使用XMM-牛顿解开AGN和星形编队连接
Disentangling the AGN and Star-Formation connection using XMM-Newton
摘要：
越来越多的证据支持星系和它们的居民SMBH的同时代增长。大多数研究还声称SMBH的活动与宿主星系的恒星形成之间存在相关性。不过，目前还不清楚这种相关性是否适用于所有的redz和LX。在这项工作中，我们使用来自X-ATLAS和XMM-XXL北场的数据，并编制了迄今为止最大的X射线样本，以研究X射线活动星系核如何影响其宿主星系在宽红带和光度基线上的恒星形成，即，0.03<z<3，log LX（2-10 keV）=（41-45.5）ergs-l。我们的样品由3336活动星系核组成。1872年X射线天体具有光谱红区。对于其余的源，我们使用TPZ（一种机器学习算法）计算光度redz。我们估计恒星质量（M*）和恒星形成率（SFR）通过应用SED拟合通过CIGALE代码，使用光学，近红外和中红外测光。我们的608个光源也有远红外测光（赫歇尔）。我们使用这些源来校准剩余X射线样本的SFR计算。我们的研究结果表明，LX和SFR之间的相关性，在所有的redz和LX跨越我们的样本。我们还发现了一个依赖的特定的SFR（sSFR）的redz，而有迹象表明，LX增强sSFR，即使在低redz。然后，我们解开的影响M* 和redz上的SFR和再次研究其对LX的依赖。为此，我们使用Schreiber等人的公式来估计具有与我们的X射线活动星系核相同的恒星质量和红移的主序星星系的SFR。我们的分析表明，活动星系核增强了它的宿主星系的恒星形成，当星系位于主序星之下和淬火的星系，它生活在主序星之上。因此，活动星系核对宿主星系SFR的影响取决于星系相对于主序星的位置。
英文摘要：
There is growing evidence supporting the coeval growth of galaxies and their resident SMBH. Most studies also claim a correlation between the activity of the SMBH and the star-formation of the host galaxy. It is unclear, though, whether this correlation extends to all redz and LX. In this work, we use data from the X-ATLAS and XMM-XXL North fields and compile the largest X-ray sample up to date, to investigate how X-ray AGN affect the star-formation of their host galaxies in a wide redz and luminosity baseline, i.e., 0.03<z<3 and log LX (2-10 keV)= (41-45.5) ergs-1. Our sample consists of 3336 AGN. 1872 X-ray objects have spectroscopic redz. For the remaining sources we calculate photometric redz using TPZ, a machine-learning algorithm. We estimate stellar masses (M*) and Star Formation Rates (SFRs) by applying SED fitting through the CIGALE code, using optical, near-IR and mid-IR photometry. 608 of our sources also have far-IR photometry (Herschel). We use these sources to calibrate the SFR calculations of the rest of our X-ray sample. Our results show a correlation between the LX and the SFR, at all redz and LX spanned by our sample. We also find a dependence of the specific SFR (sSFR) on redz, while there are indications that LX enhances the sSFR even at low redz. We then disentangle the effects of M* and redz on the SFR and study again its dependence on the LX. Towards this end, we use the Schreiber et al. formula to estimate the SFR of main sequence galaxies that have the same stellar mass and redshift as our X-ray AGN. Our analysis reveals that the AGN enhances the star-formation of its host galaxy, when the galaxy lies below the main sequence and quenches the star-formation of the galaxy it lives in, when the host lies above the main sequence. Therefore, the effect of AGN on the SFR of the host galaxy, depends on the location of the galaxy relative to the main sequence.
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