Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21531104l&link_type=abstract
American Astronomical Society, AAS Meeting #215, #311.04; Bulletin of the American Astronomical Society, Vol. 42, p.311
Astronomy and Astrophysics
Astronomy
Scientific paper
The 2 Ms Chandra Deep Field-South (CDF-S) and Chandra Deep Field-North (CDF-N) surveys are the two deepest X-ray surveys ever performed, which cover solid angles of 436 and 448 arcmin2, respectively. (1) We presented X-ray point-source catalogs for the 2 Ms CDF-S which include a total number of 578 sources. Basic source properties along with the cumulative number counts were provided. Most of the sources are AGNs. The CDF-S reaches on-axis sensitivity limits of 1.9*10-17 and 1.3*10-16 erg/cm2/s for the 0.5-2.0 and 2-8 keV bands, respectively. (2) With the numerous deep optical-to-radio surveys in the CDF-S region, we were able to identify 96% of the X-ray source in the main CDF-S catalog using the likelihood-ratio technique. We collected unprecedented multiwavelength photometric data for these sources and derived reliable photometric redshifts. We achieved an accuracy of δz/(1+zspec)=0.06, and an outlier fraction of 9%. (3) We performed a systematic survey of 24668 optical galaxies in the CDF-S and CDF-N to search for X-ray outbursts. The survey spans 1828 days for the CDF-S and 798 days for the CDF-N. No outbursts were found, and thus we set upper limits on the rate of such events in the Universe, which is about 10-4 /galaxy/yr, depending upon basic assumptions about the outburst properties. (4) We reported the discovery of the most-distant double-peaked emitter, CXOECDFS J033115.0-275518, at z=1.369 in the Extended CDF-S region. It is one of a handful of double-peaked emitters known to be a luminous quasar, with excellent multiwavelength coverage and a high-quality X-ray spectrum. The local viscous energy released from the line-emitting region of the accretion disk is probably insufficient to power the observed line flux, and external illumination of the disk appears to be required. The illumination cannot arise from a radiatively inefficient accretion flow as suggested for prototype double-peaked emitters.
Brandt Niel
Luo Bin
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