%0 Journal Article
%A Nadolny, Jakub
%A Lara López, Maritza A.
%A Cerviño, Miguel
%A Bongiovanni, Ángel
%A Cepa, Jordi
%A de Diego, José A.
%A Pérez García, Ana María
%A Pérez Martínez, Ricardo
%A Sánchez Portal, Miguel
%A Alfaro, Emilio
%A Castañeda, Héctor O.
%A Gallego Maestro, Jesús
%A González, J. Jesús
%A González-Serrano, J. Ignacio
%A Padilla Torres, Carmen P.
%A Pintos-Castro, Irene
%A Pović, Mirjana
%T The OTELO survey: Nature and mass-metallicity relation for H α emitters at z ∼0.4
%D 2020
%@ 0004-6361
%U https://hdl.handle.net/20.500.14352/130985
%X 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.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.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.Results. From 541 preliminary emission-line source candidates selected around z & x2004;=& x2004;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 similar to 5 x 10(-19) erg s(-1) cm(2) and similar to 6 angstrom, respectively. We are able to constrain the faint-end slope (alpha & x2004;=& x2004;-1.03 +/- 0.08) of the observed LF ([O III]) at a mean redshift of z & x2004;=& x2004;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-& x22c6;& x2004;< & x2004;10(10) M-circle dot.
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