Physical Models for the Clustering of Obscured and Unobscured Quasars
Physical Models for the Clustering of Obscured and Unobscured Quasars
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DOI：
10.3847/1538-4357/ab5d31
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发表时间：
2019-12
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影响因子：
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通讯作者：
Kelly E. Whalen;R. Hickox;M. Dipompeo;G. Richards;A. Myers
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文献类型：
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作者：
Kelly E. Whalen;R. Hickox;M. Dipompeo;G. Richards;A. Myers
对遮蔽类星体和未遮蔽类星体的聚类测量表明，遮蔽类星体比未遮蔽类星体存在于更大质量的暗物质晕中。这些结果与简单的统一（环面）的情况是不一致的，但可以解释的模型中，模糊的材料的分布取决于爱丁顿比或星系恒星质量。我们通过构建简单的物理模型来测试这些可能性，以与观测到的活动星系核种群进行比较。我们发现，以前观察到的昏暗和爱丁顿比或恒星质量之间的关系是不足以复制观察到的类星体聚类结果（和模糊和未模糊的人口，分别），同时保持观察到的部分模糊类星体（30%-65%）。这项工作表明，演化模型，其中的黑洞生长的典型时间尺度上的遮蔽演变，是必要的，以了解所观察到的中红外选择类星体的集群。
Clustering measurements of obscured and unobscured quasars show that obscured quasars reside in more massive dark matter halos than their unobscured counterparts. These results are inconsistent with simple unified (torus) scenarios but might be explained by models in which the distribution of obscuring material depends on Eddington ratio or galaxy stellar mass. We test these possibilities by constructing simple physical models to compare to observed active galactic nucleus populations. We find that previously observed relationships between obscuration and Eddington ratio or stellar mass are not sufficient to reproduce the observed quasar clustering results ( and for obscured and unobscured populations, respectively) while maintaining the observed fraction of obscured quasars (30%–65%). This work suggests that evolutionary models, in which obscuration evolves on the typical timescale for black hole growth, are necessary to understand the observed clustering of mid-IR-selected quasars.