An Upper Limit on the Milky Way Mass from the Orbit of the Sagittarius Dwarf Satellite

被引：32

作者：

Dierickx, Marion I. P. ^{[1
]}

Loeb, Abraham ^{[1
]}

机构：

[1] Harvard Univ, Astron Dept, 60 Garden St, Cambridge, MA 02138 USA

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 847卷 / 01期

关键词：

galaxies: interactions; Galaxy: kinematics and dynamics; Galaxy: halo; Local Group; ALL-SKY SURVEY; DARK-MATTER HALO; GALACTIC HALO; SURVEY VIEW; SPHEROIDAL GALAXY; DENSITY PROFILE; TIDAL STREAMS; STELLAR MASS; ORIGIN; STARS;

D O I：

10.3847/1538-4357/aa8767

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

As one of the most massive Milky Way (MW) satellites, the Sagittarius dwarf galaxy played an important role in shaping the Galactic disk and stellar halo morphologies. The disruption of Sagittarius over several close-in passages has populated the halo of our Galaxy with large-scale tidal streams and offers a unique diagnostic tool for measuring its gravitational potential. Here, we test different progenitor mass models for the MW and Sagittarius by modeling the full infall of the satellite. We constrain the mass of the Galaxy based on the kinematics of the satellite remnant and multiple tidal streams of Sagittarius. Our semianalytic modeling of the orbital dynamics agrees with full N-body simulations, and favors low values for the MW mass, less than or similar to 10(12) M-circle dot. This conclusion eases the tension between Lambda CDM and the observed parameters of the MW satellites.

引用

页数：10

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