The local star-formation rate density: assessing calibrations using [OII], Ha and UV luminosities

Details The local star-formation rate density: assessing calibrations using [OII], Ha and UV luminosities The local star-formation rate density: assessing calibrations using [OII], Ha and UV luminosities

2010-02-16

arxiv.org/abs/1002.3172v3

MNRAS, 405, 2594 (2010)

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

22 pages, 16 figures. This version corrects typos in equations 2, 7, and 9 of the published version, as described in the MNRAS

Scientific paper

We explore the use of simple star-formation rate (SFR) indicators (such as may be used in high-redshift galaxy surveys) in the local Universe using [OII], Ha, and u-band luminosities from the deeper 275 deg^2 Stripe 82 subsample of the Sloan Digital Sky Survey (SDSS) coupled with UV data from the Galaxy Evolution EXplorer satellite (GALEX). We examine the consistency of such methods using the star-formation rate density (SFRD) as a function of stellar mass in this local volume, and quantify the accuracy of corrections for dust and metallicity on the various indicators. Rest-frame u-band promises to be a particularly good SFR estimator for high redshift studies since it does not require a particularly large or sensitive extinction correction, yet yields results broadly consistent with more observationally expensive methods. We suggest that the [OII]-derived SFR, commonly used at higher redshifts (z~1), can be used to reliably estimate SFRs for ensembles of galaxies, but for high mass galaxies (log(M*/Msun)>10), a larger correction than is typically used is required to compensate for the effects of metallicity dependence and dust extinction. We provide a new empirical mass-dependent correction for the [OII]-SFR.

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