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تسجيل مستخدم جديدCosmic shear from STIS Pure Parallels: I Data
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Following the second HST servicing mission in 1997 when the STIS instrument was installed and the capability for parallel observations was enhanced, a substantial archive of non-proprietary parallel data has been accumulating. In this paper, we discuss the use of unfiltered STIS imaging data for a project that requires deep observations along as many independent lines-of-sight as possible. We have developed a technique to determine which datasets in the archive can safely be co-added together and have developed an iterative co-addition technique which enabled us to produce 498 high-quality, deep images. The principal motivation for this work is to measure the Cosmic Shear on small angular scales and a value derived from these data will be presented in a subsequent paper. A valuable by-product of this work is a set of high quality combined fields which can be used for other projects. The data are publicly available at http://www.stecf.org/projects/shear/
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The measurement of cosmic shear requires deep imaging with high image quality on many lines of sight to sample the statistics of large-scale structure. The expected distortion of galaxy images by cosmic shear on the STIS angular scale is a few percen
t, therefore the PSF anisotropy has to be understood and controlled to an accuracy better than 1%. In this poster we present the analysis of the PSF of STIS and a preliminary cosmic shear measurement using archival data from the STIS pure parallel program to show that the STIS camera on-board HST is well suited for our project. The data reduction and catalog production are described in an accompanying paper (astro-ph/0102330).
We report on the marginal detection of cosmic shear on sub-arcmin scales with archive data from the STIS camera on board HST. For the measurement 121 galaxy fields with a field of view of 51 x 51 are used to obtain an rms cosmic shear of ~ 4% with 1.
5sigma significance. This value is consistent with groundbased results obtained by other groups on larger scales, and with theoretical predictions for a standard LambdaCDM cosmology. To show the suitability of STIS for weak shear measurements we carefully investigated the stability of the PSF. We demonstrate that small temporal changes do not affect the cosmic shear measurement by more than ~ 10%. We also discuss the influence of various weighting and selection schemes for the galaxy ellipticities.
Following the detection of a cosmic shear signal at the 30 scale using archival parallel data from the STIS CCD camera onboard HST in Haemmerle et al. (2002), we analyzed a larger data set obtained from an HST GO pure parallel program. Although this
data set is considerably larger than the one analyzed previously, we do not obtain a significant detection of the cosmic shear signal. The potential causes of this null result are the multiple systematics that plague the STIS CCD data, and in particular the degradation of the CCD charge transfer efficiency after 4 years in space.
In June 1997, parallel observations using the Space Telescope Imaging Spectrograph (STIS) on the HST started to be taken in substantial numbers along many different lines-of-sight. We are using the imaging data to investigate the distortion of backgr
ound galaxies by the gravitational field of the large scale matter distribution, also known as Cosmic Shear. This poster presents the data and the catalog production that leads to the cosmic shear result presented in the poster First Cosmic Shear results from STIS parallel program archive data (Haemmerle et al., this conference). The data is publicly available also at http://www.stecf.org/projects/shear .
Since the Universe is inhomogeneous on scales well below the Hubble radius, light bundles from distant galaxies are deflected and distorted by the tidal gravitational field of the large-scale matter distribution as they propagate through the Universe
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