Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies

We study the stellar discs and spheroids in eight simulations of galaxy formation within Milky Way mass haloes in a Λ cold dark matter cosmology. The first paper in this series concentrated on disc properties. Here we extend this analysis to study how the formation history, structure and dynamics of...

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Detalles Bibliográficos
Publicado: 2011
Materias:
Cosmology: theory
Galaxies: evolution
Galaxies: formation
Galaxies: structure
Methods: numerical
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v417_n1_p154_Scannapieco
http://hdl.handle.net/20.500.12110/paper_00358711_v417_n1_p154_Scannapieco
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00358711_v417_n1_p154_Scannapieco
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spelling paper:paper_00358711_v417_n1_p154_Scannapieco2023-06-08T15:01:31Z Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies Cosmology: theory Galaxies: evolution Galaxies: formation Galaxies: structure Methods: numerical We study the stellar discs and spheroids in eight simulations of galaxy formation within Milky Way mass haloes in a Λ cold dark matter cosmology. The first paper in this series concentrated on disc properties. Here we extend this analysis to study how the formation history, structure and dynamics of discs and spheroids relate to the assembly history and structure of their haloes. We find that discs are generally young, with stars spanning a wide range of stellar age: the youngest stars define thin discs and have near-circular orbits, while the oldest stars form thicker discs that rotate ∼2 times slower than the thin components, and have 2-3 times larger velocity dispersions. Unlike the discs, spheroids form early and on short time-scales, and are dominated by velocity dispersion. We find great variety in their structure. The inner regions are bar- or bulge-like, while the extended outer haloes are rich in complex non-equilibrium structures such as stellar streams, shells and clumps. Our discs have very high in situ fractions, i.e. most of their stars formed in the disc itself. Nevertheless, there is a non-negligible contribution (∼15 per cent) from satellites that are accreted on nearly coplanar orbits. The inner regions of spheroids also have relatively high in situ fractions, but 65-85 per cent of their outer stellar population is accreted. We analyse the circular velocities, rotation velocities and velocity dispersions of our discs and spheroids, both for gas and stars, showing that the dynamical structure is complex as a result of the non-trivial interplay between cooling and supernova heating. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v417_n1_p154_Scannapieco http://hdl.handle.net/20.500.12110/paper_00358711_v417_n1_p154_Scannapieco
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Cosmology: theory
Galaxies: evolution
Galaxies: formation
Galaxies: structure
Methods: numerical
spellingShingle Cosmology: theory
Galaxies: evolution
Galaxies: formation
Galaxies: structure
Methods: numerical
Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies
topic_facet Cosmology: theory
Galaxies: evolution
Galaxies: formation
Galaxies: structure
Methods: numerical
description We study the stellar discs and spheroids in eight simulations of galaxy formation within Milky Way mass haloes in a Λ cold dark matter cosmology. The first paper in this series concentrated on disc properties. Here we extend this analysis to study how the formation history, structure and dynamics of discs and spheroids relate to the assembly history and structure of their haloes. We find that discs are generally young, with stars spanning a wide range of stellar age: the youngest stars define thin discs and have near-circular orbits, while the oldest stars form thicker discs that rotate ∼2 times slower than the thin components, and have 2-3 times larger velocity dispersions. Unlike the discs, spheroids form early and on short time-scales, and are dominated by velocity dispersion. We find great variety in their structure. The inner regions are bar- or bulge-like, while the extended outer haloes are rich in complex non-equilibrium structures such as stellar streams, shells and clumps. Our discs have very high in situ fractions, i.e. most of their stars formed in the disc itself. Nevertheless, there is a non-negligible contribution (∼15 per cent) from satellites that are accreted on nearly coplanar orbits. The inner regions of spheroids also have relatively high in situ fractions, but 65-85 per cent of their outer stellar population is accreted. We analyse the circular velocities, rotation velocities and velocity dispersions of our discs and spheroids, both for gas and stars, showing that the dynamical structure is complex as a result of the non-trivial interplay between cooling and supernova heating. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.
title Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies
title_short Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies
title_full Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies
title_fullStr Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies
title_full_unstemmed Formation history, structure and dynamics of discs and spheroids in simulated Milky Way mass galaxies
title_sort formation history, structure and dynamics of discs and spheroids in simulated milky way mass galaxies
publishDate 2011
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v417_n1_p154_Scannapieco
http://hdl.handle.net/20.500.12110/paper_00358711_v417_n1_p154_Scannapieco
_version_ 1768544677092392960

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