论文标题
自z $ \ sim $ 3以来
A super-linear "radio-AGN main sequence'' links mean radio-AGN power and galaxy stellar mass since z$\sim$3
论文作者
论文摘要
绘制星系种群中的平均AGN光度，随着时间的流逝，构图封装了超级质量黑洞（SMBH）和星系生长之间相互作用的重要线索。本文介绍了不同恒星质量（$ {M _ {*}} $）的跨星形星系（SFG）的无线电星系（SFG）的人口统计学，平均功率和宇宙演变。我们利用Deep VLA-COSMOS 3 GHz数据来构建RETART FRAME 1.4 GHz AGN光度功能，以0.1 $ \ LEQ $ \ leq $$ Z $$ \ leq $ 4.5 $ 4.5托管在SFGS中。将AGN光度函数分为不同的$ {m _ {*}} $ bins，表明，在更高$ {m _*} $中，无线电AGN与较低$ {m _*} $ calaxies相比，无线电AGN在更高的$ {m _*} $中更为频繁，更发光。 Radio AGN在SFGS中发挥的累积动力学光度密度为$ z $ \ sim $ 2，并且主要由Galaxies驱动，该星系为10.5 $ \ leq $ \ leq $ \ log $ \ log $（$ {M _ {*}}}}} $/$/$/$ {m_ _ _ {\ odot} $ {\ odot} $ 11 $ 11 $ 11 $ 11。在每个SFG中平均每个SFG的累积无线电活动（$ {M _ {*}} $，$ Z $）会导致“无线电 - agn Main序列”链接到时间平均的无线电功率$ \ langle $ \ langle $ \ langle $ \ langle $ \ langle $ langle langle lang {1.4}^1.4} $ \ log $$ \ langle $ [$ l_ {1.4}^{agn} $/ w hz $^{ - 1}] （1.41 $ \ pm $ 0.09）$ \ cdot $（$ \ log $ [$ {m _ {*}}} $/$/$ {m _ {\ odot}} $] -10 -10）。与恒星形成相比，在固定的红移对$ {m _ {*}} $上的超级线性依赖性表明，在更大的SFGS中增强了无线电活动。我们将这种增强性归因于更高的无线电占空比和更庞大的SFG的更明亮的无线电阶段。对于SFGS中不断发展的X射线AGN种群，可以看到一个非常一致的$ {M _ {*}} $依赖性。这种相似性被解释为可能是由世俗的冷气积聚驱动的，在银河系的寿命中以类似的方式加油和X射线AGN活动。
Mapping the average AGN luminosity across galaxy populations and over time encapsulates important clues on the interplay between supermassive black hole (SMBH) and galaxy growth. This paper presents the demography, mean power and cosmic evolution of radio AGN across star-forming galaxies (SFGs) of different stellar masses (${M_{*}}$). We exploit deep VLA-COSMOS 3 GHz data to build the rest-frame 1.4 GHz AGN luminosity functions at 0.1$\leq$$z$$\leq$4.5 hosted in SFGs. Splitting the AGN luminosity function into different ${M_{*}}$ bins reveals that, at all redshifts, radio AGN are both more frequent and more luminous in higher ${M_*}$ than in lower ${M_*}$ galaxies. The cumulative kinetic luminosity density exerted by radio AGN in SFGs peaks at $z$$\sim$2, and it is mostly driven by galaxies with 10.5$\leq$$\log$(${M_{*}}$/${M_{\odot}}$)$<$11. Averaging the cumulative radio AGN activity across all SFGs at each (${M_{*}}$,$z$) results in a "radio-AGN main sequence" that links the time-averaged radio-AGN power $\langle$$L_{1.4}^{AGN}$$\rangle$ and galaxy stellar mass, in the form: $\log$$\langle$[$L_{1.4}^{AGN}$/ W Hz$^{-1}]\rangle$ = (20.97$\pm$0.16) + (2.51$\pm$0.34)$\cdot$$\log$(1+$z$) + (1.41$\pm$0.09)$\cdot$($\log$[${M_{*}}$/${M_{\odot}}$] -10). The super-linear dependence on ${M_{*}}$, at fixed redshift, suggests enhanced radio-AGN activity in more massive SFGs, as compared to star formation. We ascribe this enhancement to both a higher radio AGN duty cycle and a brighter radio-AGN phase in more massive SFGs. A remarkably consistent ${M_{*}}$ dependence is seen for the evolving X-ray AGN population in SFGs. This similarity is interpreted as possibly driven by secular cold gas accretion fueling both radio and X-ray AGN activity in a similar fashion over the galaxy's lifetime.
