Galaxy scaling relations, which describe a connection between ostensibly unrelated physical characteristics of galaxies, testify to an underlying order in galaxy formation that requires understanding. I review the development of a scaling relation that 1) unites the well-known Fundamental Plane (FP) relation of giant elliptical galaxies and Tully-Fisher (TF) relation of disk galaxies, 2) fits low mass spheroidal galaxies, including the ultra-faint satellites of our Galaxy, 3) explains the apparent shift of lenticular (S0) galaxies relative to both FP or TF, 3) describes all stellar dynamical systems, including systems with no dark matter (stellar clusters), 4) associates explicitly the numerical coefficients that account for the apparent "tilt" of the FP away from the direct expectation drawn from the virial theorem with systematic variations in the total mass-to-light ratio of galaxies within the half-light radius, 5) connects with independent results that demonstrate the robustness of mass estimators when applied at the half-light radius, and 6) results in smaller scatter for disk galaxies than the TF relation. The relation develops naturally from the virial theorem, but implies the existence of additional galaxy formation physics that must now be a focus of galaxy formation studies. More pragmatically, the relation provides a lynchpin that can be used to measure distances and galaxy masses. I review two applications: 1) the cross-calibration of distance measurement methods, and 2) the determination of mass-to-light ratios of simple stellar populations as a function of age, and implications of the latter for the stellar initial mass function.
Stellar Kinematics and Structural Properties of Virgo Cluster Dwarf Early-Type Galaxies from the SMAKCED Project. I. Kinematically Decoupled Cores and Implications for Infallen Groups in Clusters
Tracing ionized gas kinematics in Lyman-Break Analogs. Implications for star formation compactness and outflow properties
Universidad de La Serena（拉塞雷纳大学）；Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理研究所）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理学研究中心）；INAF - Osservatorio Astronomico di Roma（意大利国家天文台罗马天文台）；Michigan Institute for Data Science, University of Michigan（密歇根大学数据科学研究所）
Radio galaxies in galaxy groups: kinematics, scaling relations and AGN feedback
我们调查了一个大的（N=998）样本的COSMOS光谱星系成员分布在79组的运动学性质。我们确定了Brilliant Group Galeries（BGG），并将我们的数据与1.4 GHz的VLA-COSMOS深度调查进行交叉匹配，将我们的母样本分类为无线电/非无线电BGG和无线电/非无线电卫星。射电光度分布从$L_R\sim2\times10^{21}$ W Hz $^{-1}$到$L_R\sim3\times$ 10 $^{25}$ W Hz $^{-1}$。通过比较速度比（视线速度除以群速度色散）与星系群中心偏移量进行的相空间分析表明，BGG（无线电和非无线电）大多数（$\sim$ 80\%）是古老的infaller。此外，最强的（$L_R>10^{23}$ W Hz $^{-1}$）射电星系总是在距离群中心0.2 $R_{\rm vir}$以内。将我们的样本与HORIZON-AGN进行比较，我们发现模拟星系的速度和偏移量与无线电BGG比非无线电BGG更相似，尽管统计测试仍然突出了模拟和真实物体之间的显着差异。我们发现，广播BGG更有可能被托管在高质量的群体。最后，我们观察到BGG射电星系的功率与宿主群的X射线温度$T_{\rm x}$和X射线光度$L_{\rm x}$之间的相关性。这支持组内介质和中央无线电源之间的链路的存在。在星系群中心出现的强大射电星系可以用混沌冷吸积来…
