星系核中的耗散和额外光：IV。椭球标度关系的演化
Dissipation and Extra Light in Galactic Nuclei: IV. Evolution in the Scaling Relations of Spheroids
摘要：
我们发展了一个模型的起源和红移演化的球体标度关系。我们考虑球体的大小，速度色散，质量，轮廓形状（Sersic指数），和黑洞（BH）的质量，以及它们相关的标度。我们的方法结合了晕占据模型和流体动力学合并模拟中的观测约束的优势。这使我们能够分离耗散，干合并，形成时间和祖先进化的相对作用，并确定它们对标度在每个红移的影响。耗散是决定球体大小和基本平面（FP）缩放的最重要因素，并且可以解释FP倾斜以及圆盘和球体缩放之间的差异。因为在高z的圆盘有更高的气体分数，合并更富含气体，产生更紧凑的球状体。这预测了球体大小的质量依赖性演化，与观测结果一致。这与FP的微妙演变有关，这对假设固定的内在FP的研究很重要。这也预测了BH-宿主相关性的温和演变，在更高的z下朝向更大的BH。干合并是有意义的，但只适用于早期形成的大质量系统：它们形成紧凑，但经历干合并（与观测一致），使得它们的尺寸在后来的时间类似于最近形成的类似质量的球体。我们对所观察到的致密高z球体的后代进行建模：大多数将成为BCGs的核心，其大小，速度分散度和BH质量与观测结果一致，但我们确定了一小部分可能完好地存活到z=0。
英文摘要：
We develop a model for the origins and redshift evolution of spheroid scaling relations. We consider spheroid sizes, velocity dispersions, masses, profile shapes (Sersic indices), and black hole (BH) masses, and their related scalings. Our approach combines advantages of observational constraints in halo occupation models and hydrodynamic merger simulations. This allows us to separate the relative roles of dissipation, dry mergers, formation time, and progenitor evolution, and identify their effects on scalings at each redshift. Dissipation is the most important factor determining spheroid sizes and fundamental plane (FP) scalings, and can account for the FP tilt and differences between disk and spheroid scalings. Because disks at high-z have higher gas fractions, mergers are more gas-rich, yielding more compact spheroids. This predicts mass-dependent evolution in spheroid sizes, in agreement with observations. This relates to subtle evolution in the FP, important to studies that assume a fixed intrinsic FP. This also predicts mild evolution in BH-host correlations, towards larger BHs at higher z. Dry mergers are significant, but only for massive systems which form early: they form compact, but undergo dry mergers (consistent with observations) such that their sizes at later times are similar to spheroids of similar mass formed more recently. We model descendants of observed compact high-z spheroids: most will become cores of BCGs, with sizes, velocity dispersions, and BH masses consistent with observations, but we identify a fraction that might survive to z=0 intact.
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