The Dynamics of the Large Magellanic Cloud Periphery: Mass Limit and Polar Ring

Details The Dynamics of the Large Magellanic Cloud Periphery: Mass Limit and Polar Ring The Dynamics of the Large Magellanic Cloud Periphery: Mass Limit and Polar Ring

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...488l.129k&link_type=abstract

Astrophysical Journal Letters v.488, p.L129

Astronomy and Astrophysics

Astrophysics

61

Scientific paper

Radial velocities of 759 carbon stars on the periphery of the LMC are used to determine the rotation curve from 3 to 12 kpc. After a peak of 42 km s-1 at 4 kpc, the velocities decline to 35 km s-1 at 6.5 kpc, suggesting that 90% of the LMC's matter lies inside this radius. The rising velocities seen at larger radii are explained by particle-particle N-body simulations as arising from tidal interactions between LMC and both the SMC and the Galaxy. For an inclination of 33 deg; the mass contained within a 5 kpc radius is 6.2+/-0.9 x 109 Msolar. An upper limit on the LMC halo mass is determined.

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