论文标题
结构，恒星人口特性，AGN分数和大规模紧凑星系的环境，$ 1 <z <z <2 $ 3D- {\ it Hst}/Candels/Candels
Structures, stellar population properties, AGN fractions, and environments of massive compact galaxies at $1 < z < 2$ in 3D--{\it HST}/CANDELS
论文作者
论文摘要
我们介绍了一项关于巨大的结构和物理特性的研究（$ m_*> 10^{10} m _ {\ sun} $）紧凑的星系，$ 1.0 <z <2.0 $ in Five 3d- {\ it Hst}/Candels fields。与扩展的星形星系（ESFG）相比，发现紧凑的星形星系（CSFG）具有较低的恒星形成水平，并且主要在{\ it uvj}图的静态区域中分布。灰尘衰减和S {é} RSIC指数的分布支持CQG的祖细胞是CSFG，并且CSFG处于ESFG和CQG之间的过渡阶段。 X射线选定的AGN（$ \ sim 28 \％$）的流行率在CSFG中以$ 1 <z <2 $确认，这表明诸如合并和磁盘不稳定性之类的暴力气体过程可能会使结构更加紧凑，并触发中央区域的星形形成和黑洞的增长。我们的结果支持CSFG $ 1 <z <2 $的“两步”方案是压实后的中级人口，但在快速淬火之前。我们对参数和非参数形态的分析表明，与CSFG（ESFGS）相比，CQGS（EQG）更集中，并且具有较少的亚结构，并且应相互关联淬灭和紧凑。 CSFG $ 1.5 <z <2 $（$ 1 <z <1.5 $）更喜欢在更高（较低的）密度环境中，与CQGS（ESFGS）相似。这表明合并或强烈的相互作用可能是较高红移下压实的主要驾驶机制，而单个星系的磁盘不稳定性可能在较低的红移在CSFG的形成中起着更重要的作用。
We present a study on structures and physical properties of massive ($M_* >10^{10} M_{\sun} $) compact galaxies at $1.0<z<2.0$ in five 3D--{\it HST}/CANDELS fields. Compared with the extended star-forming galaxies (eSFGs), compact star-forming galaxies (cSFGs) are found to have the lower level of star formation, and mainly distribute in the quiescent region of the {\it UVJ} diagram. The distributions of dust attenuation and S{é}rsic index support that the progenitors of cQGs are cSFGs, and cSFGs are at a transitional phase between eSFGs and cQGs. The prevalence of X-ray selected AGNs ($\sim 28\%$) is confirmed in the cSFGs at $1<z<2$ which indicates that the violent gas-rich processes such as merger and disk instability could drive the structure to be more compact, and trigger both star formation and black hole growth in the central regions. Our results support the "two-step" scenario that the cSFGs at $1<z<2$ are the intermediate population after compaction but before a quick quenching. Our analysis of parametric and nonparametric morphologies shows that cQGs (eQGs) are more concentrated and have less substructures than cSFGs (eSFGs), and quenching and compactness should be associated with each other. The cSFGs at $1.5<z<2$ ($1<z<1.5$) prefer to be in higher (lower) density environment, similar as cQGs (eSFGs). It suggests that merger or strong interaction might be the main driving mechanism of compaction at higher redshifts, whereas the disk instability of individual galaxies might play a more important role on the formation of cSFGs at lower redshifts.
