XMM-Newton observation of the Lockman Hole. 2. Spectral analysis - INSPIRE

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XMM-Newton observation of the Lockman Hole. 2. Spectral analysis

V. Mainieri
(
- Rome III U. and
- European Southern Observ. and
- Paris, Inst. Astrophys. and
- Garching, Max Planck Inst., MPE and
- Potsdam, Astrophys. Inst. and
- Caltech and
- Brera Observ.
)
,
J. Bergeron
(
- Rome III U. and
- European Southern Observ. and
- Paris, Inst. Astrophys. and
- Garching, Max Planck Inst., MPE and
- Potsdam, Astrophys. Inst. and
- Caltech and
- Brera Observ.
)
,
G. Hasinger
(
- Rome III U. and
- European Southern Observ. and
- Paris, Inst. Astrophys. and
- Garching, Max Planck Inst., MPE and
- Potsdam, Astrophys. Inst. and
- Caltech and
- Brera Observ.
)
,
I. Lehmann
(
- Rome III U. and
- European Southern Observ. and
- Paris, Inst. Astrophys. and
- Garching, Max Planck Inst., MPE and
- Potsdam, Astrophys. Inst. and
- Caltech and
- Brera Observ.
)
,
P. Rosati
(
- Rome III U. and
- European Southern Observ. and
- Paris, Inst. Astrophys. and
- Garching, Max Planck Inst., MPE and
- Potsdam, Astrophys. Inst. and
- Caltech and
- Brera Observ.
)

Jul, 2002

15 pages

Published in:

Astron.Astrophys. 393 (2002) 425-438

e-Print:

astro-ph/0207166 [astro-ph]

DOI:

10.1051/0004-6361:20020991

View in:

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Abstract: (arXiv)

We present the results of the X-ray spectral analysis of the first deep X-ray survey with the XMM-Newton observatory during Performance Verification. We restrict the analysis to the sample of 98 sources with more than 70 net counts (flux limit in the [0.5-7] keV band of 1.6 10^{-15} erg cm^{-2} s^{-1}) of which 61 have redshift identification. We find no correlation between the spectral index Gamma and the intrinsic absorption column density N_H and, for both the Type-1 and Type-2 AGN populations, we obtain ~2. The progressive hardening of the mean X-ray source spectrum with decreasing flux is essentially due to an increase in intrinsic absorption. The marked separation between the two AGN populations in several diagnostics diagrams, involving X-ray colour, X-ray flux, optical/near IR colour and optical brightness, is also a consequence of different absorption column densities and enables the classification of optically faint obscured AGN. About 27% of the subsample with R-K' colour are EROs (R-K>5) and most of these 18 X-ray selected EROs contain anobscured AGN as revealed by their high X-ray-to-optical/near IR flux ratios. There are six sources in our sample with L_X[0.5-10]>10^44 erg s^{-1} and log(N_H)>10^22 cm^{-2}: which are likely Type-2 QSOs and we thus derive a density of ~69 objects of this class per square degree.

GALAXY SURVEYS
AGN
QUASARS
DIFFUSE RADIATION
X-RAY GALAXIES

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