The colour of galaxies in distant groups
The colour of galaxies in distant groups
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遥远星系群的颜色
DOI：
10.1111/j.1365-2966.2009.15193.x
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发表时间：
2009
影响因子：
4.8
通讯作者：
Balogh M
中科院分区：
文献类型：
--
作者：
Balogh M
我们提出了一种新的光学和近红外成像方法，对位于0.25<；z<；0.55的98个光谱选择的星系群进行成像，其中大部分具有速度色散σ<；500 Km S−1。我们使用点扩展函数匹配孔径光度测量法来测量群成员和周围场群的精确颜色。在大约M=1×1010M⊙的恒星质量极限之上，样本在统计上是完整的。总体颜色分布在场和群样本中都是双峰的；但在固定光度下，红峰所占的群星系的比例比场大20±7%，∼为20%±7%。特别是，在哈勃太空望远镜成像中发现的具有早期类型形态的星团成员显示出一个紧密的红色序列，类似于更大质量星系团的情况。使用光学和近红外颜色，包括来自斯皮策太空望远镜的数据，我们表明，红色序列上大约20%-30%的星系可能是尘埃变红的星系，具有不可忽视的恒星形成和早期螺旋形态。无论是场样本还是组样本都是如此，并且几乎不依赖于近红外光度。因此，没有恒星形成或活动星系核活动迹象的明亮(0.4MK<；−22)群成员的比例为54%±6%，这是由它们的颜色或[OII]发射确定的。我们的野外样本包括所有环境中的星系，其中包含35%±3%的此类非活动星系，这与如果所有此类星系都位于群团和星系团中的情况下的预期数量一致。这巩固了我们早先的结论，即在z≲0.5时的致密环境与某些星系中恒星形成的提前停止有关；特别是，我们没有发现在这些环境中显著增强恒星形成的证据。简单的星系形成模型预测，恒星的形成将以过于高效的方式形成，从而使红色星序变得过于拥挤。试图通过为所有组成员平等地增加猝灭的时间尺度来解决这一问题，会以一种与观测不一致的方式扭曲颜色分布。
We present new optical and near-infrared imaging for a sample of 98 spectroscopically selected galaxy groups at 0.25 <z< 0.55, most of which have velocity dispersions σ < 500 km s−1. We use point spread function matched aperture photometry to measure accurate colours for group members and the surrounding field population. The sample is statistically complete above a stellar mass limit of approximatelyM= 1 × 1010M⊙. The overall colour distribution is bimodal in both the field and group samples; but, at fixed luminosity the fraction of group galaxies populating the red peak is larger, by ∼20 ± 7 per cent, than that of the field. In particular, group members with early-type morphologies, as identified inHubble Space Telescopeimaging, exhibit a tight red sequence, similar to that seen for more massive clusters. Using optical and near-infrared colours, including data from theSpitzer Space Telescope, we show that approximately 20–30 per cent of galaxies on the red sequence may be dust-reddened galaxies with non-negligible star formation and early-spiral morphologies. This is true of both the field and group samples, and shows little dependence on near-infrared luminosity. Thus, the fraction of bright (0.4MK< −22) group members with no sign of star formation or active galactic nuclei activity, as identified by their colours or [Oii] emission, is 54 ± 6 per cent. Our field sample, which includes galaxies in all environments, contains 35 ± 3 per cent of such inactive galaxies, consistent with the amount expected ifallsuch galaxies are located in groups and clusters. This reinforces our earlier conclusions that dense environments atz≲ 0.5 are associated with a premature cessation of star formation in some galaxies; in particular, we find no evidence for significantly enhanced star formation in these environments. Simple galaxy formation models predict a quenching of star formation in groups that is too efficient, overpopulating the red sequence. Attempts to fix this by increasing the time-scale of this quenching equally for all group members distort the colour distribution in a way that is inconsistent with observations.
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DOI：
10.1086/313426
发表时间：
2000-04
期刊：
The Astrophysical Journal Supplement Series
影响因子：
--
作者：
H. Yee;H. Yee;Simon L. Morris;Simon L. Morris;H. Lin;R. Carlberg;R. Carlberg;Patrick B. Hall;Patrick B. Hall;Marcin Sawicki;Marcin Sawicki;Marcin Sawicki;David R. Patton;David R. Patton;David R. Patton;G. Wirth;G. Wirth;G. Wirth;E. Ellingson;E. Ellingson;C. W. Shepherd
通讯作者：
H. Yee;H. Yee;Simon L. Morris;Simon L. Morris;H. Lin;R. Carlberg;R. Carlberg;Patrick B. Hall;Patrick B. Hall;Marcin Sawicki;Marcin Sawicki;Marcin Sawicki;David R. Patton;David R. Patton;David R. Patton;G. Wirth;G. Wirth;G. Wirth;E. Ellingson;E. Ellingson;C. W. Shepherd
遥远星系群的恒星质量含量
DOI：
--
发表时间：
2006
期刊：
影响因子：
--
作者：
M. Balogh;D. Wilman;Robert D E Henderson;R. Bower;D. Gilbank;R. Whitaker;S. Morris;G. Hau;J. Mulchaey;A. Oemler;R. G. C. U. O. Waterloo;Mpe;Garching;D. University;U. Toronto;Ociw
通讯作者：
Ociw
揭示星系团在大质量星系演化中的重要作用：来自中红移红外被动序列的见解
DOI：
--
发表时间：
2008
期刊：
影响因子：
--
作者：
D. Wilman;D. Pierini;K. Tyler;S. McGee;A. Oemler;S. Morris;M. Balogh;R. Bower;J. Mpe;Garching;Germany;S. Observatory;Arizona;U. Waterloo;Canada;C. Observatories;Pasadena;U. Durham;U.K.
通讯作者：
U.K.
DOI：
10.1111/j.1365-2966.2006.09994.x
发表时间：
2006-02
影响因子：
4.8
作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
通讯作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
DOI：
10.1046/j.1365-8711.2003.06292.x
发表时间：
2002-05
影响因子：
4.8
作者：
G. Kauffmann;T. Heckman;S. White;S. Charlot;C. Tremonti;E. Peng;M. Seibert;J. Brinkmann;R. Nich
通讯作者：
G. Kauffmann;T. Heckman;S. White;S. Charlot;C. Tremonti;E. Peng;M. Seibert;J. Brinkmann;R. Nich