paper

A Comparison of UIT Far-Ultraviolet and H alpha Star Formation Rates

arXiv:astro-ph/0010340 · doi:10.1086/319025

Abstract

We have used archival ultraviolet (UV) imaging of 50 nearby star-forming galaxies obtained with the Ultraviolet Imaging Telescope (UIT) to derive integrated near-UV and far-UV magnitudes, and have combined these data with H alpha, far-infrared, and thermal radio continuum measurements to explore the consistency of UV and H alpha star formation rates (SFRs). In agreement with previous studies, we find that the UV and H alpha SFRs are qualitatively consistent, even before corrections for extinction are applied. The uncorrected UV SFRs are systematically lower by a factor of 1.5 (with a factor of two scatter) among luminous galaxies with SFRs over 1 solar mass per year, indicating a higher effective attenuation of the far-UV radiation. Among less luminous galaxies there is no significant offset between the H alpha and far-UV SFR scales. Far-infrared and thermal radio continuum data available for a subset of our sample allow us to estimate the attenuation in the UV and at H alpha independently. The UV and H alpha attenuations appear to be correlated, and confirm systematically higher attenuations in the UV. Although the galaxies in our sample show modest levels of attenuation (with median values of 0.9 mag at H alpha and 1.4 mag at 1550 Angstroms), the range across the sample is large, around 4 mag for H alpha and around 5 mag in the far-UV (1550 Angstroms). This indicates that the application of a single characteristic extinction correction to H alpha or UV SFRs is only realistic for large, well-defined and well-studied galaxy samples, and that extinction bias may be important for UV or emission-line selected samples of star-forming galaxies.

14 pages; 4 embedded figures; accepted for publication in ApJ

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