II型活动星系核-宿主星系连接：VVDS和VIPERS巡天的观察
The Type II AGN-host galaxy connection: insights from the VVDS and VIPERS surveys
摘要：
本文对VIPERS和VVDS巡天中0.5 < z < 0.9的光选II型活动星系核进行了研究，以探讨活动星系核活动与其宿主星系物理性质之间的联系。通过CIGALE程序拟合光谱能量分布估计了宿主恒星的质量，恒星形成率由[OII] $λ$ 3727 $Å$谱线光度导出。我们发现，49%的活动星系核宿主星系位于主序（MS）或以上，40%位于亚MS轨迹，11%位于静止轨迹。使用[OIII] $λ$ 5007 $Å$线光度作为活动星系核功率的代表，我们发现在固定的活动星系核功率下，II型活动星系核宿主星系表现出双峰行为：主星系恒星质量<10 $^{10}$ M $_{\odot}$的系统，位于MS或星爆轨迹上（高SF II型活动星系核），而居住在大质量宿主星系（>10 $^{10}$ M $_{\odot}$）的系统显示出较低的恒星形成水平（低SF II型活动星系核）。在所有恒星质量下，MS的偏移量与AGN功率呈正相关。我们解释这种相关性作为证据的活动星系核和主机之间的共同演化，可能是由于冷气体的可用性。在最强大的活动星系核与MS以下的宿主星系中，我们发现了一个暗示，虽然很弱，在[OIII]线轮廓的不对称性，可能是由于流出的气体，与活动星系核反馈删除可用的气体和停止在最大质量的主机中的恒星形成的情况一致。
英文摘要：
We present a study of optically-selected Type II AGN at 0.5 < z < 0.9 from the VIPERS and VVDS surveys, to investigate the connection between AGN activity and physical properties of their host galaxies. The host stellar mass is estimated through spectral energy distribution fitting with the CIGALE code, and star formation rates are derived from the [OII]$λ$3727 $Å$ line luminosity. We find that 49% of the AGN host galaxies are on or above the main sequence (MS), 40% lie in the sub-MS locus, and 11% in the quiescent locus. Using the [OIII]$λ$5007 $Å$ line luminosity as a proxy of the AGN power, we find that at fixed AGN power Type II AGN host galaxies show a bimodal behaviour: systems with host galaxy stellar mass <10$^{10}$ M$_{\odot}$, reside along the MS or in the starbursts locus (high-SF Type II AGN), while systems residing in massive host-galaxies (>10$^{10}$ M$_{\odot}$) show a lower level of star formation (low-SF Type II AGN). At all stellar masses, the offset from the MS is positively correlated with the AGN power. We interpret this correlation as evidence of co-evolution between the AGN and the host, possibly due to the availability of cold gas. In the most powerful AGN with host galaxies below the MS we find a hint, though weak, of asymmetry in the [OIII] line profile, likely due to outflowing gas, consistent with a scenario in which AGN feedback removes the available gas and halts the star formation in the most massive hosts.
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