The VLT Survey Telescope ATLAS

(2) Institute of Astronomy; A. Kupcu Yoldas (2); B. Chehade (1); Durham University; E. Gonzalez-Solares (2); E.T.W. Sutorius (3); J.R. Findlay (1); J.R. Lewis (2); M.A. Read (3); M.J. Irwin (2)

The VLT Survey Telescope ATLAS

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arxiv 1502.05432 v1 pith:5P6KA3SM submitted 2015-02-18 astro-ph.GA astro-ph.CO

T. Shanks (1) , N. Metcalfe (1) , B. Chehade (1) , J.R. Findlay (1) , M.J. Irwin (2) , E. Gonzalez-Solares (2) , J.R. Lewis (2) , A. Kupcu Yoldas (2)

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R.G.Mann (3) M.A. Read (3) E.T.W. Sutorius (3) S. Voutsinas (3) ((1) Dept of Physics Durham University UK (2) Institute of Astronomy University of Cambridge UK (3) Institute for Astronomy University of Edinburgh UK)

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The VLT Survey Telescope (VST) ATLAS is an optical ugriz survey aiming to cover ~4700deg^2 of the Southern sky to similar depths as the Sloan Digital Sky Survey (SDSS). From reduced images and object catalogues provided by the Cambridge Astronomical Surveys Unit we first find that the median seeing ranges from 0.8 arcsec FWHM in i to 1.0 arcsec in u, significantly better than the 1.2-1.5 arcsec seeing for SDSS. The 5 sigma magnitude limit for stellar sources is r_AB=22.7 and in all bands these limits are at least as faint as SDSS. SDSS and ATLAS are more equivalent for galaxy photometry except in the z band where ATLAS has significantly higher throughput. We have improved the original ESO magnitude zeropoints by comparing m<16 star magnitudes with APASS in gri, also extrapolating into u and z, resulting in zeropoints accurate to ~+-0.02 mag. We finally compare star and galaxy number counts in a 250deg^2 area with SDSS and other count data and find good agreement. ATLAS data products can be retrieved from the ESO Science Archive, while support for survey science analyses is provided by the OmegaCAM Science Archive (OSA), operated by the Wide-Field Astronomy Unit in Edinburgh.

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