WFC3: On-Orbit Measurement of the Point Spread Function on the WFC3 Detectors

Details WFC3: On-Orbit Measurement of the Point Spread Function on the WFC3 Detectors WFC3: On-Orbit Measurement of the Point Spread Function on the WFC3 Detectors

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010hstc.worke..66d&link_type=abstract

"2010 Space Telescope Science Institute Calibration Workshop - Hubble after SM4. Preparing JWST, held 21-23 July 2010 at Space T

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Knowledge of the point spread function (PSF) on a detector is important for scientific applications such as photometric measurements and analysis of blended sources. It is also important for ensuring that good optical alignment of the instrument is achieved and maintained. The quality of the PSF on HST instruments varies over the detector and varies with time. The focus changes throughout an orbit as the optical bench "breathes", and the average focus changes slowly over time. Locally, the detected PSF is affected by pixelation and charge diffusion or interpixel sensitivity variation. The PSF is also dependent on wavelength. All of these factors both complicate PSF analysis and make it more challenging to provide useful PSFs to observers. Here we review the on-going measurement and analysis of the PSF on the WFC3 detectors.

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