论文标题
光学选择的Agn-host矮人星系样本的恒星种群
Stellar Populations of a Sample of Optically Selected AGN-host Dwarf Galaxies
论文作者
论文摘要
在本文中，我们介绍了Reines等人的恒星种群和星形形成历史（SFHS）的研究。从Sloan数字天空调查数据发行8中选择的136个矮星系样品，这些样品载有活性银河核（AGNS）。我们使用Stellar Messentes Code code sarlight得出了这些AGN-HOST矮人的恒星种群，并为这些AGN-Host矮人重建SFHS。我们的结果表明，这些Agn-Host矮人在狭窄的一段时间内将其恒星质量组装在一起，其恒星大规模权威的年龄在$ 10^9-10^{10} $ yr的范围内，但与亮度权威的SFHS相同，并以亮度权威的优势为$ 10^7-10^7-10^7-10^yr {10^7-10^yr。对于大多数样本，旧人口（$ t> 10^9 $ yr）对银河灯的贡献最大；年轻人口（$ t <10^8 $ yr）也出现在显着但差异很大的分数，而中级人口（$ 10^8 <t <10^9 $ yr）总体上对光学连续体的贡献较小，为4020 $Å$。我们还发现，这些矮人遵循与正常恒星形成星系相似的质量金属性关系，表明AGN对宿主星系的化学演化几乎没有影响。我们进一步研究了宿主银河系的派生SFH和形态之间的关系，并且没有发现相关性。将SFH与[OIII] $λ$ 5007行（$ l _ {\ rm [oiii]} $）的亮度进行比较，我们发现当$ l _ {\ rm [oiii]}> 10^10^{39} $ erg s $ erg s $ n is $ l _ {\ rm [oiii]这些矮星系中的活动。
In this paper we present our studies on the stellar populations and star formation histories (SFHs) for the Reines et al. sample of 136 dwarf galaxies which host active galactic nuclei (AGNs), selected from the Sloan Digital Sky Survey Data Release 8. We derive stellar populations and reconstruct SFHs for these AGN-host dwarfs using the stellar population synthesis code STARLIGHT. Our results suggest that these AGN-host dwarfs have assembled their stellar masses within a narrow period of time with the stellar mass-weighted ages in the range of $10^9-10^{10}$yr, but show a wide diversity of SFHs with the luminosity-weighted stellar ages in the range of $10^7-10^{10}$yr. The old population ($t>10^9$yr) contributes most to the galaxy light for the majority of the sample; the young population ($t<10^8$yr) also appears in significant but widely varying fractions, while the intermediate-age population ($10^8<t<10^9$yr) in general contributes less to the optical continuum at 4020 $Å$. We also find that these dwarfs follow a similar mass-metallicity relation to normal star-forming galaxies, indicating that AGNs have little effect on the chemical evolution of the host galaxy. We further investigate the relation between the derived SFHs and morphology of the host galaxy, and find no correlation. Comparing the SFHs with the luminosity of the [OIII] $λ$5007 line ($L_{\rm [OIII]}$), we find that there exists a mild correlation when $L_{\rm [OIII]} > 10^{39}$erg s$^{-1}$, indicating that there is a physical connection between star formation and AGN activities in these dwarf galaxies.
