2020/12/23 by L. S. Pilyugin, I. A. Zinchenko, M. A. Lara-López +4
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Elliptical galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Lenticular galaxy #Luminous infrared galaxy #Peculiar galaxy #RADIUS #Radio galaxy #Velocity dispersion #astro-ph.GA
paper · pdf · doi:10.1051/0004-6361/202040029
published as A&A 646, A54 (2021) · 5 pages, 4 figures, accepted to Astron.Astrophys. arXiv admin note: text overlap with arXiv:2005.12744
arxiv created 2020/12/23 · openalex publication_date 2020/12/24 · openalex created_date 2021/01/05 · arxiv updated 2021/02/10 · openalex updated_date 2026/08/05
The distribution of the gas velocity dispersion σ across the images of 1146 MaNGA galaxies is analyzed. We find that there are two types of distribution of the gas velocity dispersion across the images of galaxies: (i) the distributions of 909 galaxies show a radial symmetry with or without the σ enhancement at the center (“ R distribution”, radial symmetry in the σ distribution) and (ii) distributions with a band of enhanced σ along the minor axis in the images of 159 galaxies with or without the σ enhancement at the center (“ B distribution”, band in the σ distribution). The σ distribution across the images of 78 galaxies cannot be reliable classified. We select 806 galaxies with the best defined characteristics (this sample includes 687 galaxies with R distribution and 119 galaxies with B distribution) and compare the properties of galaxies with R and B distributions. We find that the median value of the gas velocity dispersion σ m in galaxies with B distribution is higher by around 5 km s −1 , on average, than that of galaxies with R distribution. The optical radius R 25 of galaxies with B distribution is lower by around 0.1 dex, on average, than that of galaxies with similar masses with R distribution. Thus the properties of a galaxy are related to the type of distribution of the gas velocity dispersion σ across its image. This suggests that the presence of the band of the enhanced gas velocity dispersion can be an indicator of a specific evolution (or a specific stage in the evolution) of a galaxy.