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Aperture-free star formation rate of SDSS star-forming galaxies

AutorDuarte Puertas, Salvador; Vílchez Medina, José Manuel ; Iglesias-Páramo, J. ; Kehrig, C. ; Pérez Montero, Enrique ; Rosales-Ortega, F.F.
Palabras claveGalaxies: general
Galaxies: formation
Galaxies: evolution
Galaxies: star formation
Fecha de publicación2017
EditorEDP Sciences
CitaciónAstronomy and Astrophysics 599: A71 (2017)
ResumenLarge area surveys with a high number of galaxies observed have undoubtedly marked a milestone in the understanding of several properties of galaxies, such as star-formation history, morphology, and metallicity. However, in many cases, these surveys provide fluxes from fixed small apertures (e.g. fibre), which cover a scant fraction of the galaxy, compelling us to use aperture corrections to study the global properties of galaxies. In this work, we derive the current total star formation rate (SFR) of Sloan Digital Sky Survey (SDSS) star-forming galaxies, using an empirically based aperture correction of the measured Hα flux for the first time, thus minimising the uncertainties associated with reduced apertures. All the Hα fluxes have been extinction-corrected using the Hα/Hβ ratio free from aperture effects. The total SFR for ~210 000 SDSS star-forming galaxies has been derived applying pure empirical Hα and Hα/Hβ aperture corrections based on the Calar Alto Legacy Integral Field Area (CALIFA) survey. We find that, on average, the aperture-corrected SFR is ~0.65 dex higher than the SDSS fibre-based SFR. The relation between the SFR and stellar mass for SDSS star-forming galaxies (SFR-M∗) has been obtained, together with its dependence on extinction and Hα equivalent width.We compare our results with those obtained in previous works and examine the behaviour of the derived SFR in six redshift bins, over the redshift range 0:005 ≤ z ≤ 0:22. The SFR-M∗ sequence derived here is in agreement with selected observational studies based on integral field spectroscopy of individual galaxies as well as with the predictions of recent theoretical models of disc galaxies.© ESO 2017.
Identificadoresdoi: 10.1051/0004-6361/201629044
issn: 1432-0746
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