The VLT-FLAMES Tarantula Survey VI. Evidence for rotation of the young massive cluster R136

被引：50
|
作者：
Henault-Brunet, V. [1 ]
Gieles, M. [2 ]
Evans, C. J. [1 ,3 ]
Sana, H. [4 ]
Bastian, N. [5 ]
Maiz Apellaniz, J. [6 ]
Taylor, W. D. [1 ]
Markova, N. [7 ]
Bressert, E. [8 ,9 ,10 ]
de Koter, A. [4 ]
van Loon, J. Th. [11 ]
机构：
[1] Univ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland
[2] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[3] Royal Observ Edinburg, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland
[4] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands
[5] Tech Univ Munich, D-85748 Garching, Germany
[6] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain
[7] Bulgarian Acad Sci, Inst Astron NAO, Smoljan 4700, Bulgaria
[8] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England
[9] European So Observ, D-87548 Garching, Germany
[10] Harvard Smithsonian CfA, Cambridge, MA 02138 USA
[11] Keele Univ, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England
来源：
ASTRONOMY & ASTROPHYSICS | 2012年 / 545卷
基金：
加拿大自然科学与工程研究理事会;
关键词：
galaxies: star clusters: individual: R136; Magellanic Clouds; stars: kinematics and dynamics; globular clusters: general; LARGE-MAGELLANIC-CLOUD; SPHERICAL STELLAR-SYSTEMS; GLOBULAR-CLUSTERS; 30; DORADUS; DYNAMICAL EVOLUTION; OMEGA-CENTAURI; STAR-CLUSTERS; STABILITY; COLLAPSE; GALAXIES;
D O I：
10.1051/0004-6361/201219472
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Although it has important ramifications for both the formation of star clusters and their subsequent dynamical evolution, rotation remains a largely unexplored characteristic of young star clusters (few Myr). Using multi-epoch spectroscopic data of the inner regions of 30 Doradus in the Large Magellanic Cloud obtained as part of the VLT-FLAMES Tarantula Survey, we search for rotation of the young massive cluster R136. From the radial velocities of 36 apparently single O-type stars within a projected radius of 10 pc from the centre of the cluster, we find evidence, at the 95% confidence level, for rotation of the cluster as a whole. We use a maximum likelihood method to fit simple rotation curves to our data and find a typical rotational velocity of similar to 3 km s(-1). When compared to the low velocity dispersion of R136, our result suggests that star clusters may form with at least similar to 20% of the kinetic energy in rotation.
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页数：5
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