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Centro de Astrofísica da Universidade do Porto

Chandra Counterparts of CANDELS GOODS-S Sources

N. Cappelluti, A. Comastri, A. Fontana, G. Zamorani, R. Amorin, M. Castellani, E. Merlin, P. Santini, D. Elbaz, C. Schreiber, X. W. Shu, T. Wang, J. S. Dunlop, N. Bourne, V. A. Bruce, F. Buitrago, M. J. Michałowski, S. Derriere, A. Ferguson, S. M. Faber, F. Vito

Improving the capabilities of detecting faint X-ray sources is fundamental for increasing the statistics on faint high-z active galactic nuclei (AGNs) and star-forming galaxies (SFGs). We performed a simultaneous maximum likelihood point-spread function fit in the [0.5-2] keV and [2-7] keV energy bands of the 4 Ms Chandra Deep Field South (CDFS) data at the position of the 34,930 CANDELS H-band selected galaxies. For each detected source we provide X-ray photometry and optical counterpart validation. We validated this technique by means of a ray-tracing simulation. We detected a total of 698 X-ray point sources with a likelihood { L }gt 4.98 (i.e., 〉2.7σ). We show that prior knowledge of a deep sample of optical-NIR galaxies leads to a significant increase in the detection of faint (i.e., ̃10-17 cgs in the [0.5-2] keV band) sources with respect to “blind” X-ray detections. By including previous X-ray catalogs, this work increases the total number of X-ray sources detected in the 4 Ms CDFS, CANDELS area to 793, which represents the largest sample of extremely faint X-ray sources assembled to date. Our results suggest that a large fraction of the optical counterparts of our X-ray sources determined by likelihood ratio actually coincides with the priors used for the source detection. Most of the new detected sources are likely SFGs or faint, absorbed AGNs. We identified a few sources with putative photometric redshift z 〉 4. Despite the low number statistics and the uncertainties on the photo z, this sample significantly increases the number of X-ray-selected candidate high-z AGNs.

galaxies: active, galaxies: high-redshift, quasars: supermassive black holes

The Astrophysical Journal
Volume 823
May 2016

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