Ultraviolet-to-far-infra-red self-consistent analysis of the stellar
  populations of massive starburst galaxies at intermediate redshifts
  We study in detail the properties of the stellar populations of 111 massive
($\log(M_{\star}/\mathrm{M}_\odot) \ge 10)$ dusty (FIR-selected) starburst
($SFR/SFR_\mathrm{MS}>2$) galaxies at $0.7<z<1.2$. For that purpose, we use
self-consistent methods that analyse the UV-to-FIR broadband observations in
terms of the stellar light and dust re-emission with energy-balance techniques.
We find that the emission of our starburst galaxies can be interpreted as a
recent star formation episode superimposed on a more evolved stellar
population. On average, the burst age is $\sim 80$ Myr and its attenuation
$\sim 2.4$ mag. Assuming our starburst galaxies at half their lifetimes, we
infer a duration of the starburst phase of $\sim 160$ Myr. The median stellar
mass and SFR are $\log(M_\star/\mathrm{M}_\odot)\sim 10.6$ and
$\sim220~\mathrm{M}_\odot~$yr$^{-1}$. Assuming this SFR and the inferred
duration of the starburst phase, the stellar mass added during this phase
corresponds to $\sim 40$ per cent the median stellar mass of our sample. The
young-population age determines the position of our galaxies in the
$M_{\star}-SFR$ plane. Galaxies located at the largest distances of the MS
present shorter young-population ages. The properties of the underlying stellar
population cannot be constrained accurately with our broadband data. We also
discuss the impact of including the FIR data and energy-balance techniques in
the analysis of the properties of the stellar populations in starburst
galaxies.
