Observational evidence for the evolution of nuclear metallicity and star formation rate with the merger stage
Observational evidence for the evolution of nuclear metallicity and star formation rate with the merger stage
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核金属丰度和恒星形成率随并合阶段演化的观测证据
DOI：
10.1088/1674-4527/16/7/113
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发表时间：
2016-03
影响因子：
1.8
通讯作者：
Guo Xin
中科院分区：
文献类型：
--
作者：
Guo Rui;Hao Cai-Na;Xia Xiao-Yang;Wei Peng;Guo Xin
利用光学形态学方法，研究了局域远红外选择性成星星系沿着合并序列的核气相氧丰度和星星形成率（SFR）的演化.该样本来自IRAS点源目录红移巡天和1 Jy超亮红外星系样本与斯隆数字巡天数据第7版数据库的互相关分析。调查是通过比较我们的样品与对照样品匹配的归一化红移分布在两个诊断，这是核气相金属丰度与恒星质量和核SFR与恒星质量图。不同形态类型的镓矿床表现出不同的质量-金属丰度关系。与由控制样本定义的MZR相比，孤立的螺旋在给定的恒星质量下具有与控制样本相当的金属丰度。成对的螺旋星系和相互作用星系的投影间距rp > 20 kpc，显示出0.02-0.03 dex的金属丰度稀释。rp < 20 kpc的相互作用星系、合并前星系和合并高级星系的丰度分别不足0.06、0.05和0.04 dex。这表明了一个演化趋势，即随着星系合并的进行，金属丰度逐渐降低，当两个星系相互作用密切时，金属丰度被稀释得最显著。之后，当星系合并时，星际介质（ISM）变得丰富。这是第一次在最后的合并阶段观察到这样的ISM富集，这表明超新星爆炸在影响核金属丰度方面的重要性。此外，中央SFR增强相对于对照样品的演变与核气相氧丰度的同时。我们的结果支持了数值模拟的预测。
We investigate the evolution of nuclear gas-phase oxygen abundance and star formation rate (SFR) of local far-infrared selected star-forming galaxies along the merger sequence, as traced by their optical morphologies. The sample was drawn from a cross-correlation analysis of the IRAS Point Source Catalog Redshift Survey and 1 Jy ultraluminous infrared galaxy sample with the Sloan Digital Sky Survey Data Release 7 database. The investigation is done by comparing our sample to a control sample matched in the normalized redshift distribution in two diagnostics, which are the nuclear gas-phase metallicity vs. stellar mass and the nuclear SFR vs. stellar mass diagrams. Galaxies with different morphological types show different mass-metallicity relations (MZRs). Compared to the MZR defined by the control sample, isolated spirals have comparable metallicities with the control sample at a given stellar mass. Spirals in pairs and interacting galaxies with projected separations of rp > 20 kpc show a mild metallicity dilution of 0.02–0.03 dex. Interacting galaxies with rp < 20 kpc, pre-mergers and advanced mergers are underabundant by ∼ 0.06, ∼ 0.05 and ∼ 0.04 dex, respectively. This shows an evolutionary trend that the metallicity is increasingly depressed as the merging proceeds and it is diluted most dramatically when two galaxies are closely interacting. Afterwards, the interstellar medium (ISM) is enriched when the galaxies coalesce. This is the first time that such ISM enrichment at the final coalescence stage has been observed, which demonstrates the importance of supernova explosions in affecting the nuclear metallicity. Moreover, the central SFR enhancement relative to the control sample evolves simultaneously with the nuclear gas-phase oxygen abundance. Our results support the predictions from numerical simulations.
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DOI：
10.1086/503623
发表时间：
2006-02
期刊：
The Astrophysical Journal
影响因子：
--
作者：
D. Erb;A. Shapley;M. Pettini;C. Steidel;N. Reddy;K. Adelberger
通讯作者：
D. Erb;A. Shapley;M. Pettini;C. Steidel;N. Reddy;K. Adelberger
DOI：
10.1046/j.1365-8711.2001.04022.x
发表时间：
2000-09
影响因子：
4.8
作者：
P. Kroupa
通讯作者：
P. Kroupa
影响因子：
6.5
作者：
M. Montuori;P. Matteo;M. Lehnert;F. Combes;B. Semelin
通讯作者：
M. Montuori;P. Matteo;M. Lehnert;F. Combes;B. Semelin
DOI：
10.1111/j.1365-2966.2012.21749.x
发表时间：
2012-07
影响因子：
4.8
作者：
J. Scudder;S. Ellison;P. Torrey;D. Patton;J. Mendel
通讯作者：
J. Scudder;S. Ellison;P. Torrey;D. Patton;J. Mendel
DOI：
10.1088/0004-637x/797/1/54
发表时间：
2014-10
期刊：
The Astrophysical Journal
影响因子：
--
作者：
E. Eser;T. Goto;Y. Doi
通讯作者：
E. Eser;T. Goto;Y. Doi