1. Oct 17, 2001SALT PFIS Preliminary Design Review1 Operation Concepts Definition Document (OCDD) Chip Kobulnicky University of Wisconsin

2. Oct 17, 2001SALT PFIS Preliminary Design Review2 Operational Mode Description Operational modes are fully characterized by the configuration of 4 primary subsystems (“basis vectors” in 4-D) which describe the dataset being acquired. –Focal Plane Elements (spatial) –Dispersive Elements (spectral) –Polarizing Elements (polarization) –Detector (time)

3. Oct 17, 2001SALT PFIS Preliminary Design Review3 Focal Plane Mechanism O – Open (implies direct acquisition & peak-up) S – Slit (Reflective Longslit Plate; implies visual acquisition & peak-up) M – Multi-slit mask (non-reflective carbon fiber; implies blind peak-up) Dispersive Elements I – Imaging (none) (Implies no camera articulation) F – Fabry-Perot Etalon (Implies no camera articulation) G – Grating (Articulated camera) Polarization Elements U – Unpolarized measurement (quartz block in place of waveplates) L – Linear polarization measurement (1/2 waveplate; max 4’ spatial field) C – Circular polarization measurement (1/2 and ¼ waveplate; max 4’ spatial field) A – All-stokes mode (both waveplates operational in sync; 4’ spatial field) CCD subsystem (see detector ICD for full explanation of readout modes) N - Normal readouts with exposure times of at least 3.6 s. Standard 2x2 binning H - High time resolution with frame-transfer in operation; max 4’ spatial field with lower half masked; objects confined to small region of chip just above CTB; continuous readout. V - Vertical shift operations, including vertical charge shuffling in conjunction with telescope nods to perform high-quality sky subtraction (spectroscopy) or off-band subtraction (Fabry-Perot spectroscopy), or time-series spectroscopy or spectropolarimetry. D - Drift scan or arbitrary charge-shuffling in use; CCD is clocked at a sidereal rate

4. Oct 17, 2001SALT PFIS Preliminary Design Review4 Focal Plane DisperserPolarizationCCD readout Common NameCommission? OIUNImagingY MIUHHigh Time Resolution ImagingU MILNImaging Linear PolarimetryU MILHHigh Time Resolution Imaging Linear PolarimetryU MICNImaging Circular PolarimetryU OFUNFabry-Perot Spectroscopic ImagingY MFLNFabry-Perot Spectroscopic Imaging Linear PolarimetryU MFCNFabry Perot Spectroscopic Imaging Circular PolarimetryU SGUNLongslit SpectroscopyY SGUHHigh Time Resolution Longslit SpectroscopyY SGLNLongslit Linear SpectropolarimetryU SGLHLongslit High Time Resolution Linear SpectropolarimetryU SGCNLongslit Circular SpectropolarimetryU SGCHLongslit High Time Resolution Circular Spectral-PolarimetryU MGUNMulti-slit spectroscopyY MGUHMulti-slit High Time Resolution SpectroscopyU MGLNMulti-slit Linear SpectropolarimetryY MGCNMulti-slit Circular SpectropolarimetryU OIUDDrift Scan Imaging & spectroscopyU Available Operational Modes

5. Oct 17, 2001SALT PFIS Preliminary Design Review5 Focal Plane Mechanisms O – Open (direct imaging applications, Fabry-Perot spectroscopy) 2048 2048 2048 Impalas Detector Layout with 8’ diameter FOV 4096 4’

6. Oct 17, 2001SALT PFIS Preliminary Design Review6 Reflective Slit Plate # LengthWidth (“) 17.5’0.45” 27.5’0.6” 37.5’0.9” 47.5’1.1” 57.5’1.3” 67.5’3.0” 7Central 4’1.1” (variable) for spectral polarimetry 812” above CTB1.1” (variable) for high speed spectroscopy 94’’1.1” w/ coronographic center Table 1. Complement of Standard Reflective Focal Plane Plates S – Slits (reflective tiled longslit plates) ~9 held in focal plane magazine

7. Oct 17, 2001SALT PFIS Preliminary Design Review7 Table 2: Standard Slitmasks # ConfigurationUse 1Masks lower 4’ x 8’High Time res. Imaging 2Masks upper and lower 2’ x 8’ (central 4’x8’ visible)Imaging and Fabry-Perot Polarimetry Up to 30 other user-designed masks M – carbon-fibre focal plane masks Laser-cut slits slit width: 0.11 – 0.35 mm Standard Slitmask #2: Slitmask covers upper and lower ¼ of FOV Standard Slitmask #1: Slitmask covers lower half of FOV

8. Oct 17, 2001SALT PFIS Preliminary Design Review8 Dispersive Elements I – Imaging (none) (Implies no camera articulation) F – Fabry-Perot Etalon (Implies no camera articulation) G – Grating (Articulated camera) 1 of 6 gratings

9. Oct 17, 2001SALT PFIS Preliminary Design Review9

10. Oct 17, 2001SALT PFIS Preliminary Design Review10 Polarizing Elements U – Unpolarized measurements (quartz block in beam) L – Linear polarization (half-waveplate; rotates through 8 positions) C – Circular polarization (half- and quarter-waveplate) A – All-stokes mode (synchronized half- and quarter-waveplate)

11. Oct 17, 2001SALT PFIS Preliminary Design Review11 CCD subsystem readout modes N - Normal readouts Readout time 3.6 s standard 2x2 binning, 5e- read noise 11.2 s standard 2x2 binning, 3e- read noise 22.1 s 1x2 binning, 3e- read noise

12. Oct 17, 2001SALT PFIS Preliminary Design Review12 CCD subsystem readout modes H - High time resolution with frame-transfer in operation; max 4’ spatial field with lower half masked, and possibly upper portions masked as well. Bin RdN Read ------------------------- 1x2 3e- 11.0 s 2x2 3e- 5.5 s 1x2 5e- 3.2 s 2x2 5e- 1.6 s

13. Oct 17, 2001SALT PFIS Preliminary Design Review13 CCD subsystem readout modes H – all but a subsection of chip masked Bin RdN Read ------------------------- 1x2 3e- 11.0 s 2x2 3e- 5.5 s 1x2 5e- 3.2 s 2x2 5e- 1.6 s 2x2 5e- 2.0’ field 0.80 s 0.5’ field 0.20 s 0.12’ field 0.05 s (64 pix) (but image smear during 0.05 msec per row transfer)

14. Oct 17, 2001SALT PFIS Preliminary Design Review14 CCD subsystem readout modes V - Vertical shift operations, including vertical charge shuffling in conjunction with telescope nods to perform high-quality sky subtraction (spectroscopy) or off-band subtraction (Fabry-Perot spectroscopy), or time-series spectroscopy or spectropolarimetry. D - Drift scan or arbitrary charge-shuffling in use; CCD is clocked at a sidereal or other rate

15. Oct 17, 2001SALT PFIS Preliminary Design Review15 Example of longslit spectroscopic mode operation Typical sequence of operation: Setup Telescope & Instrument (LOW OVERHEAD DESIGN GOAL FOR QUEUE MODE) Rotate telescope in Azimuth to correct location (few min; rate-limiting action) Select & insert filter (43 s) Select & insert grating (25 s) Select & insert longslit plate to be used (50 s) Articulate camera to desired position angle (<70 s) Acquire Field/Target Image field w/SALTICAM off reflective slitplate (2’ FOV) Locate desired object and move tracker to place object on slit Do Science Begin tracking/guiding using either guide probes or slit viewer camera Begin exposure Insert cal. lamp & take arc exposure Data Rate: 6154 pixels spectral x 4096 pixels spatial at >3.6 s total readout time Target acquisition: By guide probe, and using visual peak-up with SALTICAM as slit viewing camera. Tracking During Exposures: By guide probe, or by reflected light from slit viewed by SALTICAM. Simultaneous!

16. Oct 17, 2001SALT PFIS Preliminary Design Review16 Example of multi-slit (slitmask) spectroscopic mode Setup Telescope & Instrument Rotate telescope in Azimuth to correct location (few min; rate-limiting step) Select & insert filter (43 s) Select & insert grating (25) Select & insert slitmask to be used (50 s) Articulate camera to desired position angle (<70 s) Acquire Field/target (no view of slit, like nearly all multi-slit spectrographs) Insert SALTICAM fold mirror Image field with acquisition camera (SALTICAM) to locate alignment stars Perform offset to place alignment stars at proper location on focal plane (blind, but calibrated offsets) Remove fold mirror Perfect alignment by taking a series of exposures while performing a patterned dither on sky Location of maximum signal is used as final alignment position (0.5s x 9) [ fallback acquisition plan is direct imaging through unarticulated camera] Do Science Begin tracking/guiding using guide probes Begin science exposure Insert diffuser/cal lamp and do arc exposures Data Rate: 6154 pixels spectral x 4096 pixels spatial at >3.6 s total readout time Target acquisition: By SALTICAM, guide probe, and dithered exposure peak-up Tracking During Exposures: By guide probe Simultaneous Peak-up performed In spectral mode

17. Oct 17, 2001SALT PFIS Preliminary Design Review17 Instrument Commissioning Plan Let science drive commissioning Goal:6 science programs corresponding to each major instrument mode Start with simplest modes (i.e., imaging) Fully commission all “basic” modes Leave specialized modes to users for shared-risk basis Reduction Software: standard community tools

18. Oct 17, 2001SALT PFIS Preliminary Design Review18 Overview of Modes Commissioned by Instrument Team Est Time. Mode Science Program ---------------------------------------------------------------------------------------- 3 d Imaging TBD Nordsieck 5 d Longslit Spectroscopy TBD Kobulnicky 4 d High Time Res. Spectroscopy Magnetic CVs Buckley 4 d Fabry-Perot Spectroscopy TBD Williams 4 d Multi-slit Spectroscopy PNe in Nearby Galaxies Kobulnicky 5 d Polarimetric Imaging/Spectra Be Stars in the LMC Nordsieck 25 d (on telescope; based commissioning for other major instruments)

19. Oct 17, 2001SALT PFIS Preliminary Design Review19 Other possible user-commissioned modes (extensions of team-commissioned modes) High Time Resolution Spectral-Polarimetry Fabry-Perot Spectral-Polarimetry Circular polarimetry Circular Spectral-Polarimetry All-stokes Polarimetry High Time Resolution Multi-slit Spectral Polarimetry Shift+nod high-precision spectroscopy Drift scan imaging

20. Oct 17, 2001SALT PFIS Preliminary Design Review20 Commissioning tasks not requiring all mirror segments - acquisition strategies - software interfaces - focus, optical distortion, vignetting tests - wavelength calibration & stability - tracking & guiding stability Commissioning tasks requiring all mirror segments - instrumental polarization calibrations - total sensitivity calibrations - final flatfield calibrations & variability - other aspects sensitive to pupil illumination

21. Oct 17, 2001SALT PFIS Preliminary Design Review21 Calibration Issues Wavelength: He, Ne, Ar, Cu lamps fed to diffuser before moving baffle Flatfields: Continuum lamps fed to diffuser before moving baffle Flats taken next morning by re-creating actual science tracks w/baffle Observing scripts stored for easy reproduction (only a subset of spectrophotometric observations will need this precision) Observatory “superflats” created periodically in standard configurations -> enable differential flats taken on nightly basis Stray/scattered light? TBD during commissioning

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