WFC3 SMOV Proposal 11450: The Photometric Performance and Calibration of WFC3/UVIS

Details WFC3 SMOV Proposal 11450: The Photometric Performance and Calibration of WFC3/UVIS WFC3 SMOV Proposal 11450: The Photometric Performance and Calibration of WFC3/UVIS

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009wfc..rept...21k&link_type=abstract

Instrument Science Report WFC3 2009-31, 27 pages

Physics

Hubble Space Telescope, Hst, Space Telescope Science Institute, Wide Field Camera 3, Wfc3

Scientific paper

We present the photometric calibration of the UVIS camera on WFC3. Following successful instal- lation during Servicing Mission 4, we began a primary calibration program to measure the photo- metric zero points of 37 high priority filters on the UVIS1 CCD. Additional secondary observations obtained as a part of the UVIS Contamination Monitor Program with both UVIS1 and UVIS2 are also analyzed (CAL11426 - Baggett et al. 2009). All measurements are made from a set of high signal-to-noise imaging observations of the white dwarf standards GD 153 (primary program) and GRW+70d5824 (secondary program). We find that the total system throughput of both CCDs is significantly better than expected from the Thermal Vacuum 3 (TV3) testing campaign, with effi- ciency gains of ~10% at the blue and red ends of the spectral coverage, and ~20% near the central wavelength, 5500 Å. Repeat visits in a subset of filters separated by approximately 1 day, 1 week, and 1 month indicate photometric stability in the measured counts to better than 0.5%. We update the Exposure Time Calculator (ETC) with these preliminary results by fitting a smooth curve (2nd order polynomial) to the ratios of the efficiency gains over previous predictions, in the medium and wide band filters. This polynomial is interpolated at a fine wavelength grid and multiplied into the SYNPHOT throughput routines. We also provide photometric zero points for the UVIS camera in three photometric systems, STMAG, ABMAG, and VEGAMAG. A much more detailed Cycle 17 calibration plan, including observations targeting multiple primary standards, and with all filters on both CCDs, begins in October 2009.

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