Milky Way type galaxies in a ΛcDM cosmology

We analyse a sample of 52 000 Milky Way (MW) type galaxies drawn from the publicly available galaxy catalogue of the Millennium Simulation with the aim of studying statistically the differences and similarities of their properties in comparison to our Galaxy. Model galaxies are chosen to lie in halo...

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Detalles Bibliográficos
Publicado:	2009
Materias:	Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: formation
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v395_n1_p210_DeRossi http://hdl.handle.net/20.500.12110/paper_00358711_v395_n1_p210_DeRossi
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00358711_v395_n1_p210_DeRossi
record_format	dspace
spelling	paper:paper_00358711_v395_n1_p210_DeRossi2023-06-08T15:01:26Z Milky Way type galaxies in a ΛcDM cosmology Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: formation We analyse a sample of 52 000 Milky Way (MW) type galaxies drawn from the publicly available galaxy catalogue of the Millennium Simulation with the aim of studying statistically the differences and similarities of their properties in comparison to our Galaxy. Model galaxies are chosen to lie in haloes with maximum circular velocities in the range 200-250 km s -1 and to have bulge-to-disc ratios similar to that of the MW. We find that model MW galaxies formed 'quietly' through the accretion of cold gas and small satellite systems. Only ≈12 per cent of our model galaxies experienced a major merger during their lifetime. Most of the stars formed 'in situ', with only about 15 per cent of the final mass gathered through accretion. Supernovae (SNe) and active galactic nuclei (AGN) feedback play an important role in the evolution of these systems. At high redshifts, when the potential wells of the MW progenitors are shallower, winds driven by SNe explosions blow out a large fraction of the gas and metals. As the systems grow in mass, SNe feedback effects decrease and AGN feedback takes over, playing a more important role in the regulation of the star formation activity at lower redshifts. Although model MW galaxies have been selected to lie in a narrow range of maximum circular velocities, they nevertheless exhibit a significant dispersion in the final stellar masses and metallicities. Our analysis suggests that this dispersion results from the different accretion histories of the parent dark matter haloes. Statistically, we also find evidences to support the MW as a typical Sb/Sc galaxy in the same mass range, providing a suitable benchmark to constrain numerical models of galaxy formation. © 2009 RAS. 2009 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v395_n1_p210_DeRossi http://hdl.handle.net/20.500.12110/paper_00358711_v395_n1_p210_DeRossi
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: abundances Galaxies: evolution Galaxies: formation
spellingShingle	Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: formation Milky Way type galaxies in a ΛcDM cosmology
topic_facet	Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: formation
description	We analyse a sample of 52 000 Milky Way (MW) type galaxies drawn from the publicly available galaxy catalogue of the Millennium Simulation with the aim of studying statistically the differences and similarities of their properties in comparison to our Galaxy. Model galaxies are chosen to lie in haloes with maximum circular velocities in the range 200-250 km s -1 and to have bulge-to-disc ratios similar to that of the MW. We find that model MW galaxies formed 'quietly' through the accretion of cold gas and small satellite systems. Only ≈12 per cent of our model galaxies experienced a major merger during their lifetime. Most of the stars formed 'in situ', with only about 15 per cent of the final mass gathered through accretion. Supernovae (SNe) and active galactic nuclei (AGN) feedback play an important role in the evolution of these systems. At high redshifts, when the potential wells of the MW progenitors are shallower, winds driven by SNe explosions blow out a large fraction of the gas and metals. As the systems grow in mass, SNe feedback effects decrease and AGN feedback takes over, playing a more important role in the regulation of the star formation activity at lower redshifts. Although model MW galaxies have been selected to lie in a narrow range of maximum circular velocities, they nevertheless exhibit a significant dispersion in the final stellar masses and metallicities. Our analysis suggests that this dispersion results from the different accretion histories of the parent dark matter haloes. Statistically, we also find evidences to support the MW as a typical Sb/Sc galaxy in the same mass range, providing a suitable benchmark to constrain numerical models of galaxy formation. © 2009 RAS.
title	Milky Way type galaxies in a ΛcDM cosmology
title_short	Milky Way type galaxies in a ΛcDM cosmology
title_full	Milky Way type galaxies in a ΛcDM cosmology
title_fullStr	Milky Way type galaxies in a ΛcDM cosmology
title_full_unstemmed	Milky Way type galaxies in a ΛcDM cosmology
title_sort	milky way type galaxies in a λcdm cosmology
publishDate	2009
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v395_n1_p210_DeRossi http://hdl.handle.net/20.500.12110/paper_00358711_v395_n1_p210_DeRossi
_version_	1768543886094893056

Milky Way type galaxies in a ΛcDM cosmology

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