Resolving the X-ray background

M. A. Worsley, A. C. Fabian, D. M. Alexander, F. E. Bauer, W. N. Brandt, G. Hasinger, B. D. Lehmer

Research output: Chapter in Book/Report/Conference proceedingConference contribution

2 Citations (Scopus)

Abstract

We have stacked the X-ray emission from X-ray-detected sources in ∼ 3.8 Ms of Chandra Deep Field and XMM-Newton Lockman Hole observations. The fraction of the X-ray background which can be resolved into point sources is ∼ 70-90% up to 4 keV. In the 6-8 keV band this fraction decreases to ∼ 50-70% and XMM-Newton indicates only ∼ 40-60% in the 8-12 keV range. The unresolved fraction is consistent with an undiscovered population of highly obscured AGN. To attempt to uncover this population we proceeded to stack the X-ray emission from the X-ray-undetected optical sources in the Chandra Deep Fields, using Hubble source positions from the Great Observatories Origins Deep Survey. In the 0.5-6 keV range the stacked-source emission corresponds to the remaining 10-20% of the X-ray background. In the 6-8 keV band we find upper limits to the stacked X-ray flux consistent with the remaining ∼ 40% of the background, but the errors are too large to claim a detection of the obscured AGN population.

Original languageEnglish (US)
Title of host publicationAstrophysical Sources of High Energy Particles and Radiation
Pages51-56
Number of pages6
DOIs
StatePublished - Nov 22 2005
EventAstrophysical Sources of High Energy Particles and Radiation - Torun, Poland
Duration: Jun 20 2005Jun 24 2005

Publication series

NameAIP Conference Proceedings
Volume801
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616

Other

OtherAstrophysical Sources of High Energy Particles and Radiation
CountryPoland
CityTorun
Period6/20/056/24/05

Fingerprint

x rays
XMM-Newton telescope
newton
point sources
observatories

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy(all)

Cite this

Worsley, M. A., Fabian, A. C., Alexander, D. M., Bauer, F. E., Brandt, W. N., Hasinger, G., & Lehmer, B. D. (2005). Resolving the X-ray background. In Astrophysical Sources of High Energy Particles and Radiation (pp. 51-56). (AIP Conference Proceedings; Vol. 801). https://doi.org/10.1063/1.2141832
Worsley, M. A. ; Fabian, A. C. ; Alexander, D. M. ; Bauer, F. E. ; Brandt, W. N. ; Hasinger, G. ; Lehmer, B. D. / Resolving the X-ray background. Astrophysical Sources of High Energy Particles and Radiation. 2005. pp. 51-56 (AIP Conference Proceedings).
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Worsley, MA, Fabian, AC, Alexander, DM, Bauer, FE, Brandt, WN, Hasinger, G & Lehmer, BD 2005, Resolving the X-ray background. in Astrophysical Sources of High Energy Particles and Radiation. AIP Conference Proceedings, vol. 801, pp. 51-56, Astrophysical Sources of High Energy Particles and Radiation, Torun, Poland, 6/20/05. https://doi.org/10.1063/1.2141832

Resolving the X-ray background. / Worsley, M. A.; Fabian, A. C.; Alexander, D. M.; Bauer, F. E.; Brandt, W. N.; Hasinger, G.; Lehmer, B. D.

Astrophysical Sources of High Energy Particles and Radiation. 2005. p. 51-56 (AIP Conference Proceedings; Vol. 801).

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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N2 - We have stacked the X-ray emission from X-ray-detected sources in ∼ 3.8 Ms of Chandra Deep Field and XMM-Newton Lockman Hole observations. The fraction of the X-ray background which can be resolved into point sources is ∼ 70-90% up to 4 keV. In the 6-8 keV band this fraction decreases to ∼ 50-70% and XMM-Newton indicates only ∼ 40-60% in the 8-12 keV range. The unresolved fraction is consistent with an undiscovered population of highly obscured AGN. To attempt to uncover this population we proceeded to stack the X-ray emission from the X-ray-undetected optical sources in the Chandra Deep Fields, using Hubble source positions from the Great Observatories Origins Deep Survey. In the 0.5-6 keV range the stacked-source emission corresponds to the remaining 10-20% of the X-ray background. In the 6-8 keV band we find upper limits to the stacked X-ray flux consistent with the remaining ∼ 40% of the background, but the errors are too large to claim a detection of the obscured AGN population.

AB - We have stacked the X-ray emission from X-ray-detected sources in ∼ 3.8 Ms of Chandra Deep Field and XMM-Newton Lockman Hole observations. The fraction of the X-ray background which can be resolved into point sources is ∼ 70-90% up to 4 keV. In the 6-8 keV band this fraction decreases to ∼ 50-70% and XMM-Newton indicates only ∼ 40-60% in the 8-12 keV range. The unresolved fraction is consistent with an undiscovered population of highly obscured AGN. To attempt to uncover this population we proceeded to stack the X-ray emission from the X-ray-undetected optical sources in the Chandra Deep Fields, using Hubble source positions from the Great Observatories Origins Deep Survey. In the 0.5-6 keV range the stacked-source emission corresponds to the remaining 10-20% of the X-ray background. In the 6-8 keV band we find upper limits to the stacked X-ray flux consistent with the remaining ∼ 40% of the background, but the errors are too large to claim a detection of the obscured AGN population.

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Worsley MA, Fabian AC, Alexander DM, Bauer FE, Brandt WN, Hasinger G et al. Resolving the X-ray background. In Astrophysical Sources of High Energy Particles and Radiation. 2005. p. 51-56. (AIP Conference Proceedings). https://doi.org/10.1063/1.2141832