1. Detector Monitoring as part of VLT Science and Data Flow Operations Wolfgang Hummel DMO/DFO/QC group Lander de Bilbao, SDD/pipeline group Andrea Modigliani, SDD/pipeline group Lars Lundin, SDD/pipeline group Paola Amico, LPO/PSO Pascal Ballester, SDD coordinating chair Gaspare LoCurto, LPO/PSO Leonardo Vanzi, LPO/PSO SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control

2. project purpose project purpose calibration plan review calibration plan review methods and algorithm selection methods and algorithm selection quality characteristics quality characteristics iterative recipe tests iterative recipe tests deployment and commissioning deployment and commissioning SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control Detector Monitoring outline of the talk

3. Detector Monitoring project purpose There is a unified scheme to monitor optical detectors at the ESO LaSilla observatory There is a unified scheme to monitor optical detectors at the ESO LaSilla observatory A similar scheme should be implemented for the Paranal observatory to improve operations within the VLT dataflow (PSO, QC group, SDD) A similar scheme should be implemented for the Paranal observatory to improve operations within the VLT dataflow (PSO, QC group, SDD) SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control

4. Detector Monitoring project outline review the operational calibration plans for all optical 12 science detectors (FORS1,2 UVES, GIRAFFE, VIMOS) and all 11 near and mid IR science detectors (ISAAC, CONICA, SINFONI, CRIRES, AMBER, MIDI, VISIR) review the operational calibration plans for all optical 12 science detectors (FORS1,2 UVES, GIRAFFE, VIMOS) and all 11 near and mid IR science detectors (ISAAC, CONICA, SINFONI, CRIRES, AMBER, MIDI, VISIR) design and implement a detector monitoring plan, and put it in operation. design and implement a detector monitoring plan, and put it in operation. review outcome: Amico, P. et al. 2008, ‘The Detector Monitoring Project’, in ‘The 2007 ESO Instrument Calibration Workshop’ review outcome: Amico, P. et al. 2008, ‘The Detector Monitoring Project’, in ‘The 2007 ESO Instrument Calibration Workshop’ SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control

5. Detector Monitoring review outcome priority and frequency of detector related QC parameters: priority and frequency of detector related QC parameters: 1. daily: RON and BIAS/DARK level 1. daily: RON and BIAS/DARK level 2. monthly: gain and linearity 2. monthly: gain and linearity 3. other: bad pixels, crosstalk, persistence, periodic noise, shutter error, correlated noise, odd-even column effect, large scale fixed pattern noise, low scale fixed pattern noise, contamination 3. other: bad pixels, crosstalk, persistence, periodic noise, shutter error, correlated noise, odd-even column effect, large scale fixed pattern noise, low scale fixed pattern noise, contamination RON, BIAS/DARK is in place with inhomogeneous analysis RON, BIAS/DARK is in place with inhomogeneous analysis gain and linearity incomplete -> highest priority gain and linearity incomplete -> highest priority start with optical CCDs and near IR, complete for MID IR and interferometric instruments later start with optical CCDs and near IR, complete for MID IR and interferometric instruments later SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control

6. Detector Monitoring gainlin template design calibration templates must be aligned with data reduction pipeline recipes calibration templates must be aligned with data reduction pipeline recipes no template change required for UVES (ccd_test), GIRAFFE and SINFONI. no template change required for UVES (ccd_test), GIRAFFE and SINFONI. template upgrade required for FORS1/2, ISAAC, NACO (flat pairs instead of single flats and include BIAS frames). template upgrade required for FORS1/2, ISAAC, NACO (flat pairs instead of single flats and include BIAS frames). new template for VIMOS, CRIRES new template for VIMOS, CRIRES SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control

7. ESO common pipeline library (CPL) ESO common pipeline library (CPL) two versions: optical CCD, near IR arrays two versions: optical CCD, near IR arrays linearity: polynomial, inverse via Newton- Raphson (+ FPN, +opt contamination, +nir bad pixel map), an OPT and a NIR version required. linearity: polynomial, inverse via Newton- Raphson (+ FPN, +opt contamination, +nir bad pixel map), an OPT and a NIR version required. gain: photon transfer curve and inter-pixel capacitance correction gain: photon transfer curve and inter-pixel capacitance correction ron: 4 methods (incl. pre+over scan) ron: 4 methods (incl. pre+over scan) bias (median) bias (median) SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control Detector Monitoring tools selection

8. Detector Monitoring gainlin recipe tests I one recipe tested for all detectors on (partially interleaved) frame stacks. one recipe tested for all detectors on (partially interleaved) frame stacks. a) handle conventional fits frames and multi-detector frames with fits extensions (CRIRES, UVES). a) handle conventional fits frames and multi-detector frames with fits extensions (CRIRES, UVES). b) configurable confinement of the analysis region to handle vignetting (FORS, NACO, CRIRES) b) configurable confinement of the analysis region to handle vignetting (FORS, NACO, CRIRES) c) upper threshold for signal level (saturation, non- linearity regime) c) upper threshold for signal level (saturation, non- linearity regime) d) flux alignment of consecutive flat pairs d) flux alignment of consecutive flat pairs SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control

9. Detector Monitoring recipe tests II SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control FORS2 lower mosaic CCD: - saturation and vignetting - both chips in two single fits frames UVES red arm CCD: both chips in two extensions of one fits frame - confined analysis region - option to handle fits extensions - upper flux threshold option

10. Detector Monitoring recipe tests III SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control SINFONI: integral field spectrograph: No imaging flats possible. Regular pattern of 32 pseudo slits Persistence does not allow for flats of exactly the same flux level

11. Detector Monitoring recipe tests V: PTC SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control

12. Detector Monitoring inter-pixel capacitance SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control From Finger, G. et al, 2005 Smear-out effect. A lower gain is measured

13. Detector Monitoring inter-pixel capacitance SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control -Measuring gain from PTC via flat difference frames -Inter-pixel capacitance: PSF > 1 pixel -> lower noise, higher gain. - use flat difference frames ?? Fixed pattern noise ?? - Autocorrelation algorithm Finger, G. et al. 2005 ‘Conversion gain and inter-pixel capacitance …’ giraffe : 1.0009 crires

14. SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control flux aligned flat difference flat difference, 2% flux difference bad autocorrelation inter-pixel capacitance PSF good autocorrelation inter-pixel capacitance PSF

15. Detector Monitoring recipe tests IV SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control SINFONI: Gain correction: 1.09

16. Detector Monitoring project status SPIE Astronomical Instrumentation 2008, Observatory Operations: Strategies, Processes and Systems, Conference 7016, Session 3: Data Management and Quality Control detector calibration plan in operation for GIRAFFE, UVES, and SINFONI other detectors coming soon: VIMOS, ISAAC project completion expected for the end of 2008 future science detectors will benefit: HAWK-I (4), VIRCAM/OCAM (16/32 !!!), X-shooter (3), … last slide