Formation of proto-globular cluster candidates in cosmological simulations of dwarf galaxies at z > 4

被引：11

作者：

Sameie, Omid ^{[1
]}

Boylan-Kolchin, Michael ^{[1
]}

Hopkins, Philip F. ^{[2
]}

Wetzel, Andrew ^{[3
]}

Ma, Xiangcheng ^{[4
,5
]}

Bullock, James S. ^{[6
]}

El-Badry, Kareem ^{[7
,8
]}

Quataert, Eliot ^{[9
]}

Samuel, Jenna ^{[1
]}

Schauer, Anna T. P. ^{[1
]}

Weisz, Daniel R. ^{[4
,5
]}

机构：

[1] Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA

[2] CALTECH, TAPIR, Pasadena, CA 95616 USA

[3] Univ Calif Davis, Dept Phys & Astron, Davis, CA 95616 USA

[4] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[5] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA

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

[7] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[8] Harvard Soc Fellows, 78 Mt Auburn St, Cambridge, MA 02138 USA

[9] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 522卷 / 02期

基金：

美国国家科学基金会;

关键词：

methods: numerical; galaxies: evolution; galaxies: formation; galaxies: high- redshift; galaxies: starclusters: general; DARK-MATTER HALOS; INITIAL MASS FUNCTION; GIANT MOLECULAR CLOUDS; BURSTY STAR-FORMATION; MILKY-WAY; HIGH-REDSHIFT; FORMATION HISTORIES; COSMIC TIME; ERIDANUS II; FIRE;

D O I：

10.1093/mnras/stad1071

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We perform cosmological hydrodynamical simulations to study the formation of proto-globular cluster candidates in progenitors of present-day dwarf galaxies ( M-vir approximate to 10(10) M-circle dot at z = 0) as part of the 'Feedback in Realistic Environment' (FIRE) project. Compact ( r (1/2) < 30 pc), relatively massive (0.5 x 10 (5) less than or similar to M-*/M-circle dot less than or similar to 5 x 10 (5) ), self-bound stellar clusters form at 11 greater than or similar to 5 in progenitors with M (vi)r approximate to 10(9) M-circle dot. Cluster formation is triggered when at least 10 7 Me of dense, turbulent gas reaches Egas 104 Me pc-2 as a result of the compressive effects of supernova feedback or from cloud-cloud collisions. The clusters can survive for 2 - 3 Gyr ; absent numerical effects, they could possibly survive substantially longer, perhaps to z = 0. The longest lived clusters are those that form at significant distance - several hundreds of pc - from their host galaxy. We therefore predict that globular clusters forming in progenitors of present-day dwarf galaxies will be offset from any pre-existing stars within their host dark matter haloes as opposed to deeply embedded within a well-defined galaxy. Properties of the nascent clusters are consistent with observations of some of the faintest and most compact high-redshift sources in Hubble Space Telescope lensing fields and are at the edge of what will be detectable as point sources in deep imaging of non-lensed fields with JWST. By contrast, the star clusters' host galaxies will remain undetectable.

引用

页码：1800 / 1813

页数：14

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