Stellar mass function of cluster galaxies at z ~ 1.5: Evidence for reduced quenching efficiency at high redshift
Stellar mass function of cluster galaxies at z ~ 1.5: Evidence for reduced quenching efficiency at high redshift
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z ~ 1.5 处星团星系的恒星质量函数：高红移时猝灭效率降低的证据
DOI：
10.1051/0004-6361/201628663
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发表时间：
2016
影响因子：
6.5
通讯作者：
M. Cooper
中科院分区：
文献类型：
--
作者：
J. Nantais;R. Burg;C. Lidman;R. Demarco;A. Noble;G. Wilson;A. Muzzin;R. Foltz;A. DeGroot;M. Cooper
我们提出了极限质量为 10 10.1 M ⊙ 的被动星系和恒星形成星系的恒星质量函数 (SMF)，在四个光谱证实的斯皮策红序星团巡天适应 (SpARCS) 星系团中，每个星系团在 1.37 z K s 波段选择光度目录，平均有 11 个光度波段范围从 u 到 8 μm。我们将我们的星团星系与从 UltraVISTA/COSMOS 场中类似的 K s 波段选择目录中导出的场样本进行比较。 SMF 类似于现场的 SMF，但具有环境猝灭的迹象。我们发现，通常在场中形成恒星的星系中有 30 ± 20% 在星团中被淬灭。环境猝灭效率几乎不依赖于预计的~4 Mpc的星团中心距离，为该红移范围内的预处理和/或银河一致性提供了初步证据。我们还从文献中汇编了有关环境猝灭效率的可用数据，发现团簇和群体的猝灭效率似乎随着红移的增加而下降，其方式与之前的结果和基于晕质量增长的预期一致。
We present the stellar mass functions (SMFs) of passive and star-forming galaxies with a limiting mass of 10 10.1 M ⊙ in four spectroscopically confirmed Spitzer Adaptation of the Red-sequence Cluster Survey (SpARCS) galaxy clusters at 1.37 z K s-band-selected photometric catalogs for each cluster with an average of 11 photometric bands ranging from u to 8 μ m. We compare our cluster galaxies to a field sample derived from a similar K s-band-selected catalog in the UltraVISTA/COSMOS field. The SMFs resemble those of the field, but with signs of environmental quenching. We find that 30 ± 20% of galaxies that would normally be forming stars in the field are quenched in the clusters. The environmental quenching efficiency shows little dependence on projected cluster-centric distance out to ~4 Mpc, providing tentative evidence of pre-processing and/or galactic conformity in this redshift range. We also compile the available data on environmental quenching efficiencies from the literature, and find that the quenching efficiency in clusters and in groups appears to decline with increasing redshift in a manner consistent with previous results and expectations based on halo mass growth.
影响因子：
4.8
作者：
E. Cooke;N. Hatch;A. Rettura;D. Wylezalek;A. Galametz;D. Stern;M. Brodwin;S. I. Muldrew;O. Almaini;C. Conselice;P. Eisenhardt;W. Hartley;M. Jarvis;M. Jarvis;N. Seymour;S. Stanford
通讯作者：
E. Cooke;N. Hatch;A. Rettura;D. Wylezalek;A. Galametz;D. Stern;M. Brodwin;S. I. Muldrew;O. Almaini;C. Conselice;P. Eisenhardt;W. Hartley;M. Jarvis;M. Jarvis;N. Seymour;S. Stanford
DOI：
10.1088/0004-637x/768/1/74
发表时间：
2012-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-
通讯作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-