2003/06/30 by K. Weis, Kerstin Weis · 4 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Extinction (optical mineralogy) #Galaxies: Formation, Evolution, Phenomena #Large Magellanic Cloud #Milky Way #Planetary nebula #Spectral line #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20030921
published as Astron.Astrophys.408:205-230,2003 · paper accepted by A&A, 25 pages, 24 figures; paper with images in full resolution available at http://www.astro.ruhr-uni-bochum.de/kweis/publications.html
arxiv created 2003/07/10 · openalex publication_date 2003/08/22 · arxiv updated 2010/05/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present a detailed analysis of the morphology and kinematics of nebulae around LBVs and LBV candidates in the Large Magellanic Cloud. HST images and high-resolution Echelle Spectra were used to determine the size, shape, brightness, and expansion velocities of the LBV nebulae around R 127, R 143, and S 61. For S Dor, R 71, R 99, and R 84 we discuss the possible presence of nebular emission, and derive upper limits for the size and lower limits on the expansion velocities of possible nebulae. Including earlier results for the LBV candidates S 119 and Sk we find that in general the nebulae around LBVs in the LMC are comparable in size to those found in the Milky Way. The expansion velocities of the LMC nebulae, however, are significantly lower – by about a factor of 3 to 4 – than those of galactic nebulae of comparable size. Galactic and LMC nebulae show about the same diversity of morphologies, but only in the LMC do we find nebulae with outflow. Bipolarity – at least to some degree – is found in nebulae in the LMC as well as in the Milky Way, and manifests a much more general feature among LBV nebulae than previously known.