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J/ApJS/172/29 XMM-Newton survey in COSMOS field. I. (Hasinger+, 2007)
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Beginning of ReadMe :J/ApJS/172/29 XMM-Newton survey in COSMOS field. I. (Hasinger+, 2007)
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The XMM-Newton wide-field survey in the COSMOS field. I. Survey description.
Hasinger G., Cappelluti N., Brunner H., Brusa M., Comastri A., Elvis M.,
Finoguenov A., Fiore F., Franceschini A., Gilli R., Griffiths R.E.,
Lehmann I., Mainieri V., Matt G., Matute I., Miyaji T., Molendi S.,
Paltani S., Sanders D.B., Scoville N., Tresse L., Urry C.M., Vettolani P.,
Zamorani G.
<Astrophys. J. Suppl. Ser., 172, 29-37 (2007)>
=2007ApJS..172...29H
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ADC_Keywords: Surveys ; X-ray sources
Keywords: cosmology: observations - large-scale structure of universe -
dark matter - galaxies: formation - galaxies: evolution -
X-rays: galaxies
Abstract:
We present the first set of XMM-Newton EPIC observations in the
2deg^2^ COSMOS field. The strength of the COSMOS project is the
unprecedented combination of a large solid angle and sensitivity over
the whole multi-wavelength spectrum. The XMM-Newton observations are
very efficient in localizing and identifying active galactic nuclei
(AGNs) and clusters, as well as groups of galaxies. One of the primary
goals of the XMM-Newton Cosmos survey is to study the coevolution of
active galactic nuclei as a function of their environment in the
cosmic web. Here we present the log of observations, images, and a
summary of first research highlights for the first pass of 25
XMM-Newton pointings across the field. In the existing data set we
have detected 1416 new X-ray sources in the 0.52, 24.5, and 4.5-10keV
bands to an equivalent 0.5-2keV flux limit of 7x10^-16^erg/cm^2^/s.
The number of sources is expected to grow to almost 2000 in the final
coverage of the survey. From an X-ray color-color analysis we identify
a population of heavily obscured, partially leaky or reflecting
absorbers, most of which are likely to be nearby, Compton-thick AGNs.
Description:
We have surveyed an area of 1.4x1.4deg^2^ within the region of sky
bounded by 09:57:30<RA(J2000.0)<10:03:30; 1:27:30<DE(J2000.0)<2:57:30.