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arXiv 1602.02755astro-ph.GAastro-ph.CO
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2<z<3亮类星体的恒星形成

Star Formation in Luminous Quasars at 2<z<3

Kathryn Harris, Duncan Farrah, Bernhard Schulz, Evanthia Hatziminaoglou, Marco Viero, Nick Anderson, Matthieu Bethermin, Scott Chapman, David L. Clements, Asant… 展开作者

Kathryn Harris, Duncan Farrah, Bernhard Schulz, Evanthia Hatziminaoglou, Marco Viero, Nick Anderson, Matthieu Bethermin, Scott Chapman, David L. Clements, Asantha Cooray, Andreas Efstathiou, Anne Feltre, Peter Hurley, Eduardo Ibar, Mark Lacy, Sebastian Oliver, Mathew J. Page, Ismael Perez-Fournon, Sara M. Petty, Lura K. Pitchford, Dimitra Rigopoulou, Douglas Scott, Myrto Symeonidis, Joaquin Vieira, Lingyu Wang

备注：
MNRAS, accepted
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摘要：

利用Herschel和SDSS的观测数据，研究了光选1类星体的恒星形成率（$2<z<3$）与活动星系核性质之间的关系。我们发现，在$300\pm100~\rm{M}_{\odot}$ yr $^{-1}$，$\dot{\rm{M}}_s$随红移近似保持不变。相反，$\dot{\rm{M}}_s$随活动星系核亮度的增加而增加，最大值为$\sim600~\rm{M}_{\odot}$ yr $^{-1}$，并随CIV FWHM而增加。在上下文与以前的结果，这是一致的$\dot{\rm{M}}_s$和黑洞吸积率（$\dot{\rm{M}}_{bh}$）之间的关系存在于只有部分的$z-\dot{\rm{M}}_{s}-\dot{\rm{M}}_{bh}$平面，取决于自由气体分数，触发活动，和过程，可能淬火恒星形成。$\dot{\rm{M}}_s$与活动星系核光度和CIV半高宽的关系与黑洞质量标度的类星体的恒星形成率一致，尽管我们不能排除与黑洞吸积率的单独关系。观察到恒星形成率随着CIV等效宽度的增加而下降。这种下降可以部分地解释通过鲍德温效应，但可能有一个额外的贡献，从一个或多个的三个因素：$M_i$是不是一个线性示踪剂L $_{2500}$，鲍德温效应的变化形式在高AGN光度，和高CIV EW值标志着改变之间的关系$\dot{\rm{M}}_s$和$\dot{\rm{M}}_{bh}$。最后，在$\dot{\rm{M}}_s$和爱丁顿比或CIV线的不对称性之间没有强的关系。前者表明，恒星形成速率与黑洞吸积的效率无关，而后者与定向效应引起的CIV不对称性一致。

英文摘要：

We investigate the relation between star formation rates ($\dot{M}_{s}$) and AGN properties in optically selected type 1 quasars at $2<z<3$ using data from Herschel and the SDSS. We find that $\dot{\rm{M}}_s$ remains approximately constant with redshift, at $300\pm100~\rm{M}_{\odot}$yr$^{-1}$. Conversely, $\dot{\rm{M}}_s$ increases with AGN luminosity, up to a maximum of $\sim600~\rm{M}_{\odot}$yr$^{-1}$, and with CIV FWHM. In context with previous results, this is consistent with a relation between $\dot{\rm{M}}_s$ and black hole accretion rate ($\dot{\rm{M}}_{bh}$) existing in only parts of the $z-\dot{\rm{M}}_{s}-\dot{\rm{M}}_{bh}$ plane, dependent on the free gas fraction, the trigger for activity, and the processes that may quench star formation. The relations between $\dot{\rm{M}}_s$ and both AGN luminosity and CIV FWHM are consistent with star formation rates in quasars scaling with black hole mass, though we cannot rule out a separate relation with black hole accretion rate. Star formation rates are observed to decline with increasing CIV equivalent width. This decline can be partially explained via the Baldwin effect, but may have an additional contribution from one or more of three factors; $M_i$ is not a linear tracer of L$_{2500}$, the Baldwin effect changes form at high AGN luminosities, and high CIV EW values signpost a change in the relation between $\dot{\rm{M}}_s$ and $\dot{\rm{M}}_{bh}$. Finally, there is no strong relation between $\dot{\rm{M}}_s$ and Eddington ratio, or the asymmetry of the CIV line. The former suggests that star formation rates do not scale with how efficiently the black hole is accreting, while the latter is consistent with CIV asymmetries arising from orientation effects.

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