RE-ASSEMBLING THE SAGITTARIUS DWARF GALAXY

被引：119

作者：

Niederste-Ostholt, M. ^{[1
]}

Belokurov, V. ^{[1
]}

Evans, N. W. ^{[1
]}

Penarrubia, J. ^{[1
]}

机构：

[1] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 712卷 / 01期

基金：

英国科学技术设施理事会; 美国国家航空航天局; 美国国家科学基金会;

关键词：

galaxies: dwarf; galaxies: individual (Sagittarius); DIGITAL SKY SURVEY; DARK-MATTER HALOS; SPHEROIDAL GALAXY; LOCAL GROUP; MILKY-WAY; GALACTIC HALO; SURVEY VIEW; TIDAL STREAMS; STARS; SDSS;

D O I：

10.1088/0004-637X/712/1/516

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

What was the mass of the progenitor of the Sagittarius (Sgr) dwarf galaxy? Here, we reassemble the stellar debris using Sloan Digital Sky Survey and Two Micron All-Sky Survey data to find the total luminosity and likely mass. We find that the luminosity is in the range (9.6-13.2) x 10(7) L(circle dot) or M(V) similar to -15.1 to -15.5, with 70% of the light residing in the debris streams. The progenitor is somewhat fainter than the present-day Small Magellanic Cloud, and comparable in brightness to the M31 dwarf spheroidals NGC 147 and NGC 185. Using cosmologically motivated models, we estimate that the mass of Sgr's dark matter halo prior to tidal disruption was similar to 10(10) M(circle dot).

引用

页码：516 / 526

页数：11

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