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arXiv 2207.03314astro-ph.GA
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用ALMA观测孤立$z\sim 6$ QSO中的黑洞和宿主星系生长

The black hole and host galaxy growth in an isolated $z\sim 6$ QSO observed with ALMA

R. Tripodi, C. Feruglio, F. Fiore, M. Bischetti, V. D'Odorico, S. Carniani, S. Cristiani, S. Gallerani, R. Maiolino, A. Marconi, A. Pallottini, E. Piconcelli, L. Vallini, T. Zana

备注：
15 pages, 10 figures, 4 tables. Accepted in A&A
发表信息：
A&A 665, A107 (2022)
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摘要：

超大质量黑洞（SMBH）在再电离时期的显著质量增长以及它与宿主星系的同时增长的关系，对旨在解释这些系统如何在短时间尺度（<1 Gyr）内形成的理论模型提出了挑战。为了追踪类星体（QSO）及其宿主星系在BH质量-宿主质量（$M_{\rm dyn}$）平面上的平均演化路径，我们比较了由尘埃温度和尘埃质量（$T_{\rm dust}, M_{\rm dust}$）的精确估计得到的恒星形成率（SFR）与BH吸积率。为此，我们分析了深，$900$ pc分辨率ALMA观测的亚毫米连续，[CII]和H $_2$ O的$z\sim 6$类星体J2310+1855，使详细的研究尘埃性质和冷气体运动学。我们进行了精确的SED分析，获得了$T_{\rm dust} = 71$ K的尘埃温度和$M_{\rm dust}= 4.4 \times 10^8\ \rm M_{\odot}$的尘埃质量。活动星系核修正的SFR是$1240 \ \rm M_{\odot}yr^{-1}$，比以前报道的这个类星体小2倍。基于系统的动力学模型，我们导出了$r = 1.7$ kpc内动力学质量$M_{\rm dyn} = 5.2\times 10^{10}\ \rm M_{\odot}$的最佳估计。我们发现，${\rm SFR}/M_{\rm dyn}>\dot M_{\rm BH}/M_{\rm BH}$，这表明活动星系核的反馈可能有效地减缓了SMBH吸积，而恒星质量组装仍在积极地发生在宿主星系。此外，我们还能够检测到高速发射的红色和蓝色的两侧的[CII]发射线，跟踪气体流出，并为第一次，我们绘制了一个空间分辨的水蒸气盘通过H $_2$ O v=0 $3_{(2,2)}-3_{(1,3)}$发射线检测到在$ν_{\rm obs} = 274.074$ GHz，其运动学特性和大小与[CII]盘大致一致。

英文摘要：

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.

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