A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies
A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies
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DOI：
10.1093/mnras/sty1136
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发表时间：
2018-03
影响因子：
4.8
通讯作者：
Song Huang;A. Leauthaud;J. Greene;K. Bundy;Yen-Ting Lin;Masayuki Tanaka;R. Mandelbaum;S. Miyazaki;Y. Komiyama
中科院分区：
文献类型：
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作者：
Song Huang;A. Leauthaud;J. Greene;K. Bundy;Yen-Ting Lin;Masayuki Tanaka;R. Mandelbaum;S. Miyazaki;Y. Komiyama
我们使用~100平方度深（>28.5 mag arcsec$^{-2}$在i波段），高质量（中位数0.6 arcsec看到）的成像数据从超超级凸轮（HSC）的调查，以揭示晕质量依赖的表面质量密度分布和外部恒星的大质量星系的信封。HSC巡天的i波段图像比斯隆数字巡天深4个星等，使我们能够直接追踪恒星质量分布到100 kpc，而不需要叠加。我们最终表明，在固定的恒星质量，恒星配置文件的大质量星系依赖于他们的暗物质晕的质量。平均而言，在固定恒星质量下，质量为0.3 ~ 14.0$的大质量晕中，$\log M_{\星星，100\ \mathrm{kpc}}>11.6$的大质量中心星系的$R_{\mathrm{50}}$要大20%左右。这种依赖性也反映在10和100千秒差距内的恒星质量之间的关系中。与质量-尺寸关系相比，$\log M_{\星星，100\ \rm{kpc}}$-$\log M_{\星星，10\ \rm{kpc}}$关系避免了尺寸定义上的模糊性，并且可以直接与模拟结果进行比较。我们的研究结果表明，从HSC的深层图像，我们可以量化晕质量和外部恒星晕之间的联系，这可能会提供新的大质量中央星系的形成和组装的约束。
We use ~100 square deg of deep (>28.5 mag arcsec$^{-2}$ in i-band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach ~4 magnitudes deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with $\log M_{\star, 100\ \mathrm{kpc}}>11.6$ in more massive haloes at 0.3 14.0$ are ~20% larger in $R_{\mathrm{50}}$ at fixed stellar mass. Such dependence is also reflected in the relationship between the stellar mass within 10 and 100 kpc. Comparing to the mass--size relation, the $\log M_{\star, 100\ \rm{kpc}}$-$\log M_{\star, 10\ \rm{kpc}}$ relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.