Star formation in the XMMU J2235.3−2557 galaxy cluster at z= 1.39
Star formation in the XMMU J2235.3−2557 galaxy cluster at z= 1.39
复制标题
XMMU J2235.3−2557 星系团 z= 1.39 处的恒星形成
DOI：
10.1111/j.1365-2966.2010.17828.x
复制
发表时间：
2010
影响因子：
4.8
通讯作者：
M. Bergmann
中科院分区：
文献类型：
--
作者：
A. Bauer;R. Grutzbauch;I. Jørgensen;J. Varela;M. Bergmann
我们提出的大质量星系团XMMU J2235.3-2557在z = 1.39的窄带测光研究的第一个结果。我们用双子座北的近红外成像仪和光谱仪获得了深H窄带成像，对应于星系团红移处的Hα发射。我们的样本由82个星系组成，半径为1500 kpc，其中10个是光谱确认的星系团成员。16个星系被确定为多余的线发射体。我们发现，在这些多余的线发射星系中，平均星星形成率（SFR）为3.6 ± 1.3 M·yr-1。对于光谱确认的集群成员，我们发现H宽带的幅度和SFR之间的相关性，使较亮的星系有较低的SFR。的概率，SFR和确认成员的大小是不相关的是0.7%。我们还发现之间的相关性SFR和距离从集群中心的确认和多余的线发射的候选成员，有5%的概率是没有确认的成员之间的相关性。所有多余的线发射候选星系团成员都位于200千秒差距半径之外。我们的结论是，当宇宙只有4.5 Gyr时，在这个z = 1.39的大质量星系团的中心200 kpc半径（R QUENCH = 200 kpc）内，星星形成被有效地关闭。
We present the first results of a narrow-band photometric study of the massive galaxy cluster XMMU J2235.3-2557 at z = 1.39. We obtained deep H narrow-band imaging with the Near InfraRed Imager and Spectrometer on Gemini North, corresponding to Hα emission at the cluster's redshift. Our sample consists of 82 galaxies within a radius of ∼500 kpc, 10 of which are spectroscopically confirmed cluster members. 16 galaxies are identified as excess line-emitters. Among just the excess line-emitting galaxies, we find an average star formation rate (SFR) of 3.6 ± 1.3 M ⊙ yr -1 . For spectroscopically confirmed cluster members, we find a correlation between H broad-band magnitude and SFR such that brighter galaxies have lower SFRs. The probability that the SFR and magnitude of confirmed members are uncorrelated is 0.7 per cent. We also find a correlation between the SFR and distance from the cluster centre for both confirmed and excess line-emitting candidate members, with a probability of 5 per cent for there to be no correlation among confirmed members. All excess line-emitting candidate cluster members are located outside a radius of 200 kpc. We conclude that star formation is effectively shut off within the central 200 kpc radius (R QUENCH ∼ 200 kpc) of this massive galaxy cluster at z = 1.39, when the Universe was only 4.5 Gyr old.
影响因子：
6.5
作者：
P. Rosati;P. Tozzi;R. Gobat;Joana S. Santos;M. Nonino;R. Demarco;C. Lidman;C. Lidman;C. Mullis;V. Strazzullo;H. Böhringer;R. Fassbender;Kyle S. Dawson;Masayuki Tanaka;J. Jee;H. Ford;G. Lamer;A. Schwope
通讯作者：
P. Rosati;P. Tozzi;R. Gobat;Joana S. Santos;M. Nonino;R. Demarco;C. Lidman;C. Lidman;C. Mullis;V. Strazzullo;H. Böhringer;R. Fassbender;Kyle S. Dawson;Masayuki Tanaka;J. Jee;H. Ford;G. Lamer;A. Schwope
DOI：
10.1088/0004-637x/704/1/672
发表时间：
2009-08
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Myung-Kook Jee;P. Rosati;H. Ford;K. Dawson;C. Lidman;S. Perlmutter;R. Demarco;V. Strazzullo;C. Mullis;H. Böhringer;R. Fassbender
通讯作者：
Myung-Kook Jee;P. Rosati;H. Ford;K. Dawson;C. Lidman;S. Perlmutter;R. Demarco;V. Strazzullo;C. Mullis;H. Böhringer;R. Fassbender
XMMU J2235-2557 中的星系团：z ≤1 4 处大多数大质量环境中的星系群特性
影响因子：
6.5
作者：
Strazzullo;Rosati;Pannella;Santos;Nonino;Demarco;Lidman;Tanaka;Mullis;Nuñez;Rettura;Böhringer;Bender;Bouwens;Dawson;Fassbender
通讯作者：
Fassbender