The active image area of each WFC detector is 4096 by 2048 pixels. The mean scale is 0.049 arc seconds/pixel, and the combined detectors cover an approximately square area of 202 arc seconds on a side. In establishing reference pixel positions we have to consider the overscan pixel areas which extend 24 pixels beyond the edges in the long direction. So each CCD must be regarded as a 4144 by 2048 pixel area. The gap between the two CCDs is equivalent to 50 pixels. In
Figure 7.3 the letters A, B, C, and D show the corner locations of the four readout amplifiers.
We define apertures named WFC1 and
WFC2 which represent the two CCDs, with their reference points near the geometric center of each chip. The positions have been moved about 50 pixels from the center line to avoid a discontinuity at the amplifier readout boundary. However, we keep two other apertures named
WFC1-FIX and
WFC2-FIX at the original central locations (2072,1024). For extended sources, choosing new positions may not be of any advantage and it may be more effective to use these fixed positions.
The aperture WFC encompasses both detectors, and has its reference point near the overall center but about 10 arcseconds away from the inter-CCD gap. This reference point is (2124,200) on the WFC1 CCD. Again, this point has been moved away from the center line, but the reference point for
WFC-FIX remains at (2073,200). Selection of
WFC1,
WFC2 or
WFC only changes the pixel where the target will be positioned. In all three cases data is normally delivered in a file containing two science image extensions, one for each detector. See the
ACS Data Handbook for details of the ACS data format. Reading out a subarray, which consists of part of only one of the CCDs, is done only if requested.
WFCENTER is similar to
WFC, but is placed at the center of the combined WFC full field. The center is defined as the average of the four corners in the distortion corrected space. Because of the scale variation this does not appear at the center in pixel space, but rather is on WFC2 about 20 pixels from the edge. Selection of
WFCENTER can be of use in obtaining observations with maximum overlap at unique orientations and for mosaics.
For sets of observations which take place over a substantial part of a year, the telescope roll limitations will require measurements to be taken over most of the angular range. On sky, the
WFC aperture is roughly square, and it is natural to design observations in steps of 90
° to consistently cover the same area. There will be some region at the edges not covered at all four orientations. However, a square area of side 194.8 arcseconds centered on
WFCENTER, and with edges parallel to the V2 and V3 axes, is overlapped at all four positions. In designing a mosaic which combines observations at 90
° steps, a translation of about 190 arcseconds between pointings would provide continuous coverage.
There are five ramp filters. Each ramp filter consists of three segments (inner, middle, outer) that can be rotated across the WFC field of view as indicated in
Figure 7.4. The IRAMP filters can only be placed on
WFC1 in a location which will define the aperture
WFC1-IRAMP and the ORAMP filters only on WFC2 creating the aperture
WFC2-ORAMP. The MRAMP filters can lie on WFC1 or WFC2 with corresponding apertures
WFC1-MRAMP and
WFC2-MRAMP. The approximate aperture locations are indicated in
Figure 7.4, while actual data obtained during ground calibrations are overlayed on an image of a ramp filter in
Figure 7.5. Operationally, a fixed reference point will be defined for each detector and filter combination. Then the ramp filter will be rotated to place the required wavelength at the reference position.
The reference positions for all defined apertures are given in Table 7.6 in pixels, and in the telescope V2,V3 reference frame where values are measured in arc seconds. The values given here are based on in-flight calibration results. The x and y axis angles are measured in degrees from the V3 axis towards the V2 axis. This is in the same sense as measuring from North to East on the sky. The “extent” of the ramp filter apertures given in
Table 7.6 are the FWHM of the monochromatic patches (visible in
Figure 7.4) measured from a small sample of ground calibration data. To use a ramp filter in a Phase II program, specify the filter name, the central wavelength, and the aperture. The scheduling software will then automatically rotate the filter to the appropriate wavelength, and point at the reference point of the aperture chosen.
The aperture chosen may either be the full CCD or just the quadrant on which the ramp filter lies. This second choice was new as of Cycle 15, and requires that the aperture be specified. The apertures matching each filter are given in
Table 7.6. Those with names ending in Q are the quadrants. It will normally be preferable to choose the quadrant aperture to save data volume and buffer dumping time. All apertures may be used with non-ramp filters. A target may thereby be put at the same position using a ramp and a non-ramp filter. Note that the WFC2-MRAMPQ aperture is available but not supported. Please see the footnotes to
Table 7.6 for a complete list of available but unsupported apertures.
Only the middle segments of the five ramp filters could be used with the HRC. They are FR914M, FR459M, FR505N, FR388N and FR656N. All five middle segments could be used with any of the HRC apertures listed in
Table 7.7 (see
Table 7.8 for the aperture reference positions). There were no special ramp apertures with the HRC because when a ramp filter is used with the HRC it covered the entire HRC CCD. This region was defined by the HRC aperture in
Table 7.8. To use the HRC-512 or HRC-SUB1.8 subarray apertures with a ramp filter, POS TARGs had to be used to align the aperture correctly.
As with the WFC, the fixed reference point of the ramp aperture was defined operationally depending on the detector, aperture and filter combination. Please refer to
Section 7.3.1,
Section 5.3.1, and
ACS ISR 02-01 for further information.
When a filter designed for the HRC is used with the WFC, it only covers a small area on either WFC1 or WFC2. The projected filter position may be placed on either chip by selection of the filter wheel setting.
Figure 7.4 shows how the filter projection may be placed so as to avoid the borders of the CCDs. When a WFC observation is proposed using a HRC filter spacecraft commanding software automatically uses internal built-in apertures designed for these observing scenarios, called WFC1-SMFL and WFC2-SMFL. Reference positions at or near the center of these apertures are defined so that a target may be placed in the region covered by the chosen filter. Note that WFC2 SMFL is available but not supported.
The axis angles given in Table 7.6 do not refer to the edges of the apertures as drawn, but rather to the orientation of the x and y axes at the WFC reference pixel. These angles vary slightly with position due to geometric distortion.
For the polarizers and F892N used with WFC, the default will be to read out a subarray. The subarray will be a rectangular area with sides parallel to the detector edges which encompasses the indicated filtered areas. For ramp filters the default will be to readout the entire WFC detector, unless a polarizer is used with the ramp filter, in which case a subarray is read out. Users cannot override the small filter subarrays.
Apertures have been provided for use with the polarizer sets similar to the SMFL apertures. These apertures are selected automatically when a polarizing spectral element is used, and a single WFC chip quadrant readout is obtained. The aperture parameters given in
Table 7.6 are valid for all three polarizing filters in each polarizer set, UV or visible, to the stated significant figures.
The HRC has an area of 1062 pixels by 1024 pixels including 19 physical overscan pixels at each end in the x direction. The active area is 1024 by 1024 pixels. The mean scales along the x and y directions are 0.028 and 0.025 arcseconds/pixel, thus providing a field of view of about 29 by 26 arcseconds in extent. The anisotropy and variation of scales is discussed in
Section 10.3 of this Instrument Handbook. The reference point for the aperture labelled
HRC-FIX, and initially for
HRC, is at the geometric center, (531,512). As with the
WFC apertures, there may be reason to move the HRC reference point later.
The HRC is equipped with two coronagraphic spots, nominally 1.8 and 3.0 arcseconds in diameter and a coronagraphic finger, 0.8 arcseconds in width. Apertures
HRC-CORON1.8,
HRC-CORON3.0, and
HRC-OCCULT0.8 are defined to correspond to these features. The coronagraphic spots are only in the optical train and thus in the data if HRC-CORON1.8 or HRC-CORON 3.0 are specified. Their positions are shown in
Figure 7.6 (left panel). In addition we define a target acquisition aperture,
HRC-ACQ designed for acquiring targets which are subsequently automatically placed behind a coronagraphic spot or the occultation finger.
The positions of the coronagraphic spots have been found to fluctuate. Observations will need to incorporate a
USE OFFSET special requirement to allow current values to be inserted at the time of the observation.
A substantial region masked out by the occulting finger will be present in the HRC data (
Figure 7.6, right panel). The occulting finger is not retractable. It will be in every HRC exposure. However as with any other detector feature or artifact, the “lost” data can be recovered by combining exposures which were suitably shifted with respect to each other. A dither pattern,
ACS-HRC-DITHER-LINE has been defined for this purpose and spans the area flagged for the HRC occulting finger (~1.6 arcseconds or ~56 pixels wide), with an extra ~0.3 arcseconds or ~10 pixels of overlap.
Use of the prism PR200L requires specifying aperture HRC, but results in a reference point of (671,512) to optimally center the target coordinates within the somewhat vignetted prism field of view. Although the HRC direct imaging and PR200L prism apertures have the same name in APT, they are actually distinct, and
HST executes a small angle maneuver between observations of a given target with them, to compensate for the positional deflection by the prism. One consequence is that the Special Requirement
SAME POS AS cannot be used among mixed direct and prism exposures, as always with different apertures.
The SBC aperture is 1024 pixels square. There are no overscan pixels to consider. The x and y scales are 0.034 and 0.030 arcseconds/pixel leading to a coverage on the sky of 35 by 31 arcseconds. The reference point has been moved to (512,400) to place targets further from a bad anode which disables several rows of the detector near y = 600. As with the CCDs we maintain an
SBC-FIX aperture which will always have position (512,512). MAMA detectors slowly lose efficiency with each exposure, therefore the SBC reference point may be shifted again if the chosen position shows this effect to a measurable degree.
Use of either prism PR110L or PR130L requires use of aperture SBC and results in a reference point of (425,400) to optimally center the target coordinates with respect to vignetting on the right side of the field and to avoid a set of bad rows at 599 to 605.
Although the SBC direct imaging and prism apertures have the same name in APT, they are actually distinct, and
HST executes a small angle maneuver between observations of a given target with them, to compensate for the positional deflection by the prisms. One consequence is that the Special Requirement
SAME POS AS cannot be used among mixed direct and prism exposures.
Figure 7.7 shows a direct and prism observation of the same field. The prism now is vignetted on the positive x side. The reference points and the small angle maneuver place the same target near the reference point of each view.
