Several circular patterns consisting of a dark ring with a bright center, are visible in
the ACS flat fields, with typical diameters of ~30
pixels on HRC and ~100
pixels on WFC. These artifacts are shadows of dust on the CCD windows and are weaker on the f/25
WFC than on the f/68
HRC. The motes can be seen in WFC and HRC flats in Figure 4.16
and Figure 4.17
Since the shapes and depths of these motes are almost independent of wavelength,
their effects will be removed by the flats to <<
1%, unless any of these particulate contaminants move to different positions on the CCD windows. In case of particulate migrations, the internal lamp flats have a lower f
-ratio with a wider angular distribution and cannot be used to patch the flat fields because they wash out the mote shadows. To correct for new motes, patches to the pipeline flats must be made using the original laboratory flats, corrected for the low-frequency flats derived in-flight or, for short wavelengths, using observations of the bright Earth.
Larger motes are sometimes present due to dust and blemishes on several ACS
filters, including F606W, POL0V, and POL60V. Because the filters are located farther from the detector windows in a converging light beam, imperfections on the filters produce an out-of-focus image at the detector, where typical mote diameters are about 350
- 400 pixels on the WFC and about 250
300 pixels on the HRC. One of these large motes can be seen on chip 2 of the WFC F606W flat in Figure 4.16
Until April 2004, the positioning accuracy of the filter wheels has been within
motor steps of the nominal position. This delta corresponds to a distance on the detectors of ~18 HRC pixels and ~20 WFC pixels. Features with sharp transmission gradients at the filter wheels cause a corresponding flat-field instability, where errors are 1%
3% for a few pixels near the blemishes. If the filter wheel lands in a different place the dust mote will move. Blemish mis-registration is an error in the pixel-to-pixel high frequency component of the flat fields and is not related to the low-frequency L-flat correction, which has been applied for all standard and polarizing filters. For details on the L-flat correction, see Section 4.4.2
This problem was recognized and addressed before launch by a laboratory
calibration campaign to obtain flat fields at the nominal position and at plus and minus one step for the F606W
CLEAR on the WFC and for the two POLV filters in combination with the highest priority F475W, F606W, and F775W filters on both HRC and WFC. Since the resolver position uniquely determines the filter wheel step, the ACS pipeline data processing has been enhanced to automatically apply the proper flat for the wheel step position. The keyword FWOFFSET
has been added to the ACS image headers to indicate the position of the filter wheel. In April 2004, an update was made to the ACS flight software and the filter wheel is now always positioned at its nominal position. For more information on flat fields for filter wheel offset positions, refer to ACS ISR 2003-11
ACS was designed with a requirement that no single stray light feature may contain
more than 0.1% of the detected energy in the object that produced it. This goal has generally been met, but during extensive ground and SMOV test programs, a few exceptions have been identified (Hartig et al. 2002, Proc. SPIE 4854
) such as the WFC elliptical haloes and the F660N ghosts. While these ghosts exceed the specified intensity, their origin and characteristics are well defined and they should have minimal impact on the ACS science program. Details about some optical ghosts relevant for ACS are described below.
|WFC elliptical haloes: these ghosts are caused by reflection from the CCD
surface (which lies at an ~20°
angle to the chief ray) up to the detector windows and back to the CCD. They show up as pairs of elliptical annuli, aligned along the negative diagonal of the FOV (see Figure 4.19
), and are observed when bright sources are placed on the lower right (D amplifier) quadrant of the WFC detector. The surface brightness of the annuli increases and size decreases with proximity to the corner. Two pairs of ghosts are seen, produced by reflection from the four window surfaces. The total energy fraction in each ghost may exceed 0.2% of the target signal.
|F660N ghosts: the F660N narrow band filter produces pairs of relatively
bright circular annuli stationed near to (but radially outward from) the target image (see Figure 4.20
). This is due to reflection from the two surfaces of the second “blocker” substrate back to the many-layer dielectric stack on the first substrate, which in turn reflects at high efficiency at the filter wavelength range. These haloes contain ~2% of the detected target energy and are always about 10 and 20 pixels in diameter.
Annular ghosts: large annular ghosts1
near their parent images are caused by reflection from the detector windows, back to the filters, then returning to the CCD (see Figure 4.19
). Another type of annular ghost arises from reflections between the inner and outer window surfaces; these are much smaller in diameter, relatively low in intensity (well within the specification) and are displaced radially from the parent image by a small amount.
In general, little can be done about ghosts and blooming in the post-observation
data processing phase. Instead, some judicious planning of the actual observations, particularly if bright sources are expected in, or near, the field of view, is recommended. For instance, the impact of diffraction spikes (which for ACS lie along X and Y axes) and of CCD blooming (which occurs along the Y direction) due to a bright star, can be reduced by choosing an ORIENT2
which prevents the source of interest from being connected to the bright star along either of these axes. Alternatively, a suitable ORIENT3
could move the bright star(s) into the interchip gap or off the field of view altogether. Similarly, the impact of WFC elliptical haloes can be minimized by avoiding a bright star in the quadrant associated with amplifier D.
is a shower of scattered light from a very bright star that is just off the edge of the CCD. This rare anomaly occurs when a star falls at the edge of the mask in front of the chip; the starlight reflects off the CCD, then off the mask, and back to the detector.
The ACS/WFC detector has four amplifiers (A, B, C, D; see Figure 1.1
) through which the four quadrants of the detector are read separately and simultaneously. As the quadrants are read out, electronic cross-talk between the amplifiers can be induced. As a result, an imaged source in one quadrant may appear as a faint, mirror-symmetric ghost image in the other quadrants. The ghost image is often negative; therefore, bright features on the “offending” quadrant show up as dark depressions on the “victim” quadrants. See Figure 4.22
and Figure 4.23
for actual examples.
The latest calacs
corrects for cross-talk in post-SM4 full frame WFC images as part of the doBlev
stage (see Section 3.4.1
). Additional information about calacs
is also available at
|In general, the conclusions from the ACS/WFC cross-talk character
ization are as follows:
After SM4, cross-talk due to low signal sources is much weaker than before SM4, and can be safely ignored for both GAIN = 1 and GAIN = 2.
For the current default GAIN = 2, the post-SM4 cross-talk is insignificant (< ~0.0001% (between amplifier pairs on different WFC CCDs, but intra-CCD amplifier cross-talk is relatively uniform at ~0.009% and is removed by calacs
in the ‘doBlev’ stage.
This image (from program ID 10594, image j9ew02wlq
, GAIN = 2) shows the galaxy in quadrants C and D. Its cross-talk ghosts, seen as dark oval shapes in quadrants A and B, are due to low signal offending sources of ~100 e−
to 1000 e−
in the area of the reddish rim of the galaxy. Also the ghosts of three largest galaxies in quadrant B are easily identifiable in quadrant A. The image in quadrants A and B is stretched within a narrow signal range centered at the sky background level, which makes the ghosts distinctly stand out against the background.
Most observers will not experience significant issues with scattered Earth light in
their observations. Normally observations are scheduled only when the bright Earth limb is more than 20°
from the HST
pointing direction. This is sufficient to eliminate serious impacts from scattered Earth light—the most severe impact will be for observers with targets in the CVZ3
who may notice the sky background increased by a factor of 2 or 3.
It is possible to make arrangements for observations at smaller bright Earth limb
angles, and these images have a potential for serious impacts from scattered light. There are two types of impact: elevated background and non-uniformity in the background. For example, at a bright Earth avoidance angle of 14°
, it is possible for the sky level to be increased by a factor of 100 compared to normal pointings away from the Earth; this will of course have a serious impact on the background noise and detection of faint targets. Also, non-uniformity can arise since the scattered light is taking an increasingly non-standard path through the HST
optics, and hence the flat-fielding becomes corrupted. At this same angle of 14°
, it is possible to have both large scale gradients across the field of view (up to ~20% amplitude in the WFC) and small scale features in the background (up to ~12% in WFC and ~30% in the HRC). See ACS ISR 2003-05
for more details.
Each ACS filter is designed to maintain confocality with both the WFC and HRC
when paired with a clear aperture in the other filter wheel. To maintain this confocality when filters are paired with polarizers, the polarizers were fabricated with additional lensing power which alters the pixel scale and geometric distortion of each camera. The additional distortion is further complicated by localized optical defects (bubbles and wrinkles) in the polaroid materials (See ACS ISR 2004-09
Polynomial solutions of the geometric distortion for each filter are used by the AstroDrizzle
stage of the ACS calibration pipeline to produce geometrically rectified and resampled WFC and HRC images for photometric and astrometric use. These rectified images are provided as FITS images with the drz.fits
Presently, distortion solutions have not been derived for HRC images obtained with
the UV or visible polarizers. Such images constitute about 4% of the HRC datasets in the HST
archive. Consequently, the drz.fits
files produced by AstroDrizzle
for polarized HRC images have a pixel scale that differs by ~3% from the correct pixel scale obtained for non-polarized images. A correct distortion solution will be generated before the planned creation of a static HRC image Archive. Until then, users must exercise caution when performing astrometry or surface brightness measurements with polarized HRC images.