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The OTELO survey. Nature and mass-metallicity relation for Hα emitters at z ∼ 0.4

AuthorsNadolny, Jakub; Lara-López, Maritza A.; Cerviño, Miguel CSIC ORCID CVN ; Bongiovanni, Ángel; Cepa, Jordi; Diego, J. A. de; Pérez-García, Ana M.; Pérez Martínez, Ricardo; Sánchez-Portal, Miguel; Alfaro, Emilio J. CSIC ORCID ; Castañeda, Héctor; Gallego, Jesús; González, José Jesús; González-Serrano, José Ignacio CSIC ORCID CVN ; Padilla Torres, Carmen P.; Pintos-Castro, Irene; Pović, Mirjana
KeywordsGalaxies: evolution
Galaxies: formation
Galaxies: fundamental parameters
Galaxies: star formation
Galaxies: structure
Issue Date24-Apr-2020
PublisherEDP Sciences
Abstract[Contex]: 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.
Publisher version (URL)http://dx.doi.org/10.1051/0004-6361/201936205
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