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Space Telescope Science Institute |
ACS Data Handbook V7.2 |
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4.6.1 The IssueThe charge traps degrade the efficiency with which charge is transferred from pixel to pixel during the readout of the CCD array. This is seen directly, as shown in Figure 4.24, in the “charge trails” that follow hot pixels, cosmic rays, and bright stars that can extend to over 50 pixels in length.Figure 4.24: CTE TrailsObservations with very low background (<100 e− for ACS) will suffer large losses for very faint sources. This is likely to be problematic for narrow band filters and observations in the UV where the background is very low. In these cases, raising the background will greatly improve the CTE and thus the S/N of these sources. For users planning to stack multiple images to reach very faint limits, they should plan to achieve a background level of ~100 e- for ACS.The ACS team has developed and implemented a post-observation correction algorithm based upon the Anderson and Bedin (2010PASP..122.1035A) methodology. This empirical algorithm first develops a model to reproduce the observed trails, then inverts the model to convert observed pixel values in any image to an estimate of the original pixel values, undoing the effects of the degraded CTE.The original version of the code worked very well for intermediate to high flux levels (> 200 electrons). Improvements in the new version of the code have made corrections more effective at low flux levels (< 100 electrons), and employs more accurate time- and temperature-dependent corrections for CTE over ACS’s lifetime. Recent developments on this subject can be found in Bohlin, R. & Anderson, J. (ACS ISR 2011-01); Ubeda, L. & Anderson, J. (ACS ISR 2012-03); and Sokol, J. et al. (ACS ISR 2012-04).Figure 4.25: An Example of the Pixel-Based CCD Corrections(Left) A 1000 x 1000 pixel region at the top of the chip 1 extension in image jbmncoakq_flt.fits. CTE vertical trails are clearly visible. (Right) The reconstructed CTE-corrected flc.fits image after the execution of calacs.An alternate method for post-observation restoration involves a simple recalibration of the photometry using correction curves that have been provided in Chiaberge M. (ACS ISR 2012-05). This can be effective for isolated point sources on flat backgrounds, but is less effective for extended sources or sources in crowded regions. Please refer to Section 5.1.5 for more detailsThese empirical corrections, available as an online tool at the ACS Web site, are also useful for planning observations: they allow an estimate of the CTE losses for point-like sources that can be expected in a near-future observation for a given background and source flux. The expected losses should be taken into consideration for a decision on the best CTE mitigation strategy, and if necessary, to adjust integration times to meet signal to noise requirements.