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The Large-scale Structure in the Chandra Deep Field South

Published online by Cambridge University Press:  05 December 2011

Dario Trevese
Affiliation:
Sapienza Università di Roma, P.le Aldo Moro 5, 001865 Roma, Italy email: dario.trevese@roma1.infn.it
Fabrizio Fiore
Affiliation:
INAF-Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy
Enrico Piconcelli
Affiliation:
INAF-Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy
Marco Castellano
Affiliation:
INAF-Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy
Laura Pentericci
Affiliation:
INAF-Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy
Piero Ranalli
Affiliation:
Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
Andrea Comastri
Affiliation:
INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
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Abstract

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We have studied the large scale distribution of matter in the Chandra Deep Field South on the basis of photometric redshifts and we have identified several over-densities between redshift 0.6 and 2.3. We analyse two of these structures using the deepest X-ray observations ever obtained: 4 Ms with the Chandra satellite and 2.5 Ms with XMM-Newton. We set a very faint upper limit on the X-ray luminosity of a structure at redshift 1.6, and we find an extended X-ray emission from a structure at redshift 0.96 of which we can estimate the gas temperature and make a comparison with the scaling relations between the X-ray luminosity and mass or temperature of high redshift galaxy clusters.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

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