Jul 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008hst..prop11904k&link_type=abstract
HST Proposal ID #11904. Cycle 17
Physics
Scientific paper
To characterize the effects of the contamination {i.e., droplets} on the UVIS window, we will observe a star cluster in three wide band filters {F225W, F555W, and F814W} as well as a narrow band filter {F502N} and step the stars in the cluster across randomly located droplets. The step size is 20 pixels, and we execute a five point line dither for each filter. This should provide for observations both on and off the droplets, for the same star. Internal flat fields are also obtained, but, due to the high f/# of the internal calibration system, the flats will be of limited utility, but will serve to map and crudely track any changes in the droplets. The cluster needs to contain both hot and cool stars, and therefore we select NGC 6752, a nearby globular with a hot horizontal branch. Note, although the total population of HB stars may be larger in systems such as NGC 2419, NGC 6715, and NGC 2808, those clusters are much further away and will not provide a high density of stars over the global image {the droplets are located over the entire frame}. There will be three visits {initial, 7 days later, and 30 days later}, with each visit requiring 4 orbits. The total program thus requires 12 orbits total.;
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