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arXiv 2012.02922astro-ph.GA
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星系与质量集合（GAMA）：成对星系集合中星系质量、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

L. E. Garduño, M. A. Lara-López, O. López-Cruz, A. M. Hopkins, M. S. Owers, K. A. Pimbblet, B. W. Holwerda

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摘要：

利用GAMA巡天研究了4，636个星系对的恒星形成率（SFR）、恒星质量（$M_{\star}$）和气体金属丰度（Z）。我们的星系对位于0 $<$ $z$ $<$ 0.35的红移范围内，质量范围为7.5 $<$ log（M $_{\star}$ / M $_\odot$）$<$ 11.5和$ΔV$ $<$ 1000 km s $^{-1}$。我们从三个角度探讨SFR和Z的变化：多重性，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量，并首次分析了SFR和Z的变化，单对和对具有更高的多重性。对于后者，我们发现SFR从0.025-0.15 dex增强，这将使单对的M-SFR关系移动27 PDMATHAMT到更高的SFR。另一方面，Z的效果仅为4 PDMATHAMT。我们分析了最大和最小的大/小对星系作为对分离的函数。我们定义那些质量比为0.5 $<$ $M_1$ / $M_2$ $<$ 2的主要对，而质量比更不一致的对被归类为次要对。我们发现SFR增强高达2和4倍，相对于他们的控制样本，主要和次要的对。对于Z的情况下，我们发现最接近的对的递减高达0.08 dex。当我们专注于动力学，Z增强被发现与高速色散$(σ_p > 250 \; \mathrm{km\,s ^{-1}})$和高多重性的次要对。

英文摘要：

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.

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