We analyze the formation histories of 19 galaxies from cosmological smoothed
particle hydrodynamics zoom-in resimulations. We construct mock three-colour
images and show that the models reproduce observed trends in the evolution of
galaxy colours and morphologies. However, only a small fraction of galaxies
contains bars. Many galaxies go through phases of central mass growth by
in-situ star formation driven by gas-rich mergers or misaligned gas infall.
These events lead to accretion of low-angular momentum gas to the centres and
leave imprints on the distributions of z=0 stellar circularities, radii and
metallicities as functions of age. Observations of the evolution of structural
properties of samples of disc galaxies at z=2.5-0.0 infer continuous mass
assembly at all radii. Our simulations can only explain this if there is a
significant contribution from mergers or misaligned infall, as expected in a
LambdaCDM universe. Quiescent merger histories lead to high kinematic disc
fractions and inside-out growth, but show little central growth after the last
`destructive' merger at z>1.5. For sufficiently strong feedback, as assumed in
our models, a moderate amount of merging does not seem to be a problem for the
z=0 disc galaxy population, but may rather be a requirement. The average
profiles of simulated disc galaxies agree with observations at z>=1.5. At z<=1,
there is too much growth in size and too little growth in central mass,
possibly due to the under-abundance of bars. The discrepancies may partly be
caused by differences between the star formation histories of the simulations
and those assumed for observations.
Описание
[1404.6926] The diverse formation histories of simulated disc galaxies
%0 Generic
%1 aumer2014diverse
%A Aumer, Michael
%A White, Simon D. M.
%A Naab, Thorsten
%D 2014
%K disk sfh simulation
%R 10.1093/mnras/stu818
%T The diverse formation histories of simulated disc galaxies
%U http://arxiv.org/abs/1404.6926
%X We analyze the formation histories of 19 galaxies from cosmological smoothed
particle hydrodynamics zoom-in resimulations. We construct mock three-colour
images and show that the models reproduce observed trends in the evolution of
galaxy colours and morphologies. However, only a small fraction of galaxies
contains bars. Many galaxies go through phases of central mass growth by
in-situ star formation driven by gas-rich mergers or misaligned gas infall.
These events lead to accretion of low-angular momentum gas to the centres and
leave imprints on the distributions of z=0 stellar circularities, radii and
metallicities as functions of age. Observations of the evolution of structural
properties of samples of disc galaxies at z=2.5-0.0 infer continuous mass
assembly at all radii. Our simulations can only explain this if there is a
significant contribution from mergers or misaligned infall, as expected in a
LambdaCDM universe. Quiescent merger histories lead to high kinematic disc
fractions and inside-out growth, but show little central growth after the last
`destructive' merger at z>1.5. For sufficiently strong feedback, as assumed in
our models, a moderate amount of merging does not seem to be a problem for the
z=0 disc galaxy population, but may rather be a requirement. The average
profiles of simulated disc galaxies agree with observations at z>=1.5. At z<=1,
there is too much growth in size and too little growth in central mass,
possibly due to the under-abundance of bars. The discrepancies may partly be
caused by differences between the star formation histories of the simulations
and those assumed for observations.
@misc{aumer2014diverse,
abstract = {We analyze the formation histories of 19 galaxies from cosmological smoothed
particle hydrodynamics zoom-in resimulations. We construct mock three-colour
images and show that the models reproduce observed trends in the evolution of
galaxy colours and morphologies. However, only a small fraction of galaxies
contains bars. Many galaxies go through phases of central mass growth by
in-situ star formation driven by gas-rich mergers or misaligned gas infall.
These events lead to accretion of low-angular momentum gas to the centres and
leave imprints on the distributions of z=0 stellar circularities, radii and
metallicities as functions of age. Observations of the evolution of structural
properties of samples of disc galaxies at z=2.5-0.0 infer continuous mass
assembly at all radii. Our simulations can only explain this if there is a
significant contribution from mergers or misaligned infall, as expected in a
LambdaCDM universe. Quiescent merger histories lead to high kinematic disc
fractions and inside-out growth, but show little central growth after the last
`destructive' merger at z>1.5. For sufficiently strong feedback, as assumed in
our models, a moderate amount of merging does not seem to be a problem for the
z=0 disc galaxy population, but may rather be a requirement. The average
profiles of simulated disc galaxies agree with observations at z>=1.5. At z<=1,
there is too much growth in size and too little growth in central mass,
possibly due to the under-abundance of bars. The discrepancies may partly be
caused by differences between the star formation histories of the simulations
and those assumed for observations.},
added-at = {2014-04-29T07:39:14.000+0200},
author = {Aumer, Michael and White, Simon D. M. and Naab, Thorsten},
biburl = {https://www.bibsonomy.org/bibtex/2b44ff551e5de9bbeafc864bfaaaf536b/miki},
description = {[1404.6926] The diverse formation histories of simulated disc galaxies},
doi = {10.1093/mnras/stu818},
interhash = {d1b17c51993a9fb7cf722585b1223ee4},
intrahash = {b44ff551e5de9bbeafc864bfaaaf536b},
keywords = {disk sfh simulation},
note = {cite arxiv:1404.6926Comment: 19 pages, 13 figures, accepted for publication in MNRAS},
timestamp = {2014-04-29T07:39:14.000+0200},
title = {The diverse formation histories of simulated disc galaxies},
url = {http://arxiv.org/abs/1404.6926},
year = 2014
}