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arXiv 2205.02497astro-ph.GAastro-ph.CO
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星系团A2142：晕边界，“红色序列”，根据SDSS的星系性质

Galaxy cluster A2142: halo boundary, `red sequence', properties of galaxies according to SDSS

Flera G. Kopylova, Alexander I. Kopylov

备注：
12 pages, 3 figures, 4 tables, accepted: Astrophys. Bull., 01, 2022
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摘要：

利用Sloan数字巡天的资料，对A2142星系的动力学、早型星系的性质、淬灭恒星形成（QG）星系的性质进行了研究。我们发现所观察到的晕边界，回溅半径$R_{sp}$，这是等于4.12 Mpc（$M_r < -20\,.\!\!^{\rm m}3$）和4.06 Mpc（$M_r < -21\,.\!\!^{\rm m}3$）的积分分布的星系数量作为一个函数的平方距离中心。我们研究了早型星系在星系团（$R/R_{200}$ < 3，$M_r < -20\,.\!\!^{\rm m}3$）中心和外围的分布情况，并绘制了红色序列（g - r）= $(-0.024\pm0.001)M_r + (0.441\pm0.005$）。在所有的星系团星系中，具有淬灭恒星形成（$- 12\,yr^{- 1} < \log sSFR < - 10.75\,yr^{- 1}$）的星系约占三分之一。我们发现，当$16\,.\!\!^{\rm h}5$、$31^{\circ}$的中心坐标和$300'$的大小相同时，在相同的z坐标下，在回溅$R_{sp}$之外的QG的分数与场中的QG的分数相同.对于恒星质量为$\log M_*/M_{\odot}$ = [10.5;11.0]（这是QG的主要质量范围）的星系，进入星系团后，当向中心移动时，半径$R_{90,r}$减小约30%。

英文摘要：

The paper presents the results of studying the dynamics of galaxies, properties of early-type galaxies, properties of galaxies with the quenched star formation (QGs) in the A 2142 based on the archival data from the Sloan Digital Sky Survey. We found the observed halo boundary, the splashback radius $R_{sp}$, which is equal to 4.12 Mpc ($M_r < -20\,.\!\!^{\rm m}3$) and 4.06 Mpc ($M_r < -21\,.\!\!^{\rm m}3$) over the integral distribution of the number of galaxies as a function of the squared distance from the center. We have studied how early-type galaxies are distributed in the center and in the outskirts of the cluster ($R/R_{200}$ < 3, $M_r < -20\,.\!\!^{\rm m}3$) and plotted the red sequence in the form of (g - r) = $(-0.024\pm0.001)M_r + (0.441\pm0.005$). Among all the cluster galaxies, the galaxies with the quenched star formation ( $- 12\,yr^{- 1} < \log sSFR < - 10.75\,yr^{- 1}$) make up about one third. We have found that the fraction of QGs beyond the splashback $R_{sp}$ is the same as in the field at the same z with coordinates of the center of $16\,.\!\!^{\rm h}5$, $31^{\circ}$ and a size of $300'$. For galaxies with the stellar masses $\log M_*/M_{\odot}$ = [10.5;11.0] (this is the main mass range of QGs), after entering the cluster, there is a decrease in the radii $R_{90,r}$ by about 30\% when moving towards the center.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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