Other
Scientific paper
Jul 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010hstc.worke..21s&link_type=abstract
"2010 Space Telescope Science Institute Calibration Workshop - Hubble after SM4. Preparing JWST, held 21-23 July 2010 at Space T
Other
Scientific paper
Flat fielding is a standard calibration step for astronomical data, which allows us to correct for variations in the local response of a detector and improve the accuracy of photometric analysis. As for other Hubble Space Telescope (HST) instruments, ground based flat-fields are, and will be, the base to remove the pixel-to-pixel variations in the Wide Field Camera 3 (WFC3) data. Tests performed during the Servicing Mission Observatory Verification (SMOV4), that followed the installation of WFC3 on Hubble, indicate that ground based flat-fields do not completely remove local variation in the response of the detector, but that low-frequency structures are still present in both the UVIS and IR data. As part of the WFC3 standard calibration process we have used observations of the rich globular cluster Omega Centauri to compare the flux of the same stars at different positions on the WFC3 detectors and derive a correction to remove the remaining low-frequency structures. Here we will present the characteristics of the ground-based high frequency flat (better known as P-flat) and the low-frequency (or L-flat) flat fields, how these files are created and their impact on the processed astronomical data.
Kalirai Jason S.
Mack Jennifer
Pirzkal Nor
Sabbi Elena
Viana Alex
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