Counterrotating core in the LMC: accretion and or merger

Subramaniam, A; Prabhu, T. P

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dc.contributor.author	Subramaniam, A
dc.contributor.author	Prabhu, T. P
dc.date.accessioned	2009-09-11T14:18:03Z
dc.date.available	2009-09-11T14:18:03Z
dc.date.issued	2007-05-24
dc.identifier.citation	De Jong, R. S. ed., Island Universes: structure and evolution of disk galaxies., Astrophysics and space science proceedings; Vol. 3., pp. 83 - 88	en
dc.identifier.isbn	978-1-4020-5572-0
dc.identifier.issn	1570-6591
dc.identifier.uri	http://hdl.handle.net/2248/4815
dc.description	The original publication is available at springerlink.com
dc.description	Restricted Access
dc.description.abstract	The stellar radial velocity in the central region of the Large Magellanic Cloud (LMC) is used to estimate the radial velocity curve along various position angles (PA) including the line of nodes (LON). The central part of the radial velocity profile along the LON shows a V-shaped profile instead of a straight line profile. This is a clear indication of counterrotation. To explain the observed velocity profile, we propose the existence of two disks in the inner LMC, with one coun-terrotating. This two disk model is found to match the Hi velocities as well. The presence of a counter-rotating core could be due to internal (secondary bar) / external (gas accretion) origin.	en
dc.language.iso	en	en
dc.publisher	Springer	en
dc.relation.ispartofseries	Astrophysics and Space Science Proceedings; Vol. 3
dc.relation.uri	http://www.springerlink.com/content/u234u75j45005323/	en
dc.rights	© Springer	en
dc.subject	Counterrotating Core	en
dc.subject	LMC	en
dc.subject	Stellar Radial Velocity	en
dc.subject	Large Magellanic Cloud	en
dc.subject	Line of Nodes	en
dc.title	Counterrotating core in the LMC: accretion and or merger	en
dc.type	Article	en