|Space Telescope Science Institute|
|WFC3 Data Handbook v. 3.0|
Because the WFC3 focal plane is tilted with respect to the incoming beam, the projected pixel area on the sky varies across the field of view in calibrated (_flt.fits) images. As a result, pixels in different regions of the detector collect a different amount of light simply due to the projected area. Observations of a constant surface brightness object would therefore have count rates per pixel that vary over the detector, even if every pixel had the same sensitivity.In order to produce images that appear uniform for uniform illumination, the WFC3 flat fields include the effect of the variable pixel area across the field. As a consequence of dividing by the flat field, two stars of equal brightness in an flt.fits image falling on different portions of the detector would not have the same total counts. To correct for this effect, the calibrated ‘flt.fits’ images may be multiplied by the effective pixel area map (see WFC3 ISR 2010-08). For the UVIS channel, this represents a 7% effect across a diagonal of the mosaicked image. For the IR channel, the area of the pixels varies by 8% from the bottom to the top of the image.Alternatively, this effect is accounted for in the pipeline by drizzling, where the geometric distortion solution is used to correct all pixels to equal area on the sky in ‘drz.fits’ data products. Because drizzling conserves flux, users should recover the same photometry from drz images and from flt images multiplied by the pixel area map.4.2.1 AstroDrizzle in the PipelineWFC3 data obtained from MAST are corrected for geometric distortion with AstroDrizzle, which replaced MultiDrizzle in the OPUS pipeline for WFC3 data on June 7, 2012. During pipeline processing, calibrated data that belong to an association are corrected for distortion and drizzle-combined with cosmic ray rejection. If the associated images are dithered, they are aligned using the WCS information in their headers before being combined. If there is no association table, each single-exposure WFC3 image is drizzled to correct for geometric distortion. Additionally, images in a visit with the same filter and pointing are associated and thus combined.AstroDrizzle uses the MDRIZTAB reference table to define the best parameter values to use based on the type of observations being processed. Each detector has its own MDRIZTAB, and each row provides the parameter settings specific to the filter and number of input images per association. AstroDrizzle relies on the Image Distortion Correction Table (IDCTAB) and the Detector to Image Distortion Correction (D2IMFILE, UVIS only) reference files for a description of the WFC3 distortion. Additional reference files to correct for filter-dependent residuals (NPOLFILE) are added once on-orbit measurements are made.
Users may obtain the latest IDCTAB, D2IMFILE, and MDRIZTAB reference files from the following page:
http://www.stsci.edu/hst/observatory/cdbs/SIfileInfo/WFC3/reftablequeryindexInformation about the geometric distortion is extracted from these reference files and stored as SIP header keywords and as FITS extensions in the *_flt.fits images. Please refer to Section 3.2.3 in the DrizzlePac Handbook for details.The steps performed by AstroDrizzle include the following:
• In general, pipeline drizzled products are recommended to be used as “quick-look” products. Reprocessing is highly recommended to achieve the most scientifically accurate data products. Four main areas for improvement may include: (1) image alignment, (2) sky subtraction, (3) cosmic ray rejection, and (4) final image resolution.4.2.2 Manual ReprocessingDrizzled images combined in the pipeline were produced using a default set of parameters that are suitable for the widest range of scientific applications. These defaults, however, may not produce the optimum science data quality for many programs, and those images will require post-pipeline processing. Additionally, MAST only creates drizzled products for images obtained in a single visit, so additional visits may only be drizzled together by reprocessing.While single visit data with small dithers (like the 4-point dither box) are usually aligned to better than 0.1 pixels, the drizzled products are created using the native detector plate scale, and with a drop size or PIXFRAC of 1.0. In these cases, the resolution of the drizzled products can be improved by fine-tuning the final sampling by experimenting with the scale and pixfrac parameters.Single visit data with larger dithers (for example, to create mosaics) may have residual shifts of a few tenths of a pixel or more and residual rotations of a few thousandths of a degree. When combining data from different visits, tweaks to the image alignment are usually necessary since different sets of guide star pairs may have been used. Offsets of the same target at different rolls are typically ~0.3 to 0.5 arcseconds. See Appendix B of the DrizzlePac Handbook for more information.Poor alignment can lead to improper cosmic-ray rejection, and when astronomical sources are flagged as cosmic rays, the photometric accuracy of the final data products may be compromised. Additionally, a poor estimate of the sky background, for example in images where a bright target fills the frame, may also affect the accuracy of cosmic ray rejection, and in turn,of the resulting photometry.4.2.3 AstroDrizzle DocumentationAstroDrizzle is available as part of the DrizzlePac software which contains all the tools for manually reprocessing (aligning and combining) calibrated HST data. This software may be obtained from the DrizzlePac webpage.This webpage also provides useful resources such as the DrizzlePac Handbook, which includes a set of worked examples for simple use cases, and some basic video tutorials.