Structural and dynamical modeling of WINGS clusters
Structural and dynamical modeling of WINGS clusters
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WINGS 集群的结构和动力学建模
DOI：
--
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发表时间：
2019
影响因子：
6.5
通讯作者：
D. Bettoni
中科院分区：
文献类型：
--
作者：
G. Mamon;A. Cava;A. Biviano;A. Moretti;B. Poggianti;D. Bettoni
不同类别星系的轨道形状是它们形成和演化的探测器。使用贝叶斯MAMPOSSt质量轨道建模算法，对来自广域邻近星系团调查(WINDS)的54个规则星系团的至少30个成员速度的三个伪星系团(通过将其位置和速度重新归一化后堆叠而成)在投影相空间中联合拟合椭圆星系、螺旋不规则星系和透镜状星系的分布。我们的伪星系团(即堆栈)包含近5000个具有可用速度和形态类型的星系。给出了具有不同先验知识的MAMPOSSt的30次运行。对于星系团和最亮的星系团，具有更陡峭内斜率的广义Navarro-Frenk-White(NFW)模型、自由指数Einasto模型和双NFW模型获得了最高的MAMPOSSt可能性。然而，没有强有力的贝叶斯证据支持比NFW模型更陡峭的轮廓。质量浓度与宇宙学模拟的预测相符。当SOS接近时，椭圆体通常能最好地跟踪质量分布。螺旋星系显示出半径越来越大的拉长轨道，两个堆栈上的SOS也是如此，一个堆栈上的椭圆轨道也是如此。三种堆栈中的三种类型的内轨道都符合各向同性。考虑到螺旋星系在星系团中的范围要大得多，它们应该会迅速转变为早期类型。螺旋线预计会有拉长的外部轨道，这是它们最近径向进入星系团的结果。对于早期类型，我们发现的较小的拉长轨道可能与这些星系在星系团中花费的时间较长有关。我们证明了二体松弛太慢，不能解释早期类型的内部各向同性，这表明内部各向同性是主要星系团合并时的剧烈松弛或作用于亚星系团的动力摩擦和潮汐制动的结果。我们认为，短寿命螺线的内部各向同性是一种选择效应，即螺线在转变为早期形态之前只经过中心一次。
The orbital shapes of galaxies of different classes are a probe of their formation and evolution. The Bayesian MAMPOSSt mass-orbit modeling algorithm is used to jointly fit the distribution of elliptical, spiral-irregular, and lenticular galaxies in projected phase space, on three pseudo-clusters (built by stacking the clusters after re-normalizing their positions and velocities) of 54 regular clusters from the Wide-field Nearby Galaxy-clusters Survey (WINGS), with at least 30 member velocities. Our pseudo-clusters (i.e., stacks) contain nearly 5000 galaxies with available velocities and morphological types. Thirty runs of MAMPOSSt with different priors are presented. The highest MAMPOSSt likelihoods are obtained for generalized Navarro-Frenk-White (NFW) models with steeper inner slope, free-index Einasto models, and double NFW models for the cluster and the brightest cluster galaxy. However, there is no strong Bayesian evidence for a steeper profile than the NFW model. The mass concentration matches the predictions from cosmological simulations. Ellipticals usually best trace the mass distribution while S0s are close. Spiral galaxies show increasingly elongated orbits at increasing radii, as do S0s on two stacks, and ellipticals on one stack. The inner orbits of all three types in the three stacks are consistent with isotropy. Spiral galaxies should transform rapidly into early-types given their much larger extent in clusters. Elongated outer orbits are expected for the spirals, a consequence of their recent radial infall into the cluster. The less elongated orbits we find for early-types could be related to the longer time spent by these galaxies in the cluster. We demonstrate that two-body relaxation is too slow to explain the inner isotropy of the early types, which suggests that inner isotropy is the consequence of violent relaxation during major cluster mergers or dynamical friction and tidal braking acting on subclusters. We propose that the inner isotropy of the short-lived spirals is a selection effect of spirals passing only once through pericenter before being transformed into early-type morphologies.
影响因子：
4.8
作者：
N. Okabe;Graham P. Smith
通讯作者：
N. Okabe;Graham P. Smith
LoCuSS：星系团中恒星形成的缓慢淬灭以及预处理的需要
DOI：
10.1088/0004-637x/806/1/101
发表时间：
2015
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Haines C
通讯作者：
Haines C
DOI：
10.1088/2041-8205/730/2/l13
发表时间：
2011-02
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
F. Bigiel;A. Leroy;F. Walter;E. Brinks;W. D. Blok;C. Kramer;H. Rix;A. Schruba;K. Schuster;A. Usero;H. Wiesemeyer
通讯作者：
F. Bigiel;A. Leroy;F. Walter;E. Brinks;W. D. Blok;C. Kramer;H. Rix;A. Schruba;K. Schuster;A. Usero;H. Wiesemeyer