THE XMM-NEWTON WIDE FIELD SURVEY IN THE COSMOS FIELD: REDSHIFT EVOLUTION OF AGN BIAS AND SUBDOMINANT ROLE OF MERGERS IN TRIGGERING MODERATE-LUMINOSITY AGNs AT REDSHIFTS UP TO 2.2
THE XMM-NEWTON WIDE FIELD SURVEY IN THE COSMOS FIELD: REDSHIFT EVOLUTION OF AGN BIAS AND SUBDOMINANT ROLE OF MERGERS IN TRIGGERING MODERATE-LUMINOSITY AGNs AT REDSHIFTS UP TO 2.2
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DOI：
10.1088/0004-637x/736/2/99
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发表时间：
2011-05
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通讯作者：
V. Allevato;A. Finoguenov;N. Cappelluti;N. Cappelluti;T. Miyaji;T. Miyaji;G. Hasinger;M. Salvato;M. Brusa;R. Gilli;G. Zamorani;F. Shankar;J. B. James;J. B. James;H. McCracken;A. Bongiorno;A. Merloni;J. Peacock;J. Silverman;A. Comastri
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作者：
V. Allevato;A. Finoguenov;N. Cappelluti;N. Cappelluti;T. Miyaji;T. Miyaji;G. Hasinger;M. Salvato;M. Brusa;R. Gilli;G. Zamorani;F. Shankar;J. B. James;J. B. James;H. McCracken;A. Bongiorno;A. Merloni;J. Peacock;J. Silverman;A. Comastri
本文研究了从2.13 deg 2 XMM-宇宙演化巡天（COSMOS）的0.5-2 keV X射线镶嵌图中提取的593个IAB < 23、光谱红移z < 4的X射线选择活动星系核（AGN）的投影相关函数的红移演化。我们介绍了一种方法来估计活动星系核样本的平均偏差和活动星系核托管晕的质量，解决样本方差使用晕模型，并考虑到随着时间的推移结构的增长。我们发现XMM-COSMOS活动星系核总群的偏置因子从到发生红移演化的证据，宿主暗物质（DM）晕的平均质量log M0（h-1 M）13.12 ± 0.12，在z < 2时保持不变。将我们的样本分为宽谱线活动星系核（BL）、无宽谱线活动星系核（NL）以及X射线无遮蔽和遮蔽活动星系核，我们观察到随着红移的增加，偏差在这个范围内增加，这对应于BL/X射线无遮蔽活动星系核和NL/X射线无遮蔽活动星系核的恒定晕质量log M0（h − 1 M返）<$13.28 ± 0.07和log M0（h−1 M返）<$13.00 ± 0.06。射线遮蔽活动星系核。理论模型假设类星体的相位是由主要的合并所触发的，因此无法重现在X射线选择的BL活动星系核中发现的高偏置因子和DM晕质量，其LBOL为1045 erg s−1。我们的工作扩展到z <$2.2的z <$1声明，对于中等亮度的X射线选择BL活动星系核，主要合并的贡献是由其他过程，可能是长期的，如潮汐破裂或磁盘不稳定性超过。
We present a study of the redshift evolution of the projected correlation function of 593 X-ray selected active galactic nuclei (AGNs) with IAB < 23 and spectroscopic redshifts z < 4, extracted from the 0.5–2 keV X-ray mosaic of the 2.13 deg2 XMM- Cosmic Evolution Survey (COSMOS). We introduce a method to estimate the average bias of the AGN sample and the mass of AGN hosting halos, solving the sample variance using the halo model and taking into account the growth of the structure over time. We find evidence of a redshift evolution of the bias factor for the total population of XMM-COSMOS AGNs from to with an average mass of the hosting dark matter (DM) halos log M0(h−1 M☉) ∼ 13.12 ± 0.12 that remains constant at all z < 2. Splitting our sample into broad optical line AGNs (BL), AGNs without broad optical lines (NL), and X-ray unobscured and obscured AGNs, we observe an increase of the bias with redshift in the range and which corresponds to a constant halo mass of log M0(h−1 M☉) ∼ 13.28 ± 0.07 and log M0(h−1 M☉) ∼ 13.00 ± 0.06 for BL/X-ray unobscured AGNs and NL/X-ray obscured AGNs, respectively. The theoretical models, which assume a quasar phase triggered by major mergers, cannot reproduce the high bias factors and DM halo masses found for X-ray selected BL AGNs with LBOL ∼ 2 × 1045 erg s−1. Our work extends up to z ∼ 2.2 the z ≲ 1 statement that, for moderate-luminosity X-ray selected BL AGNs, the contribution from major mergers is outnumbered by other processes, possibly secular ones such as tidal disruptions or disk instabilities.