The Evolution of the Stellar Mass Functions of Star-Forming and Quiescent Galaxies to z = 4 from the COSMOS/UltraVISTA Survey
Adam Muzzin, Danilo Marchesini, Mauro Stefanon, Marijn Franx, Henry J. McCracken, Bo Milvang-Jensen, James S. Dunlop, J. P. U. Fynbo, Gabriel Brammer, Ivo Labbe, Pieter van Dokkum
备注：
18 pages paper, 12 pages appendix, 23 figures. Accepted for publication in the ApJ
我们目前的恒星质量函数（SMF）的恒星形成和静止星系z = 4使用的样本中的95 675个星系的COSMOS/UltraVISTA字段的测量。从DR 1 UltraVISTA K_{s}波段成像中选择了源，该波段成像覆盖了宽区域（1.62 deg^2）到显著深度（K_{s,tot} = 23.4）的独特组合。合并后的星族的SMF与先前的测量结果非常一致，表明宇宙的恒星质量密度在z = 0.75、2.0和3.5时分别只有当前值的50%、10%和1%。静止的星族驱动了大部分的整体增长，这些星系的恒星质量密度从z = 3.5开始增加了2.71^{+0.93}_{-0.22} dex。在z > 2.5时，恒星形成星系在所有恒星质量的总SMF中占主导地位，尽管静止星系的非零种群持续到z = 4。K_{s}选择的恒星形成星系SMF与紫外选择的SMF在2.5 < z 3.5的比较< 4 show reasonable agreement and suggests UV-selected samples are representative of the majority of the stellar mass density at z >。我们估计的平均质量增长的个别星系选择星系在固定的累积数密度。在z = 0.3时Log（M_{*} / M_{sun}）= 11.5的星系，平均质量自z = 2.0（3.5）起只增长了0.2 dex（0.3 dex），而Log（M_{*} / M_{sun}）= 10.5的星系自z = 2起增长了> 1.0 dex。在z < 2时，质量增长的时间导数对于较低质量的星系总是较大的，这表明星系中的质量增长是由红移决定的，并且主要是自下而上的。最后，我们研究了SMF的系统不确定性的潜在来源，并发现那些从photo-z模板，SPS建模，和静止星系的定义占主导地位的SMF的总误差预算。
英文摘要：
We present measurements of the stellar mass functions (SMFs) of star-forming and quiescent galaxies to z = 4 using a sample of 95 675 galaxies in the COSMOS/UltraVISTA field. Sources have been selected from the DR1 UltraVISTA K_{s}-band imaging which covers a unique combination of a wide area (1.62 deg^2), to a significant depth (K_{s,tot} = 23.4). The SMFs of the combined population are in good agreement with previous measurements and show that the stellar mass density of the universe was only 50%, 10% and 1% of its current value at z ~ 0.75, 2.0, and 3.5, respectively. The quiescent population drives most of the overall growth, with the stellar mass density of these galaxies increasing by 2.71^{+0.93}_{-0.22} dex since z = 3.5. At z > 2.5, star-forming galaxies dominate the total SMF at all stellar masses, although a nonzero population of quiescent galaxies persists to z = 4. Comparisons of the K_{s}-selected star-forming galaxy SMFs to UV-selected SMFs at 2.5 < z < 4 show reasonable agreement and suggests UV-selected samples are representative of the majority of the stellar mass density at z > 3.5. We estimate the average mass growth of individual galaxies by selecting galaxies at fixed cumulative number density. The average galaxy with Log(M_{*}/M_{sun}) = 11.5 at z = 0.3 has grown in mass by only 0.2 dex (0.3 dex) since z = 2.0(3.5), whereas those with Log(M_{*}/M_{sun}) = 10.5 have grown by > 1.0 dex since z = 2. At z < 2, the time derivatives of the mass growth are always larger for lower-mass galaxies, which demonstrates that the mass growth in galaxies since that redshift is mass-dependent and primarily bottom-up. Lastly, we examine potential sources of systematic uncertainties on the SMFs and find that those from photo-z templates, SPS modeling, and the definition of quiescent galaxies dominate the total error budget in the SMFs.
Mass assembly in quiescent and star-forming galaxies since z=4 from UltraVISTA
我们估计了0.2<z<4的恒星形成星系和静止星系的星系质量函数和恒星质量密度。我们构建了一个深K<24的样本220000星系选择使用UltraVISTA DR 1数据发布。我们的分析是基于精确的30波段光度红移。通过将这些测光红移与来自zCOSMOS亮巡天和暗巡天的10800个光谱红移进行比较，我们发现在i<22.5时，sigma（dz/（1+z））=0.008，在1.5<z 10^10.7 Msun时，sigma（dz/（1+zs））=0.03<4. We derive the stellar mass function and correct for the Eddington bias. We find a mass-dependent evolution of the global and star-forming populations. This mass-dependent evolution is a direct consequence of the star formation being quenched in galaxies more massive than M>。对于静止星系的质量函数，我们没有发现z<1的高质量端有任何显著的演化;但是我们观察到暗端斜率明显变平。从z~3到z~1，静止星系的密度在整个质量范围内增加。它们的同向恒星质量…
A Strongly-Lensed Massive Ultra-Compact Quiescent Galaxy at z ~ 2.4 in the COSMOS/UltraVISTA Field
We report the discovery of a massive ultra-compact quiescent galaxy that has been strongly-lensed into multiple images by a foreground galaxy at z = 0.960. This system was serendipitously discovered as a set of extremely Ks-bright high-redshift galaxies with red J - Ks colors using new data from the UltraVISTA YJHKs near-infrared survey. The system was also previously identified as an optically-faint lens/source system using the COSMOS ACS imaging by Faure et al. (2008, 2011). Photometric redshifts for the three brightest images of the source galaxy determined from twenty-seven band photometry…
Spitzer Matching survey of the UltraVISTA ultra-deep Stripes (SMUVS): Full-mission IRAC Mosaics and Catalogs
本文介绍了新的深3.6和4.5微米成像的三个UltraVISTA近红外探测条纹内的COSMOS领域。这些观测是用斯皮策的红外线阵列相机（IRAC）进行的，用于斯皮策对Ultra-VISTA深条纹的匹配调查（SMUVS）。在这项工作中，我们提出了我们的数据减少技术，并记录所产生的马赛克，覆盖地图，目录在两个IRAC通带的三个最东端的UltraVISTA调查条纹，覆盖约0.66平方度的组合面积，其中0.45平方度至少有20小时的集成时间。SMUVS在3.6和4.5微米处达到约25.0 AB mag的点源灵敏度，具有4-sigma的显著性，占调查灵敏度和源混淆。在这个极限下，SMUVS星表总共包含大约350，000个源，每个源至少在一个IRAC波段中被显著检测到。由于其均匀和高灵敏度，相对较大的区域覆盖范围，以及COSMOS提供的广泛的辅助数据，SMUVS调查将有助于大量的宇宙学研究。我们将通过斯皮策科学中心公开提供本文所述的所有图像和目录。
Using precise galaxy stellar mass function measurements in the COSMOS field we determine the stellar-to-halo mass relationship (SHMR) using a parametric abundance matching technique. The unique combination of size and highly complete stellar mass estimates in COSMOS allows us to determine the SHMR over a wide range of halo masses from $z\sim0.2$ to $z\sim5$. At $z\sim 0.2$ the ratio of stellar-to-halo mass content peaks at a characteristic halo mass $M_{\rm h} =10^{12} M_\odot$ and declines at higher and lower halo masses. This characteristic halo mass increases with redshift reaching $M_{\rm …
Spitzer bright, UltraVISTA faint sources in COSMOS: the contribution to the overall population of massive galaxies at z=3-7
我们分析了UltraVISTA超深COSMOS场上574个斯皮策4.5微米选择星系的样本，[4.5] <23 and Ks_auto>24（AB）。我们的目标是调查这些中红外明亮，近红外暗淡的来源是否对红移z>=3的大质量星系的总体人口有显着贡献。通过使用多达30个光度带进行光谱能量分布（SED）分析，我们已经确定了我们的样品峰的红移分布在红移z~2.5-3.0，约32%的星系位于z>=3。我们研究了在高红移下这些源对星系恒星质量函数（GSMF）的贡献。我们发现，[4.5]<23，Ks_auto>24的星系对先前在3=<z<4时Ks_auto<24的源所确定的GSMF产生的变化可以忽略不计，但在4=<z<5时它们的贡献更重要，占恒星质量Mst>~6 x 10^10 Msun的星系的>~50%。我们还将GSMF限制在z>=5时的最高质量端（Mst>~2 x 10^11 Msun）。根据它们在5=<z<6处的存在，以及在较高红移处的实际不存在，我们可以相当精确地确定第一个最大质量星系出现的时刻发生在z~6和z~5之间的约0.2 Gyr的时间内。或者，如果非常大的星系在宇宙时间的早期就存在，它们应该被大量的尘埃遮蔽，从而超出当前大面积深近红外探测的探测极限。
This paper seeks to test if the large-scale galaxy distribution can be characterized as a fractal system. Tools appropriate for describing galaxy fractal structures with a single fractal dimension $D$ in relativistic settings are developed and applied to the UltraVISTA galaxy survey. A graph of volume-limited samples corresponding to the redshift limits in each redshift bins for absolute magnitude is presented. Fractal analysis using the standard $Λ$CDM cosmological model is applied to a reduced subsample in the range $0.1\le z \le 4$, and the entire sample within $0.1\le z\le 6$. Three relati…
Quiescent Compact Galaxies at Intermediate Redshift in the COSMOS Field II. The Fundamental Plane of Massive Galaxies
我们研究了宇宙场中中等红移静止星系的表面亮度、速度色散和基本面$-$大小之间的关系。COSMOS样本由平均速度色散为$σ\sim 250$ km s $^{-1}$的$\sim150$大质量静止星系组成，红移在$0.2<z<0.8$之间。样本中超过一半的星系是紧凑的。COSMOS星系的表面亮度、速度色散和大小之间存在紧密的关系（$\sim0.1$ dex散射）。在速度色散和大小的固定组合下，COSMOS星系比本地宇宙中的星系更亮。这些表面亮度偏移与静止坐标系的$g-z$颜色和$D_n4000$指数相关;蓝色星系和那些具有较小$D_n4000$指数的星系具有较大的偏移。星族合成模型表明，大质量的宇宙星系比本地宇宙中同样大质量的静止星系更年轻，因此更明亮。被动演化单独带来了巨大的紧凑的静止宇宙星系的本地基本平面在$z = 0$。因此，大质量致密静止星系自$z\sim1$以来的尺寸或速度色散演化受到在基本面观测到的小散射的限制。我们的结论是，在$z\lesssim1$的大规模紧凑的静止星系是不是一个特殊的一类对象，而是正常的静止星系人口的质量和大小分布的尾巴。
COSMOS-Web galaxy groups: Evolution of red sequence and quiescent galaxy fraction
University of Bologna（博洛尼亚大学）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所空间天文观测站）；Zentrum für Astronomie, Universität Heidelberg（海德堡大学天体物理中心）；Institut für Theoretische Physik, Universität Heidelberg（海德堡大学理论物理研究所）；INFN – Sezione di Bologna（意大利国家核物理研究所博洛尼部分会）；Aalto University（阿尔托大学）；University of Helsinki（赫尔辛基大学）；University of California, Riverside（加州大学河滨分校）
We investigate spectroscopic properties of galaxy systems identified based on deep X-ray observations in the COSMOS field. The COSMOS X-ray system catalog we use George et al. (2011) includes 180 X-ray systems to a limiting flux of $1.0 \times 10^{-15}$ erg cm$^{-2}$ s$^{-1}$, an order of magnitude deeper than future e-ROSITA survey. We identify spectroscopic members of these X-ray systems based on the spectroscopic catalog constructed by compiling various spectroscopic surveys including 277 new measurements; 137 X-ray systems are spectroscopically identified groups with more than three spectr…
A Large Population of Massive Compact Post-Starburst Galaxies at z>1: Implications for the Size Evolution and Quenching Mechanism of Quiescent Galaxies
我们通过一个0<z<2的年轻和年老静止星系样本的数密度和结构演化来研究红色序列的增长。这些星系是从宇宙演化巡天（COSMOS）领域的NEWFIRM中带巡天（NMBS）中选出的。我们发现了大量的大质量年轻星系，这些星系在z>1时刚刚熄灭（“后星爆”），而在z<1时几乎不存在;它们的数密度在z=2时为5 x 10^{-5} Mpc^{-3}，而在z=0.5时要小10倍。在z>1时，观测到的年轻和年老静止星系的数密度与一个简单的模型相一致，在这个模型中，所有年老静止星系都曾被认为是后星暴星系。我们发现，总体人口的静止星系有较小的尺寸和略长的形状在较高的红移，与其他最近的研究。有趣的是，最近在1<z<2处淬灭的星系并不比那些红移的老星系大，甚至可能更小。这一结果与静止星系的平均大小的演化主要是由较大的恒星形成星系的连续转变驱动的观点不一致：在这种情况下，最年轻的静止星系也是最大的。相反，合并或其他机制似乎需要解释从z=2到现在的静止星系的大小增长。
The Deep Extragalactic VIsible Legacy Survey (DEVILS) is an ongoing high-completeness, deep spectroscopic survey of $\sim$60,000 galaxies to Y$<$21.2 mag, over $\sim$6 deg2 in three well-studied deep extragalactic fields: D10 (COSMOS), D02 (XMM-LSS) and D03 (ECDFS). Numerous DEVILS projects all require consistent, uniformly-derived and state-of-the-art photometric data with which to measure galaxy properties. Existing photometric catalogues in these regions either use varied photometric measurement techniques for different facilities/wavelengths leading to inconsistencies, older imaging data a…
Galaxy evolution is driven by a variety of physical processes which are predicted to proceed at different rates for different dark matter haloes and environments across cosmic times. A record of this evolution is preserved in galaxy stellar populations, which we can access using absorption-line spectroscopy. Here we explore the large LEGA-C survey (DR3) to investigate the role of the environment and stellar mass on stellar populations at z~0.6-1.0 in the COSMOS field. Leveraging the statistical power and depth of LEGA-C, we reveal significant gradients in D4000 and H-delta equivalent widths (E…
On the unique evolutionary mechanisms of massive quiescent galaxies in the epoch of reionisation
Swinburne University of Technology（斯威本科技大学）；JWST Australia Data Centre [JADC], Swinburne Advanced Manufacturing and Design Centre [AMDC]（JWST澳大利亚数据中心，斯威本先进制造与设计中心）
We study how star formation is regulated in low-mass field dwarf galaxies ($10^5 \leq M_{\star} \leq 10^6 \, \text{M}_{\odot}$), using cosmological high-resolution ($3 \, \text{pc}$) hydrodynamical simulations. Cosmic reionization quenches star formation in all our simulated dwarfs, but three galaxies with final dynamical masses of $3 \times 10^{9} \,\text{M}_{\odot}$ are subsequently able to replenish their interstellar medium by slowly accreting gas. Two of these galaxies re-ignite and sustain star formation until the present day at an average rate of $10^{-5} \, \text{M}_{\odot} \, \text{yr…
The FourStar Galaxy Evolution Survey (ZFOURGE): ultraviolet to far-infrared catalogs, medium-bandwidth photometric redshifts with improved accuracy, stellar masses, and confirmation of quiescent galaxies to z~3.5
pop-cosmos: Galaxy size evolution across structural and star-formation classifications in COSMOS-Web
Institute of Astronomy, University of Cambridge（剑桥大学天体物理学研究所）；Cavendish Laboratory, Department of Physics, University of Cambridge（剑桥大学物理学院卡文迪许实验室）；The Oskar Klein Centre, Department of Physics, Stockholm University（斯德哥尔摩大学物理学院奥斯卡·克莱因中心）；Astrophysics Group, Imperial College London（伦敦帝国理工学院天体物理学组）；Department of Mathematics, Imperial College London（伦敦帝国理工学院数学系）；Research Computing Services, University of Cambridge（剑桥大学研究计算服务）
