  We study dust attenuation and stellar mass of $\rm z\sim 0.6$ star-forming
galaxies using new SWIRE observations in IR and GALEX observations in UV. Two
samples are selected from the SWIRE and GALEX source catalogs in the
SWIRE/GALEX field ELAIS-N1-00 ($\Omega = 0.8$ deg$^2$). The UV selected sample
has 600 galaxies with photometric redshift (hereafter photo-z) $0.5 \leq z \leq
0.7$ and NUV$\leq 23.5$ (corresponding to $\rm L_{FUV} \geq 10^{9.6} L_\sun$).
The IR selected sample contains 430 galaxies with $f_{24\mu m} \geq 0.2$ mJy
($\rm L_{dust} \geq 10^{10.8} L_\sun$) in the same photo-z range. It is found
that the mean $\rm L_{dust}/L_{FUV}$ ratios of the z=0.6 UV galaxies are
consistent with that of their z=0 counterparts of the same $\rm L_{FUV}$. For
IR galaxies, the mean $\rm L_{dust}/L_{FUV}$ ratios of the z=0.6 LIRGs ($\rm
L_{dust} \sim 10^{11} L_\sun$) are about a factor of 2 lower than local LIRGs,
whereas z=0.6 ULIRGs ($\rm L_{dust} \sim 10^{12} L_\sun$) have the same mean
$\rm L_{dust}/L_{FUV}$ ratios as their local counterparts. This is consistent
with the hypothesis that the dominant component of LIRG population has changed
from large, gas rich spirals at z$>0.5$ to major-mergers at z=0. The stellar
mass of z=0.6 UV galaxies of $\rm L_{FUV} \leq 10^{10.2} L_\sun$ is about a
factor 2 less than their local counterparts of the same luminosity, indicating
growth of these galaxies. The mass of z=0.6 UV lunmous galaxies (UVLGs: $\rm
L_{FUV} > 10^{10.2} L_\sun$) and IR selected galaxies, which are nearly
exclusively LIRGs and ULIRGs, is the same as their local counterparts.
