Chemical Evolution of Blue Compact Galaxies
Chemical Evolution of Blue Compact Galaxies
复制标题
DOI：
10.1088/1009-9271/6/6/01
复制
发表时间：
2006-12
期刊：
影响因子：
--
通讯作者：
F. Shi;X. Kong;F. Cheng
中科院分区：
文献类型：
--
作者：
F. Shi;X. Kong;F. Cheng
基于中国科学院国家天文台2.16m望远镜观测到的72个蓝致密星系(BCG)和斯隆数字巡天约4000个强发射线星系，利用Larsen等人修正的化学演化模型分析了它们的化学演化历史。我们的样品涵盖了更大的金属丰度范围(7.2<；12+log(O/H)<；9.0)。我们发现，为了在整个金属丰度范围内再现观测到的丰度模式和气体分数，高金属丰度星系需要一个相对连续的恒星形成历史，而低金属丰度星系则需要一系列长静止期(一些回旋)的瞬时爆发。模型计算还表明，只有闭箱模型才能重现整个金属丰度范围内的观测数据。考虑普通风和/或入流的模式只能在低金属丰度范围内对观测数据进行拟合，而具有丰富风速的模式不能在整个金属丰度范围内对观测数据进行拟合。这意味着，目前采用的简单的风和流入模型不适用于大质量星系，因为在大质量星系中，星系风或流入的基本物理可能更复杂。
Based on a sample of 72 Blue Compact Galaxies (BCGs) observed with the 2.16 m telescope of the National Astronomical Observatories, Chinese Academy of Sciences (NAOC) and about 4000 strong emission line galaxies from the Sloan Digital Sky Survey, we analyzed their chemical evolution history using the revised chemical evolution model of Larsen et al. Our sample covers a much larger metallicity range (7.2 < 12 + log(O/H) < 9.0). We found that, in order to reproduce the observed abundance pattern and gas fraction over the whole metallicity range, a relatively continuous star formation history is needed for high metallicity galaxies, while assuming a series of instantaneous bursts with long quiescent periods (some Gyrs) for low metallicity galaxies. Model calculations also show that only the closed-box model is capable of reproducing the observational data over the whole metallicity range. Models that consider the ordinary winds and/or inflow can only fit the observations in the low metallicity range, and a model with enriched wind cannot fit the data in the whole metallicity range. This implies that the current adopted simple wind and inflow models are not applicable to massive galaxies, where the underlying physics of galactic winds or inflow could be more complicated.