ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITH SUZAKU
ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITH SUZAKU
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DOI：
10.1088/0004-637x/783/1/8
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发表时间：
2013-12
期刊：
影响因子：
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通讯作者：
S. Konami;K. Matsushita;Ryo Nagino;T. Tamagawa
中科院分区：
文献类型：
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作者：
S. Konami;K. Matsushita;Ryo Nagino;T. Tamagawa
我们分析了朱雀观测到的17个早期型星系、13个椭圆星系和4个S0星系，并研究了星际介质（ISM）中的金属丰度（O、Mg、Si和Fe）和丰度比（O/Fe、Mg/Fe和Si/Fe）。每个源上区域的发射是有效半径 re 的四倍，使用 APEC 等离子体代码版本 2.0.1，通过单温度 (1T) 或双温度 (2T) 热等离子体模型以及多温度模型来重现。多温度模型给出了与 1T 或 2T 模型几乎相同的丰度和丰度比。根据 Lodders 2003 年太阳丰度表，通过多温度模型拟合得出的所有样本星系的 O、Mg、Si 和 Fe 丰度的加权平均值分别为 0.83 ± 0.04、0.93 ± 0.03、0.80 ± 0.02 和 0.80 ± 0.02 个太阳单位，这些丰度与形态没有显着相关性。和环境。研究了 APEC 等离子体代码版本 2.0.1 和 1.3.1 之间衍生金属丰度的系统差异。 ISM 中导出的 O 和 Mg 丰度与从光谱导出的半径为 1 的孔径内的恒星金属丰度一致。根据这些结果，我们讨论了过去和现在的 Ia 型超新星发生率和早期型星系中的恒星形成历史。
We have analyzed 17 early-type galaxies, 13 ellipticals and 4 S0 galaxies, observed with Suzaku, and investigated metal abundances (O, Mg, Si, and Fe) and abundance ratios (O/Fe, Mg/Fe, and Si/Fe) in the interstellar medium (ISM). The emission from each on-source region, which is four times the effective radius, re, is reproduced with one-temperature (1T) or two-temperature (2T) thermal plasma models as well as a multi-temperature model, using APEC plasma code version 2.0.1. The multi-temperature model gave almost the same abundances and abundance ratios with the 1T or 2T models. The weighted averages of the O, Mg, Si, and Fe abundances of all the sample galaxies derived from the multi-temperature model fits are 0.83 ± 0.04, 0.93 ± 0.03, 0.80 ± 0.02, and 0.80 ± 0.02 solar, respectively, in solar units according to the solar abundance table by Lodders in 2003. These abundances show no significant dependence on the morphology and environment. The systematic differences in the derived metal abundances between versions 2.0.1 and 1.3.1 of the APEC plasma codes were investigated. The derived O and Mg abundances in the ISM agree with the stellar metallicity within an aperture with a radius of one re derived from optical spectroscopy. From these results, we discuss the past and present Type Ia supernova rates and star formation histories in early-type galaxies.