论文标题
黑洞和寄主银河系在一个孤立的$ z \ sim 6 $ qSO中观察到了Alma
The black hole and host galaxy growth in an isolated $z\sim 6$ QSO observed with ALMA
论文作者
论文摘要
超级质量黑洞（SMBH）在回报时期的杰出质量增长及其与宿主星系的并发增长有何关系，对旨在解释这些系统在短时间内形成的理论模型构成了挑战（<1 Gyr）。要追踪准固定物体（QSO）及其宿主星系的平均进化路径（$ m _ {\ rm dyn} $）飞机，我们比较恒星形成速率（SFR），从灰尘温度和灰尘质量和灰尘质量（$ t _ {$ rm dust）中获得的恒星形成速率（SFR），增生率。为此，我们分析了$ Z \ sim 6 $ QSO J2310+1855的深度PC分辨率Alma观察Alma观察[CII]和H $ _2 $ o，从而详细研究了粉尘特性和冷气动力学。我们进行了精确的SED分析，获得了$ t _ {\ rm dust} = 71 $ k的防尘温度，而灰尘质量为$ m _ {\ rm dust} = 4.4 \ times 10^8 \ \ rm m _ {\ odot} $。隐含的AGN校正的SFR为$ 1240 \ \ rm m _ {\ odot} yr^{ - 1} $，比以前报告的QSO小2个。我们得出了动态质量$ m _ {\ rm dyn} = 5.2 \ times 10^{10} \ \ rm m _ {\ odot} $在$ r = 1.7 $ kpc之内的最佳估计。我们发现，$ {\ rm sfr}/m _ {\ rm dyn}> \ dot m _ {\ rm bh}/m _ {\ rm bh} $，表明AGN反馈可能有效地采取有效的行动来减慢SMBH的积累，而Stellar Massblys仍在启动了天然气的天然气，该反馈仍然有力地进行了天然的天气。此外，我们还能够检测[CII]发射线的红色和蓝色侧面的高速发射，从而追踪气态流出，并且首次通过H $ _2 $ o V = 0 $ 3 _ {（2,2,2,2）{（2,2,3 _}}（1,1,3 _ {1,1,1,3 _ {（1,1,3 _ {1,1,3 _ {1,1,3 _ {1,1,3 _ {（1,1,3 _），我们首次绘制了空间分辨的水蒸气磁盘。 $ν_ {\ rm obs} = 274.074 $ GHz，其运动属性和大小与[CII]磁盘的大小一致。
The outstanding mass growth of supermassive black holes (SMBHs) at the Reionisation Epoch and how it is related to the concurrent growth of their host galaxies, poses challenges to theoretical models aimed at explaining how these systems formed in short timescales (<1 Gyr). To trace the average evolutionary paths of quasi-stellar objects (QSOs) and their host galaxies in the BH mass-host mass ($M_{\rm dyn}$) plane, we compare the star formation rate (SFR), derived from the accurate estimate of the dust temperature and the dust mass ($T_{\rm dust}, M_{\rm dust}$), with the BH accretion rate. To this aim, we analysed a deep, $900$ pc resolution ALMA observation of the sub-mm continuum, [CII] and H$_2$O of the $z\sim 6$ QSO J2310+1855, enabling a detailed study of dust properties and cold gas kinematics. We performed an accurate SED analysis obtaining a dust temperature of $T_{\rm dust} = 71$ K and a dust mass of $M_{\rm dust}= 4.4 \times 10^8\ \rm M_{\odot}$. The implied AGN-corrected SFR is $1240 \ \rm M_{\odot}yr^{-1}$, a factor of 2 smaller than previously reported for this QSO. We derived the best estimate of the dynamical mass $M_{\rm dyn} = 5.2\times 10^{10}\ \rm M_{\odot}$ within $r = 1.7$ kpc, based on a dynamical model of the system. We found that ${\rm SFR}/M_{\rm dyn}>\dot M_{\rm BH}/M_{\rm BH}$, suggesting that AGN feedback might be efficiently acting to slow down the SMBH accretion, while the stellar mass assembly is still vigorously taking place in the host galaxy. In addition, we were also able to detect high-velocity emission on the red and blue sides of the [CII] emission line, that traces a gaseous outflow, and for the first time, we mapped a spatially-resolved water vapour disk through the H$_2$O v=0 $3_{(2,2)}-3_{(1,3)}$ emission line detected at $ν_{\rm obs} = 274.074$ GHz, whose kinematic properties and size are broadly consistent with those of the [CII] disk.
