Two types of distribution of the gas velocity dispersion of MaNGA galaxies

¹ Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St, 03680 Kiev, Ukraine
e-mail: pilyugin@mao.kiev.ua
² Faculty of Physics, Ludwig-Maximilians-Universitt, Scheinerstr. 1, 81679 Munich, Germany
³ Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, Northern Ireland, UK
⁴ Kazan Federal University, 18 Kremlyovskaya St., 420008 Kazan, Russian Federation
⁵ Instituto de Astrofísica de Andalucía, CSIC, Apdo 3004, 18080 Granada, Spain

Received: 30 November 2020
Accepted: 18 December 2020

Abstract

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 R₂₅ 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.