论文标题
Otelo调查。 [O III] 4959,5007发射器的案例研究<z> = 0.83
The OTELO survey. A case study of [O III]4959,5007 emitters at <z> = 0.83
论文作者
论文摘要
Otelo调查是对延长的球状带的选定区域的非常深刻的盲目探索，旨在查找排放线来源（ELS）。在先前的贡献中，描述了调查设计，观察结果，数据降低，天文学和光度法以及与用于获得最终目录的辅助数据的相关性，包括Photo-Z估计值和ELS的初步选择。在这里，我们旨在确定Otelo [O III] ELS样本的主要特性和光度函数（LF），以作为其对其他调查的能力，优势和互补性的科学演示。描述了使用可调滤波器（TF）伪谱获得的ELS候选者的选择和分析程序。我们在调查的参数空间中进行了模拟，以获得发射线检测概率。提出了[O III]发射器和LF（[O III]）的相关特征，包括主要的选择偏见和不确定性。总共有184个来源被证实为平均红移Z = 0.83的[O III]发射器。此ELS样本中的最小可检测线通量和等效宽度（EW）为$ \ sim $ 5 $ \ times $ 10 $^{ - 19} $ erg S $^{ - 1} $ cm $^{2} $和$ \ sim $6Å。我们能够在z = 0.83处限制观察到的LF（[O III]）的微弱末端斜率（$α= -1.03 \ pm0.08 $）。该LF的值比其他调查低约十倍。形态学上的绝大多数（84 \％）[O III] ELS是类似碟片的来源，该样本中有87％由带有M $ _ \ star $ $ $ $ $ $ $ $ $ $ $ $ <$ 10 $^{10 $^{10} {10} $ m $ m $ m $ m $ _ {\ odot}的星系组成。
The OTELO survey is a very deep, blind exploration of a selected region of the Extended Groth Strip and is designed for finding emission-line sources (ELSs). The survey design, observations, data reduction, astrometry, and photometry, as well as the correlation with ancillary data used to obtain a final catalogue, including photo-z estimates and a preliminary selection of ELS, were described in a previous contribution. Here, we aim to determine the main properties and luminosity function (LF) of the [O III] ELS sample of OTELO as a scientific demonstration of its capabilities, advantages, and complementarity with respect to other surveys. The selection and analysis procedures of ELS candidates obtained using tunable filter (TF) pseudo-spectra are described. We performed simulations in the parameter space of the survey to obtain emission-line detection probabilities. Relevant characteristics of [O III] emitters and the LF([O III]), including the main selection biases and uncertainties, are presented. A total of 184 sources were confirmed as [O III] emitters at a mean redshift z=0.83. The minimum detectable line flux and equivalent width (EW) in this ELS sample are $\sim$5 $\times$ 10$^{-19}$ erg s$^{-1}$ cm$^{2}$ and $\sim$6 Å, respectively. We are able to constrain the faint-end slope ($α= -1.03\pm0.08$) of the observed LF([O III]) at z=0.83. This LF reaches values that are approximately ten times lower than those from other surveys. The vast majority (84\%) of the morphologically classified [O III] ELSs are disc-like sources, and 87\% of this sample is comprised of galaxies with stellar masses of M$_\star$ $<$ 10$^{10}$ M$_{\odot}$.
