2006
DOI: 10.1051/0004-6361:20065004
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Ground-based CCD astrometry with wide field imagers

Abstract: This paper is the first of a series of papers in which we will apply the methods we have developed for high-precision astrometry (and photometry) with the Hubble Space Telescope (HS T ) to the case of wide-field ground-based images. In particular, we adapt the software originally developed for WFPC2 to ground-based, wide field images from the WFI at the ESO 2.2 m telescope. In this paper, we describe in details the new software, we characterize the WFI geometric distortion, discuss the adopted local transforma… Show more

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Cited by 158 publications
(159 citation statements)
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“…4. In all, our method follows a different approach than that described in Anderson et al (2006) and references therein for the astrometry of WFI mosaics.…”
Section: Discussionmentioning
confidence: 99%
“…4. In all, our method follows a different approach than that described in Anderson et al (2006) and references therein for the astrometry of WFI mosaics.…”
Section: Discussionmentioning
confidence: 99%
“…The Hercules r Sloan -band datasets define a time baseline of 4.94 years and cover a common area of 0.30 deg 2 . To measure the stellar displacements between the two epochs, we followed the prescriptions given in Anderson et al (2006). To do this, it is mandatory to select a set of reference objects against which to compute relative PMs.…”
Section: Proper Motionsmentioning
confidence: 99%
“…In the multislit and multifiber spectroscopic facilities, an accuracy of 0.2 arcsec or better is essential to position point-like sources in the slits/fibers. The mosaic-like CCD camera as wide field imager (WFI) mounted on the 2.2 m ESO telescope allows astrometric measurements with an accuracy far better than the nominal 0.2 arcsec (Anderson et al 2006). A particularly useful application of astrometry, however, is to determine proper motions for a large number of stars.…”
Section: Introductionmentioning
confidence: 99%
“…Therefore, a catalogue with membership information covering a wide field centered on the cluster is very much needed. The archival data taken with the WFI at the 2.2 m ESO telescope enable us to derive proper motions by using an epoch gap of only a few years, deeper by several magnitudes, and covering a larger region (Anderson et al 2006;Yadav et al 2008Yadav et al , 2013Bellini et al 2009;Sariya et al 2012). We selected the WFI at the 2.2 m ESO telescope because it is one of the first wide-field cameras available, thus it has a long time baseline in its public archive.…”
Section: Introductionmentioning
confidence: 99%