The GEEC2 spectroscopic survey of Galaxy groups at 0.8 < z < 1
The GEEC2 spectroscopic survey of Galaxy groups at 0.8 < z < 1
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DOI：
10.1093/mnras/stu1332
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发表时间：
2014-06
影响因子：
4.8
通讯作者：
M. Balogh;S. McGee;A. Mok;D. Wilman;A. Finoguenov;R. Bower;J. Mulchaey;L. Parker;Masayuki Tanaka Waterloo;Leiden;McMaster;Mpie;Helsinki;Durham;Ociw;Naoj
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作者：
M. Balogh;S. McGee;A. Mok;D. Wilman;A. Finoguenov;R. Bower;J. Mulchaey;L. Parker;Masayuki Tanaka Waterloo;Leiden;McMaster;Mpie;Helsinki;Durham;Ociw;Naoj
我们提出的双子座南GMOS光谱的数据发布领域的11个星系群在$0.8 50$ %完成的维里半径内的星系，和恒星质量$M_{\rm星星}>10^{10.3}M_\odot$。包括具有光度红移的星系，我们在这些星系群的维里半径内有$\sim 400$星系的有效样本量。我们目前的群速度色散，动力学和恒星质量。结合GCLASS中相同红移的大质量星团样本，我们发现恒星的总质量与动力学质量有很强的相关性，$\log{M_{200}}=1.20\left（\log{M_{\rm星星}}-12\right）+14.07$.这恒星的分数为$\sim 1$ %是低于一些晕占领分布模型预测，虽然弱依赖晕质量是在良好的协议。大多数群体有一个容易识别的最大质量的星系（MMG）附近的星系分布的中心，我们提出的光谱特性和表面亮度适合这些星系。总的恒星质量分布的集团，不包括MMG，比较以及与NFW配置文件的浓度为4 $，超过$\sim 0.2R_{200}$。这比数量密度分布更集中，表明存在一些质量偏析。
We present the data release of the Gemini-South GMOS spectroscopy in the fields of 11 galaxy groups at $0.8 50$ per cent complete for galaxies within the virial radius, and with stellar mass $M_{\rm star}>10^{10.3}M_\odot$. Including galaxies with photometric redshifts we have an effective sample size of $\sim 400$ galaxies within the virial radii of these groups. We present group velocity dispersions, dynamical and stellar masses. Combining with the GCLASS sample of more massive clusters at the same redshift we find the total stellar mass is strongly correlated with the dynamical mass, with $\log{M_{200}}=1.20\left(\log{M_{\rm star}}-12\right)+14.07$. This stellar fraction of $~\sim 1$ per cent is lower than predicted by some halo occupation distribution models, though the weak dependence on halo mass is in good agreement. Most groups have an easily identifiable most massive galaxy (MMG) near the centre of the galaxy distribution, and we present the spectroscopic properties and surface brightness fits to these galaxies. The total stellar mass distribution in the groups, excluding the MMG, compares well with an NFW profile with concentration $4$, for galaxies beyond $\sim 0.2R_{200}$. This is more concentrated than the number density distribution, demonstrating that there is some mass segregation.