[O II] as a tracer of current star formation

Abstract

[O II] lambda 3727 Angstrom is often used as a tracer of star formation at intermediate redshifts (z > 0.4), where Halpha is not easily observed. We use the spectrophotometric data of the Nearby Field Galaxy Survey to investigate the range and systematic variation in observed [O II]/Halpha emission line ratio as a function of galaxy luminosity at low redshift. We find that the observed [O II]/Halpha ratio varies by a factor of 7 at luminosities near M_B*. The [O II]/Halpha ratio is inversely correlated with luminosity. The scatter in the [O II]/Halpha ratio and the dependence of the ratio on luminosity are due in equal parts to reddening and to the metallicity dependent excitation of the ISM. The uncertainty in star formation rates derived from [O II] fluxes is therefore large. If Halpha cannot be observed, high S/N Hbeta fluxes are much preferable to [O II] fluxes for deriving star formation rates. We present several purely empirical corrections for extinction.

10 pages, LateX, 7 figures included, accepted for publication in The Astrophysical Journal (Part 1)

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