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Dependence of Dust Obscuration on Star Formation Rates in Galaxies
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Draft version February 2, 2008
Preprint typeset using LATEX style emulateapj v. 11/12/01
DEPENDENCE OF DUST OBSCURATION ON STAR FORMATION RATES IN GALAXIES
J. Afonso1,2,3, A. Hopkins4,5, B. Mobasher6,7, and C. Almeida1,8
Draft version February 2, 2008
ABSTRACT
Many investigations of star formation rates (SFRs) in galaxies have explored details of dust obscura-
tion, with a number of recent analyses suggesting that obscuration appears to increase in systems with
high rates of star formation. To date these analyses have been primarily based on nearby (z ≤ 0.03)
or UV selected samples. Using 1.4GHz imaging and optical spectroscopic data from the Phoenix Deep
Survey, the SFR-dependent obscuration is explored. The use of a radio selected sample shows that
previous studies exploring SFR-dependent obscurations have been biased against obscured galaxies. The
observed relation between obscuration and SFR is found to be unsuitable to be used as an obscuration
measure for individual galaxies. Nevertheless, it is shown to be successful as a first order correction for
large samples of galaxies where no other measure of obscuration is available, out to intermediate redshifts
(z ≈ 0.8).
Subject headings: galaxies: evolution — galaxies: starburst — radio continuum: galaxies
1. introduction
Dust obscuration is currently recognized as one of the
most serious sources of uncertainty in studies of galaxy
evolution. With the recent results of far-infrared (FIR)
and sub-mm observations revealing an ever increasing
number of dusty star forming galaxies (e.g., Genzel Ce-
sarsky 2000; Ivison et al. 2000; Smail et al. 2002), the need
to unify measures of star formation rate (SFR) from inde-
pendent indicators at different wavelengths (e.g., UV, Hα,
FIR, radio continuum) is as pressing as ever.
A relatively simple prescription for dust extinction cor-
rection to SFR has been suggested by Hopkins et al. (2001)
and Sullivan et
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