MAGiiCAT III. INTERPRETING SELF-SIMILARITY OF THE CIRCUMGALACTIC MEDIUM WITH VIRIAL MASS USING Mg ii ABSORPTION
MAGiiCAT III. INTERPRETING SELF-SIMILARITY OF THE CIRCUMGALACTIC MEDIUM WITH VIRIAL MASS USING Mg ii ABSORPTION
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MAGiiCAT III. 使用 Mg ii 吸收解释环银河介质与维里质量的自相似性
DOI：
10.1088/0004-637x/779/1/87
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
G. Kacprzak
中科院分区：
文献类型：
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作者：
C. Churchill;Sebastian Trujillo;N. Nielsen;G. Kacprzak
在丘吉尔等人的研究中，我们对Mg ii吸收体星系表中的182个星系进行了晕丰度匹配（MAGiiCAT），并表明平均Mg ii λ2796等效宽度遵循严格的平方反比幂律，Wr（2796）<$（D/Rvir）−2，投影位置相对于星系维里半径，Mg ii吸收覆盖分数与星系维里质量M h有效不变，在10.7 μ log M h/M回流13.9的范围内。在这项工作中，我们探索Wr（2796），维里质量，碰撞参数，维里半径，和理论冷却半径之间的多元关系，进一步阐明自相似性的冷/暖（T = 104-104.5 K）环星系介质（CGM）维里质量。我们发现，维里质量决定的程度和强度的Mg II吸收气体，使平均Wr（2796）增加与维里质量在固定的距离，而减少与银河系距离固定维里质量。大部分吸收气体位于D/Rvir = 0.3的范围内，与维里质量和最小吸收阈值无关;在这个范围内，也许在0.3 < D/Rvir = 1的范围内，平均Wr（2796）与维里质量无关。相反，银河系交叉相关的研究，我们表明，Wr（2796）和维里质量之间没有反相关。我们讨论了如何模拟和理论约束的观测支持自相似性的冷/暖CGM通过物理管理星星的形成，气相金属富集，回收效率的星系尺度风，灯丝和合并吸积，和过密度的局部环境作为维里质量的函数。
In Churchill et al., we used halo abundance matching applied to 182 galaxies in the Mg ii Absorber–Galaxy Catalog (MAGiiCAT) and showed that the mean Mg ii λ2796 equivalent width follows a tight inverse-square power law, Wr(2796)∝(D/Rvir)−2, with projected location relative to the galaxy virial radius and that the Mg ii absorption covering fraction is effectively invariant with galaxy virial mass, M h, over the range 10.7 ⩽ log M h/M☉ ⩽ 13.9. In this work, we explore multivariate relationships between Wr(2796), virial mass, impact parameter, virial radius, and the theoretical cooling radius that further elucidate self-similarity in the cool/warm (T = 104–104.5 K) circumgalactic medium (CGM) with virial mass. We show that virial mass determines the extent and strength of the Mg ii absorbing gas such that the mean Wr(2796) increases with virial mass at fixed distance while decreasing with galactocentric distance for fixed virial mass. The majority of the absorbing gas resides within D ≃ 0.3 Rvir, independent of both virial mass and minimum absorption threshold; inside this region, and perhaps also in the region 0.3 < D/Rvir ⩽ 1, the mean Wr(2796) is independent of virial mass. Contrary to absorber–galaxy cross-correlation studies, we show there is no anti-correlation between Wr(2796) and virial mass. We discuss how simulations and theory constrained by observations support self-similarity of the cool/warm CGM via the physics governing star formation, gas-phase metal enrichment, recycling efficiency of galactic scale winds, filament and merger accretion, and overdensity of local environment as a function of virial mass.