Dust Attenuation in Clumpy, Star-Forming Galaxies at 0.07 < z < 0.14
  Dust attenuation in galaxies has been extensively studied nearby, however,
there are still many unknowns regarding attenuation in distant galaxies. We
contribute to this effort using observations of star-forming galaxies in the
redshift range z = 0.05-0.15 from the DYNAMO survey. Highly star-forming DYNAMO
galaxies share many similar attributes to clumpy, star-forming galaxies at high
redshift. Considering integrated Sloan Digital Sky Survey observations, trends
between attenuation and other galaxy properties for DYNAMO galaxies are well
matched to star-forming galaxies at high redshift. Integrated gas attenuations
of DYNAMO galaxies are 0.2-2.0 mags in the V-band, and the ratio of stellar
E(B-V) and gas E(B-V) is 0.78-0.08 (compared to 0.44 at low redshift). Four
highly star-forming DYNAMO galaxies were observed at H-alpha using the Hubble
Space Telescope and at Pa-alpha using integral field spectroscopy at Keck. The
latter achieve similar resolution (~0.8-1 kpc) to our HST imaging using
adaptive optics, providing resolved observations of gas attenuations of these
galaxies on sub-kpc scales. We find < 1.0 mag of variation in attenuation (at
H-alpha) from clump to clump, with no evidence of highly attenuated star
formation. Attenuations are in the range 0.3-2.2 mags in the V band, consistent
with attenuations of low redshift star-forming galaxies. The small spatial
variation on attenuation suggests that a majority of the star-formation
activity in these four galaxies occurs in relatively unobscured regions and,
thus, star-formation is well characterised by our H-alpha observations.
