论文标题
漫画星系的气速分散的两种类型的分布
Two types of distribution of the gas velocity dispersion of MaNGA galaxies
论文作者
论文摘要
分析了气速度分散体在1146个漫画星系图像中的分布。 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 sigma enhancement at the center (R distribution) and (ii) distributions with a band of enhanced sigma along the minor axis in the images of 159 galaxies with or without the sigma enhancement at the center (B distribution) The sigma distribution across the images在78个星系中，不能可靠地分类。我们选择具有最佳定义特性的806个星系（该样本包括687个带有R分布的星系和119个带有B分布的星系），并比较了带有R和B分布的星系的性质。我们发现，B分布的星系中气体速度分散sigma_m的中位数的平均值高约5 km/s约5 km/s。 B分布的星系的光半径R_25平均比具有R分布的质量相似的星系低于0.1 dex。因此，银河系的性质与气速分散在其图像上的分布类型有关。这表明，增强气体速度分散体的带子的存在可以指示星系的特定进化（或进化中的特定阶段）。
The distribution of the gas velocity dispersion sigma 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 sigma enhancement at the center (R distribution) and (ii) distributions with a band of enhanced sigma along the minor axis in the images of 159 galaxies with or without the sigma enhancement at the center (B distribution) The sigma 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 sigma_m in galaxies with B distribution is higher by around 5 km/s, 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 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.
