我们代表了一个联合X射线，弱透镜，光学分析的光学选择合并集群，HSC J 085024 +001536，从斯巴鲁HSC-SSP调查。成员星系密度和弱透镜质量图都表明该星系团由东南和西北两部分组成。二维弱透镜分析表明，东南分量是主团，次团与主团的质量比为$0.32^{+0.75}_{-0.23}$。西北子星系团与主星系团中心的距离为$\sim700$ kpc，它们的相对视向速度为成员星系光谱红移的$\sim1300\,{\rm km s^{-1}}$。X射线辐射主要集中在主团簇周围，而在$1'$半径范围内的子团簇气体质量分数仅为$f_{\mathrm{gas}}=4.0^{+2.3}_{-3.3}\%$，表明子团簇气体被冲压压力剥离。X线余像显示三个弧形多余图案，其中两个对称地位于距X线形态中心$\sim550$ kpc处，另一个靠近X线核心。靠近子星系团的过剩有一个冷锋特征，在那里稠密的冷气体和稀薄的热气体接触。这两个外部的过剩是切向延长约$\sim 450-650$ kpc，表明该集群合并与非零的碰撞参量。多波长数据集显示的总体特征表明，该集群是在第二次或更晚的影响。由于光学定义的合并目录是无偏见的合并促进内集群介质，X射线后续观测将铺平道路，以了解合并物理在各个阶段。
英文摘要：
We represent a joint X-ray, weak-lensing, and optical analysis of the optically-selected merging cluster, HSC J085024+001536, from the Subaru HSC-SSP survey. Both the member galaxy density and the weak-lensing mass map show that the cluster is composed of southeast and northwest components. The two-dimensional weak-lensing analysis shows that the southeast component is the main cluster, and the sub- and main-cluster mass ratio is $0.32^{+0.75}_{-0.23}$. The northwest subcluster is offset by $\sim700$ kpc from the main cluster center, and their relative line-of-sight velocity is $\sim1300\,{\rm km s^{-1}}$ from spectroscopic redshifts of member galaxies. The X-ray emission is concentrated around the main cluster, while the gas mass fraction within a sphere of $1'$ radius of the subcluster is only $f_{\mathrm{gas}}=4.0^{+2.3}_{-3.3}\%$, indicating that the subcluster gas was stripped by ram pressure. X-ray residual image shows three arc-like excess patterns, of which two are symmetrically located at $\sim550$ kpc from the X-ray morphological center, and the other is close to the X-ray core. The excess close to the subcluster has a cold-front feature where dense-cold gas and thin-hot gas contact. The two outer excesses are tangentially elongated about $\sim 450-650$ kpc, suggesting that the cluster is merged with a non-zero impact parameter. Overall features revealed by the multi-wavelength datasets indicate that the cluster is at the second impact or later. Since the optically-defined merger catalog is unbiased for merger boost of the intracluster medium, X-ray follow-up observations will pave the way to understand merger physics at various phases.
Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV Luminosity Functions at $z \sim 4-7$ Derived with the Half-Million Dropouts on the 100 deg$^2$ Sky
A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). II. Physical Properties derived from the SED Fitting with Optical, Infrared, and Radio Data
Starburst Driven Galactic Superbubbles Radiating to 10 K
我们的三维流体动力学模拟的星爆检查形成的超级气泡在一系列的驱动光度和质量负载，确定超级气泡的增长和风速。由此，我们确定了星系风的速度和星暴的能量之间的关系。我们找到了风的形成阈值，在该阈值以上，风速不受网格分辨率或辐射冷却的温度下限的影响。我们调查的效果，两个不同的温度地板在我们的辐射冷却处方风的运动学和内容。我们发现，冷却到$10$ K而不是$10^4$ K增加了银河风中冷中性和热X射线气体的质量分数，而在温暖的H $α$中则减少了一半。我们的模拟表明，冷气体的质量输送到低晕不依赖于星暴的强度。光学上明亮的细丝形成于合并的超级气泡的边缘，或者是寒冷的密集云被风破坏的地方。如果锚定在恒星形成复合体上，由合并超级气泡形成的细丝将持续存在并长到$>400$ pc长。嵌入炽热星系风中的丝状体包含冷暖气体，其移动速度比周围的风慢$300-1200$ km s $^{-1}$，最冷的气体几乎不相对于星系移动。星系风中的冷物质和热物质表现出与观测结果一致的非对称吸收剖面，在风速上有一个薄的尾巴。
DAVOS: Dwarf Active Galactic Nuclei from Variability for the Origins of Seeds: Properties of Variability-Selected Active Galactic Nuclei in the COSMOS Field and Expectations for the Rubin Observatory
Unveiling the mask on the ULIRG-to-QSO transition object [H89]1821+643 at z=0.3: a gas-poor/gas-rich galaxy merger and the implications for CO-based dynamical mass estimates
