  Panchromatic analysis of galaxy spectral energy distributions, spanning from
the ultraviolet to the far-infrared, probes not only the stellar population but
also the properties of interstellar dust through its extinction and
long-wavelength reemission. However little work has exploited the full power of
such fitting to constrain the redshift evolution of dust temperature in
galaxies. To do so, we simultaneously fit ultraviolet, optical and infrared
observations of stacked galaxy subsamples at a range of stellar masses and
photometric redshifts at 0<$z$<5, using an energy-balance formalism. However,
we find UV-emission beyond the Lyman limit in some photometric redshift
selected galaxy subsamples, giving rise to the possibility of contaminated
observations. We carefully define a robust, clean subsample which extends to no
further than $z$~2. This has consistently lower derived temperatures by
$4.0^{+5.0}_{-1.9}$ K, relative to the full sample. We find a linear increase
in dust temperature with redshift, with $T_d(z)=(4.8\pm1.5) \times z +
(26.2\pm1.5)$ K. Our inferred temperature evolution is consistent with a modest
rise in dust temperature with redshift, but inconsistent with some previous
analyses. We also find a majority of photometrically-selected subsamples at
$z$>4.5 under-predict the IR emission while giving reasonable fits to the
UV-optical. This could be due to a spatial disconnect in the locations of the
UV and IR emission peaks, suggesting that an energy-balance formalism may not
always be applicable in the distant Universe.
