8.16 Cycle 9 Calibration Plan

The Cycle 9 calibration program is aimed at maintaining the calibration of WFPC2 via monitoring programs, as well as continuing two proposals from previous Cycles into Cycle 9 (photometric and PSF characterizations) and performing several new tests (on-orbit red leak check, CTE, wavelength stability check of narrowbands and linear ramp filters). Table 8.9 summarizes the programs proposed for calibrating WFPC2 in Cycle 9, followed by detailed descriptions of each program (including proposal numbers, statement of purpose, observing description, products, and accuracy expected).

Table 8.9: WFPC2 Cycle 9 Calibration Plan.

ID	Proposal Title	Frequency	Estimated Time (orbits)		Scheduling Required	Products	Accuracy Required	Notes
			"External"	"Internal"
Routine Monitoring Programs
8822- 8825	WFPC2 Decons & Associated Observations	1-2/4 wks	30	82	every 28 d	Synphot, CDBS	1-2%	Decons, phot. & focus monitor, internals, UV throughput, VISFLATs, and UV FLATs
8811	Standard Darks	weekly		366	every 7 d	CDBS	1 e-/hr	Also hot pixel lists on WWW.
8826- 8828	Supplemental Darks (8460, 8461)	0-3/day		1282	anytime		n/a	For archive only, no analysis provided
8812	Internal Monitor	weekly		76	every 7d	CDBS	0.8e/pixel	Includes INTFLAT monitor, for possible future preflashed observations.
8815	Earth Flats	continuous		210	mid-cycle	CDBS	0.3%
8816	UV Earth Flats	continuous		400	mid-cycle	CDBS	3-10%	Outsourcing candidate.
8813	Astrometric Monitor	2/cycle	2		early & late	ISR	0.05''	Omega Cen as well as K-spots.
8817	Intflat Sweep and Linearity Test	1/cycle		21	mid-cycle	TIR	0.3%
Special Calibration Programs
8818	Photometric Characterization	1	2		mid-cycle	ISR	2-3%	GRW+70D5824; nonstandard filters.
8819	PSF Characterization	1	6		late in cycle	CDBS	10%	Omega Cen; standard broadband filters.
8814	Read Leak Check	1	2		mid-cycle	Synphot, CDBS	2%	Solar analogs used to measure UV filter read leaks.
8821	CTE - Monitor and Absolute Calibration	1	15		mid/late	ISR	0.01 mag	Includes monitor as well as follow up to ground based observations. Outsourcing candidate.
8820	Wavelength Stability of Narrowband and Linear Ramp Filters	1	4	15	mid/late	CDBS, ISR	2Å	Check of wavelength/aperture mapping and test for changes in LRFs.
	~10% reserve		6					Placeholder.
TOTAL TIME (including all executions)			67	2452

8822, 8823, 8824, 8825: Decontaminations and Associated Observations

• Purpose: Monthly WFPC2 decons. Other programs tied to decons are also included: photometric stability check, focus monitor, pre- and post-decon internals, UV throughput checks, VISFLAT sweep, and internal UV flat check.
• Description: Decontamination: UV-blocking contaminants removed and hot pixels annealed by warming the CCDs to +20C for 6 hours. Internals: intflats, biases, darks & kspots, before/after decons.
  Photometric Monitor: GRW+70D5824 is observed after each decon and before every other decon: (1) F170W in all chips to monitor far UV contamination. (2) As many as possible of F160BW, F218W, F255W, F336W, F439W, F555W, F814W will be observed in a different chip each month.
  Focus Monitor: two PC, F555W observations of GRW+70D5824 will be taken during every photometric monitoring orbit (one at orbit start, one near orbit end).
  UV Throughput: PC & WF3 UV observations in most UV filters, popular UV filters in all chips, to verify that the UV spectral response curve is unchanged. In addition, two PC, F555W observations will be included as an extra focus monitor.
  Internal UV flat fields: obtained with the CAL channel's ultraviolet lamp (UVFLAT) using the UV filters F122M, F170W, F160BW, F185W, & F336W. The UV flats are used to monitor UV flat field stability and the stability of the F160BW filter by using F170W as the control. The F336W ratio of VISFLAT to UVFLAT provides a diagnostic of the UV flat field degradation & ties the UVFLAT and VISFLAT flat field patterns. Two supplemental dark frames must be obtained immediately after each use of the lamp to check for possible after-images.
• Products: SYNPHOT, CDBS, Instr. Handbook, TIPS meetings, WWW reports, TIR, ISR; new UV flat fields if changes are detected.
• Accuracy Goals: Photometry: less than 2% discrepancy between results, 1% rms expected. Focus measurement: 1.5 µm accuracy with a goal of 1 µm. UV throughput: better than 3%. Flat field: temporal variations monitored at 1% level. Gain ratios: stable to better than 0.1%. UV flats: About 2-8% pixel-to-pixel expected (filter dependent). VISFLATs: stable to better than 1% in overall level and spatial variations (after correcting for lamp degradation). Contamination effects should be < 1%.

8811:WFPC2 Cycle 9 Standard Darks

• Purpose: Measure dark current & identify hot pixels.
• Description: Six 1800s exp/week with the shutter closed, five with clocks off, one with clocks on. This frequency is required due to the high formation rate of new hot pixels (several tens/CCD/day). Five darks per week are required for cosmic ray rejection, counterbalancing losses due to residual images, & improving the noise of individual measurements. Sometimes, no usable darks are available for a given week due to residual images, resulting in a longer-than-usual gap in the hot pixel lists, but in a decon week, information on hot pixels that became hot and then annealed would be lost irretrievably. As a result, pre-decon darks (see Decon proposal) are executed NON-INT and at least 30 min after any WFPC2 activity.
• Products: Weekly darks delivered to CDBS and monthly tables of hot pixels on the WWW. Superdark reference files.
• Accuracy Goals: Require ~1 e^-/hr (single-pixel rms) accuracy for most science applications. Expected accuracy in a typical superdark is 0.05 e^-/hour for normal pixels. The need for regular darks is driven by systematic effects, such as dark glow (a spatially and temporally variable component of dark signal) and hot pixels, which cause errors that may exceed these limits significantlly.

8826, 8827, 8828: WFPC2 Cycle 9 Supplemental Darks

• Purpose: Images will allow for frequent monitoring of hot pixels.
• Description: This program is designed to provide up to three short (1000s) darks per day, to be used primarily for the identification of hot pixels. Shorter darks are used so that the observations can fit into almost any occultation period, making automatic scheduling feasible. These supplemental darks are low priority, and should be taken only when there is no other requirement for that specific occultation period. This program complements the higher priority Standard Darks proposal that has longer individual observations for producing high-quality pipeline darks and superdarks. Hot pixels are often a cause of concern for relatively short science programs, since they can mimic stars or mask key features of the observations: about 400 new hot pixels/CCD are formed between executions of the Standard Darks program. The supplemental darks are available to the GO community from the archive; there is no plan to use them in our standard analysis and products.
• Products: None.
• Accuracy Goals: For archive only, no STScI analysis provided.

8812: WFPC2 Cycle 9 Internal Monitor

• Purpose: Verify the short-term instrument stability at both gain settings and provide INTFLATs for calibrating preflashed observations.
• Description: Each set of internal observations consists of 8 biases (4 at each gain) and 4 INTFLATs (2 at each gain). The entire set should be run once per week, except for decon weeks, on a non-interference basis. During the decon week, INTFLATs in F502N will be taken, with each shutter blade and at a variety of exposure times to test for linearity. The F502N filter is likely to be the recommended filter for preflashing observations.
• Products: Superbiases delivered annually to CDBS; TIPS reports on possible buildup of contaminants on the CCD windows (worms) as well as gain ratio stability, based on INTFLATs. A Technical Instrument Report will be issued if significant changes occur. Possible preflash correction images will be generated.
• Accuracy Goals: Approximately 120 bias frames are used for each superbias pipeline reference file, generated once a year; accuracy is required to be better than 1.5 e^-/pixel, and is expected to be 0.8 e^-/pixel.

8815: WFPC2 Cycle 9 Earth Flats

• Purpose: Monitor flat field stability. This proposal obtains sequences of Earth streak flats to construct high quality flat fields for the WFPC2 filter set. These flat fields will allow mapping of the OTA illumination pattern and will be used in conjunction with previous internal and external flats to generate new pipeline superflats. These Earth flats will complement the Earth flat data obtained during SMOV and Cycles 4-8.
• Description: Observations of the bright Earth (earthcals) are obtained in a variety of filters. Approximately 200 exposures in each of four narrowband filters (F375N, F502N, F656N, F953N) are required, as well as about 50 exposures in other filters (F160BW, F336W, F343N, F390N, F437N, F469N, F487N, F631N, F658N, F673N -- the F160BW filter is included to provide pinhole information). In addition, if dark-earth pointing becomes available, some of the broadband filters are requested (F336W, F439W, F555W, F675W, and F814W; all marked as on-hold for now), 10 exposures in each filter.
• Products: New flat fields generated and delivered to CDBS if changes detected.
• Accuracy Goals: The single-pixel signal-to-noise ratio expected in the flat field is 0.3%.

8816: WFPC2 Cycle 9 UV Earth Flats

• Purpose: Monitor flat field stability. This proposal obtains sequences of earth streak flats to improve the quality of pipeline flat fields for the WFPC2 UV filter set. These Earth flats will complement the UV earth flat data obtained during Cycle 8.
• Description: Earth streak-flats are taken in UV filters (F170W, F185W, F218W, F255W, F300W, F336W, and F343N). Those UV filters with significant read leak will also be observed crossed with selected broadband filters (F450W, F606W, F675W, and F814W), in order to assess and remove the read leak contribution. Earthflats required: 100 for each of the 7 UV filters plus 20 with each of the crossed filter sets (16 combinations). The entire proposal should be done within 7 months, with the observations evenly distributed over that period of time. The observations are divided into 10 batches, with each batch done 21 days apart.
• Products: Updated flat fields for pipeline via CDBS.
• Accuracy Goals: 3-10%. Outsourcing candidate.

8813: WFPC2 Cycle 9 Astrometric Monitor

• Purpose: Verify relative positions of WFPC2 chips with respect to one another.
• Description: The positions of the WFPC2 chips with respect to each other appear to be shifting slowly (by about 1 pixel, since 1994). The rich field in Cen (same positions as Cycle 8 proposal 7627) is observed with large shifts (35'') in F555W only, every ~six months. This will allow monitoring of shifts in the relative positions of the chips or changes in the astrometric solution at the sub-pixel level. Kelsall spot images will be taken in conjunction with each execution.
• Products: TIPS reports, ISR, update of chip positions in PDB and of geometric solution in STSDAS tasks metric and wmosaic if significant changes are found.
• Accuracy Goals: At least 0.01'' in relative shifts; 0.05" or better for absolute.

8817: WFPC2 Cycle 9 Intflat Sweeps and Linearity Test

• Purpose: Using INTFLAT observations, this WFPC2 proposal is designed to monitor the pixel to pixel flat field response and provide a linearity check. The INTFLAT sequences, to be done once during the year, are similar to those from the Cycle 8 program 8448. The images will provide a backup database in the event of complete failure of the VISFLAT lamp as well as allow monitoring of the gain ratios. The sweep is a complete set of internal flats, cycling through both shutter blades and both gains. The linearity test consists of a series of INTFLATs in F555W, in each gain and each shutter.
• Description: Intflat sweep -- flat fields are obtained with a variety of filters (F336W, F439W, F547M, F555W, F569W, F606W, F622W, F631N, F502N, F656N, F675W, F673N, F702W, F785LP, F814W, F1042M) using shutters A and B, and gains 7 and 15; the BLADE optional parameter is used throughout. A smaller set is obtained only at gain 7 using any shutter blade (F160BW, F300W, F380W, F390N, F410M, F437N, F450W, F469N, F487N, F467M, F588N, F658N, F791W, F850LP, F953N).
  Linearity test -- flat fields are taken with F555W at a variety of exposure times, using shutters A & B, and gains 7 & 15. In addition, a set is done with clocks=YES (only gain 7, shutter A; gain 7 shutter B set was taken during Cycle 8). Since the INTFLATs have significant spatial structure, any non-linearity should appear as a non-uniform ratio of INTFLATs with different exposure times.
• Products: TIPS, TIR if any significant variations are observed.
• Accuracy Goals: INTFLATs: Stable to better than 1%. (INTFLATs will provide a baseline comparison of INTFLAT vs. VISFLAT (taken in decon proposal) if the CAL channel system fails.)

8818: WFPC2 Cycle 9 Photometric Characterization

• Purpose: Provide a check of the zeropoints and contamination rates in non-standard WFPC2 filters.
• Description: Observations of the standard star GRW+70D5824 in PC1 and WF3 will be made using filters that are not routinely monitored (F380W, F410M, F450W, F467M, F547M, F569W, F606W, F622W, F702W, F785LP, F791W, F850LP, and F1042M). Images should be taken within 7 days after a decon, to minimize any contamination effects. Results from this program will be compared with data from the Cycle 7 program 7628 and Cycle 8 program 8451.
• Products: TIR, SYNPHOT update if necessary.
• Accuracy Goals: 2% photometry.

8819: WFPC2 Cycle 9 PSF Characterization

• Purpose: Provide a subsampled PSF over the full WFPC2 field of view in order to support PSF fitting photometry and provide data to test PSF subtraction as well as dithering techniques (e.g., effects of OTA breathing and gain).
• Description: Measure PSF over full field in photometric filters in order to update the TIM and TinyTIM models and to allow accurate empirical PSFs to be derived for PSF fitting photometry. These observations will also be useful in order to test PSF subtraction and dithering techniques at various locations on the CCD chips. With ~1 orbit per photometric filter, each star is measured 16 times per filter at different pixel phase, providing a high S/N, critically sampled PSF. This will improve the quality of PSF fitting photometry. The step size is 0.125 arcseconds, very close to 1.25 pixels in the WFs and 2.75 pixels in the PC - so that fractional steps of 0.25, 0.5, and 0.75 pixels are used in each camera. This provides a critically sampled PSF over most of the visible range. The crowded Cen field is used, with 40 sec (gain = 15) images taken through each of the wide standard photometric filters (F336W, F439W, F555W, F675W and F814W). The Cycle 9 observations use the same pointings as in Cycles 7 and 8. The proposal also allows a check for subpixel phase effects on the integrated photometry.
• Products: PSF library (WWW). Updates for TIM and TinyTIM. Accurate empirical PSFs to be derived for PSF fitting photometry.
• Accuracy Goals: If breathing is less than 5 microns peak to peak, the resulting PSFs should be good to about 10% in each pixel. PSF fitting results using this calibration would of course be much more accurate. In addition, the test gives a direct measurement of sub-pixel phase effects on photometry, which should be measured to better than 1%.

8814: WFPC2 Cycle 9 Red Leak Check

• Purpose: Obtain an on-orbit verification of the red leak in WFPC2 UV filters by observing solar analog standards in the UV.
• Description: Two targets, for which FOS spectrophotometry is available, will be chosen from those used in the solar analog photometric verification program (P041-C, P177-D, or P330-E; Cycle 6 proposal 6934 and 6179). Observed count rates will be compared to SYNPHOT predictions of the expected count rates from the UV proper and from the red leak. A robust verification of the red leak will benefit programs that rely on precision multicolor photometry and comparison with model spectra. Some discrepancies seen thus far could be explained by a significant (> 10%) error in the estimated red leak.
• Products: TIR and SYNPHOT update if necessary.
• Accuracy Goals: 2% on the flux measurements; accuracy of read leak determination will vary by filter.

8821: WFPC2 Cycle 9 CTE - Monitor and Absolute Calibration

• Purpose: Monitor CTE changes during Cycle 9 and provide complementary suite of observations to ground based CTE proposal.
• Description: Monitor: Observations of Cen (NGC 5139) are taken every 6 months during Cycle 9 to monitor changes in the CTE (charge transfer efficiency) of WFPC2. An extension of proposals 7629 and 8447, the principal observations will be at gain 7, in F814W and F555W, in WF2 and WF4, at a variety of preflash (background) levels (20 to 1000 electrons).
  Absolute Calibration: Observations of three of the globular clusters Eridanus, NGC 2419, Pal 3, Pal 4, and Pal 14 are planned, to match the targets selected for a companion ground based proposal - subject to approval of the latter. Direct comparison with ground based observations permits a direct verification of the absolute photometric calibration of WFPC2 in observations that may be affected by CTE, and therefore a more robust determination of the zero point for many WFPC2 observations. While there is no evidence that the current WFPC2 zero point is inapplicable to faint sources, enough corrections need to be applied that a direct verification is extremely desirable. Comparison to a well-populated field observed from the ground can also yield a direct, independent determination of the CTE effect in such observations (Stetson 1998). Five suitable fields with existing WFPC2 observations have been selected, and a WYIN 3.5m proposal (PI Whitmore) has been submitted for ground based observations of these fields with exposure times sufficient to reach 1% photometric accuracy at V=22. The ground based proposal asks for observations of three of these five fields, to be chosen on the basis of their RA and the time of the observations.
• Products: Instrument Science Report. Outsourcing candidate?
• Accuracy Goals: 0.01 magnitudes.

8820: WFPC2 Wavelength Stability of Narrowband and Linear Ramp Filters

• Purpose: Verify the mapping of wavelength as a function of CCD position on LRFs; check for changes in central wavelengths of narrow band filters.
• Description: On-orbit VISFLATs taken through the ramps crossed with the narrow band filters will constrain the wavelength calibration of the ramps filters relative to the narrow band filters. Comparison with similar Cycle 4 data will show whether the filter properties have evolved with time due to annealing / shrinkage of the thin film materials. The uncrossed VISFLATs can also be used to constrain the transverse (cross-wavelength) placement of the ramp filters. In addition, 4 external orbits are required for external observations of an extended line emission source (planetary nebula) through ramp filters. These will provide an absolute test for changes in the ramp filters.
• Products: New aperture locations if necessary. Updated wavelengths / throughput curves for both ramp and narrow band filters in SYNPHOT.
• Accuracy Goals: Central wavelengths to 2Å.