J-PLUS: Uncovering a large population of extreme [OIII] emitters in the local Universe^⋆

¹ Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Unidad Asociada al CSIC, Plaza San Juan 1, 44001 Teruel, Spain
e-mail: alumbrerascalle@gmail.com
² Department of Physics, Lancaster University, Lancaster LA1 4YB, UK
³ Instituto de Astrofísica de Andalucía (IAA-CSIC), PO Box 3004, 18080 Granada, Spain
⁴ Observatório Nacional – MCTI (ON), Rua Gal. José Cristino 77, São Cristóvão, 20921-400 Rio de Janeiro, Brazil
⁵ Donostia International Physics Centre (DIPC), Paseo Manuel de Lardizabal 4, 20018 Donostia-San Sebastián, Spain
⁶ IKERBASQUE, Basque Foundation for Science, 48013 Bilbao, Spain
⁷ University of Michigan, Department of Astronomy, 1085 South University Ave., Ann Arbor, MI 48109, USA
⁸ University of Alabama, Department of Physics and Astronomy, Gallalee Hall, Tuscaloosa, AL 35401, USA
⁹ Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, 05508-090 São Paulo, Brazil
¹⁰ Instituto de Astrofísica de Canarias, La Laguna, 38205 Tenerife, Spain
¹¹ Departamento de Astrofísica, Universidad de La Laguna, 38206 Tenerife, Spain

Received: 13 December 2021
Accepted: 9 February 2022

Abstract

Context. Over the past decades, several studies have discovered a population of galaxies that undergo very strong star formation events. They are called extreme emission line galaxies (EELGs).

Aims. We exploit the capabilities of the Javalambre Photometric Local Universe Survey (J-PLUS), a wide-field multifilter survey, with which 2000 square degrees of the northern sky are already observed. We use it to identify EELGs at low redshift by their [OIII]5007 emission line. We intend to provide a more complete, deep, and less biased sample of local EELGs.

Methods. We selected objects with an excess of flux in the J-PLUS medium-band J0515 filter, which covers the [OIII] line at z < 0.06. We removed contaminants (stars and higher-redshift systems) using J-PLUS and WISE infrared photometry, with SDSS spectra as a benchmark. We performed spectral energy distribution fitting to estimate the physical properties of the galaxies: line fluxes, equivalent widths (EWs), masses, stellar population ages, and so on.

Results. We identify 466 EELGs at z < 0.06 with [OIII] EW over 300 Å and an r-band magnitude below 20, of which 411 were previously unknown. Most show compact morphologies, low stellar masses (log(M_⋆/_M⊙) ∼ 8.13_−0.58^+0.61), low dust extinction (E(_B−V) ∼ 0.1_−0.1^+0.2), and very young bursts of star formation (3.0_−2.0^+2.7 Myr). Our method is up to ∼20 times more efficient in detecting EELGs per Mpc³ than broadband surveys, and it is as complete as magnitude-limited spectroscopic surveys (but reaches fainter objects). The sample is not directly biased against strong Hα emitters, in contrast with works using broadband surveys.

Conclusions. We demonstrate that J-PLUS can identify a large sample of previously unknown EELGs showing unique properties following a clear selection process. A fraction of the EELGs are probably similar to the first galaxies in the Universe, but they are at a much lower redshift, which makes them ideal targets for follow-up studies.