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dc.contributor.author
Favole, G.
dc.contributor.author
González Perez, V.
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Ascasibar, Y.
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Corcho Caballero, P.
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Montero Dorta, A. D.
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Benson, A. J.
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Comparat, J.
dc.contributor.author
Cora, Sofia Alejandra
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dc.contributor.author
Croton, D.
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Guo, H.
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Izquierdo Villalba, D.
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Knebe, A.
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Orsi, A.
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Stoppacher, D.
dc.contributor.author
Vega Martínez, Cristian Antonio
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dc.date.available
2024-05-31T17:00:36Z
dc.date.issued
2024-01
dc.identifier.citation
Favole, G.; González Perez, V.; Ascasibar, Y.; Corcho Caballero, P.; Montero Dorta, A. D.; et al.; Characterizing the ELG luminosity functions in the nearby Universe; EDP Sciences; Astronomy and Astrophysics; 683; A46; 1-2024; 46-84
dc.identifier.uri
http://hdl.handle.net/11336/236746
dc.description.abstract
Context. Nebular emission lines are powerful diagnostics for the physical processes at play in galaxy formation and evolution. Moreover, emission-line galaxies (ELGs) are one of the main targets of current and forthcoming spectroscopic cosmological surveys.Aims. We investigate the contributions to the line luminosity functions (LFs) of di erent galaxy populations in the local Universe, providing a benchmark for future surveys of earlier cosmic epochs.Methods. The large statistics of the observations from the SDSS DR7 main galaxy sample and the MPA-JHU spectral catalog enabled us to precisely measure the H , H , [O II], [O III], and, for the first time, the [N II], and [S II] emission-line LFs over 2:4 Gyrs in the low-z Universe, 0.02 < z < 0.22. We present a generalized 1=Vmax LF estimator capable of simultaneously correcting for spectroscopic,r-band magnitude, and emission-line incompleteness. We studied the contribution to the LF of di erent types of ELGs classified using two methods: (i) the value of the specific star formation rate (sSFR), and (ii) the line ratios on the Baldwin–Phillips–Terlevich (BPT) and the WHAN (i.e., H equivalent width, EWH , versus the [N ii]/H line ratio) diagrams.Results. The ELGs in our sample are mostly star forming, with 84 percent having sSFR > 10^11 yr^-1. When classifying ELGs using the BPT+WHAN diagrams, we find that 63:3 percent are star forming, only 0.03 are passively evolving, and 1:3 have nuclear activity (Seyfert). The rest are low-ionization narrow emission-line regions (LINERs) and composite ELGs.We found that a Saunders functionis the most appropriate to describe all of the emission-line LFs, both observed and dust-extinction-corrected (i.e., intrinsic). They are dominated by star-forming regions, except for the bright end of the [O III] and [N II] LFs (i.e., L[N II] > 1042erg s^-1, L[O III] > 1043erg s^-1), where the contribution of Seyfert galaxies is not negligible. In addition to the star-forming population, composite galaxies, and LINERs are the ones that contribute the most to the ELG numbers at L < 10^41 erg s^-1. We do not observe significant evolution with redshift of our ELGs at 0.02 < z < 0.22. All of our results, including data points and analytical fits, are publicly available.Conclusions. Local ELGs are dominated by star-forming galaxies, except for the brightest [N II] and [O III] emitters, which have a large contribution of Seyfert galaxies. The local line luminosity functions are best described by Saunders functions. We expect these two conclusions to hold up at higher redshifts for the ELG targeted by current cosmological surveys, such as DESI and Euclid.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
galaxies: distances and redshifts
dc.subject
galaxies: luminosity function, mass function
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galaxies: Seyfert
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galaxies: starburst
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galaxies: star formation
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galaxies: stellar content
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Characterizing the ELG luminosity functions in the nearby Universe
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2024-05-07T13:28:20Z
dc.identifier.eissn
1432-0746
dc.journal.volume
683
dc.journal.number
A46
dc.journal.pagination
46-84
dc.journal.pais
Estados Unidos
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dc.description.fil
Fil: Favole, G.. Instituto de Astrofísica de Canarias; España
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Fil: González Perez, V.. Universidad Autónoma de Madrid; España
dc.description.fil
Fil: Ascasibar, Y.. Universidad Autónoma de Madrid; España
dc.description.fil
Fil: Corcho Caballero, P.. Universidad Autónoma de Madrid; España
dc.description.fil
Fil: Montero Dorta, A. D.. Universidad Técnica Federico Santa María; Chile
dc.description.fil
Fil: Benson, A. J.. Carnegie Observatories; Estados Unidos
dc.description.fil
Fil: Comparat, J.. Max-planck-institut Für Extraterrestrische Physik; Alemania
dc.description.fil
Fil: Cora, Sofia Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
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Fil: Croton, D.. Centre For Astrophysics & Supercomputing; Australia
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Fil: Guo, H.. Shanghai Astronomical Observatory; China
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Fil: Izquierdo Villalba, D.. Università Degli Studi Di Milano-bicocca; Italia
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Fil: Knebe, A.. Universidad Autónoma de Madrid; España
dc.description.fil
Fil: Orsi, A.. Planttech Research Institute Limited; Nueva Zelanda
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Fil: Stoppacher, D.. Universidad Autónoma de Madrid; España
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Fil: Vega Martínez, Cristian Antonio. Universidad de La Serena; Chile. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
dc.journal.title
Astronomy and Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/202346443
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2024/03/aa46443-23/aa46443-23.html
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