期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 450, 期 3, 页码 2327-2353出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv740
关键词
galaxies: elliptical and lenticular; cD; galaxies: evolution; galaxies: formation; galaxies: kinematics and dynamics; galaxies: spiral
资金
- ISF [24/12, 1829/12]
- GIF [G-1052-104.7/2009]
- DIP
- I-CORE Program of the PBC
- NSF [AST-1010033, AST-1405962]
- MINECO [AYA2012-31101]
- MICINN [AYA-2009-13875-C03-02]
- Juan-de-la-Cierva fellowship
We use cosmological simulations to study a characteristic evolution pattern of high-redshift galaxies. Early, stream-fed, highly perturbed, gas-rich discs undergo phases of dissipative contraction into compact, star-forming systems ('blue' nuggets) at z similar to 4-2. The peak of gas compaction marks the onset of central gas depletion and inside-out quenching into compact ellipticals (red nuggets) by z similar to 2. These are sometimes surrounded by gas rings or grow extended dry stellar envelopes. The compaction occurs at a roughly constant specific star formation rate (SFR), and the quenching occurs at a constant stellar surface density within the inner kpc (I (1)) pound. Massive galaxies quench earlier, faster, and at a higher I (1) pound than lower mass galaxies, which compactify and attempt to quench more than once. This evolution pattern is consistent with the way galaxies populate the SFR-size-mass space, and with gradients and scatter across the main sequence. The compaction is triggered by an intense inflow episode, involving (mostly minor) mergers, counter-rotating streams or recycled gas, and is commonly associated with violent disc instability. The contraction is dissipative, with the inflow rate > SFR, and the maximum I (1) pound anticorrelated with the initial spin parameter. The central quenching is triggered by the high SFR and stellar/supernova feedback (maybe also active galactic nucleus feedback) due to the high central gas density, while the central inflow weakens as the disc vanishes. Suppression of fresh gas supply by a hot halo allows the long-term maintenance of quenching once above a threshold halo mass, inducing the quenching downsizing.
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