arXiv 2107.056412021-07astro-ph.COastro-ph.GA

根据GAMA巡天的光谱星系群的Subaru HSC弱透镜质量-可观测标度关系

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

Divya Rana, Surhud More, Hironao Miyatake, Takahiro Nishimichi, Masahiro Takada, Aaron S. G. Robotham, Andrew M. Hopkins, Benne W. Holwerda

备注：: 17 pages, 11 figures, Accepted for publication in MNRAS
DOI：: 10.1093/mnras/stac007

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摘要：

我们利用斯巴鲁超级超级相机巡天（HSC）第一年数据发布的星系形状目录，使用弱透镜研究宇宙中星系群的暗物质含量。我们使用的星系群来自星系质量和集合星系调查，大约$100$平方。度的天空重叠的HSC调查作为镜头。我们将我们的分析限制在至少有五个成员的$1587$组。我们将这些组分为6个箱组的光度和组成员的速度色散和测量的透镜信号与$55$和$51$的信噪比为这两个不同的选择，分别。我们使用贝叶斯晕模型框架来推断我们的组在两个不同的可观察属性中的晕质量分布，并约束幂律标度关系，以及平均晕质量和两个组可观察属性之间的分散。我们得到了5%的限制与$\avg{M} = (0.81\pm 0.04)\times10^{14}\hinvMsun$的晕质量和集团光度之间的标度关系的振幅与$L_{\rm grp}=10^{11.5}\hinvsqLsun$，和一个幂律指数的$α=1.01\pm 0.07$。我们约束的幅度晕质量和速度色散之间的标度关系为$\avg{M}=(0.93\pm 0.05)\times10^{14}\hinvMsun$的$σ=500 \kms$和幂律指数为$α=1.52\pm0.10$。然而，这些比例关系对应用于组成员数量的确切切割是敏感的。与文献中相似标度关系的比较表明，我们的结果是一致的，并显着减少了误差。

英文摘要：

We utilize the galaxy shape catalogue from the first-year data release of the Subaru Hyper Suprime-cam Survey (HSC) to study the dark matter content of galaxy groups in the Universe using weak lensing. We use galaxy groups from the Galaxy Mass and Assembly galaxy survey in approximately $100$ sq. degrees of the sky that overlap with the HSC survey as lenses. We restrict our analysis to the $1587$ groups with at least five members. We divide these groups into six bins each of group luminosity and group member velocity dispersion and measure the lensing signal with a signal-to-noise ratio of $55$ and $51$ for these two different selections, respectively. We use a Bayesian halo model framework to infer the halo mass distribution of our groups binned in the two different observable properties and constrain the power-law scaling relation, and the scatter between mean halo masses and the two group observable properties. We obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and group luminosity with $\avg{M} = (0.81\pm 0.04)\times10^{14}\hinvMsun$ for $L_{\rm grp}=10^{11.5}\hinvsqLsun$, and a power-law index of $α=1.01\pm 0.07$. We constrain the amplitude of the scaling relation between halo mass and velocity dispersion to be $\avg{M}=(0.93\pm 0.05)\times10^{14}\hinvMsun$ for $σ=500 \kms$ and a power-law index to be $α=1.52\pm0.10$. However, these scaling relations are sensitive to the exact cuts applied to the number of group members. Comparisons with similar scaling relations from the literature show that our results are consistent and have significantly reduced errors.

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