The Morphologies of Massive Galaxies at 1<z<3 in the CANDELS-UDS Field: Compact Bulges, and the Rise and Fall of Massive Disks
The Morphologies of Massive Galaxies at 1<z<3 in the CANDELS-UDS Field: Compact Bulges, and the Rise and Fall of Massive Disks
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DOI：
10.1111/j.1365-2966.2012.22087.x
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发表时间：
2012-06
期刊：
影响因子：
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通讯作者：
V. Bruce;J. Dunlop;M. Cirasuolo;M. Cirasuolo;R. McLure;T. Targett;E. Bell;D. Croton;A. Dekel-A.
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文献类型：
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作者：
V. Bruce;J. Dunlop;M. Cirasuolo;M. Cirasuolo;R. McLure;T. Targett;E. Bell;D. Croton;A. Dekel-A.
摘要我们利用高分辨率的HST WFC 3/IR近红外成像对CANDELS-UDS场中1 < z < 3处的200个最大质量（M* > 1011 M *）星系的形态进行了详细的膨胀盘分解。我们发现，虽然这种大规模的星系在低红移一般是膨胀为主，在红移1 - 2，他们大多是磁盘为主。有趣的是，我们发现，虽然大多数的静止星系是膨胀为主，一个显着的分数（25-40%）的最静止的星系，有磁盘为主的形态。因此，我们的研究结果表明，淬火恒星形成活动的物理机制并不简单地连接到那些负责大质量星系的形态转变。
Abstract We have used high-resolution, HST WFC3/IR, near-infrared imaging to conduct a detailed bulge-disk decomposition of the morphologies of ≃ 200 of the most massive (M* > 1011 M⊙) galaxies at 1 < z < 3 in the CANDELS-UDS field. We find that, while such massive galaxies at low redshift are generally bulge-dominated, at redshifts 1 2 they are mostly disk-dominated. Interestingly, we find that while most of the quiescent galaxies are bulge-dominated, a significant fraction (25–40%) of the most quiescent galaxies, have disk-dominated morphologies. Thus, our results suggest that the physical mechanisms which quench star-formation activity are not simply connected to those responsible for the morphological transformation of massive galaxies.