CLASH-VLT: The stellar mass function and stellar mass density profile of the z=0.44 cluster of galaxies MACS J1206.2-0847
CLASH-VLT: The stellar mass function and stellar mass density profile of the z=0.44 cluster of galaxies MACS J1206.2-0847
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CLASH-VLT：z=0.44 星系团 MACS J1206.2-0847 的恒星质量函数和恒星质量密度剖面
DOI：
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
B. Ziegler
中科院分区：
文献类型：
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作者：
M. Annunziatella;A. Biviano;A. Mercurio;M. Nonino;P. Rosati;I. Balestra;V. Presotto;M. Girardi;R. Gobat;C. Grillo;D. Kelson;E. Medezinski;M. Postman;M. Scodeggio;M. Brescia;R. Demarco;A. Fritz;A. Koekemoer;D. Lemze;M. Lombardi;B. Sartoris;K. Umetsu;E. Vanzella;L. Bradley;D. Coe;M. Donahue;L. Infante;U. Kuchner;C. Maier;E. Regős;M. Verdugo;B. Ziegler
上下文。研究星系恒星质量函数(SMF)与星系环境和恒星质量密度剖面Rho(R)的关系是约束星系演化模型的有力工具。目标。我们确定了z=0.44星系团MACS J1206.2-0847对于被动星系和恒星形成(SF)星系的SMF，从星系团的不同区域，从中心到大约2维里半径。我们还确定了Rho(R)，以将其与数密度和总质量密度分布进行比较。方法：研究方法。我们使用来自Clash-VLT调查的数据集。恒星质量是通过对斯巴鲁望远镜获得的5个波段的光度数据进行SED拟合得到的。我们发现了1363个星系团成员，其恒星质量为10.95mSolar。结果。用双谢克特函数对整个簇的SMF进行了很好的拟合。SF星系团和被动星系的SMF在统计上是不同的。SF星系团星系的SMF不依赖于环境。被动种群的SMF在最内侧(<；0.50MPC)、密度最高的聚集区的斜率(绝对值)明显小于较外部、低密度的区域。巨型/亚巨型星系的数量比在这个最内侧区域最大，在邻近区域最小，但随后又向星系团的外围缓慢增加。这也反映在每个星系团的平均恒星质量的径向趋势上。另一方面，恒星质量分数，即恒星与总星团质量的比率，并没有表现出任何明显的径向趋势。结论。我们的结果似乎与SF星系由于密度相关的环境过程而演化为被动星系的情景一致，并最终在星系团中心附近被摧毁，成为弥漫的星系团内介质的一部分。
Context. The study of the galaxy stellar mass function (SMF) in relation to the galaxy environment and the stellar mass density profile, rho(r), is a powerful tool to constrain models of galaxy evolution. Aims. We determine the SMF of the z=0.44 cluster of galaxies MACS J1206.2-0847 separately for passive and star-forming (SF) galaxies, in different regions of the cluster, from the center out to approximately 2 virial radii. We also determine rho(r) to compare it to the number density and total mass density profiles. Methods. We use the dataset from the CLASH-VLT survey. Stellar masses are obtained by SED fitting on 5-band photometric data obtained at the Subaru telescope. We identify 1363 cluster members down to a stellar mass of 10^9.5 Msolar. Results. The whole cluster SMF is well fitted by a double Schechter function. The SMFs of cluster SF and passive galaxies are statistically different. The SMF of the SF cluster galaxies does not depend on the environment. The SMF of the passive population has a significantly smaller slope (in absolute value) in the innermost (<0.50 Mpc), highest density cluster region, than in more external, lower density regions. The number ratio of giant/subgiant galaxies is maximum in this innermost region and minimum in the adjacent region, but then gently increases again toward the cluster outskirts. This is also reflected in a decreasing radial trend of the average stellar mass per cluster galaxy. On the other hand, the stellar mass fraction, i.e., the ratio of stellar to total cluster mass, does not show any significant radial trend. Conclusions. Our results appear consistent with a scenario in which SF galaxies evolve into passive galaxies due to density-dependent environmental processes, and eventually get destroyed very near the cluster center to become part of a diffuse intracluster medium.
DOI：
10.1088/0067-0049/199/2/25
发表时间：
2011-06
期刊：
The Astrophysical Journal Supplement Series
影响因子：
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作者：
M. Postman;D. Coe;N. Benı́tez;L. Bradley;T. Broadhurst;M. Donahue;H. Ford;O. Graur;G. Graves-G.-G
通讯作者：
M. Postman;D. Coe;N. Benı́tez;L. Bradley;T. Broadhurst;M. Donahue;H. Ford;O. Graur;G. Graves-G.-G