论文标题
在正确的时间在正确的位置淬灭：追踪使用其结构和多尺度环境的Starburst，AGN和Starburst星系的共同历史
Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, AGNs, and Post-starburst Galaxies Using Their Structures and Multiscale Environments
论文作者
论文摘要
这项工作利用斯隆数字天空调查中星系的多尺度环境和结构，作为一致检查从星爆到静止的一致性，以红移$ z <0.2 $。 The environmental indicators include fixed aperture mass overdensities ($δ_{x\mathrm{Mpc}}$, $x \in \{0.5, 1, 2, 4, 8\}\,h^{-1}$Mpc), $k$-nearest neighbor distances, the tidal parameter, halo mass ($M_h$), and satellite/central classification.特定恒星形成率的残差（$δ\，\ mathrm {ssfr} $）用于选择starbursts（$δ\，\ m athrm {ssfr}> 0.6 \，$ dex，$ n \ $ n \ y \ 8，\ 8，\，600 $）。使用H $α<3 \，$ h $Δ_A> 4 \，$ angstrom吸收（$ n \ of $ n \ 750 $），选择了淬火后的季后赛（QPSB）。将Starburst和QPSB的环境与活跃的银河核（AGN）和不同$δ\，\ Mathrm {Ssfr} $的非活性星系进行了比较。 Starburst，AGN和QPSB的环境与大多数静态星系（QGS）的环境不同。大约$ 70 \％-90 \％$ $的starbursts，带有H $Δ_A> 4 $的Agns和QPSB是中心的，$ \ sim 80 \％-90 \％$具有$ m_h <10^{13} {13} {13}} {13} {13}} 10^{14} \，m_ \ odot $或在集群中活。他们的$ M_H $和卫星分数也与QGS不同。所有QPSB都与类似$ M_ \ Star $，环境，浓度指数和速度分散的一些SFG，Starburst，AGN和QGS匹配。 Starbursts的大量分数（$ \ sim 20 \％-30 \％$）不能与QPSB或QGS匹配。含义是：（1）某些星光爆炸不会迅速淬火。 （2）在高密度环境中运行的卫星淬灭机制无法解释大多数QPSB。 （3）从星爆，QPSB到QGS的演变不是$ z <0.2 $的主要路径。 （4）Starburst并非主要是由潮汐相互作用触发的。
This work uses multiscale environments and structures of galaxies in the Sloan Digital Sky Survey as consistency checks of the evolution from starburst to quiescence at redshift $z < 0.2$. The environmental indicators include fixed aperture mass overdensities ($δ_{x\mathrm{Mpc}}$, $x \in \{0.5, 1, 2, 4, 8\}\,h^{-1}$Mpc), $k$-nearest neighbor distances, the tidal parameter, halo mass ($M_h$), and satellite/central classification. The residuals of specific star formation rates ($Δ\,\mathrm{SSFR}$) is used to select starbursts ($Δ\,\mathrm{SSFR} > 0.6\,$dex, $N \approx 8,\,600$). Quenched post-starbursts (QPSBs) are selected using H$α< 3\,$angstrom in emission and H$δ_A > 4\,$ angstrom in absorption ($N \approx 750$). The environments of starbursts and QPSBs are compared with those of active galactic nuclei (AGNs) and inactive galaxies of varying $Δ\,\mathrm{SSFR}$. The environments of starbursts, AGNs, and QPSBs are unlike the environments of most quiescent galaxies (QGs). About $70\%-90\%$ of starbursts, AGNs with H$δ_A > 4$, and QPSBs are centrals, $\sim 80\%-90\%$ have $M_h < 10^{13}\,M_\odot$, and only $\sim 2\%-4\%$ have $M_h > 10^{14}\,M_\odot$ or live in clusters. Their $M_h$ and satellite fractions are also different from those of QGs. All QPSBs are matched to some SFGs, starbursts, AGNs, and QGs of similar $M_\star$, environments, concentration indices, and velocity dispersions. A significant fraction ($\sim 20\%-30\%$) of starbursts cannot be matched to QPSBs or QGs. The implications are: (1) some starbursts do not quench rapidly. (2) Satellite-quenching mechanisms operating in high density environments cannot account for most QPSBs. (3) The evolution from starbursts to QPSBs to QGs is not the dominant path at $z < 0.2$. (4) Starbursts are not mainly triggered by tidal interactions.
