The Magellanic Edges Survey I: Description and first results

被引：20
作者：
Cullinane, L. R. [1 ]
Mackey, A. D. [1 ]
Da Costa, G. S. [1 ]
Koposov, S. E. [2 ,3 ]
Belokurov, V [2 ]
Erkal, D. [4 ]
Koch, A. [5 ]
Kunder, A. [6 ]
Nataf, D. M. [7 ,8 ]
机构：
[1] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia
[2] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England
[3] Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA
[4] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England
[5] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12, D-69120 Heidelberg, Germany
[6] St Martins Univ, 5000 Abbey Way SE, Lacey, WA 98503 USA
[7] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA
[8] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 497卷 / 03期
基金：
美国国家航空航天局; 澳大利亚研究理事会; 美国国家科学基金会;
关键词：
stars: kinematics and dynamics; galaxies: kinematics and dynamics; Magellanic Clouds; galaxies: stellar content; galaxies: structure; CHEMICAL ENRICHMENT HISTORY; RED GIANTS; TRIPLET SPECTROSCOPY; STELLAR STREAMS; CLOUD STRUCTURE; LMC CLUSTERS; TOTAL MASS; VMC SURVEY; MILKY-WAY; DYNAMICS;
D O I：
10.1093/mnras/staa2048
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present an overview of, and first science results from, the Magellanic Edges Survey (MagES), an ongoing spectroscopic survey mapping the kinematics of red clump and red giant branch stars in the highly substructured periphery of the Magellanic Clouds. In conjunction with Gaia astrometry, MagES yields a sample of similar to 7000 stars with individual 3D velocities that probes larger galactocentric radii than most previous studies. We outline our target selection, observation strategy, data reduction, and analysis procedures, and present results for two fields in the northern outskirts (>10 degrees on-sky from the centre) of the Large Magellanic Cloud (LMC). One field, located in the vicinity of an arm-like overdensity, displays apparent signatures of perturbation away from an equilibrium disc model. This includes a large radial velocity dispersion in the LMC disc plane, and an asymmetric line-of-sight velocity distribution indicative of motions vertically out of the disc plane for some stars. The second field reveals 3D kinematics consistent with an equilibrium disc, and yields V-circ = 87.7 +/- 8.0 km s(-1) at a radial distance of similar to 10.5 kpc from the LMC centre. This leads to an enclosed mass estimate for the LMC at this radius of (1.8 +/- 0.3) x 10(10) M-circle dot.
引用
收藏
页码：3055 / 3075
页数：21
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