Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ∼ 1–2
Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ∼ 1–2
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DOI：
10.3847/1538-4357/835/2/153
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发表时间：
2016-11
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影响因子：
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通讯作者：
M. Fossati;D. Wilman;J. Mendel;R. Saglia;A. Galametz;A. Beifiori;R. Bender;J. Chan;M. Fabricius-M.
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文献类型：
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作者：
M. Fossati;D. Wilman;J. Mendel;R. Saglia;A. Galametz;A. Beifiori;R. Bender;J. Chan;M. Fabricius-M.
我们公开提供了一个校准的环境措施，在五个三维哈勃太空望远镜（HST）/CANDELS深场星系的目录。利用光谱和棱镜的红移从3D-HST调查，多波长测光从CANDELS，和更广泛的领域的公共数据的边缘校正，我们得出密度在固定的光圈来表征环境的星系明亮的红移范围内比mag。通过将观测到的星系与模拟样本联系起来，选择模拟样本来重现3D-HST样本选择和红移精度，每个3D-HST星系都被分配了宿主晕质量的概率密度函数，以及它是中央星系还是卫星星系的概率。同样的过程也适用于从斯隆数字巡天中选择的z = 0样本。我们计算的被动中心和卫星星系的恒星和晕质量的函数，和红移的分数，然后推导出的星系，被淬火的环境特定的过程的分数。利用模拟样本，我们估计了卫星猝灭的时间尺度在较低的恒星质量或较低的红移下较长，但与晕质量显著无关。这表明，在3D-HST样本中常见的环境范围内（），在没有宇宙吸积的情况下，卫星因其气体储存库的耗尽而熄灭。我们发现，淬火时间可以分为一个延迟阶段，在此期间，卫星星系的行为类似于中心在固定的恒星质量，和一个阶段的星星形成率迅速下降（陀螺仪），如前所示，在z = 0。我们的结论是，这种情况下需要卫星星系保持一个大水库的多相气体吸积后，即使在高红移，这种气体维持星星形成的长时间淬火观察。
We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-Hubble Space Telescope (HST)/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multiwavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than mag in the redshift range . By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that it is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from Sloan Digital Sky Survey. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is it is longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample ( ), satellites are quenched by exhaustion of their gas reservoir in the absence of cosmological accretion. We find that the quenching times can be separated into a delay phase, during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly ( Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.