The kinematics of the planetary nebulae in the Large Magellanic Cloud
Citations Over TimeTop 10% of 1988 papers
Abstract
The radial velocities of a total of 94 planetary nebulae (PN) in the Large Magellanic Cloud (LMC) have been determined. This kinematics of the population of planetary nebulae is compared with the H I data in the context of a reanalysis of the survey by Rohlfs et al., taking into account the transverse velocity of the LMC. We find that the best solution for this transverse velocity is 275+/-65 km s^-1^ and that the LMC is near perigalacticon. This is consistent with a maximum Galactic mass of order 4.5 x 10^11^ M_sun_ out to 51 kpc. The rotation curve obtained after correction for this velocity implies a mass of (4.6+/-0.3) x 10^9^ M_sun_ within a radius of 3^deg^, or about 6 x 10^9^ M_sun_, total. The rotation solution for the PN population is essentially identical with that of the H I but the vertical velocity dispersion of 19.1 km s^-1^ is much greater than the value of 5.4 km s^-1^ found for the H I. This increase in velocity dispersion is consistent with it being the result of orbital heating and diffusion operating in the LMC in a manner essentially identical with that found for the solar neighborhood.
Related Papers
- → Radial velocity measurements in the Pleiades(1991)32 cited
- → RADIAL VELOCITIES OF THREE POORLY STUDIED CLUSTERS AND THE KINEMATICS OF OPEN CLUSTERS(2014)20 cited
- → Measurement of radial velocities and velocity dispersion of stars in circumnuclear regions of galaxies using the 2D spectrosopy technique(2001)
- → A multi-wavelength investigation of newly discovered planetary nebulae in the Large Magellanic Cloud: Central stars(2012)
- → Radial Velocity Study of NGC 6712(1988)