Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies

The [O ii]λ3727 emission line is frequently used as an indicator of the star formation rate (SFR) despite its complex dependence on metallicity and excitation conditions. We have analysed the properties of the [O II] and Hα emission lines for a complete sample of local Hα-selected galaxies, the Univ...

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Authors: Aragón Salamanca, A., Alonso Herrero, A., Gallego Maestro, Jesús, García Dabó, C. E., Pérez González, Pablo Guillermo, Zamorano Calvo, Jaime, Gil De Paz, Armando
Format: book part
Publication Date:2003
Country:España
Institution:Universidad Complutense de Madrid (UCM)
Repository:Docta Complutense
Language:English
OAI Identifier:oai:docta.ucm.es:20.500.14352/53497
Online Access:https://hdl.handle.net/20.500.14352/53497
Access Level:Open access
Keyword:52
Madrid survey galaxies
Nearby field galaxies
Spectroscopic properties
Universidad Complutense
O-II
Emission
Photometry
Astrofísica
Astronomía (Física)
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repository_id_str
spelling Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxiesAragón Salamanca, A.Alonso Herrero, A.Gallego Maestro, JesúsGarcía Dabó, C. E.Pérez González, Pablo GuillermoZamorano Calvo, JaimeGil De Paz, Armando52Madrid survey galaxiesNearby field galaxiesSpectroscopic propertiesUniversidad ComplutenseO-IIEmissionPhotometryAstrofísicaAstronomía (Física)The [O ii]λ3727 emission line is frequently used as an indicator of the star formation rate (SFR) despite its complex dependence on metallicity and excitation conditions. We have analysed the properties of the [O II] and Hα emission lines for a complete sample of local Hα-selected galaxies, the Universidad Complutense de Madrid (UCM) survey. We find a large scatter in the [O II]/Hα line ratios, although the scatter in the extinction-corrected [O II]^0/Hα^0 ratio is considerably smaller. We also find that the [O II]/Hα ratios are reasonably well correlated with the absolute B- and K-band magnitudes and with EW([O II]). However, the extinction-corrected [O II]^0/Hα^0 ratio is largely independent of these quantities, indicating that extinction is the main driver of the correlations. These correlations allow us to statistically predict-with varying degrees of accuracy-the observed and extinction-corrected Hα fluxes from the observed [O II] flux using the information contained in EW([O II]) and/or the absolute magnitudes, but extreme caution is needed to make sure that the sample selection effects are correctly taken into account.Astronomical Society of the PacificUniversidad Complutense de Madrid20032003-01-0120032003-01-01book parthttp://purl.org/coar/resource_type/c_3248info:eu-repo/semantics/bookPartapplication/pdfhttps://hdl.handle.net/20.500.14352/53497reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/534972026-06-02T12:44:21Z
dc.title.none.fl_str_mv Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
title Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
spellingShingle Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
Aragón Salamanca, A.
52
Madrid survey galaxies
Nearby field galaxies
Spectroscopic properties
Universidad Complutense
O-II
Emission
Photometry
Astrofísica
Astronomía (Física)
title_short Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
title_full Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
title_fullStr Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
title_full_unstemmed Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
title_sort Star Formation Rate estimators: [O II]λ3727 vs. Hα for local star-forming galaxies
dc.creator.none.fl_str_mv Aragón Salamanca, A.
Alonso Herrero, A.
Gallego Maestro, Jesús
García Dabó, C. E.
Pérez González, Pablo Guillermo
Zamorano Calvo, Jaime
Gil De Paz, Armando
author Aragón Salamanca, A.
author_facet Aragón Salamanca, A.
Alonso Herrero, A.
Gallego Maestro, Jesús
García Dabó, C. E.
Pérez González, Pablo Guillermo
Zamorano Calvo, Jaime
Gil De Paz, Armando
author_role author
author2 Alonso Herrero, A.
Gallego Maestro, Jesús
García Dabó, C. E.
Pérez González, Pablo Guillermo
Zamorano Calvo, Jaime
Gil De Paz, Armando
author2_role author
author
author
author
author
author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 52
Madrid survey galaxies
Nearby field galaxies
Spectroscopic properties
Universidad Complutense
O-II
Emission
Photometry
Astrofísica
Astronomía (Física)
topic 52
Madrid survey galaxies
Nearby field galaxies
Spectroscopic properties
Universidad Complutense
O-II
Emission
Photometry
Astrofísica
Astronomía (Física)
description The [O ii]λ3727 emission line is frequently used as an indicator of the star formation rate (SFR) despite its complex dependence on metallicity and excitation conditions. We have analysed the properties of the [O II] and Hα emission lines for a complete sample of local Hα-selected galaxies, the Universidad Complutense de Madrid (UCM) survey. We find a large scatter in the [O II]/Hα line ratios, although the scatter in the extinction-corrected [O II]^0/Hα^0 ratio is considerably smaller. We also find that the [O II]/Hα ratios are reasonably well correlated with the absolute B- and K-band magnitudes and with EW([O II]). However, the extinction-corrected [O II]^0/Hα^0 ratio is largely independent of these quantities, indicating that extinction is the main driver of the correlations. These correlations allow us to statistically predict-with varying degrees of accuracy-the observed and extinction-corrected Hα fluxes from the observed [O II] flux using the information contained in EW([O II]) and/or the absolute magnitudes, but extreme caution is needed to make sure that the sample selection effects are correctly taken into account.
publishDate 2003
dc.date.none.fl_str_mv 2003
2003-01-01
2003
2003-01-01
dc.type.none.fl_str_mv book part
http://purl.org/coar/resource_type/c_3248
dc.type.openaire.fl_str_mv info:eu-repo/semantics/bookPart
format bookPart
dc.identifier.none.fl_str_mv https://hdl.handle.net/20.500.14352/53497
url https://hdl.handle.net/20.500.14352/53497
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Astronomical Society of the Pacific
publisher.none.fl_str_mv Astronomical Society of the Pacific
dc.source.none.fl_str_mv reponame:Docta Complutense
instname:Universidad Complutense de Madrid (UCM)
instname_str Universidad Complutense de Madrid (UCM)
reponame_str Docta Complutense
collection Docta Complutense
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869406181363023872
score 15,300719

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