The OTELO survey. A case study of [O III] λ4959,5007 emitters at ⟨z⟩ = 0.83

DOI: 
10.1051/0004-6361/201833656
Publication date: 
01/03/2020
Main author: 
Bongiovanni, Ángel
IAA authors: 
Cerviño, Miguel;Alfaro, Emilio J.;Fernández-Lorenzo, Mirian;Pović, Mirjana
Authors: 
Bongiovanni, Ángel;Ramón-Pérez, Marina;Pérez García, Ana María;Cerviño, Miguel;Cepa, Jordi;Nadolny, Jakub;Pérez Martínez, Ricardo;Alfaro, Emilio J.;Castañeda, Héctor O.;Cedrés, Bernabé;de Diego, José A.;Ederoclite, Alessandro;Fernández-Lorenzo, Mirian;Gallego, Jesús;de Jesús González, José;González-Serrano, José Ignacio;Lara-López, Maritza A.;Oteo Gómez, Iván;Padilla Torres, Carmen P.;Pintos-Castro, Irene;Pović, Mirjana;Sánchez-Portal, Miguel;Heath Jones, D.;Bland-Hawthorn, Joss;Cabrera-Lavers, Antonio
Journal: 
Astronomy and Astrophysics
Refereed: 
Yes
Publication type: 
Article
Volume: 
635
Pages: 
A35
Abstract: 
Context. The OSIRIS Tunable Filter Emission Line Object (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. <BR /> Aims: 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. <BR /> Methods: The selection and analysis procedures of ELS candidates obtained using tunable filter 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. <BR /> Results: From 541 preliminary emission-line source candidates selected around z = 0.8, a total of 184 sources were confirmed as [O III] emitters. Consistent with simulations, the minimum detectable line flux and equivalent width in this ELS sample are ∼5 × 10<SUP>-19</SUP> erg s<SUP>-1</SUP> cm<SUP>2</SUP> and ∼6 Å, respectively. We are able to constrain the faint-end slope (α = -1.03 ± 0.08) of the observed LF ([O III]) at a mean redshift of 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<SUB>⋆</SUB> &lt; 10<SUP>10</SUP> M<SUB>☉</SUB>.
Database: 
ADS
URL: 
https://ui.adsabs.harvard.edu/#abs/2020A&A...635A..35B/abstract
ADS Bibcode: 
2020A&A...635A..35B
Keywords: 
techniques: imaging spectroscopy;surveys;catalogs;galaxies: starburst;galaxies: active;galaxies: luminosity function;mass function;Astrophysics - Astrophysics of Galaxies