Bibcode
Lumbreras-Calle, A.; López-Sanjuan, C.; Sobral, D.; Fernández-Ontiveros, J. A.; Vílchez, J. M.; Hernán-Caballero, A.; Akhlaghi, M.; Díaz-García, L. A.; Alcaniz, J.; Angulo, R. E.; Cenarro, A. J.; Cristóbal-Hornillos, D.; Dupke, R. A.; Ederoclite, A.; Hernández-Monteagudo, C.; Marín-Franch, A.; Moles, M.; Sodré, L.; Vázquez Ramió, H.; Varela, J.
Referencia bibliográfica
Astronomy and Astrophysics
Fecha de publicación:
12
2022
Revista
Número de citas
13
Número de citas referidas
11
Descripción
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.
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.
Full Tables 3 and 4 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/668/A60