Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XII. Extended [C ii] Structure (Merger or Outflow) in a z = 6.72 Red Quasar-猫眼课题宝

DOI：

10.3847/1538-4357/abd7ef

发表时间：

2021-01

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

T. Izumi;M. Onoue;Y. Matsuoka;M. Strauss;S. Fujimoto;H. Umehata;M. Imanishi;T. Kawamuro;T. Nagao;Y. Toba;K. Kohno;N. Kashikawa;K. Inayoshi;T. Kawaguchi;K. Iwasawa;A. Inoue;T. Goto;S. Baba;M. Schramm;H. Suh;Y. Harikane;Y. Ueda;J. Silverman;T. Hashimoto;Y. Hashimoto;S. Ikarashi;D. Iono;Chien-Hsiu Lee;Kianhong Lee;T. Minezaki;K. Nakanishi;Suzuka Nakano;Y. Tamura;Ji-Jia Tang

我们展示了阿塔卡马大型毫米/亚毫米阵列[C ii] 158 μm线和远红外（FIR）连续辐射观测，观测对象是z = 6.72的HSC J120505.09−000027.9（J1205−0000），光束大小为1.00 × 0.8 × 0.5（或4.1 kpc × 2.6 kpc），这是迄今为止已知的最遥远的红色类星体。红色类星体被尘埃适度地变红，并且被认为是在从模糊的恒星暴到未模糊的正常类星体的快速过渡中，由强大的活动星系核（AGN）反馈驱动，吹出星际介质的茧。J1205−0000的远红外连续光谱是明亮的，估计光度为L FIR <$3 × 1012 L <$。[C ii]线发射扩展到r = 5 kpc的尺度，大于FIR连续谱的尺度。扩展区域的线剖面复杂而宽广（FWHM 630-780 km s-1）。虽然确定这种扩展结构的性质是不切实际的，但可能的解释包括（i）伴星系/合并星系和（ii）大规模活动星系核驱动的外流。对于（i）的情况，伴星是适度的恒星形成（大约10 M yr−1），但没有被我们的斯巴鲁光学观测发现（y AB，5σ = 24.4等）。对于（ii）的情况，我们对冷中性流出速率的下限是100 M·yr-1。外流动能和动量都比能量守恒风模型预测的要低得多，这表明该类星体中的活动星系核反馈不能完全抑制其星星的形成。

We present Atacama Large Millimeter/submillimeter Array [C ii] 158 μm line and far-infrared (FIR) continuum emission observations toward HSC J120505.09−000027.9 (J1205−0000) at z = 6.72 with a beam size of ∼0.″8 × 0.″5 (or 4.1 kpc × 2.6 kpc), the most distant red quasar known to date. Red quasars are modestly reddened by dust and are thought to be in rapid transition from an obscured starburst to an unobscured normal quasar, driven by powerful active galactic nucleus (AGN) feedback that blows out a cocoon of interstellar medium. The FIR continuum of J1205−0000 is bright, with an estimated luminosity of L FIR ∼ 3 × 1012 L ⊙. The [C ii] line emission is extended on scales of r ∼ 5 kpc, greater than that of the FIR continuum. The line profiles at the extended regions are complex and broad (FWHM ∼ 630–780 km s−1). Although it is not practical to identify the nature of this extended structure, possible explanations include (i) companion/merging galaxies and (ii) massive AGN-driven outflows. For the case of (i), the companions are modestly star-forming (∼10 M ⊙ yr−1) but are not detected by our Subaru optical observations (y AB,5σ = 24.4 mag). For the case of (ii), our lower limit to the cold neutral outflow rate is ∼100 M ⊙ yr−1. The outflow kinetic energy and momentum are both much lower than predicted in energy-conserving wind models, suggesting that the AGN feedback in this quasar is not capable of completely suppressing its star formation.

Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XII. Extended [C ii] Structure (Merger or Outflow) in a z = 6.72 Red Quasar

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