Unveiling Obscured Accretion in the Chandra Deep Field-South
Unveiling Obscured Accretion in the Chandra Deep Field-South
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DOI：
10.1086/523348
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发表时间：
2007-05
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影响因子：
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通讯作者：
F. Fiore;A. Grazian;P. Santini;P. Santini;S. Puccetti;M. Brusa;C. Feruglio;A. Fontana;E. Giall
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作者：
F. Fiore;A. Grazian;P. Santini;P. Santini;S. Puccetti;M. Brusa;C. Feruglio;A. Fontana;E. Giall
我们利用 Chandra Deep Field-South 的深层 HST、VLT、Spitzer 和 Chandra 数据来限制该区域康普顿厚活动星系核的数量。我们表明，具有高 24 μm 光通量比和红色的光源形成了独特的光源群，并且它们的红外光度主要由活动星系核发射主导。对这些极端源的 X 射线特性的分析表明，它们中的大多数（80% ± 15%）确实很可能是高度模糊的、康普顿厚的活动星系核。红外选择的康普顿厚 AGN 的数量，其光度高于 1044.2 ergs s−1 的 5.8 μm，与红移箱 1.2-2.6 中光度高于 1043 ergs s−1 的 X 射线选择的、未遮蔽的和中度遮蔽的 AGN 的数量相似，其光度为 2-10 keV。这种“2 倍”源群体正是解决模型预测和 X 射线活动星系核选择之间的差异所需要的。
We make use of deep HST, VLT, Spitzer, and Chandra data on the Chandra Deep Field-South to constrain the number of Compton-thick AGNs in this field. We show that sources with high 24 μm-to-optical flux ratios and red colors form a distinct source population, and that their infrared luminosity is dominated by AGN emission. Analysis of the X-ray properties of these extreme sources shows that most of them (80% ± 15%) are indeed likely to be highly obscured, Compton-thick AGNs. The number of infrared-selected, Compton-thick AGNs with 5.8 μm luminosity higher than 1044.2 ergs s−1 turns out to be similar to that of X-ray-selected, unobscured, and moderately obscured AGNs with 2-10 keV luminosity higher than 1043 ergs s−1 in the redshift bin 1.2-2.6. This “factor of 2” source population is exactly what is needed to solve the discrepancies between model predictions and X-ray AGN selection.