The GOGREEN survey: Internal dynamics of clusters of galaxies at redshift 0.9 − 1.4
The GOGREEN survey: Internal dynamics of clusters of galaxies at
redshift 0.9 − 1.4
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GOGREEN 调查：红移 0.9 – 1.4 处星系团的内部动力学
DOI：
10.1051/0004-6361/202140564
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发表时间：
2021
影响因子：
6.5
通讯作者：
H. Shipley
中科院分区：
文献类型：
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作者：
A. Biviano;R. Burg;M. Balogh;E. Munari;M. Cooper;G. Lucia;R. Demarco;P. Jablonka;A. Muzzin;J. Nantais;L. Old;G. Rudnick;B. Vulcani;G. Wilson;H. Yee;D. Zaritsky;P. Cerulo;J. Chan;A. Finoguenov;D. Gilbank;C. Lidman;I. Pintos;H. Shipley
上下文。星系团质量对LES(M(R))的研究提供了对暗物质的性质和影响质量分布的物理过程的约束(ff)。星系团速度各向异性过程(β(R))的研究为星系团内星系的轨道提供了信息，这与星系的演化有关。结合质量过程和速度各向异性过程，我们可以确定伪相空间密度过程fi过程(Q(R))；数值模拟预测，这些过程fi过程在团心距离内遵循简单的幂定律。目标。我们详细地确定了迄今所研究的红移量最大的星系团的质量、速度各向异性和伪相空间密度。方法：研究方法。我们利用GOGREEN和GCLASS光谱数据的组合，对14个质量为M200≥10 14M(CID：12)红移为0的星团进行了研究。9≤z≤1.4.我们通过堆积581个光谱识别的星系团成员和恒星质量M(fi：63)≥109构建了系综星系团。5M(Cid：12)。我们使用MAMPOSSt方法来约束几个M(R)和β(R)模型，然后我们用非参数的方法逆Jeans方程来确定系综团簇β(R)。最后，我们结合M(R)和β(R)分析的结果来确定系综团簇的Q(R)。结果。系综团簇质量ProfiLe的浓度c200与Λ冷暗物质(Λ)宇宙学数值模拟的预测，以及之前从引力透镜和X射线数据获得的质量相似、红移相似的星系团的测定结果非常一致。我们发现总质量密度与星系数密度分布或恒星质量分布之间没有明显的fiff差别。在空间上，恒星形成星系的密度明显低于静止星系。(fi)星系团的轨道在中心附近是各向同性的，而在外部则是放射状的。恒星形成星系和低恒星质量的星系往往比静止的星系和高恒星质量的星系在更大的径向拉长轨道上运动。由总质量或数密度确定的Profile Q(R)与数值模拟预测的幂函数行为非常接近。结论。到目前为止详细探测的最高红移星团的内部动力学与低红移星团的内部动力学非常相似，并与数值模拟的预测非常一致。我们的样品中的团簇已经达到了高度的动力学松弛。
Context. The study of galaxy cluster mass profiles ( M ( r )) provides constraints on the nature of dark matter and on physical processes a ff ecting the mass distribution. The study of galaxy cluster velocity anisotropy profiles ( β ( r )) informs the orbits of galaxies in clusters, which are related to their evolution. The combination of mass profiles and velocity anisotropy profiles allows us to determine the pseudo phase-space density profiles ( Q ( r )); numerical simulations predict that these profiles follow a simple power law in cluster-centric distance. Aims. We determine the mass, velocity anisotropy, and pseudo phase-space density profiles of clusters of galaxies at the highest redshifts investi- gated in detail to date. Methods. We exploited the combination of the GOGREEN and GCLASS spectroscopic data-sets for 14 clusters with mass M 200 ≥ 10 14 M (cid:12) at redshifts 0 . 9 ≤ z ≤ 1 . 4. We constructed an ensemble cluster by stacking 581 spectroscopically identified cluster members with stellar mass M (cid:63) ≥ 10 9 . 5 M (cid:12) . We used the MAMPOSSt method to constrain several M ( r ) and β ( r ) models, and we then inverted the Jeans equation to determine the ensemble cluster β ( r ) in a non-parametric way. Finally, we combined the results of the M ( r ) and β ( r ) analysis to determine Q ( r ) for the ensemble cluster. Results. The concentration c 200 of the ensemble cluster mass profile is in excellent agreement with predictions from Λ cold dark matter ( Λ CDM) cosmological numerical simulations, and with previous determinations for clusters of similar mass and at similar redshifts, obtained from gravita- tional lensing and X-ray data. We see no significant di ff erence between the total mass density and either the galaxy number density distributions or the stellar mass distribution. Star-forming galaxies are spatially significantly less concentrated than quiescent galaxies. The orbits of cluster galaxies are isotropic near the center and more radial outside. Star-forming galaxies and galaxies of low stellar mass tend to move on more radially elongated orbits than quiescent galaxies and galaxies of high stellar mass. The profile Q ( r ), determined using either the total mass or the number density profile, is very close to the power-law behavior predicted by numerical simulations. Conclusions. The internal dynamics of clusters at the highest redshift probed in detail to date are very similar to those of lower-redshift clusters, and in excellent agreement with predictions of numerical simulations. The clusters in our sample have already reached a high degree of dynamical relaxation.