Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
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2014-07
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en
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EDP Sciences
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Atribution 4.0 International (CC BY 4.0)
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https://creativecommons.org/licenses/by/4.0/deed.es
Resumen
Context. The standard disc formation scenario postulates that the disc forms as the gas cools and flows into the centre of the dark
matter halo, conserving the specific angular momentum. Major mergers have been shown to be able to destroy or highly perturb
the disc components. More recently, the alignment of the material that is accreted to form the galaxy has been pointed out as a key
ingredient to determine galaxy morphology. However, in a hierarchical scenario galaxy formation is a complex process that combines
these processes and others in a non-linear way so that the origin of galaxy morphology remains to be fully understood.
Aims. We aim at exploring the differences in the formation histories of galaxies with a variety of morphologies, but quite recent
merger histories, to identify which mechanisms are playing a major role. We analyse when minor mergers can be considered relevant
to determine galaxy morphology. We also study the specific angular momentum content of the disc and central spheroidal components
separately.
Methods. We used cosmological hydrodynamical simulations that include an effective, physically motivated supernova feedback that
is able to regulate the star formation in haloes of different masses. We analysed the morphology and formation history of a sample
of 15 galaxies of a cosmological simulation. We performed a spheroid-disc decomposition of the selected galaxies and their progenitor
systems. The angular momentum orientation of the merging systems as well as their relative masses were estimated to analyse the
role played by orientation and by minor mergers in the determination of the morphology.
Results. We found the discs to be formed by conserving the specific angular momentum in accordance with the classical disc forma tion model. The specific angular momentum of the stellar central spheroid correlates with the dark matter halo angular momentum and
determines a power law. Our results suggest that gas accretion to rebuild the disc component is a necessary but not sufficient ingredient
for a disc-dominated galaxy in a hierarchical clustering scenario. The survival of the discs is tightly linked to their subsequent history
of accretion, as previously reported. Minor mergers play an important role. It is more likely that they will destroy the disc and feed
the central spheroid if their angular momentum is misaligned with respect to that of the main galaxy. Conversely, if they are aligned,
they can contribute to the disc formation.
Notas
Indexación Scopus.
Palabras clave
Galaxies: Formation, Galaxies: Evolution, Galaxies: Structure
Citación
Astronomy and Astrophysics. Volume 567. July 2014. Article number A47
DOI
10.1051/0004-6361/201323079