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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >A high dust emissivity index beta for a CO-faint galaxy in a filamentary Ly alpha nebula at z=3.1
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A high dust emissivity index beta for a CO-faint galaxy in a filamentary Ly alpha nebula at z=3.1

机译：在Z = 3.1的丝状物α星云中的一个高尘发射率指数β用于丝状物α星云中的共微弱星系

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摘要

We present CO J = 4-3 line and 3 mm dust continuum observations of a 100 kpc-scale filamentary Ly alpha nebula (SSA22 LAB18) at z = 3.1 using the Atacama Large Millimeter/submillimeter Array (ALMA). We detected the CO J = 4-3 line at a systemic z(CO) = 3.093 +/- 0.001 at 11 sigma from one of the ALMA continuum sources associated with the Ly alpha filament. We estimated the CO J = 4-3 luminosity of L'(CO(4-3)) = (2.3 +/- 0.2) x 10(9) Kkms(-1) pc(2) for this CO source, which is one order of magnitude smaller than those of typical z > 1 dusty star-forming galaxies (DSFGs) of similar far-infrared luminosity L-IR similar to 10(12) L-circle dot. We derived a molecular gas mass of M-gas = (4.4(-0.6)(+0.9)) x 10(9) M-circle dot and a star-formation rate of SFR = 270 +/- 160M(circle dot) yr(-1). We also estimated a gas depletion time of tau(dep) = 17 +/- 10 Myr, which is shorter than those of typical DSFGs. It is suggested that this source is in the transition phase from DSFG to a gas-poor, early-type galaxy. From ALMA to Herschel multi-band dust continuum observations, we measured a dust emissivity index beta = 2.3 +/- 0.2, which is similar to those of local gas-poor, early-type galaxies. From recent laboratory experiments, the specific chemical compositions needed to reproduce such a high beta for interstellar dust at the submillimeter wavelengths. ALMA CO and multi-band dust continuum observations can constrain the evolutionary stage of high-redshift galaxies through tau(dep) and beta, and thus we can investigate the chemical composition of dust even in the early Universe.
机译：我们使用ATACAMA大毫米/亚颌骨阵列（ALMA），在Z = 3.1上呈现CO J = 4-3线和3毫米粉尘连续观察100 kpc尺寸丝状物α星云（SSA22 LAB18）。从与LYα丝相关的Alma连续源之一，我们在系统Z（CO）= 3.093 +/- 0.001处检测到X j = 4-3线。我们估计了L'的CO J = 4-3亮度（CO（4-3））=（2.3 +/- 0.2）x 10（9）Kkms（-1）PC（2），这是一个数量级小于典型的Z> 1粉尘星形星系（DSFG）的类似远红外发光度L-IR类似于10（12）升圆点。我们衍生M-气体的分子气体=（4.4（-0.6）（+ 0.9））×10（9）m圆点和SFR = 270 +/- 160m（圆点）的星形成速率（-1）。我们还估计了TAU的气体耗尽时间（DEP）= 17 +/- 10 MYR，这短于典型的DSFG。建议该来源从DSFG到瓦斯贫乏早期星系的转变阶段。从Alma到Herschel多带尘埃连续观测，我们测量了灰尘发射率指数β= 2.3 +/- 0.2，类似于当地煤气贫乏，早期星系的粉尘。从最近的实验室实验中，特定的化学组合物需要在亚颌下波长下繁殖这种高β进行外星形灰尘。 Alma Co和多频带尘埃连续性观测可以限制通过Tau（Dep）和Beta的高射频星系的进化阶段，因此我们即使在早期宇宙中也可以调查灰尘的化学成分。

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