Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers
Entidad
UAM. Departamento de Física TeóricaEditor
Oxford University PressFecha de edición
2015-03-11Cita
10.1093/mnras/stu2694
Monthly Notices of Royal Astronomical Society 447.4 (2015): 3291-3210
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stu2694Financiado por
This work was partly supported, by MINECO grant AYA2012-31101, by MICINN grant AYA-2009-13875-C03-02, by ISF grant 24/12, by GIF grant G-1052-104.7/2009, by a DIP grant, by NSF grant AST-1010033, and by the I-CORE Program of the PBC and the ISF grant 1829/12. DC is a Juan de la Cierva fellowProyecto
Gobierno de España. AYA2012-31101; Gobierno de España. AYA-2009-13875-C03-02Versión del editor
http://dx.doi.org/10.1093/mnras/stu2694Materias
Cosmology; Galaxies: evolution; Galaxies: formation; FísicaNota
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedDerechos
© 2015 The AuthorsResumen
We address the formation of massive stellar spheroids between redshifts z = 4 and 1 using a suite of AMR hydro-cosmological simulations. The spheroids form as bulges, and the spheroid mass growth is partly driven by violent disc instability (VDI) and partly by mergers. A kinematic decomposition to disc and spheroid yields that the mass fraction in the spheroid is between 50% and 90% and is roughly constant in time, consistent with a cosmological steady
state of VDI discs that are continuously fed from the cosmic web. The density profile of the spheroid is typically “classical”, with a Sersic index n = 4.5 ± 1, independent of whether it grew by mergers or VDI and independent of the feedback strength. The disc is characterized
by n = 1.5±0.5, and the whole galaxy by n = 3±1. The high-redshift spheroids are compact due to the dissipative inflow of gas and the high universal density. The stellar surface density within the effective radius of each galaxy as it evolves remains roughly constant in time after its first growth. For galaxies of a fixed stellar mass, the surface density is higher at higher redshifts
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Google Scholar:Ceverino Rodríguez, Daniel
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Dekel, Avishai
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Tweed, Dylan
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Primack, Joel
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