The Chandra COSMOS Survey: Source Detection and Photometry.

Details The Chandra COSMOS Survey: Source Detection and Photometry. The Chandra COSMOS Survey: Source Detection and Photometry.

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21347104p&link_type=abstract

American Astronomical Society, AAS Meeting #213, #471.04; Bulletin of the American Astronomical Society, Vol. 41, p.423

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We have developed a multi-stage source detection process to deal with the heavily overlapped tiling of the C-COSMOS isurvey. The resulting method combines the ability to separate close pairs of sources with accurate positions and photometry, and so may be useful in other applications.
In C-COSMOS every position on the sky was observed in typically 4 overlapping pointings, and so with a corresponding PSFs, in the central 0.5 sq.deg and in two overlapping pointings in most of the outer 0.4 sq.deg. area. To full yexploitthe C-COSMOS data requires a dedicated and accurate analysis focused on three main issues: (1) maximizing the sensitivity when the PSF changes so wildly among different observations of the same source (from few arcsec to 10 arcsec); (2) resolving close pairs; and (3) obtaining the best source localization and count rate accuracy.
We made detailed comparisons between different detection algorithms and photometry tools using extensive simulations. Our final method consists of a procedure that takes advantage of the good positional accuracy and ability to separate close groups of sources of PWDETECT, and the accurate photometry and well-defined detection probability of EMLDETECT.

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