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arXiv 2109.06189astro-ph.GAastro-ph.CO
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SAMI星系巡天：作为星系动力学独立驱动力的质量和环境

The SAMI Galaxy Survey: Mass and Environment as Independent Drivers of Galaxy Dynamics

Jesse van de Sande, Scott M. Croom, Joss Bland-Hawthorn, Luca Cortese, Nicholas Scott, Claudia D. P. Lagos, Francesco D'Eugenio, Julia J. Bryant, Sarah Brough, … 展开作者

Jesse van de Sande, Scott M. Croom, Joss Bland-Hawthorn, Luca Cortese, Nicholas Scott, Claudia D. P. Lagos, Francesco D'Eugenio, Julia J. Bryant, Sarah Brough, Barbara Catinella, Caroline Foster, Brent Groves Katherine E. Harborne, Ángel R. López-Sánchez, Richard McDermid, Anne Medling, Matt S. Owers, Samuel N. Richards, Sarah M. Sweet, Sam P. Vaughan

备注：
22 pages and 17 figures, accepted for publication in MNRAS. Abstract abridged for Arxiv. The key figures of the paper are: 6, 8, 10, and 12
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摘要：

星系的运动学形态-密度关系通常归因于星系恒星质量分布随局部环境的变化。然而，早期的研究主要集中在慢旋转的整体人口的动态特性与环境的关注较少。我们使用SAMI星系巡天的$\sim$ 1800早期和晚期类型的星系与$\log(M_*/M_{\odot})>9.5$作为一个函数的平均环境过密度（$Σ_{5}$）和他们的排名在一个组或集群的动力学特性进行了调查。通过将星系分为快旋和慢旋，在固定的恒星质量以上的$\log(M_*/M_{\odot})>10.5$，我们检测到一个更高的分数（$\sim3.4σ$）的慢旋组和集群的中心和卫星相比，孤立的中央星系。聚焦于快速旋转人口，我们还发现星系运动学和它们的恒星质量以及它们所处的环境之间存在显着的相关性。具体来说，通过使用倾角校正或固有的$λ_{R_e}$值，我们发现，在固定的质量，卫星星系平均有最低的$λ_{\,R_e,intr}$，孤立的中心星系有最高的$λ_{\,R_e,intr}$，集团和集群中心之间的谎言。同样，在高密度环境中的星系有较低的平均$λ_{\,R_e,intr}$值相比，在低环境密度的星系。然而，在固定的$Σ_{5}$下，低质量和高质量星系的平均$λ_{\,R_e,intr}$差异与改变$Σ_{5}$ {（$Δλ_{\,R_e,intr} \sim 0.05$ .我们的研究结果表明，恒星质量后，环境中起着重要的作用，在创建缓慢的旋转，而对于快速旋转，我们也检测到一个独立的，虽然较小的，质量和环境对他们的运动学性质的影响。

英文摘要：

The kinematic morphology-density relation of galaxies is normally attributed to a changing distribution of galaxy stellar masses with the local environment. However, earlier studies were largely focused on slow rotators; the dynamical properties of the overall population in relation to environment have received less attention. We use the SAMI Galaxy Survey to investigate the dynamical properties of $\sim$1800 early and late-type galaxies with $\log(M_*/M_{\odot})>9.5$ as a function of mean environmental overdensity ($Σ_{5}$) and their rank within a group or cluster. By classifying galaxies into fast and slow rotators, at fixed stellar mass above $\log(M_*/M_{\odot})>10.5$, we detect a higher fraction ($\sim3.4σ$) of slow rotators for group and cluster centrals and satellites as compared to isolated-central galaxies. Focusing on the fast-rotator population, we also detect a significant correlation between galaxy kinematics and their stellar mass as well as the environment they are in. Specifically, by using inclination-corrected or intrinsic $λ_{R_e}$ values, we find that, at fixed mass, satellite galaxies on average have the lowest $λ_{\,R_e,intr}$, isolated-central galaxies have the highest $λ_{\,R_e,intr}$, and group and cluster centrals lie in between. Similarly, galaxies in high-density environments have lower mean $λ_{\,R_e,intr}$ values as compared to galaxies at low environmental density. However, at fixed $Σ_{5}$, the mean $λ_{\,R_e,intr}$ differences for low and high-mass galaxies are of similar magnitude as when varying $Σ_{5}$ {($Δλ_{\,R_e,intr} \sim 0.05$. Our results demonstrate that after stellar mass, environment plays a significant role in the creation of slow rotators, while for fast rotators we also detect an independent, albeit smaller, impact of mass and environment on their kinematic properties.

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