论文标题
自z $ \ sim $ 3自X射线光度函数编码以来，星系中不断发展的AGN占空比
The evolving AGN duty cycle in galaxies since z$\sim$3 as encoded in the X-ray luminosity function
论文作者
论文摘要
我们介绍了活性银河核（AGN）的X射线光度函数（XLF）的新建模，向z $ \ sim $ 3介绍，解剖了主序列（MS）和Starburst（SB）星系的贡献。对于每个星系人群，我们将观察到的星系恒星质量（m $ _ {\ star} $）发挥作用，其网格为m $ _ {\ star} $ - 独立的Eddington比率（$λ_{\λ_{\ rm Edd} $），通过经验性黑洞的估计率（Bhhar）的经验范围（BHHAR）正常于SIRTAINT（BHHAR）。由于z $ \ sim $ 3，我们的简单方法与观察到的XLF达成了极好的一致性。我们发现，只有通过$λ_{\ rm edd} $分布的固有扁平化，并且随着断裂$λ^{*} $的积极转移，才能复制所观察到的XLF的红移演变，与反外层行为一致。 AGN积聚历史主要是由巨大的（10 $^{10} <$ m $ _ {\ star} <$ 10 $ 10 $^{11} $ m $ _ {\ odot} $ MS Galaxies，而SB驱动的BH积分，而可能与Galaxy Mergers $相关，在$ quass中，$ x} $/erg s $^{ - 1} $）$> $ 44.36 + 1.28 $ \ cdot $（1 + z）。我们推断，发现高度精神的概率（$λ_ {\ rm edd}> $ 10％）AGN随着红移的增长而大大增加，从0.4％（3.0％）在z = 0.5％= 0.5％至6.5％至6.5％（15.3％）到MS（SB）星系的Z = 3时，含量更长的AGN星系，暗示了更长的AGN早期Univer in the Early Univer Cyce in the Early Univer Cycece。我们的结果强烈利用BHAR和SFR之间的M $ _ {\ Star} $ - 依赖性比率，因为Bhar/sfr $ \ propto $ m $ _ {\ star}^{0.73 [+0.22，-0.29]} $，支撑了与主机相对的非线性BH堆积。最后，该框架为超级 - 埃德丁顿BH积聚和不同的$λ_ {\ rm edd} $处方提供了潜在的问题，以理解宇宙BH质量组件。
We present a new modeling of the X-ray luminosity function (XLF) of Active Galactic Nuclei (AGN) out to z$\sim$3, dissecting the contribution of main-sequence (MS) and starburst (SB) galaxies. For each galaxy population, we convolved the observed galaxy stellar mass (M$_{\star}$) function with a grid of M$_{\star}$-independent Eddington ratio ($λ_{\rm EDD}$) distributions, normalised via empirical black hole accretion rate (BHAR) to star formation rate (SFR) relations. Our simple approach yields an excellent agreement with the observed XLF since z$\sim$3. We find that the redshift evolution of the observed XLF can only be reproduced through an intrinsic flattening of the $λ_{\rm EDD}$ distribution, and with a positive shift of the break $λ^{*}$, consistent with an anti-hierarchical behavior. The AGN accretion history is predominantly made by massive (10$^{10}<$M$_{\star}<$10$^{11}$ M$_{\odot}$) MS galaxies, while SB-driven BH accretion, possibly associated with galaxy mergers, becomes dominant only in bright quasars, at $\log$(L$_{\rm X}$/erg s$^{-1}$)$>$44.36 + 1.28$\cdot$(1+z). We infer that the probability of finding highly-accreting ($λ_{\rm EDD}>$ 10%) AGN significantly increases with redshift, from 0.4% (3.0%) at z=0.5 to 6.5% (15.3%) at z=3 for MS (SB) galaxies, implying a longer AGN duty cycle in the early Universe. Our results strongly favor a M$_{\star}$-dependent ratio between BHAR and SFR, as BHAR/SFR $\propto$ M$_{\star}^{0.73[+0.22,-0.29]}$, supporting a non-linear BH buildup relative to the host. Finally, this framework opens potential questions on super-Eddington BH accretion and different $λ_{\rm EDD}$ prescriptions for understanding the cosmic BH mass assembly.
