The unresolved hard X-ray background: The missing source population implied by the Chandra and XMM-Newton deep fields

M. A. Worsley; A. C. Fabian; F. E. Bauer; D. M. Alexander; G. Hasinger; S. Mateos; H. Brunner; W. N. Brandt; D. P. Schneider

doi:10.1111/j.1365-2966.2005.08731.x

The unresolved hard X-ray background: The missing source population implied by the Chandra and XMM-Newton deep fields

M. A. Worsley, A. C. Fabian, F. E. Bauer, D. M. Alexander, G. Hasinger, S. Mateos, H. Brunner, W. N. Brandt, D. P. Schneider

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Abstract

We extend our earlier work on X-ray source stacking in the deep XMM-Newton observation of the Lockman Hole, to the 2-Ms Chandra Deep Field North (CDF-N) and the 1-Ms Chandra Deep Field South (CDF-S). The XMM-Newton work showed the resolved fraction of the X-ray background (XRB) to be ∼80-100 per cent at ≲ 2 keV but this decreased to only ∼50 per cent above ∼8 keV. The CDF-N and CDF-S probe deeper, and are able to fill in some of the missing fraction in the 4-6 keV range, but the resolved fraction in the 6-8 keV band remains only ∼60 per cent, confirming the trend seen with XMM-Newton. The missing XRB component has a spectral shape that is consistent with a population of highly obscured active galactic nuclei (AGN) at redshifts ∼0.5-1.5 and with absorption column densities of ∼10²³-10²⁴ cm-².

Original language	English (US)
Pages (from-to)	1281-1287
Number of pages	7
Journal	Monthly Notices of the Royal Astronomical Society
Volume	357
Issue number	4
DOIs	https://doi.org/10.1111/j.1365-2966.2005.08731.x
State	Published - Mar 11 2005

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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Worsley, M. A., Fabian, A. C., Bauer, F. E., Alexander, D. M., Hasinger, G., Mateos, S., Brunner, H., Brandt, W. N., & Schneider, D. P. (2005). The unresolved hard X-ray background: The missing source population implied by the Chandra and XMM-Newton deep fields. Monthly Notices of the Royal Astronomical Society, 357(4), 1281-1287. https://doi.org/10.1111/j.1365-2966.2005.08731.x

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abstract = "We extend our earlier work on X-ray source stacking in the deep XMM-Newton observation of the Lockman Hole, to the 2-Ms Chandra Deep Field North (CDF-N) and the 1-Ms Chandra Deep Field South (CDF-S). The XMM-Newton work showed the resolved fraction of the X-ray background (XRB) to be ∼80-100 per cent at ≲ 2 keV but this decreased to only ∼50 per cent above ∼8 keV. The CDF-N and CDF-S probe deeper, and are able to fill in some of the missing fraction in the 4-6 keV range, but the resolved fraction in the 6-8 keV band remains only ∼60 per cent, confirming the trend seen with XMM-Newton. The missing XRB component has a spectral shape that is consistent with a population of highly obscured active galactic nuclei (AGN) at redshifts ∼0.5-1.5 and with absorption column densities of ∼1023-1024 cm-2.",

author = "Worsley, {M. A.} and Fabian, {A. C.} and Bauer, {F. E.} and Alexander, {D. M.} and G. Hasinger and S. Mateos and H. Brunner and Brandt, {W. N.} and Schneider, {D. P.}",

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Worsley, MA, Fabian, AC, Bauer, FE, Alexander, DM, Hasinger, G, Mateos, S, Brunner, H, Brandt, WN & Schneider, DP 2005, 'The unresolved hard X-ray background: The missing source population implied by the Chandra and XMM-Newton deep fields', Monthly Notices of the Royal Astronomical Society, vol. 357, no. 4, pp. 1281-1287. https://doi.org/10.1111/j.1365-2966.2005.08731.x

TY - JOUR

T1 - The unresolved hard X-ray background

T2 - The missing source population implied by the Chandra and XMM-Newton deep fields

AU - Worsley, M. A.

AU - Fabian, A. C.

AU - Bauer, F. E.

AU - Alexander, D. M.

AU - Hasinger, G.

AU - Mateos, S.

AU - Brunner, H.

AU - Brandt, W. N.

AU - Schneider, D. P.

PY - 2005/3/11

Y1 - 2005/3/11

N2 - We extend our earlier work on X-ray source stacking in the deep XMM-Newton observation of the Lockman Hole, to the 2-Ms Chandra Deep Field North (CDF-N) and the 1-Ms Chandra Deep Field South (CDF-S). The XMM-Newton work showed the resolved fraction of the X-ray background (XRB) to be ∼80-100 per cent at ≲ 2 keV but this decreased to only ∼50 per cent above ∼8 keV. The CDF-N and CDF-S probe deeper, and are able to fill in some of the missing fraction in the 4-6 keV range, but the resolved fraction in the 6-8 keV band remains only ∼60 per cent, confirming the trend seen with XMM-Newton. The missing XRB component has a spectral shape that is consistent with a population of highly obscured active galactic nuclei (AGN) at redshifts ∼0.5-1.5 and with absorption column densities of ∼1023-1024 cm-2.

AB - We extend our earlier work on X-ray source stacking in the deep XMM-Newton observation of the Lockman Hole, to the 2-Ms Chandra Deep Field North (CDF-N) and the 1-Ms Chandra Deep Field South (CDF-S). The XMM-Newton work showed the resolved fraction of the X-ray background (XRB) to be ∼80-100 per cent at ≲ 2 keV but this decreased to only ∼50 per cent above ∼8 keV. The CDF-N and CDF-S probe deeper, and are able to fill in some of the missing fraction in the 4-6 keV range, but the resolved fraction in the 6-8 keV band remains only ∼60 per cent, confirming the trend seen with XMM-Newton. The missing XRB component has a spectral shape that is consistent with a population of highly obscured active galactic nuclei (AGN) at redshifts ∼0.5-1.5 and with absorption column densities of ∼1023-1024 cm-2.

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The unresolved hard X-ray background: The missing source population implied by the Chandra and XMM-Newton deep fields

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