;89
6;Part III Session 2: Optical Multi-object Spectrographs;90
6.1;IOT Overview: Optical Multi-Object Spectrographs;91
6.1.1;1 What is Multi-Object Spectroscopy?;91
6.1.2;2 ESO’s Optical MOS Instruments;91
6.1.3;3 Science that Is Done Using MOS Modes;94
6.1.4;4 Calibration of MOS Data;94
6.1.5;5 Monitoring the Instrument Performance;95
6.1.6;References;96
6.2;Quantitative Spectroscopy with FLAMES;97
6.2.1;1 Preparing the FLAMES Observations;97
6.2.2;2 Analysis of Gira.e Data;99
6.2.3;References;101
6.2.4;Discussion;101
6.3;Good News for MOS, MXU & Co. – The New Spectroscopic Pipeline for the FORSes;103
6.3.1;1 How Does the Pipeline Work?;103
6.3.2;2 Strengths and Weaknesses;105
6.3.3;3 Quality Control;106
6.3.4;4 Concluding Remarks;108
6.3.5;Discussion;108
6.4;Calibrating the VIMOS Redshift Survey Data;110
6.4.1;1 The VIMOS Spectrograph and the Redshift Survey Data;110
6.4.2;2 The VIMOS Data Reduction Pipeline;111
6.4.3;3 The Calibration of VIMOS Spectroscopic Data;113
6.4.4;4 The VIMOS Data Wavelength Calibration;116
6.4.5;5 Redshift Measurements;117
6.4.6;6 Conclusions;119
6.4.7;References;119
6.4.8;Discussion;120
7;Part IV Session 3: Near-IR and mid-IR Spectro-Imagers;121
7.1;IOT Overview: IR Instruments;122
7.1.1;1 Introduction;122
7.1.2;2 The Calibration Plan;123
7.1.3;3 Calibrations for Science: A Few Notes;124
7.1.4;4 Calibrations for Monitoring: Examples;129
7.1.5;5 Conclusions;131
7.1.6;References;131
7.2;Some (Little) Thing(s) about VISIR;132
7.2.1;1 The Instrument;132
7.2.2;2 The Warm Calibration Unit (WCU);133
7.2.3;3 Detector Features;134
7.2.4;4 Instrument Performances;135
7.2.5;5 Instrument Characteristics and Signatures;137
7.2.6;6 Conclusions;141
7.2.7;References;141
7.2.8;Discussion;141
7.3;Infrared Spectrograph Calibration Issues: Using CRIRES, the High Resolution Infrared Spectrograph for ESO’s VLT as an Example;143
7.3.1;1 Introduction: General Spectrograph Calibration Issues;143
7.3.2;2 CRIRES in a Nut Shell;144
7.3.3;3 Special Challenges for Calibrating CRIRES;146
7.3.4;4 Other Tricky Calibrations;147
7.3.5;5 Conclusions and Outlook;148
7.3.6;References;148
7.3.7;Discussion;148
7.4;Calibrating Mid-Infrared Standard Stars;150
7.4.1;1 Introduction;150
7.4.2;2 The MIR Spectro-Photometric Standard Star Catalog;151
7.4.3;3 Data Processing and Quality Control;151
7.4.4;4 Results;153
7.4.5;References;155
7.4.6;Discussion;155
7.5;Stellar Calibrators for the Medium Resolution Spectrometer of the Mid Infra-Red Instrument on Board the JWST;156
7.5.1;1 The James Webb Space Telescope and the MIRI MRS;156
7.5.2;2 Calibration Method for the MRS;156
7.5.3;3 The Candidate Calibration Sources;157
7.5.4;4 Conclusions and Future Work;158
7.5.5;References;159
7.6;ISAAC LW Telluric Line Atlas;160
7.6.1;1 Project Description;160
7.6.2;2 Reduction & Analysis Procedure;160
7.6.3;3 Future Work;162
7.6.4;References;163
7.7;Building-Up a Database of Spectro-Photometric Standard Stars from the Ultraviolet to the Near-Infrared;164
7.7.1;1 Motivation;164
7.7.2;2 Instrumental Setup;165
7.7.3;3 Strategy;166
7.7.4;4 Current Status;167
7.7.5;References;167
8;Part V Session 4: Data Flow and Data Reduction Software;168
8.1;The VLT Data Flow System;169
8.1.1;1 Introduction;169
8.1.2;2 Program Handling (Phase I);170
8.1.3;3 Observation Handling (Phase II);170
8.1.4;4 Science Archive;171
8.1.5;5 Pipelines and Quality Control;172
8.1.5.1;5.1 The ESO Common Pipeline Library;173
8.1.5.2;5.2 Interactive Pipeline Environments: EsoRex and Gasgano;173
8.1.5.3;5.3 Interactive Pipeline Environments: the SAMPO Project;174
8.1.6;6 Evolution of the DFS: Support of Survey Facilities;175
8.1.7;7 The User Portal;176
8.1.8;References;177
8.1.9;Discussion;177
8.2;ESO Reflex: A Graphical Work.ow Engine for Running Recipes;178
8.2.1;1 The ESO Context;178
8.2.2;2 The Sampo Project;179
8.2.3;3 ESO Reflex;180
8.2.4;4 Advantages of the Work.ow Approach;182
8.2.5;5 Current and Future Activities;183
8.2.6;References;183
8.2.7;Discussion;183
8.3;Astronomical Data Reduction Pipelines at NASA: 30 Years and Counting;185
8.3.1;1 Introduction;185
8.3.2;2 The International Ultraviolet Explorer;186
8.3.3;3 Hubble Space Telescope;188
8.3.4;4 Summary: Lessons Learned;191
8.3.5;References;192
8.3.6;Discussion;192
8.4;The End-to-End Pipeline for HST Slitless Spectra PHLAG;193
8.4.1;1 The Hubble Legacy Archive;193
8.4.2;2 Slitless Spectroscopy;194
8.4.3;3 The Modules of PHLAG;195
8.4.4;4 Status;197
8.4.5;References;198
8.5;A Bottom-Up Approach to Spectroscopic Data Reduction;199
8.5.1;1 Robustness and Flexibility;199
8.5.2;2 Identification of Reference Objects;199
8.5.3;3 Application to the FORS Spectroscopic Pipeline;202
8.5.4;4 Application to the CRIRES Pipeline;203
8.5.5;References;204
8.5.6;Discussion;205
8.6;Model Based Instrument Calibration;206
8.6.1;1 Introduction;206
8.6.2;2 CRIRES;207
8.6.3;3 X-Shooter;210
8.6.4;4 Conclusions;211
8.6.5;References;212
8.6.6;Discussion;212
8.7;From Predictive Calibration to Forward Analysis – Preparing for the ELT Era;214
8.7.1;1 Introduction;214
8.7.2;2 Wavelength Calibration or Approximating Dispersion Data;214
8.7.3;3 A Historical Analogon;216
8.7.4;4 Predictive Calibration from Physical Instrument Models;217
8.7.5;5 A Striking Lesson on Predictive Power;219
8.7.6;6 Onwards to the E-ELT Era – Forward Analysis;219
8.7.7;7 Concluding Thoughts;220
8.7.8;References;222
8.7.9;Discussion;222
8.8;Efits: A New E.cient and Flexible FITS Library;224
8.8.1;1 Introduction;224
8.8.2;2 The Efits Library;225
8.8.3;3 The Shared Memory I/O Implementation;226
8.8.4;4 Conclusion;227
8.8.5;References;227
8.9;Error Propagation in the X-shooter Pipeline;228
8.9.1;1 Motivations;228
8.9.2;2 Calculations and Data Formats;228
8.9.3;3 The Problem of Covariance;229
8.9.4;References;230
8.10;The CRIRES Data Reduction Challenges;231
8.10.1;1 Data Reduction;231
8.10.2;2 Spectrum Extraction;231
8.10.3;3 Physical Model;233
8.10.4;4 Wavelength Calibration;233
8.10.5;References;234
8.11;THELI - A Pipeline for UV- to Mid-IR Imaging Data Reduction;235
8.11.1;1 Overview;235
8.11.2;2 Instrument Independence;236
8.11.3;3 Further Capabilities and Availability;237
8.11.4;References;238
8.12;MUSE: Design and Status of the Data Reduction Pipeline;239
8.12.1;1 The Instrument;239
8.12.2;2 The Data Reduction Pipeline;240
8.12.3;3 Status and Outlook;241
8.12.4;References;242
9;Part VI Session 5: Adaptive Optics Instruments;243
9.1;IOT Overview: Adaptive Optics;244
9.1.1;1 Introduction;244
9.1.2;2 AO Specific Calibrations;247
9.1.3;3 The Case of the MACAO(s);247
9.1.4;4 The NAOS Case;250
9.1.5;5 Conclusion;253
9.2;AO Assisted Spectroscopy with SINFONI: PSF, Background, and Interpolation;254
9.2.1;1 A Short Introduction to SINFONI;254
9.2.2;2 The Adaptive Optics Point Spread Function;254
9.2.3;3 Improving the Background Subtraction;258
9.2.4;4 Interpolating in 3 Dimensions;259
9.2.5;References;261
9.2.6;Discussion;262
9.3;Imaging and Treatment of the PSF in AO Instruments: Application to NACO;264
9.3.1;1 Introduction;264
9.3.2;2 Adaptive Optics PSF Characteristics;265
9.3.3;3 Adaptive Optics PSF Variability;267
9.3.4;4 Adaptive Optics PSF Reconstruction;270
9.3.5;5 Conclusions;273
9.3.6;References;273
9.3.7;Discussion;274
9.3.8;Probing µ-arcsec Astrometry with NACO;275
9.4;Probing µ-arcsec Astrometry with NACO;275
9.4.1;1 Motivation and Introduction;275
9.4.2;2 Results from the Feasibility Study;276
9.4.3;3 Improvements: NACO Cube Mode;277
9.4.4;4 Calibration Issues;277
9.4.5;References;278
9.4.6;Discussion;278
10;Part VII Session 6: Integral Field Spectroscopy;280
10.1;IOT Overview: Integral Field Spectroscopy;281
10.1.1;1 Introduction;281
10.1.2;2 Integral Field Spectrographs at the VLT;283
10.1.3;3 VIMOS;284
10.1.4;4 FLAMES-GIRAFFE;286
10.1.5;5 SINFONI;288
10.1.6;References;290
10.1.7;Discussion;290
10.2;Integral Field Spectrographs: A User’s View;291
10.2.1;1 Introduction;291
10.2.2;2 Specifics;291
10.2.3;3 Pushing the Limits;292
10.2.4;4 Implications and the Fear of Resampling;293
10.2.5;5 Conclusions and Perspectives;294
10.2.6;References;295
10.2.7;Discussion;295
10.3;Specsim: A Software Simulator for Integral Field Unit Spectrometers;297
10.3.1;1 Introduction;297
10.3.2;2 Modelling the Field of View;299
10.3.3;3 Modelling the IFU Spectrometer;302
10.3.4;References;302
10.4;Integral Field Spectroscopy with VIMOS;303
10.4.1;1 Introduction;303
10.4.2;2 Science with the VIMOS IFU;303
10.4.3;3 Data Reduction;307
10.4.4;4 Instrument Performance;308
10.4.5;References;312
10.4.6;Discussion;312
10.5;KMOS: Design Overview and Calibration Requirements;313
10.5.1;1 Introduction;313
10.5.2;2 Science Case and Functional Speci.cation;313
10.5.3;3 Instrument Description;314
10.5.4;4 Calibration Requirements;317
10.5.5;References;318
10.5.6;Discussion;319
10.6;Calibration of the KMOS Multi-Field Imaging Spectrometer;320
10.6.1;1 An Introduction to KMOS;320
10.6.2;2 Planning KMOS Observations;321
10.6.3;3 Calibration of Spatial and Spectral Distortions;323
10.6.4;4 KMOS Sky Subtraction Modes;323
10.6.5;5 Calibration Unit Design and Performance;324
10.6.6;References;325
10.7;MUSE: A Second-Generation Integral-Field Spectrograph for the VLT;326
10.7.1;1 Imaging and Spectroscopic Surveys;327
10.7.2;2 MUSE;327
10.7.3;3 MUSE Science Case;329
10.7.4;4 Opto-Mechanical Concept;332
10.7.5;5 Operation and Data Reduction;334
10.7.6;6 Project Status;335
10.7.7;7 Conclusions;336
10.7.8;References;336
10.8;SPHERE-IFS: A Tool for Direct Detection of Giant Planets;338
10.8.1;1 Science Goal;338
10.8.2;2 SPHERE;338
10.8.3;3 SPHERE IFS: Instrument Concept;339
10.8.4;4 Calibrations;339
10.8.5;5 Spectroscopic SDI Technique;340
10.8.6;References;341
10.9;The Origin of Fringing in the VIMOS IFU;343
10.9.1;1 Introduction;343
10.9.2;2 Grism and Filter E.ect;343
10.9.3;3 Shift due to Instrument Movements;343
10.9.4;4 Di.erence Between the Sky FF and the Screen FF;345
10.9.5;5 Variations Inside a Single Mask;345
10.9.6;6 Conclusion;346
10.9.7;Reference;346
10.10;A User’s View of VIMOS-IFU Calibrations;347
10.10.1;1 VIMOS IFU Mode;347
10.10.2;2 Accuracy of the Wavelength Calibration and Resolving Power;348
10.10.3;3 Conclusions;349
10.10.4;Reference;350
11;Part VIII Session 7: High Resolution Spectroscopy;351
11.1;IOT Overview: High Resolution Spectrographs;352
11.1.1;1 Introduction;352
11.1.2;2 Instrumentation;352
11.1.3;3 Calibrations;357
11.1.4;4 Instrument Monitoring and Stability;360
11.1.5;5 Conclusions;361
11.1.6;References;361
11.2;Quantitative Spectroscopy with UVES;363
11.2.1;1 Introduction;363
11.2.2;2 Removal of CCD Fringing;364
11.2.3;3 Removal of Telluric Lines;365
11.2.4;4 Continuum Rectification;368
11.2.5;5 Conclusions;371
11.2.6;References;371
11.2.7;Discussion;371
11.3;High Resolution and High Precision-Spectroscopy with HARPS;373
11.3.1;1 Introduction;373
11.3.2;2 The Doppler Measurement;374
11.3.3;3 The Wavelength Calibration;375
11.3.4;4 Outlook on a “Perfect Calibrator”;381
11.3.5;5 Conclusions;382
11.3.6;References;382
11.3.7;Discussion;382
11.4;Laser Comb: A Novel Calibration System for High Resolution Spectrographs;383
11.4.1;1 Introduction;383
11.4.2;2 Requirements and Speci.cations;385
11.4.3;3 Status and Perspectives;386
11.4.4;References;387
11.4.5;Discussion;387
11.5;Instrumental Line Shape Function for High Resolution Fourier Transform Molecular and Atmospheric Spectroscopy;389
11.5.1;1 Introduction;389
11.5.2;2 Atmospheric Remote Sensing Requirements;389
11.5.3;3 Least Squares Line Parameter Fitting;390
11.5.4;4 Analysis of Pure Rotational Spectra of Ozone;391
11.5.5;References;392
11.6;Calibration Sources for CRIRES;394
11.6.1;1 CRIRES Wavelength Calibration;394
11.6.2;2 CRIRES and Its Calibration Sources;395
11.6.3;3 Laboratory Work, Results and Outlook;396
11.6.4;References;397
11.7;Recent Developments in the Optimal Extraction of UVES Spectra;399
11.7.1;1 Introduction;399
11.7.2;2 Algorithm;399
11.7.3;3 Robust Automatic Data Reduction;401
11.7.4;References;403
11.8;A new Generation of Spectrometer Calibration Techniques Based on Optical Frequency Combs;404
11.8.1;1 Calibration of High Resolution Spectrometers;404
11.8.2;2 Calibration of Mid Resolution Spectrometers;407
11.8.3;References;407
12;Part IX Session 8: Atmospheric E.ects;408
12.1;Photometric Calibration of LSST Data;409
12.1.1;1 Introduction;409
12.1.2;2 Calibration Requirements and Goals;410
12.1.3;3 Calibration Issues and Strategy;411
12.1.4;4 Instrumental Calibration;414
12.1.5;5 Monitoring Observing Conditions;416
12.1.6;References;417
12.2;The GTC Photometric Calibration Programme;418
12.2.1;1 Introduction;418
12.2.2;2 The Importance of a Proper Set of Standard Stars for GTC;419
12.2.3;3 The GTC;419
12.2.4;4 The GTC Calibration Approach for the Optical and Near IR;420
12.2.5;5 Conclusions;424
12.2.6;References;425
12.2.7;Discussion;425
12.3;Measuring the Amount of Precipitable Water Vapour with VISIR;426
12.3.1;1 Introduction;426
12.3.2;2 PWV Based on VISIR Sky Spectra;427
12.3.3;3 Conclusion;430
12.3.4;References;430
12.3.5;Discussion;431
12.4;NIR Extinction Coe.cients in Paranal;432
12.4.1;1 Introduction;432
12.4.2;2 The Sample;432
12.4.3;3 Data Analysis;432
12.4.4;References;435
12.5;Improvements in the Residual OH Emission Removal in SINFONI Pipeline Spectra;436
12.5.1;1 Introduction;436
12.5.2;2 Sky Emission;436
12.5.3;3 Algorithm;437
12.5.4;Summary;439
12.5.5;References;439
12.6;Calibration of the Relationship Between Precipitable Water Vapor and 225GHz Atmospheric Opacity via Optical Echelle Spectroscopy at Las Campanas Observatory;440
12.6.1;References;440
13;Part X Session 9: Interferometric Instrumentation;441
13.1;IOT Overview: Calibrations of the VLTI Instruments (MIDI and AMBER);442
13.1.1;1 Introduction;442
13.1.2;2 Interferometric Instrumentation at Paranal;444
13.1.3;3 Interferometric Calibration Requirements;445
13.1.4;4 VLTI Calibrator Catalogs;447
13.1.5;5 Flux Calibrations;449
13.1.6;6 Internal Calibrations and Daily Monitoring;449
13.1.7;7 Conclusion and Perspectives;450
13.1.8;References;451
13.1.9;Discussion;451
13.2;AMBER on the VLTI: Data Processing and Calibration Issues;452
13.2.1;1 Introduction;452
13.2.2;2 The AMBER Instrument;452
13.2.3;3 AMBER and the VLTI;454
13.2.4;4 Conclusion;459
13.2.5;References;460
13.2.6;Discussion;461
13.3;QC and Analysis of MIDI Data Using mymidigui and OYSTER;462
13.3.1;1 Introduction;462
13.3.2;2 Tools;462
13.3.3;3 Acquisition;463
13.3.4;4 Photometry;463
13.3.5;5 Transfer Function;464
13.3.6;6 SCI PHOT Mode;466
13.3.7;7 Conclusions;467
13.3.8;References;467
13.3.9;Discussion;467
13.4;Calibration of AMBER Visibilities at Low Spectral Resolution;469
13.4.1;1 AMBER Observations;469
13.4.2;2 Raw Data Pre-Processing;469
13.4.3;3 Aberrant Data Removal;470
13.4.4;4 Visibility Calibration;471
13.4.5;5 Visibility Model-Fitting;471
13.5;VLTI Instruments: From J to N Band Instrumental Calibrations, from Short to Long Baseline Astronomical Calibrations;473
13.5.1;1 VLTI Layout, Instruments and Sub-systems;473
13.5.2;2 VLTI Daily Calibrations and Reference Frames;473
13.5.3;3 Monitoring of the VLTI Sub-systems;474
13.5.4;4 Conclusions;476
13.5.5;References;476
14;Part XI Session 10: Polarimetry;477
14.1;IOT Overview: Polarimetry;478
14.1.1;1 Introduction;478
14.1.2;2 Near-IR Polarimetric Instruments;479
14.1.3;3 “Optical” Instruments;481
14.1.4;4 Conclusion;485
14.1.5;References;486
14.2;Polarimetry with ESO Instruments;487
14.2.1;1 Scientific Use of ESO Polarimetry;487
14.2.2;2 Polarimetry with FORS1 and EFOSC2;489
14.2.3;3 Polarimetry with SOFI, ISAAC and NACO;493
14.2.4;4 Polarimetric Calibration of ZIMPOL/SPHERE;495
14.2.5;References;496
14.2.6;Discussion;497
14.3;Faint NIR Polarimetric Standards;498
14.3.1;1 The Polarimetry Mode of LIRIS;498
14.3.2;2 The Case for Faint Polarimetric Standards in the NIR?;499
14.3.3;3 The First Standards;500
14.3.4;4 For the Future ...;501
14.3.5;References;501
14.4;Developmental Aspects of a Multi-Slit Spectro-Polarimeter;502
14.4.1;1 Introduction;502
14.4.2;2 New Technologies;503
14.4.3;3 System Requirements;504
14.4.4;4 Optical Design & Current Status;505
14.4.5;References;505
14.5;Current and Future Instruments Providing a Spectro-Polarimetric Mode;506
14.5.1;1 Introduction;506
14.5.2;2 Existing Spectropolarimetric Facilities;506
14.5.3;3 Planned Spectropolarimetric Facilities on Large Telescopes;509
14.5.4;4 Future Instruments at ESO;509
14.6;Circular Polarization Observations at ESO Using UT2 and FORS1;510
14.6.1;1 Intermediate Polars;510
14.6.2;2 Circular Polarimetric Observations of IPs, Using FORS1;511
14.6.3;3 Preliminary Results;512
14.6.4;References;513
15;Part XII Session 11: Wide Field Imagers;514
15.1;IOT Overview: Wide-Field Imaging;515
15.1.1;1 The Science;515
15.1.2;2 WFI@2.2m MPG Telescope at La Silla: An Overview;516
15.1.3;3 WFI Operations;518
15.1.4;4 What We Could Have Done Better;521
15.1.5;5 Conclusions;524
15.1.6;References;525
15.1.7;Discussion;526
15.2;Processing Wide Field Imaging Data;527
15.2.1;1 Introduction;527
15.2.2;2 Overall Data Structure;527
15.2.3;3 Overall Processing Philosophy;528
15.2.4;4 Image Processing;530
15.2.5;5 Object Cataloging;531
15.2.6;6 Astrometric Calibration;532
15.2.7;7 Photometric Calibration;534
15.2.8;8 Quality Control Measures;535
15.2.9;References;536
15.2.10;Discussion;537
15.3;The Garching-Bonn Deep Survey (GaBoDS) Wide-Field-Imaging Reduction Pipeline;538
15.3.1;1 Introduction;538
15.3.2;2 Structure;538
15.3.3;3 Processing;539
15.3.4;4 Reduction of the ESO Deep Public Survey;541
15.3.5;References;543
15.3.6;Discussion;543
15.4;Calibrating VISTA Data;544
15.4.1;1 Introduction;544
15.4.2;2 Strategy: Prepare for VISTA with WFCAM;545
15.4.3;3 Instrument Characteristics;545
15.4.4;4 Astrometric Calibration;547
15.4.5;5 Photometric Calibration;548
15.4.6;6 Conclusion;549
15.4.7;References;549
15.4.8;Discussion;549
15.5;The VISTA Data Flow System;550
15.5.1;1 Introduction to CASU and VDFS;550
15.5.2;2 IR Data Reduction;551
15.5.3;3 Pipelines and Project Status;555
15.5.4;References;555
15.5.5;Discussion;556
15.6;SkyMapper and the Southern Sky Survey a Resource for the Southern Sky;557
15.6.1;1 The SkyMapper Telescope;557
15.6.2;2 Detectors and Filters;557
15.6.3;3 The Southern Sky Survey;559
15.6.4;4 Global Photometric Calibration;559
15.6.5;5 A Filter Set for Stellar Astrophysics;560
15.6.6;6 Data Products and Their Possible Application to ESO Calibration;562
15.6.7;References;562
15.6.8;Discussion;562
15.7;Quality Control Monitoring for WFCAM;564
15.7.1;1 WFCAM Data Quality Control;564
15.7.2;2 NIR Sky Brightness;566
15.7.3;References;569
15.7.4;Discussion;570
15.8;Relative and Absolute Calibration for Multi-Band Data Collected with the 2.2m ESO/MPI and 1.54m Danish Telescopes;571
15.8.1;1 WFI Data Set;571
15.8.2;2 Danish Data Set;573
15.8.3;3 Conclusions;574
15.8.4;References;575
15.9;ALBUM: A Tool for the Analysis of Slitless Spectra and its Application to ESO WFI Data;576
15.9.1;1 Data Reduction;576
15.9.2;2 Results: Frequency of Be Stars vs. Metallicity;578
15.9.3;3 Conclusions;579
15.9.4;References;579
16;Part XIII Workshop Summary;580
16.1;The 2007 ESO Instrument Calibration Workshop – A Personal Summary;581
16.1.1;1 Introduction;581
16.1.2;2 Calibrations at ESO;582
16.1.3;3 Calibration Challenges from VLT to ELT;583
16.1.4;4 Conclusions;590
17;Index;591