FGS Instrument Handbook for Cycle 11

Instrument Configuration

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This section is designed to complement the section on FGS instrument parameters contained in the Phase II Proposal Instructions. Table 6.1 summarizes the FGS instrument parameters.

Table 6.1: FGS Instrument Parameters

Config	Aperture	Sp_Element	Opmode	Optional_Parameters
FGS	PRIME (=1) 1, 2, 3 (FGS1=FGS1r)	F5ND F550W F583W F605W(FGS1r,FGS3) F650W (FGS 2) PUPIL	POS	ACQ-DIST, ACQ-MODE, COUNT, FESTIME, NULL, LOCK
			TRANS	ACQ-DIST, ACQ-MODE, SCANS, STEP-SIZE

Aperture

The aperture must be defined as either Prime or "1" on the logsheet. One FGS is designated as the astrometer: FGS1r is designated for Cycle 8 and beyond. For illustrations of the FGS1r field of view in the HST focal plane, refer to Chapter 1.

Spectral Element

"Spectral Element" refers to filters, etc. chosen for the observation. For FGS1r, the available filters are: F583W, F5ND, PUPIL, F605W, and F550W. Only one filter can be in place for an exposure, though multiple filters can be used during a visit (check that calibrations are available for the configuration). Recommendations for specific mode and filter combinations are discussed in Chapters 5 and 7. Table 6.2 presents a summary of the calibrated modes and filter configurations.

Table 6.2: Summary of Calibrated Mode and Filter Combination

Mode	Filter	Status	Comments
Position Mode:	F583W	Calibrated across entire FOV	OFAD in F583W only
	F5ND	Calibrated at the center of the FOV	Cross-filter calibration with F583W
Transfer Mode:	F583W; Others as needed	All calibrations at FOV center Select reference S-Curves from library of standard stars If needed, propose for calibration time to observe a reference standard star at the same epoch as the science visit (see Chapter 7).	Availability of standard stars with appropriate spectral energy distributions, i.e., colors of reference star and science target should differ by no more than (B-V) ~ 0.3

Mode

Two operation modes are available: Position Mode (POS) for measuring relative astrometric positions of targets in the FGS FOV and Transfer Mode (TRANS) for obtaining high resolution interferometry.

Optional Parameters for FGS Exposures

A program is customized by specifying optional parameters for each exposure. Table 6.3 and Table 6.4 list the optional parameters, default values, and recommended settings for Position and Transfer Modes, respectively.

Many of the optional parameters have default values. In such cases, the entry for that optional parameters may be omitted. If an observer wishes to override the default value, the parameter and its value must be specified.

Table 6.3: Position Mode Optional Parameters

Optional Parameter	Allowed Values	Comments and Recommendations
ACQ-DIST	DEF (default=15), 0.0 to 90.0 Units: arcsec	Determines the size (in arcseconds) of the search region. For ACQ-MODE=SEARCH, ACQ-DIST is the maximum radius of the search spiral. Recommendation: Although Search radii up to 90 arcsec are allowed, larger values must be used with caution, i.e., the larger the search radius, the more potential to acquire a spurious nearby star. If the target coordinates are expressed with respect to the Guide Star System, the default value of 15 arcsec (radius) should be sufficient to find the target. Typically the target is found with 0.3 to 1.0 arcsec. Reference: Appendix 1: Target Acquisition
ACQ-MODE	SEARCH (default) Units: None	Determines the strategy for locating the target. The Search Phase is the initial outward spiral to find and identify the target. The sequence of Search, CoarseTrack, WalkDown, and FineLock is the standard astrometry target acquisition scenario. No other options are available. Requirement: Default "SEARCH" Reference: Appendix 1: Target Acquisition
COUNT	DEF (default), 1-2621400 Units: FGS PMT counts	Expected count rate [target + background]. When the default is set, the count rate is calculated (by the proposal processing software) from the target V magnitude, filter, and aperture. The default background rate (from in-orbit measurements) is 712 counts/sec for all four PMTs. Recommendation: Allow the system to select the default. The default values are calculated using in-orbit photometric calibrations with accuracies appropriate for guiding purposes and for the calculation of exposure times. A few special cases may require non-default values and are discussed in the text. Reference: Chapter 7: See sections on Position and Transfer Mode Signal to Noise and Exposure calculation sections.
FESTIME	DEF (default), 0.025, 0.05, 0.1, 0.2, 0.4, 0.8, 1.6, 3.2 Units: seconds	Sets the averaging time for the Fine Error Signal (in seconds). The FESTIME also determines the rate at which the star selectors are adjusted to null the fine error signal. The default value for Position Mode is calculated from the COUNT parameter if explicitly entered, or if COUNT defaults to the V magnitude and the filter. All Transfer Mode observations use FESTIME = 0.025 seconds. Recommendation: The algorithm that selects the default FESTIMEs from the specified brightness of the target is based on photon statistics and a conversion from photon noise to equivalent positional error. For fainter targets, longer integration times are supplied by the default algorithm to assure that the FGS can track the fringe and remain in FineLock. For non-point sources, the S-Curve amplitude is reduced because of the increased contribution of the background or companion. In these cases, it may be desirable to adjust the FESTIME. Please consult with STScI. Reference: Chapter 7: See Sections on Position and Transfer Mode Signal to Noise and Exposure calculation sections.
LOCK	FINE (default), COARSE, 0.0-1.0 Units: None	The method used by the astrometer to track the science or reference target. (Note, this parameter does not specify the HST guiding mode). Because of the excessive wear to bearings inside the instrument, CoarseLock is no longer allowed. Requirement: Fine. Reference: Chapter 5 and Chapter 7.
NULL	YES, NO (default) Units: None	Determines whether the next FESTIME begins immediately after the previous one or not until the star selectors have been repositioned. This parameter may be applicable for very fast moving target. Observers should consult with STScI before specifying non-default values. Recommendation: This use of this parameter is limited to a few specific observation scenarios. Most standard astrometry programs require NULL=NO. Reference: STScI will alert the proposer if a non-default value is required.

Table 6.4: Transfer Mode Optional Parameters

Optional Parameter	Allowed Values	Comments and Recommendations
ACQ-DIST	DEF (default = 15), 0.0 - 90.0 Units: arcsec	Determines the size (in arcseconds) of the search region. For ACQ-MODE=SEARCH, ACQ-DIST is the maximum radius of the search spiral. Recommendation: Although a search radius of up to 90 arcsec is allowed, larger values must be used with caution, i.e., the larger the search radius, the more potential to acquire a spurious nearby star (spoiler). If the target coordinates are expressed with respect to the Guide Star System, the default value of 15 arcsec (radius) should be sufficient to find the target. HST's pointing accuracy usually places the target within 1 arcsec of the expected location in the FGS. Reference: Appendix 1: Target Acquisition
ACQ-MODE	SEARCH (default) Units: arcsec	Determines the strategy for locating the target. The search phase is the initial outward spiral to find and identify the target. The sequence of Search, CoarseTrack, WalkDown, and FineLock is the standard astrometry target acquisition scenario. No other options are available. Requirement: Default "SEARCH" Reference: Appendix 1: Target Acquisition
SCANS	1 (default)-200 Units: None	Determines the number of separate scan lines. Successive scans are taken in opposite directions. Recommendation: Determine the number of scans to achieve the required signal-to-noise. Reference: Chapter 7
STEP-SIZE	1.0 (default) 0.3-10.0 Units: mas	The angular distance (in mas) stepped by the IFOV along an interferometric axis in 0.025 seconds. To achieve the best results, step sizes of 0.6 or 1 mas should be selected. Recommendation: Value depends on the science target and goals of the observation, required resolution and signal-to-noise. Reference: Chapter 7