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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Detalles Bibliográficos
Autores: Aragón Salamanca, A., Alonso Herrero, A., Gallego Maestro, Jesús, García Dabó, C. E., Pérez González, Pablo Guillermo, Zamorano Calvo, Jaime, Gil De Paz, Armando
Tipo de recurso: capítulo de libro
Fecha de publicación:2003
País:España
Institución:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/53497
Acceso en línea:https://hdl.handle.net/20.500.14352/53497
Access Level:acceso abierto
Palabra clave:52
Madrid survey galaxies
Nearby field galaxies
Spectroscopic properties
Universidad Complutense
O-II
Emission
Photometry
Astrofísica
Astronomía (Física)
Descripción
Sumario: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.

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