2002/01/17 by A. Moretti, Davide Lazzati, D. Lazzati +2
Mathematics · Physics and Astronomy · #Adaptive optics and wavefront sensing #Algorithm #Artificial intelligence #Astrophysical Phenomena and Observations #Astrophysics #Chandra Deep Field South #Computer science #Field (mathematics) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Limiting #Mathematics #Physics #Redshift #Sky #Wavelet #astro-ph
paper · pdf · doi:10.1086/339727
27 pages 16 figures, accepted for publication in the Astrophysical Journal
arxiv created 2002/01/17 · openalex publication_date 2002/05/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Chandra Deep Fields represent the deepest look at the X-ray sky. We analyzed the Chandra Deep Field-South (CDF-S) with the aid of a dedicated wavelet-based algorithm. Here we present a detailed description of the procedures used to analyze this field, tested and verified by means of extensive simulations. We show that we can safely reconstruct the log N - log S source distribution of the CDF-S down to limiting fluxes of 2.4 × 10 -17 and 2.1 × 10 -16 ergs s -1 cm -2 in the soft (0.5-2 keV) and hard (2-10 keV) bands, respectively, fainter by a factor of ≳2 than current estimates. At these levels we can account for ≳90% of the 1-2 keV and 2-10 keV X-ray background.