MUSEQuBES：探测星系际介质中气体和金属分布的各向异性
MUSEQuBES: Probing Anisotropies in Gas and Metal Distributions in the Circumgalactic Medium
AI总结：
MUSEQuBES研究了低质量星系环状星系际介质中H I和O VI气体的各向异性分布，发现其覆盖分数在盘面和极向方向增强，而高质量星系则分布更均匀。
摘要：
我们研究了113个红移范围为0.12 < z < 0.75的孤立星系的环状星系际介质（CGM）中H I和O VI承载气体的方位依赖性，包括91个新的测量值，这些测量值来自MUSE准星盲发射调查（MUSEQuBES）。对于低质量（7 < log10(M*/Msun)< 9）星系，H I覆盖分数（k_HI）在virial半径（Rvir）内，当临界柱密度为log10(N(HI)/cm^-2) = 14.5时，在盘面（方位角phi < 20度）和极向（phi > 70度）方向上显示出增强。相比之下，对于更高质量星系（9 < log10(M*/Msun) < 11.3），这种双峰分布并未被观察到。同样，对于O VI覆盖分数（k_OVI），当临界值为log10(N(OVI)/cm^-2) = 14.0时，低质量星系在投影的主要轴和次要轴上显示出初步的增强。相比之下，高质量星系周围的O VI承载气体分布更均匀，没有显著的方位依赖性。最后，利用暗物质圆速度标准化像素速度二点相关函数（TPCF），我们发现O VI吸收体在宿主星系的盘面方向上比极向方向上更窄。观察到的高质量暗物质中的O VI分布的各向同性表明，其空间分布由全局暗物质属性决定；然而，O VI的运动学保留了其起源位置的记忆。
英文摘要：
We investigate the azimuthal dependence of HI and OVI-bearing gas in the circumgalactic medium (CGM) of 113 isolated galaxies in the redshift range $0.12<z<0.75$, including 91 new measurements from the MUSE Quasar-fields Blind Emitters Survey (MUSEQuBES). Of these, measurements for 46 galaxies lie within the virial radius ($R_{\rm vir}$), including 36 non-face-on systems for which azimuthal angle ($ϕ$) measurements are robust. The HI covering fraction (k_HI) within $R_{\rm vir}$ of low-mass ($7<\log(M/M_{\odot})\leq 9$) galaxies, for a threshold column density of ${\rm log}_{10}(N(HI)/{\rm cm}^{-2})=14.5$, exhibits an enhancement along both the disk plane ($ϕ\lesssim20^{\circ}$) and in the polar direction ($ϕ\gtrsim70^{\circ}$). In contrast, such a bimodal distribution is not observed for higher mass galaxies ($9<\log(M/M_{\odot})\leq 11.3$). Similarly, the OVI covering fraction (k_OVI), for a threshold of ${\rm log}_{10}(N(OVI)/{\rm cm}^{-2})=14.0$, shows a tentative enhancement along both the projected major and minor axes for low-mass galaxies. In contrast, \OVI-bearing gas around higher-mass galaxies appears more uniformly distributed, with no significant azimuthal dependence. Finally, using the halo circular-velocity-normalized pixel-velocity two-point correlation function (TPCF), we find that OVI absorbers are kinematically narrower along the disk plane compared to the polar directions of the host galaxies with similar stellar mass distributions. The observed isotropic distribution of OVI in high-mass halos suggests that its spatial distribution is governed by global halo properties; however, the OVI kinematics retain memory of the site of origin.
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