Resolving the X-ray background

被引：0

作者：

Worsley, MA ^{[1
]}

Fabian, AC ^{[1
]}

Alexander, DM ^{[1
]}

Bauert, FE ^{[1
]}

Brandt, WN ^{[1
]}

Hasinger, G ^{[1
]}

Lehmer, BD ^{[1
]}

机构：

[1] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

来源：

ASTROPHYSICAL SOURCES OF HIGH ENERGY PARTICLES AND RADIATION | 2005年 / 801卷

关键词：

X-ray observations; active galactic nuclei; starburst galaxies; X-ray background; DEEP FIELD-SOUTH; CHANDRA; SPECTRUM; GALAXIES; ORIGIN;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have stacked the X-ray emission from X-ray-detected sources in similar to 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 similar to 70-90% up to 4 keV. In the 6-8 keV band this fraction decreases to similar to 50-70% and XMM-Newton indicates only similar to 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 similar to 40% of the background, but the errors are too large to claim a detection of the obscured AGN population.

引用

页码：51 / 56

页数：6