Formation and settling of a disc galaxy during the last 8 billion years in a cosmological simulation
We present results of a high-resolution zoom cosmological simulation of the evolution of a low-mass galaxy with a maximum velocity of V ≃ 100 km s−1 at z ≃ 0, using the initial conditions from the AGORA project (Kim et al.). The final disc-dominated galaxy is consistent with local disc scaling relat...
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| Main Author: | |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
02 February 2017
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2017, Volume: 467, Issue: 3, Pages: 2664-2672 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stx289 |
| Online Access: | Verlag, kostenfrei, Volltext: http://dx.doi.org/10.1093/mnras/stx289
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| Author Notes: | Daniel Ceverino, Joel Primack, Avishai Dekel and Susan A. Kassin |
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| 520 | |a We present results of a high-resolution zoom cosmological simulation of the evolution of a low-mass galaxy with a maximum velocity of V ≃ 100 km s−1 at z ≃ 0, using the initial conditions from the AGORA project (Kim et al.). The final disc-dominated galaxy is consistent with local disc scaling relations, such as the stellar-halo mass relation and the baryonic Tully-Fisher. The galaxy evolves from a compact, dispersion-dominated galaxy into a rotation-dominated but dynamically hot disc in about 0.5 Gyr (from z = 1.4 to 1.2). The disc dynamically cools down for the following 7 Gyr, as the gas velocity dispersion decreases over time, in agreement with observations. The primary cause of this slow evolution of velocity dispersion in this low-mass galaxy is stellar feedback. It is related to the decline in gas fraction, and to the associated gravitational disc instability, as the disc slowly settles from a global Toomre Q > 1 turbulent disc to a marginally unstable disc (Q ≃ 1). | ||
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