论文标题
银河系和质量组装（GAMA）：配对星系中的星系质量，SFR和重元素丰度之间的相互作用
Galaxy And Mass Assembly (GAMA): the interplay between galaxy mass, SFR and heavy element abundance in paired galaxy sets
论文作者
论文摘要
我们使用Galaxy和Mass Assembly（GAMA）调查研究了4,636个星系对，研究恒星形成率（SFR），恒星质量（$ M _ {\ Star} $）和气体金属性（Z）。我们的星系对在0 $ <$ $ z $ <$ <$ 0.35，7.5 $ <$ <$ <$ log（m $ _ {\ star} $/ m $ _ \ odot $）$ 11.5和$ΔV$ <$ <$ <$ <$ 1000 km s $^{ - 1} $中。我们从三个观点探索SFR和Z中的变化：多样性，成对分离和动力学。我们将多重性定义为与单个星系配对的星系数，并分析了SFR和Z中首次变化的单个对，具有较高多重性的单对和对。对于后者，我们发现从0.025-0.15 dex的SFR增强功能将使单对的M-SFR关系将27 $ \％$的M-SFR关系转移到更高的SFRS。另一方面，Z的效果仅为4 $ \％$。我们分析了主要/次要对的最大和最少的星系，这是对分离的函数。我们定义了质量比为0.5 $ <$ $ $ $ m_1 $/$ m_2 $ $ <$ <$ 2的主要成对，而具有更多差异质量比的对成对。对于主要和次要对，我们发现SFR的增强最多2和4倍。对于Z的情况，我们发现最接近的对减小了高达0.08 DEX。当我们专注于动力学时，发现具有高速散布的次要对z增强功能$（σ_p> 250 \; \ mathrm {km \，s ^{ - 1}}}）$ and High Ulluctlicity。
We study the star formation rate (SFR), stellar mass ($M_{\star}$) and the gas metallicity (Z) for 4,636 galaxy pairs using the Galaxy And Mass Assembly (GAMA) survey. Our galaxy pairs lie in a redshift range of 0 $<$ $z$ $<$ 0.35, mass range of 7.5 $<$ log( M$_{\star}$/ M$_\odot$) $<$ 11.5 and $ΔV$ $<$ 1000 km s$^{-1}$. We explore variations in SFR and Z from three point of views: multiplicity, pair separation and dynamics. We define multiplicity as the number of galaxies paired with a single galaxy, and analyzed for the first time variations in SFR and Z for both, single pairs and pairs with higher multiplicity. For the latter, we find SFR enhancements from 0.025-0.15 dex, that would shift the M-SFR relation of single pairs by 27$\%$ to higher SFRs. The effect of Z on the other hand, is of only 4$\%$. We analyze the most and least massive galaxy of major/minor pairs as a function of the pair separation. We define major pairs those with mass ratios of 0.5 $<$ $M_1$/$M_2$ $<$ 2, while pairs with more discrepant mass ratios are classified as minor pairs. We find SFR enhancements of up to 2 and 4 times with respect to their control sample, for major and minor pairs. For the case of Z, we find decrements of up to 0.08 dex for the closest pairs. When we focus on dynamics, Z enhancements are found for minor pairs with high velocity dispersion $(σ_p > 250 \; \mathrm{km\,s ^{-1}})$ and high multiplicity.
