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>NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY-GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1*
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NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY-GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1*
Using data from the COSMOS survey, we perform the first joint analysis of galaxy-galaxy weak lensing, galaxy spatial clustering, and galaxy number densities. Carefully accounting for sample variance and for scatter between stellar and halo mass, we model all three observables simultaneously using a novel and self-consistent theoretical framework. Our results provide strong constraints on the shape and redshift evolution of the stellar-to-halo mass relation (SHMR) from z = 0.2 to z = 1. At low stellar mass, we find that halo mass scales as Mh ∝M 0.46 * and that this scaling does not evolve significantly with redshift from z = 0.2 to z = 1. The slope of the SHMR rises sharply at M * 5 × 1010 M ☉ and as a consequence, the stellar mass of a central galaxy becomes a poor tracer of its parent halo mass. We show that the dark-to-stellar ratio, Mh /M *, varies from low to high masses, reaching a minimum of Mh /M * ~ 27 at M * = 4.5 × 1010 M ☉ and Mh = 1.2 × 1012 M ☉. This minimum is important for models of galaxy formation because it marks the mass at which the accumulated stellar growth of the central galaxy has been the most efficient. We describe the SHMR at this minimum in terms of the "pivot stellar mass," M piv *, the "pivot halo mass," M piv h , and the "pivot ratio," (Mh /M *)piv. Thanks to a homogeneous analysis of a single data set spanning a large redshift range, we report the first detection of mass downsizing trends for both M piv h and M piv *. The pivot stellar mass decreases from M piv * = 5.75 ± 0.13 × 1010 M ☉ at z = 0.88 to M piv * = 3.55 ± 0.17 × 1010 M ☉ at z = 0.37. Intriguingly, however, the corresponding evolution of M piv h leaves the pivot ratio constant with redshift at (Mh /M *)piv ~ 27. We use simple arguments to show how this result raises the possibility that star formation quenching may ultimately depend on Mh /M * and not simply on Mh , as is commonly assumed. We show that simple models with such a dependence naturally lead to downsizing in the sites of star formation. Finally, we discuss the implications of our results in the context of popular quenching models, including disk instabilities and active galactic nucleus feedback.
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机译：使用来自COSMOS调查的数据，我们对星系-星系弱透镜，星系空间聚类和星系数密度进行了首次联合分析。仔细考虑样本差异以及恒星和晕圈质量之间的分散，我们使用新颖且自洽的理论框架同时对所有三个可观测对象进行建模。我们的结果对恒星与晕质量关系（SHMR）从z = 0.2到z = 1的形状和红移演化提供了强大的约束。在低恒星质量下，我们发现晕质量标度为Mh ∝M 0.46 *和从z = 0.2到z = 1的红移，该缩放比例不会显着发展。SHMR的斜率在M *> 5×1010 M☉时急剧上升，结果，中央星系的恒星质量变成了不良的示踪剂它的母晕质量。我们表明，暗星比Mh / M *从低到高变化，在M * = 4.5×1010 M☉和Mh = 1.2×1012 M reaching时达到最小值Mh / M *〜27 。该最小值对于星系形成模型很重要，因为它标志着中央星系累积的恒星生长最有效的质量。我们以“枢轴恒星质量”，M piv *，“枢轴晕质量”，M piv h和“枢轴比率”（Mh / M *）piv来描述最小的SHMR。由于对跨越大红移范围的单个数据集进行了均质分析，我们报告了首次检测到M piv h和M piv *的质量缩减趋势。枢轴恒星质量从z = 0.88时的M piv * = 5.75±0.13×1010 M decreases降低到z = 0.37时的M piv * = 3.55±0.17×1010 M☉。然而，有趣的是，M piv h的相应演化使枢轴比保持不变，在（Mh / M *）piv〜27处有红移。我们使用简单的论点来证明这一结果如何提高恒星形成淬灭可能最终取决于Mh的可能性。 / M *，而不是通常假设的Mh。我们表明，具有这种依赖性的简单模型自然会导致恒星形成部位的尺寸缩小。最后，我们在流行的淬灭模型（包括磁盘不稳定性和活跃的银河核反馈）的背景下讨论了结果的含义。
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