论文标题
魔鬼：SED衍生金属性的宇宙演变及其与星形成历史的联系
DEVILS: Cosmic evolution of SED-derived metallicities and their connection to star-formation histories
论文作者
论文摘要
星系的气相金属度通常是通过极光或星云发射线测量的，但是金属性也留下了银河系的整体光谱分布（SED）的烙印，并且可以通过SED拟合来估计。我们使用具有灵活的参数星形成历史的Prospect SED拟合代码，并具有不断发展的金属性历史记录，以$ \ sim90 \，000 $ 000 $的Galaxies，从深度的外层面可见的遗产调查（Devils）和Galaxy和Galaxy和Galaxy和Galaxy和Galame（Gama）（Gama）（Gama）（GAMA）（Gama）中，以$ \ sim90 \，000 $ Galaxies的形式来衡量金属性，恒星质量和其他Galaxy Properties。我们使用这些来追踪质量金属关系（MZR）的演变，并表明MZR仅在$ \ sim0.1 \，$ dex中的归一化演变为恒星质量$ m_ \ star = 10^{10.5} {10.5} \ \，m_ \ odot $。我们发现在低红移（$ z <0.3 $）处有活性银河核排放的星系之间的MZR没有差异。我们的结果表明，金属性和恒星形成活动在固定恒星质量上的金属性和恒星形成活动之间的星系质量为$ M_ \ Star> 10^{10.5} \，M_ \ odot $，for $ z <0.3 $。使用前景提取的恒星形成历史，我们探索了MZR的高阶相关性，其特性具有恒星形成历史的特性，包括年龄，宽度和形状。我们发现，在给定的恒星质量下，具有较高金属性的星系在较短的时间尺度和峰值恒星形成速率之前形成了大部分质量。这项工作突出了探索银河系当前的气相金属与其星形形成历史记录的连接的价值，以了解塑造MZR的物理过程。
Gas-phase metallicities of galaxies are typically measured through auroral or nebular emission lines, but metallicity also leaves an imprint on the overall spectral energy distribution (SED) of a galaxy and can be estimated through SED fitting. We use the ProSpect SED fitting code with a flexible parametric star formation history and an evolving metallicity history to self-consistently measure metallicities, stellar mass, and other galaxy properties for $\sim90\,000$ galaxies from the Deep Extragalactic VIsible Legacy Survey (DEVILS) and Galaxy and Mass Assembly (GAMA) survey. We use these to trace the evolution of the mass-metallicity relation (MZR) and show that the MZR only evolves in normalisation by $\sim0.1\,$dex at stellar mass $M_\star = 10^{10.5}\,M_\odot$. We find no difference in the MZR between galaxies with and without SED evidence of active galactic nuclei emission at low redshifts ($z<0.3$). Our results suggest an anti-correlation between metallicity and star formation activity at fixed stellar mass for galaxies with $M_\star > 10^{10.5}\,M_\odot$ for $z<0.3$. Using the star formation histories extracted using ProSpect we explore higher-order correlations of the MZR with properties of the star formation history including age, width, and shape. We find that at a given stellar mass, galaxies with higher metallicities formed most of their mass over shorter timescales, and before their peak star formation rate. This work highlights the value of exploring the connection of a galaxy's current gas-phase metallicity to its star formation history in order to understand the physical processes shaping the MZR.
