In early 2001, flat-field images for the ACS were produced in the laboratory (see ACS ISR 2001-11
) using the Refractive Aberrated Simulator/Hubble Opto-Mechanical Simulator (RAS/HOMS). The RAS/HOMS is a HST
simulator capable of delivering OTA-like external monochromatic point source and broad-band full field illumination above its refractive cutoff wavelength of ~3500 Å.
Because the RAS/HOMS optics are opaque below 3500 Å, flats for the UV filters F330W and F344N (see ACS ISR 2003-02
and ACS ISR 2005-12
) were created using in-flight observations of the bright Earth (see Section 4.4.4
).Unfortunately, red leaks in F220W and F250W are so large that the out-of-band light dominates, and the lab flats made with the deuterium lamp illumination are superior to the Earth flats for these two filters.
More information on the HRC and WFC ground flats may be obtained from ACS ISR 2001-11
for the standard filters, polarizers, and coronagraph, from ACS ISR 2002-01
for the ramp filters, and from ACS ISR 2002-04
for the prism and grism. The stability of P-flats is tested in each cycle. Please see ACS ISR 2007-01
for more information about the stability of P-flats after the cooldown to -81°C in 2006. Observations made during SMOV SM4 show that WFC P-flats are stable.
Flat fields for the full set of SBC filters were also taken in the laboratory (ACS ISR 1999-02
), but were later replaced with in-flight observations using the internal deuterium lamp (ACS ISR 2005-04
). With total integration time of 20.5 hours through the F125LP filter, a flat field with a total signal of 12,000 counts per pixel was produced. Analysis of original laboratory flats indicates that the P-flat response is independent of wavelength, so the F125LP lamp flat was used for all filters. The internal lamp illumination does not simulate the OTA optics and, therefore, is useful only for correcting the pixel-to-pixel detector response. In order to accurately model the low-frequency variations in sensitivity, which may depend on wavelength, dithered star field observations were required. (See Section 4.4.2
for a discussion of the SBC L-flats.)
L-flats were determined from in-flight observations using filters F435W, F555W, F606W, F775W, F814W, and F850LP for both the WFC and HRC. The HRC study included two additional filters: F475W and F625W. The L-flat correction for the remaining filters was derived by using linear interpolation as a function of wavelength. The pivot wavelength of each filter was used for the interpolation, where the resulting L-flat is equal to the weighted average of the L-flat for the two filters nearest in wavelength. Due to red leaks in the F220W and F250W HRC filters, no L-flat correction has been applied, and errors in the flats of % to %, corner-to-corner, are expected for these filters. For a detailed discussion of ACS L-flat corrections, refer to ACS ISR 2002-08
. For a discussion of the mathematical algorithm used to derive the L-flats, refer to ACS ISR 2003-10
As was done for the CCDs, the SBC L-flats were derived using dithered star field observations. Instead of 47 Tucanae, however, the UV-bright globular cluster NGC 6681, which is rich in blue horizontal branch stars, was selected. This work is summarized in ACS ISR 2005-13
. The required corrections to the in-flight lamp flats are given in Figure 4.15
and range from
%, depending on wavelength. Since insufficient observations with the F122M filter exist, this L-flat is simply a copy of the F115LP filter correction. Six new flat fields have been delivered for use in the calibration pipeline, and the resulting photometric accuracy is now
% for F115LP, F122M, and F140LP, and
% for F150LP and F165LP.
WFC Low Frequency (L-flat) Flat-Field Corrections Required for the Laboratory Data.
shows the corrected WFC laboratory flats for several broad-band filters. Note that on the sky, a gap of ~50 pixels exists between the top and bottom halves that is not shown here. The central donut-like structure is due to variations in chip thickness (see ACS ISR 2003-06
) and is dependent on wavelength. Pixels in the central region, for example, are less sensitive than surrounding pixels in the blue F435W filter, and more sensitive in the red F850LP filter.
For the HRC, corrected laboratory flats for the same broad-band filters are shown in Figure 4.17
. The donut-like structure seen in the WFC response is not found in the HRC flats. The small dark rings are shadows of dust on the CCD window (see Section 4.5.1
). The large dust mote seen in the WFC F606W flat is due to dust on the F606W filter. That portion of the filter is not “seen” by the HRC detector.
Accuracy of pipeline flats can be verified using a variety of complementary methods. Section 4.4.2
explained how follow-up observations of the same stellar field can be used to verify the derived L-flat corrections. Alternately, observations of the bright Earth can provide a uniform flat-field source for the complete OTA optical complement and incorporate both the low frequency L-flat and the high frequency pixel-to-pixel P-flat response. Earth flats are described in Section 4.4.4
. For most filters, the flats agree to within ~1%, except for the interpolated L-flat filters which usually agree to within ~2%.
The third method for verifying the ACS pipeline flats is with sky flats. These can be made by filtering and summing many observations of a sparse field. Sky flats have been created for a few of the most frequently used broad-band WFC filters and are discussed in detail in Section 4.4.5
. The sky flats are generally similar to corrected ground flats at the 1% level, in accordance with the results of the previous two methods. While the WFC can show residuals in the central donut-region which are as large as 2%, these are most likely due to differences in the color of the spectrum of the sky from that of the bright globular cluster stars used for the L-flat determination.
Because the RAS/HOMS optics are opaque below 3500 Å (see Section 4.4.1
), flat fields for the HRC UV filters were created using in-flight observations of the bright Earth. The Earth is a poor flat-field source at optical wavelengths because structure in the cloud cover can cause streaking in the flat. However, HRC modes that utilized the F220W, F250W, F330W, and F344N were immune to streaks because of the large optical depth down to the tropospheric cloud layers. The bright Earth then provided a uniform flat-field source for the complete OTA+HRC optical complement.
The required calibration flats, which incorporates both the low frequency L-flat and the high frequency pixel-to-pixel P-flat response, can be easily produced from these observations. Unfortunately, the red leaks in F220W and F250W are so large that the out-of-band light dominated, and the lab flats made with the deuterium lamp illumination (see ACS ISR 2001-11
for details) are superior to the observed Earth flats for the modes that included these two filters. Because no L-flat correction has been applied, errors in the flats of
%, corner-to-corner, are expected for these filters. HRC F330W and F344N pipeline flats, on the other hand, are defined entirely by Earth flat data (see ACS ISR 2003-02
and ACS ISR 2005-12
). With ~20 - 30 observations, each over the course of 3 years, these flats have very high signal-to-noise and showed repeatability to much better than the required 1% accuracy.
Several hundred observations of the bright Earth were obtained using the full set of HRC standard filters (ACS ISR 2005-12
). In general, the pipeline flat fields are confirmed to a precision of ~1%, validating the stellar L-flat corrections. The “interpolated” L-flats are not significantly worse than the L-flats derived from the Earth observations (see Section 4.4.2
). One exception is the F550M filter which shows a total deviation of more than 2%. Other exceptions are the four longest wavelength HRC filters which show large systematic differences with the pipeline flats. These differences appear to be caused by stray light originating from the detector surface, where most of the long wavelength photons were reflected and then scattered back from nearby focal plane structures. Any filter transmitting at these long wavelengths would have seen the extra pattern from this light, though the strength of the additional stray light is proportional to the total flux of the source. Thus, for large diffuse objects that fully illuminated the detector, these Earth flats are more appropriate for calibration than the existing pipeline flats, which are appropriate for point sources.
The sky flats were created by median-combining the pipeline-reduced flt.fits
files after removing cosmic rays and masking all of the sources. Because the GOODS data contained 2 - 4 dithers at each pointing, masking was necessary to eliminate the high values at each pixel. In addition, before combining, each image was corrected for the pedestal bias signature and inspected for scattered light.
Because sky flats are created from the pipeline calibrated flt.fits
files, any flat-field signatures that are not in the pipeline flats should appear in the ratio. The combined sky flat in each filter was box-medianed for comparison to the corrected ground flat. The resulting ratios of pipeline to sky flats show variations across the field of view of < 2% for each of the three filters. The sky flats independently created from the two separate GOODS fields, showed excellent agreement (< 1%) for all three filters.