FPRD Required Telescope Tests:
(From Instrument Acceptance Testing Plan)

• Field Size (all modes)
• Image Quality (all modes)
• Detector Pixel Scale (all modes)
• Flexure (all modes)
• Stray Light/Ghosts (all modes)
• Resolution (all spectroscopic modes)
• Efficiency (all modes)
• Instrumental Polarization (polarimetric modes)

Modes to be commissioned (from OCDD):

• Imaging
• Long Slit Spectroscopy
• Multi-Slit Spectroscopy
• High time resolution Long Slit Spectroscopy
• Fabry-Perot Imaging
• Long Slit Linear Spectropolarimetry
• Multi-Slit Linear Spectropolarimetry

Mode by mode description of potential science programs that would fulfill commissioning requirements.

1. Imaging

Technical goals:

• Quantify offsets and distortions between acquisition camera, guide probes, and PFIS.
• Test image quality over the field by observing a stellar field with known astrometry and stellar sources.
• Calibrate filter set with standard stars.
• Test telescope pointing and tracking: produce plots of seeing and image motion as a function of exposure time, hour angle, tracker position, and rotator motion.
• Test ADC by taking images of same field in different filters.
• Test non-sidereal tracking.
• Test shutter mechanism and check for timing errors.

Tests that will meet these goals:

• Measure Telescope Image Quality/Distortion: Observe field with multitude of targets with known astrometry (see table below). Compute image quality as a function of field. Compute SALT/SAC/ADC distortion by undistorting PFIS astrometry via PFIS distortion measured in ATP test 5.4. Test for various track geometries. (on-sky)
• Measure Guider Offset: Observe field at set guider position. Measure astrometrically center of field on PFIS image. Compute offset between measured center and tracker reported position. Repeat for multiple guider positions. (on-sky)
• Measure Acquisition Camera Offset: Observer field with PFIS and SALTICAM. Measure astrometrically center of field on both PFIS and SALTICAM images. Compute offset between measured centers. (on-sky)
• Test Telescope Tracking: Measure image motion as a function of exposure time, hour angle, tracker position, and rotator motion. This will need to be decoupled from flexure (measured in PFIS ATP test 5.7). (on-sky)
• Linearity/Dynamic Range:

• Astrometric calibration:
  

  Field	RA (2000)	Dec (2000)	notes	Obs Window
  47 Tuc	00 24 05.2	-72 04 49	Globular cluster (Cudworth astrometry)	Jun-Nov
  Omega Cen	03 26 45.8	-47 28 36	Globular cluster	Jul-Mar
  LMC	05 11 00.0	-70 00 00	LMC bar/disk Smecker-Hane HST program	Aug-Mar
  NGC 3603	11 15 09.1	-61 16 17	Young open cluster	Nov-Jul
  M5	15 18 33.7	+02 04 58	Globular cluster (Cudworth astrometry)	Feb-Aug
  M4	16 23 35.4	-26 31 32	Globular cluster (Cudworth astrometry)	Feb-Sep
  NGC 6397	17 40 41.3	-53 40 25	Globular cluster (Cudworth astrometry)	Feb-Sep
  M22	18 36 24.4	-23 54 12	Globular cluster (Cudworth astrometry)	Mar-Oct

2. Long Slit Spectroscopy

Technical goals:

• Test use of standard long slits and target acquisition operations.
• Produce plots of spectrophotometric sensitivities with each grating.
• Produce plots of slit illumination function and image quality at several different pupil illumination positions.
• Produce wavelength solution for each grating and how it varies with time, tracker position, etc.
• Develop flatfielding techniques.

Tests that will meet these goals:

• Measure Effective Slit Width for Longslits: Using flat field measure effective slit width and variation along the slit length for each longslit. (lab)
• Focus Acquisition Camera in Slitviewer Mode: Insert longslit in PFIS focal plane. Observe field and determine best focus for SALTICAM. (on-sky)
• Measure Wavelength Solution Stability: Using calibration system and given grating position, measure wavelength solution for various tracks and measure variations within a track. (on-sky)
• Measure Spectrophotometric Sensitivities of Gratings: For each grating, choose finite set of camera/grating angles. Observe standard stars and determine on-axis sensitivity. Test accuracy of interpolation for intermediate angles. (on-sky)

• Spectroscopy of Standard Stars
  • ESO's Optical and UV Spectrophotometric Standard Stars, in particular: Hamuy et al. Spectrophotometric Standards, PASP 106, 566 (1994)
• Galactic Superwinds:
  • Observe edge-on galaxies with slit orthogonal to plane
  • Measure velocities of emission lines
• Magellanic Cloud Supernova remnants/superbubbles (?)

2.1 Longslit Nod & Shuffle

3. Multi-Slit Spectroscopy

Technical goals:

• Test astrometric solutions and slitmask fabrication.
• Test slitmask insertion and position repeatability.
• Check for slitmask flexure with position, temperature.
• Test multi-slit acquisition strategy.
• Test multi-slit flatfields, spectral calibration.
• Plots of spectral senstivity versus field position for each grating.
• Plots of slit illumination function for "typical" slitmask (ideally a standard mask used for calibration).

Test that will meet these goals:

• Measure Off-axis Blaze Shift:
• Multi-slit Calibration:

Science programs:

• Off-axis spectroscopy of standard stars (see Long-slit spectroscopy)
• Chemical abundances and kinematics of planetary nebulae in NGC 1399

3.1 Multi-slit Nod & Shuffle

4. High time resolution Long Slit Spectroscopy

Technical goals:

• Test data acquisition and storage under heavy throughput.
• Test use of CCD frame transfer mode.

Science programs:

• High-time resolution spectroscopy/spectropolarimetry of accretion columns in highly magnetic CVs.

5. Fabry-Perot Imaging

Technical goals:

• Test etalon movement under full range of tracker motion.
• Test Fabry-Perot wavelength calibration.
• Measure FP efficiency.

Science programs:

• Intermediate-Redshift Galaxy Clusters
  • Ca K 3933 line is redshifted into FP range between z=0.1 and z=1.187
  • [O II] 3727 line is redshifted into FP range between z=0.15 and z=1.3

6. Long Slit Linear Spectropolarimetry

Technical goals:

• Test instrumental polarization as a function of field position.
• Test instrumental polarization as a function of pupil illumination.
• Verify waveplate mechanism performance.

Polarized Stars:
Name	Vmag	RA(2000)	Dec(2000)	Type	%P_B	PA	Obs Window
HD298383	9.68	09 22 29.76	-52 28 57.4	A0Ib	5.23	148.6	Oct-Jun
HD110984	8.95	12 46 44.91	-61 11 11.7	B0IV	5.7	91.6	Dec-Aug
HD111579	9.50	12 51 03.61	-61 14 37.8	B2Ib	6.46	103.1	Dec-Aug
HD126593	8.50	14 28 51.06	-60 32 24.8	B0.5IV	5.02	75.2	Jan-Sep
sigma Sco	4.57	16 20 38.20	-24 10 10.3	B5II	4.17	32.9	Feb-Sep
HD155197	9.20	17 10 15.62	-04 50 03.1	A0	4.38	103.2	Feb-Sep

7. Multi-Slit Linear Spectropolarimetry

Technical goals:

Science programs:

• Circumstellar Disks in LMC/SMC clusters: Requires low-resolution, full wavelength span - G0900 in blue and red tilts.
  • NGC 1818 (LMC)
  • NGC 330 (SMC)

7.1 Multi-Object Polarimetric Imaging