论文标题
Otelo调查：$ z \ sim \，0.4 $的h $α$发射器的自然和质量金属关系
The OTELO survey: Nature and mass-metallicity relation for H$α$ emitters at $z\sim\,0.4$
论文作者
论文摘要
在$ z \，\ sim \，0.4 $的低质量H $α$发射线源（ELS）的样本中，在质量 - 金属关系（MZR）的背景下进行了研究及其可能的演变。我们从Osiris可调发射线对象（Otelo）调查中汲取了样品，该调查利用了在Gran望远镜加拿大加拿大的Osiris的红色可调节过滤器，以在延伸Groth带的选定磁场中执行盲边光谱扫描。我们能够直接测量Otelo伪谱分析的发射线通量和等效宽度。这项研究旨在探索非常低的质量制度中的MZR。我们的样本达到了恒星质量（$ M _*$），低至$ 10^{6.8} \，m_ \ odot $，其中63 \％的样本具有$ m _*\，<10^9 \，m_ \ odot $。我们还探讨了与$ M _*$和气相氧的关系以及$ M _*$ - 大小关系和形态学分类的恒星形成率（SFR）和特定SFR（SSFR）的关系。 $ m _*$是使用合成静电架颜色估算的。使用$χ^2 $最小化方法，我们将\ nii $λ$ 6583的贡献分开对H $α$排放线。使用N2指数，我们将活动的银河系核与星形星系（SFG）分离，并估计气体金属性。我们使用\ textIt {Hubble Space望远镜} -ACS的高分辨率数据（在视觉上）和定量（自动）（自动）（自动）（自动）（自动）（自动）研究了采样星系的形态。星系的物理大小是使用\ texttt {galapagos2/galfit}的形态分析得出的，我们将单sérsic2d模型拟合到每个源。
A sample of low-mass H$α$ emission line sources (ELS) at $z\,\sim\,0.4$ was studied in the context of the mass-metallicty relation (MZR) and its possible evolution. We drew our sample from the OSIRIS Tunable Emission Line Object (OTELO) survey, which exploits the red tunable filter of OSIRIS at the Gran Telescopio Canarias to perform a blind narrow-band spectral scan in a selected field of the Extended Groth Strip. We were able to directly measure emission line fluxes and equivalent widths from the analysis of OTELO pseudo-spectra. This study aims to explore the MZR in the very low-mass regime. Our sample reaches stellar masses ($M_*$) as low as $10^{6.8}\,M_\odot$, where 63\% of the sample have $M_*\,<10^9\,M_\odot$. We also explore the relation of the star formation rate (SFR) and specific SFR (sSFR) with $M_*$ and gas-phase oxygen abundances, as well as the $M_*$-size relation and the morphological classification. The $M_*$ were estimated using synthetic rest-frame colours. Using an $χ^2$ minimization method, we separated the contribution of \Nii$λ$6583 to the H$α$ emission lines. Using the N2 index, we separated active galactic nuclei from star-forming galaxies (SFGs) and estimated the gas metallicity. We studied the morphology of the sampled galaxies qualitatively (visually) and quantitatively (automatically) using high-resolution data from the \textit{Hubble Space Telescope}-ACS. The physical size of the galaxies was derived from the morphological analysis using \texttt{GALAPAGOS2/GALFIT}, where we fit a single-Sérsic 2D model to each source.
