The Effect of Environment On Milky Way-Mass Galaxies in a Constrained Simulation of the Local Group
Entidad
UAM. Departamento de Física TeóricaFecha de edición
2015-01-14Cita
10.1088/2041-8205/800/1/L4
Astrophysical Journal Letters 800.1 (2015): L4
ISSN
2041-8205 (print); 2041-8213 (online)DOI
10.1088/2041-8205/800/1/L4Financiado por
The simulation was performed on the MareNostrum cluster in Barcelona. CS and PC acknowledge support from the Leibniz Gemeinschaft through grant SAW-2012-AIP-5 129. SEN acknowledges support from the Deutsche Forschungsgemeinschaft under the grants MU 1020 16-1 and NU 332/2-1, and GY thanks MINECO (Spain) for supporting his research through different projects: AYA2012-31101, FPA2012-34694 and Consolider Ingenio SyeC CSD2007-0050Proyecto
Gobierno de España. AYA2012-31101; Gobierno de España. FPA2012-34694; Gobierno de España. CSD2007-0050Versión del editor
http://dx.doi.org/10.1088/2041-8205/800/1/L4Materias
Galaxies: formation; Galaxies: evolution; Cosmology: theory; Methods: numerical; Astronomía; FísicaNota
Astrophysical Journal Letters 800.1 (2015): L4 reproduced by permission of the AASDerechos
American Astronomical SocietyResumen
In this letter we present, for the first time, a study of star formation rate, gas fraction and galaxy morphology of a constrained simulation of the Milky Way (MW) and Andromeda (M31) galaxies, compared to other MW-mass galaxies. By combining with unconstrained simulations we cover a sufficient volume to compare these galaxies environmental densities ranging from the field to that of the Local Group (LG). This is particularly relevant as it has been shown that, quite generally, galaxy properties depend intimately upon their environment, most prominently when galaxies in clusters are compared to those in the field. For galaxies in loose groups such as the LG, however, environmental effects have been less clear. We consider the galaxy's environmental density in spheres of 1200 kpc (comoving) and find that whilst environment does not appear to directly affect morphology, there is a positive trend with star formation rates. This enhancement in star formation occurs systematically for galaxies in higher density environments, regardless whether they are part of the LG or in filaments. Our simulations suggest that the richer environment at Mpc-scales may help replenish the star-forming gas, allowing higher specific star formation rates in galaxies such as the MW
Lista de ficheros
Google Scholar:Creasey, Peter
-
Scannapieco, Cecilia
-
Nuza, Sebastián E.
-
Yepes Alonso, Gustavo
-
Gottlöber, Stefan
-
Steinmetz, Matthias
Lista de colecciones del ítem
Registros relacionados
Mostrando ítems relacionados por título, autor, creador y materia.