TY - JOUR
T1 - Formation and settling of a disc galaxy during the last 8 billion years in a cosmological simulation
AU - Ceverino, Daniel
AU - Primack, Joel
AU - Dekel, Avishai
AU - Kassin, Susan A.
N1 - Publisher Copyright:
© 2017 The Authors.
PY - 2017/6/1
Y1 - 2017/6/1
N2 - We present results of a high-resolution zoom cosmological simulation of the evolution of a lowmass 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).
AB - We present results of a high-resolution zoom cosmological simulation of the evolution of a lowmass 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).
KW - Galaxies: evolution
KW - Galaxies: formation
UR - http://www.scopus.com/inward/record.url?scp=85040240835&partnerID=8YFLogxK
U2 - 10.1093/mnras/stx289
DO - 10.1093/mnras/stx289
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AN - SCOPUS:85040240835
SN - 0035-8711
VL - 467
SP - 2664
EP - 2672
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -