Star Formation and Gas Kinematics of Quasar Host Galaxies at z~6: New insights from ALMA
Ran Wang, Jeff Wagg, Chris L. Carilli, Fabian Walter, Lindley Lentati, Xiaohui Fan, Dominik A. Riechers, Frank Bertoldi, Desika Narayanan, Michael A. Strauss, P… 展开作者
Ran Wang, Jeff Wagg, Chris L. Carilli, Fabian Walter, Lindley Lentati, Xiaohui Fan, Dominik A. Riechers, Frank Bertoldi, Desika Narayanan, Michael A. Strauss, Pierre Cox, Alain Omont, Karl M. Menten, Kirsten K. Knudsen, Roberto Neri, Linhua Jiang
备注：
25 pages, 5 figures, accepted for publication in ApJ
We present ALMA observations of the [C II] 158 micron fine structure line and dust continuum emission from the host galaxies of five redshift 6 quasars. We also report complementary observations of 250 GHz dust continuum and CO (6-5) line emission from the z=6.00 quasar SDSS J231038.88+185519.7. The ALMA observations were carried out in the extended array at 0.7" resolution. We have detected the line and dust continuum in all five objects. The derived [C II] line luminosities are 1.6x10^{9} to 8.8x10^{9} Lsun and the [C II]-to-FIR luminosity ratios are 3.0-5.6x10^{-4}, which is comparable to the values found in other high-redshift quasar-starburst systems and local ultra-luminous infrared galaxies. The sources are marginally resolved and the intrinsic source sizes (major axis FWHM) are constrained to be 0.3" to 0.6" (i.e., 1.7 to 3.5 kpc) for the [C II] line emission and 0.2" to 0.4" (i.e., 1.2 to 2.3 kpc) for the continuum. These measurements indicate that there is vigorous star formation over the central few kpc in the quasar host galaxies. The ALMA observations also constrain the dynamical properties of the atomic gas in the starburst nuclei. The intensity-weighted velocity maps of three sources show clear velocity gradients. Such velocity gradients are consistent with a rotating, gravitationally bound gas component, although they are not uniquely interpreted as such. Under the simplifying assumption of rotation, the implied dynamical masses within the [C II]-emitting regions are of order 10^{10} to 10^{11} Msun. Given these estimates, the mass ratios between the SMBHs and the spheroidal bulge are an order of magnitude higher than the mean value found in local spheroidal galaxies, which is in agreement with results from previous CO observations of high redshift quasars.
利用阿塔卡马大型毫米波阵列（ALMA）对27个z>6类星体的[CII] 158 $μ$ m谱线及其下的远红外尘埃连续谱辐射进行了观测。在23个源（85%）中显著检测到[CII]线（在>5-sigma）。我们发现了$L_{\rm [CII]}=10^{9-10}$ L $_\odot$的典型谱线亮度，平均谱线宽度约为385 km/s。我们的光源中的[CII]与远红外光度比（[CII]/FIR）跨越一个数量级，突出了恒星形成介质中的各种条件。四个类星体宿主星系的[CII]发射在几kpc尺度上清晰地分辨出来。宿主星系动力学质量的基本估计值在$2\times10^{10}$和$2\times10^{11}$ M $_\odot$之间，即，在给定中心黑洞质量的极限（$>3\times10^8$ M $_\odot$，假设是爱丁顿极限吸积）的情况下，比从局部标度关系中预期的要低一个数量级以上。在我们的样本中，在单个源的堆叠ALMA [CII]光谱中，我们没有发现偏离单个高斯分布的证据。类星体的光度与[CII]光度或等效宽度都没有很强的相关性。这次巡天（典型的源上积分时间为8分钟）展示了ALMA在毫米波长下无与伦比的灵敏度，并为宇宙中第一个大质量星系的研究提供了独特的参考样本。
Resolving circumgalactic gas flows around a z$\approx$3.6 quasar using MUSE and ALMA
Università degli Studi di Milano-Bicocca（米兰比可卡大学）；DTU Space, Technical University of Denmark（丹麦技术大学空间中心）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；INAF–Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；INAF–Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所天文与空间科学观测站）；IUCAA（印度天体物理学与宇宙学大学研究中心）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
ALMA survey of a massive node of the Cosmic Web at $z\sim 3$. II. A dynamically cold and massive disk galaxy in the proximity of a hyperluminous quasar
Constraining Sub-Parsec Binary Supermassive Black Holes in Quasars with Multi-Epoch Spectroscopy. II. The Population with Kinematically Offset Broad Balmer Emission Lines
一小部分类星体长期以来一直被认为在相对于宿主星系的系统红移的宽巴耳末线中显示出整体速度偏移。解释这些偏移的模型通常会引用单个黑洞（BH）周围的宽线区域气体运动学/不对称性，大质量（~sub-pc）双黑洞（BBHs）的轨道运动，或反冲BH，但单历元光谱无法区分这些情况。来自长期光谱监测的视线（LOS）径向速度（RV）偏移可用于检验BBH假设。我们从SDSS DR 7类星体目录中选取了399个具有宽H-β线偏移的类星体样本，并对其中的50个进行了第二历元光谱学研究。结合现有的SDSS光谱，新的观测使我们能够限制LOS RV移动的广泛的H-β线与休息帧基线的几年到近十年。使用互相关分析，我们检测到显着（99%的置信度）的径向加速度在宽的H-β线在24的50个对象。我们建议，9的24个检测子PC BBH候选人，这表明一致的速度变化独立测量的第二条宽线（无论是H-α或镁II）没有显着变化的宽线配置文件。结合论文I中对一般类星体总体的研究结果，我们发现第一个历元谱中的速度偏移与两个历元之间的平均加速度之间存在一种试探性的反相关，当两个历元之间的时间间隔是引起线位移的运动的轨道周期的一个不可忽略的分数时，这种反相关可以用轨道相位调制来解释。我们讨论了我们的研究结果的影响，在偏置线类星体的子pc BBH候选人的识别和对他们的频率和轨道参数的约束。[摘要]
Cold molecular gas distribution and kinematics in the low-metallicity dusty starburst of Mrk 996 resolved with ALMA
Universidad de Talca（塔尔卡大学）；Universidad de La Serena（拉塞雷纳大学）；Instituto de Astrofísica de Andalucía, CSIC（安达卢西亚天体物理学研究所，西班牙国家研究委员会）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理研究中心）；University of Michigan（密歇根大学）；Space Telescope Science Institute（太空望远镜科学研究所）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）
