Feedback and the formation of dwarf galaxy stellar haloes

被引：109

作者：

Stinson, G. S. ^{[1
,2
]}

Dalcanton, J. J. ^{[1
]}

Quinn, T. ^{[1
]}

Gogarten, S. M. ^{[1
]}

Kaufmann, T. ^{[3
]}

Wadsley, J. ^{[3
]}

机构：

[1] Univ Washington, Dept Astron, Seattle, WA 98195 USA

[2] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada

[3] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2009年 / 395卷 / 03期

基金：

瑞士国家科学基金会;

关键词：

methods: N-body simulations; galaxies: evolution; galaxies: formation; STAR-FORMATION HISTORY; LARGE-MAGELLANIC-CLOUD; DARK-MATTER HALOES; POLAR RING GALAXY; LOCAL GROUP; IRREGULAR GALAXY; SPHEROIDAL GALAXY; METALLICITY DISTRIBUTION; SPATIAL-DISTRIBUTION; WFPC2; OBSERVATIONS;

D O I：

10.1111/j.1365-2966.2009.14555.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Stellar population studies show that low-mass galaxies in all environments exhibit stellar haloes that are older and more spherically distributed than the main body of the galaxy. In some cases, there is a significant intermediate age component that extends beyond the young disc. We examine a suite of Smoothed Particle Hydrodynamic simulations and find that elevated early star formation activity combined with supernova feedback can produce an extended stellar distribution that resembles these haloes for model galaxies ranging from nu(200) = 15 to 35 km s(-1), without the need for accretion of subhaloes.

引用

页码：1455 / 1466

页数：12

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