Distant monsters: high redshift AGN predictions from a $\Lambda$CDM cosmological model
Distant monsters: high redshift AGN predictions from a $\Lambda$CDM cosmological model
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DOI：
10.1093/mnras/stz1216
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发表时间：
2018-06
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通讯作者：
Andrew J Griffin;C. Lacey;V. Gonzalez-Perez;C. Lagos;C. Baugh;Nikos Fanidakis Icc Durham;Portsmouth;Perth;Mpia Heidelberg
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作者：
Andrew J Griffin;C. Lacey;V. Gonzalez-Perez;C. Lagos;C. Baugh;Nikos Fanidakis Icc Durham;Portsmouth;Perth;Mpia Heidelberg
未来十年有望彻底改变高红移宇宙的研究：即将到来的 JWST、EUCLID 和 ATHENA 等任务将极大地增进我们对星系形成早期阶段的理解。我们使用更新的超大质量黑洞 (SMBH) 质量和自旋演化模型，结合使用普朗克宇宙学的最新版本的星系形成半解析模型 GALFORM，以及新的高分辨率千禧年式暗物质模拟，对 JWST、EUCLID 和 ATHENA 宽带滤波器中红移范围 $0 6$ 的多波长活动星系核 (AGN) 光度函数进行预测。我们预测这三项调查将选择三个略有不同的SMBH样本，EUCLID揭示了质量较大、吸积率较高的SMBH，JWST揭示了质量较小、吸积率较低的SMBH，而ATHENA则覆盖了其间的天体。总体而言，典型的探测到的超大质量黑洞的质量为 $M_{\mathrm{BH}} \sim 10^{6-7} M_{\odot}$，无量纲质量吸积率为 $\dot{M}/\dot{M}_{\mathrm{Edd}} \sim 1-10$，在恒星质量的宿主星系中为 $M_{\star} \sim 10^{8-9} M_{\odot}$。未来这些预测与观测结果的比较将为我们对星系形成中超大质量黑洞的理解提供见解。
The next decade promises to revolutionise the study of the high redshift Universe: upcoming missions such as JWST, EUCLID and ATHENA will greatly advance our understanding of the early stages of galaxy formation. We use an updated model for the evolution of masses and spins of supermassive black holes (SMBHs), coupled to the latest version of the semi-analytical model of galaxy formation GALFORM using the Planck cosmology, and a new high resolution Millennium style dark matter simulation to make predictions for multiwavelength Active Galactic Nuclei (AGN) luminosity functions in the redshift range $0 6$ in the broadband filters of JWST, EUCLID and ATHENA. We predict that these three surveys will select three somewhat different samples of SMBHs, with EUCLID unveiling the more massive, high accretion rate SMBHs, JWST the less massive, lower accretion rate SMBHs and ATHENA covering objects inbetween. Overall, typical detected SMBHs will have masses, $M_{\mathrm{BH}} \sim 10^{6-7} M_{\odot}$, with dimensionless mass accretion rates, $\dot{M}/\dot{M}_{\mathrm{Edd}} \sim 1-10$, in host galaxies of stellar mass, $M_{\star} \sim 10^{8-9} M_{\odot}$. The future comparison of these predictions to observations will provide insights into our understanding of SMBHs in galaxy formation.