1. First, a typo:  introduction, paragraph 1, line 3,
... dust emission features (diffuse interstellar bands)...

emission --> absorption.
Also, it is now generally thought that the diffuse interstellar
bands are caused by free-flying molecules, not by solid dust.
(But of course, it is ok to call dust a huge molecule).
 
--Fixed.  Thanks!
 
2. In section 4.1., you mentioned alpha_SED, it would be
helpful if you explain it a bit more so that a reader who is
not familiar with Dale+Helou_2002 will understand.
is there any trend for alpha_SED varying with galaxy morphology
or IR/UV ratio? irregulars have flat alpha_SED (so more heating
from intenser regions)? early type galaxies with steeper alpha_SED?

--There is a weak trend for lower alpha with later Hubble type, which
  makes sense.  There is a similar result for alpha vs TIR/UV.  But the 
  dispersions in these trends are so broad that I guess I prefer to not
  talk about it in detail -- but I have added a note to the text that
  there are broad trends...

3. For the IR-to-UV ratio, how about consider a simple
extinction correction for one case (say, plot a similar 
figure for Fig.12, but with dust extinction corrected)?
 
A simple approach to correct the extinction is based
on the dust mass derived from the Dale & Helou fitting
to the SED, assuming a Milky way R_V=3.1 extinction curve.
 
Another simple way to correct the extinction is just to 
multiply the stellar curve by exp(-A_V/1.086*[A_lambda/A_V])
and assume the Milky Way R_V=3.1 A_lambda/A_V law
so to see how much A_V is needed and then correct for
the GALEX UV fluexs by multiplying exp(A_V*A_lambda/A_V).
(Of course, here you need to assume that the 2mass bands are
not affected by extinction).
 
With extinction corrected IR-to-UV ratios, I guess you will get
very different dependence of this ratio with galax. optical morphology
(Figure 12). The current Figure 12 shows lower IR-to-UV ratios
for both early-type galax. and irregular galax, although for different
reasons. With extinction corrected, you will be able to differentiate
them and get insight into a lower IR/UV ratio is simply due to a lower
IR or a higher UV. 

--This is a logical suggestion.  By agreement between the SINGS and
  GALEX teams, such an analysis has been reserved for the next
  analysis paper.