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[O II] lambda 3727 Angstrom is often used as a tracer of star formation atintermediate redshifts (z > 0.4), where Halpha is not easily observed. We usethe spectrophotometric data of the Nearby Field Galaxy Survey to investigatethe range and systematic variation in observed [O II]/Halpha emission lineratio as a function of galaxy luminosity at low redshift. We find that theobserved [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 inthe [O II]/Halpha ratio and the dependence of the ratio on luminosity are duein equal parts to reddening and to the metallicity dependent excitation of theISM. The uncertainty in star formation rates derived from [O II] fluxes istherefore large. If Halpha cannot be observed, high S/N Hbeta fluxes are muchpreferable to [O II] fluxes for deriving star formation rates. We presentseveral purely empirical corrections for extinction.Comment: 10 pages, LateX, 7 figures included, accepted for publication in The  Astrophysical Journal (Part 1

[Oii] As a Tracer of Current Star Formation