Phase Retrieval toMonitor HST Focus: I. WFC3 UVIS Software Implementation

Details Phase Retrieval toMonitor HST Focus: I. WFC3 UVIS Software Implementation Phase Retrieval toMonitor HST Focus: I. WFC3 UVIS Software Implementation

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010tel..rept....1n&link_type=abstract

Instrument Science Report TEL 2010-01, 19 pages

Physics

Optics

Hubble Space Telescope, Hst, Space Telescope Science Institute, Acs, Wfc3, Advanced Camera For Surveys, Wide Field Camera 3

Scientific paper

A monthly focus monitoring of the Hubble Space Telescope (HST) is performed via the Phase Retrieval technique. This has recently relied on Advanced Camera for Surveys (ACS) Wide Field Camera (WFC) data. Due to the installation of Wide Field Camera 3 (WFC3) on board the HST as a part of Servicing Mission 4, a new camera suitable for the monthly focus monitoring has become available. This document briefly describes the Phase Retrieval technique used for the focus monitoring, and outlines the implementation of the WFC3 UVIS channel into the existing software package called FITPSF. This implementation required not only major code changes, but also accurate geometric distortion solutions, charge diffusion kernels, and the properties of the camera optics to be included. Testing of the new software is also described. This showed that unlike ACS, the WFC3 UVIS channel shows a field dependent 3rd order spherical Zernike polynomial. Even so, WFC3 UVIS channel data are well-suited for the focus monitoring and result in a smaller scatter between focus values of different stars than ACS data. This is likely due to a better point spread function (PSF) sampling in the WFC3 UVIS channel, but also due to the relatively large charge transfer inefficiency present in ACS. 1

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