Journal
ASTRONOMY & ASTROPHYSICS
Volume 545, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201219472
Keywords
galaxies: star clusters: individual: R136; Magellanic Clouds; stars: kinematics and dynamics; globular clusters: general
Categories
Funding
- European Southern Observatory [182.D-0222]
- Scottish Universities Physics Alliance (SUPA)
- Natural Science and Engineering Research Council of Canada (NSERC)
- Royal Society
- DFG cluster of excellence Origin and Structure of the Universe
- Spanish Government Ministerio de Educacion y Ciencia [AYA2010-15081, AYA2010-17631]
- Consejeria de Educacion of the Junta de Andalucia [P08-TIC-4075]
- Bulgarian NSF [DO 02-85]
- STFC [ST/G002355/1, ST/J000035/1, ST/J001384/1, PP/D000955/1, PP/F000057/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/G002355/1, ST/J000035/1, PP/D000955/1, ST/J001384/1, PP/F000057/1] Funding Source: researchfish
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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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