PRIMUS: An observationally motivated model to connect the evolution of the AGN and galaxy populations out to z~1
James Aird, Alison L. Coil, John Moustakas, Aleksandar M. Diamond-Stanic, Michael R. Blanton, Richard J. Cool, Daniel J. Eisenstein, Kenneth C. Wong, Guangtun Zhu
备注：
11 pages, 5 figures, emulateapj format, updated to match version accepted for publication in ApJ
We present an observationally motivated model to connect the AGN and galaxy populations at 0.2<z<1.0 and predict the AGN X-ray luminosity function (XLF). We start with measurements of the stellar mass function of galaxies (from the Prism Multi-object Survey) and populate galaxies with AGNs using models for the probability of a galaxy hosting an AGN as a function of specific accretion rate. Our model is based on measurements indicating that the specific accretion rate distribution is a universal function across a wide range of host stellar mass with slope gamma_1 = -0.65 and an overall normalization that evolves with redshift. We test several simple assumptions to extend this model to high specific accretion rates (beyond the measurements) and compare the predictions for the XLF with the observed data. We find good agreement with a model that allows for a break in the specific accretion rate distribution at a point corresponding to the Eddington limit, a steep power-law tail to super-Eddington ratios with slope gamma_2 = -2.1 +0.3 -0.5, and a scatter of 0.38 dex in the scaling between black hole and host stellar mass. Our results show that samples of low luminosity AGNs are dominated by moderately massive galaxies (M* ~ 10^{10-11} M_sun) growing with a wide range of accretion rates due to the shape of the galaxy stellar mass function rather than a preference for AGN activity at a particular stellar mass. Luminous AGNs may be a severely skewed population with elevated black hole masses relative to their host galaxies and in rare phases of rapid accretion.
The coevolution of the velocity and mass functions of galaxies and dark haloes
我们采用偏差校正的丰度匹配技术，调查的LCDM暗晕质量函数（HMF），观测导出的速度色散和恒星质量函数（VDF，SMF）的z=1和0之间的星系的共同演化。我们首次使用Chae（2010）通过强透镜统计约束的VDF演化进行星系-晕丰度匹配研究。作为本地基准，我们使用了两个z ~ 0 VDF（基于SDSS DR 5的Monte-Carlo实现的VDF和基于SDSS DR 6的直接测量的VDF）。然后，我们专注于连接的VDF演化的HMF演化预测的N体模拟和SMF演化星系调查的约束。在VDF-HMF联系上，我们发现局域暗晕维里质量-中心恒星速度色散（Mvir-sigma）关系与已被研究的低红移暗晕的个别性质吻合得很好，并且VDF演化与HMF演化密切平行，意味着Mvir-sigma关系几乎没有演化.在VDF-SMF联系上，把丰度匹配结果与其他独立观测结果和流体动力学模拟结果结合起来，恒星质量-恒星速度色散（Mstar-sigma）关系也可能演化不大。我们的研究结果支持的简单的图片，作为晕层次的增长，恒星质量和中央恒星速度色散平行增长。我们讨论了这种平行的共同演化的星系形成和演化下的LCDM范式的可能影响。
Multiprobe cosmology forecasts from halo-occupation-distribution-based forward modeling of galaxy and void statistics
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Physics, University of Arizona（亚利桑那大学物理系）；Aix-Marseille Université, CNRS/IN2P3, CPPM（艾克斯-马赛大学，法国国家科学研究中心/法国国家核子和粒子物理研究所，粒子与宇宙学中心）；Department of Astrophysical Sciences, Peyton Hall, Princeton University（普林斯顿大学天体物理学系）；Universitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-Universität（慕尼黑大学天文台，慕尼黑大学物理学院）
The shape alignment of satellite galaxies in galaxy pairs in SDSS
无论是在模拟还是观测中，都已经表明，一个大星系的潮汐场可以扭转它的卫星星系，使得卫星星系的主轴指向它们的宿主。这种所谓的“形状排列”在孤立的银河系中被观察到，但在“本星系群”中却没有。在这项研究中，我们调查的星系对的卫星星系的形状排列类似于斯隆数字巡天数据发布13（SDSS DR 13）中确定的本星系群。通过在主星系对周围堆叠数万个卫星星系，我们发现了两个统计上很强的对齐信号。(1)卫星星系的主轴位于两原色之间的（投影）面积（{ \it面向}区域）倾向于垂直于连接卫星和其主机的线（切向对准），而（2）卫星星系的主轴位于远离另一个主星系的区域（{ \it远离}区域）倾向于与连接卫星到其主机的线对准（径向对准）。这些比对在$\sim5σ$水平得到证实。对准信号随着主亮度的增加、对间隔的减小和卫星距离的减小而增加。对准信号也被发现在非常规环境中更强。这些发现将有助于理解潮汐场对星系对中卫星星系的影响机制，并有助于在弱引力透镜分析中研究星系的内在排列。
Luminosity-Dependent Assembly Bias of Central Galaxies from Weak Lensing and Clustering
Shanghai Jiao Tong University（上海交通大学）；Graduate School of Science, Nagoya University（名古屋大学理学研究科）；Kobayashi-Maskawa Institute for the Origin of Particles and the Universe (KMI), Nagoya University（名古屋大学小林-益川粒子宇宙起源研究所）；Institute for Advanced Research, Nagoya University（名古屋大学高等研究院）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学理化学研究所 Kavli 宇宙粒子物理学研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Lorentz Institute for Theoretical Physics, Leiden University（莱顿大学洛伦兹理论物理研究所）；Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理研究所）
The Galaxy--Halo Connection in High-Redshift Universe: Details and Evolution of Stellar-to-Halo Mass Ratios of Lyman Break Galaxies on CFHTLS Deep Fields
