Stellar and Dust Properties of a Complete Sample of Massive Dusty
  Galaxies at $1 \le z \le 4$ from MAGPHYS Modeling of UltraVISTA DR3 and
  Herschel Photometry
  We investigate the stellar and dust properties of massive (log$(M_*/M_\odot)
\ge 10.5$) and dusty ($A_V \ge 1$) galaxies at $1 \le z \le 4$ by modeling
their spectral energy distributions (SEDs) obtained from the combination of
UltraVISTA DR3 photometry and \textit{Herschel} PACS-SPIRE data using MAGPHYS.
Although the rest-frame U-V vs V-J (UVJ) diagram traces well the star-formation
rates (SFR) and dust obscuration (A$_V$) out to $z \sim 3$, $\sim$15-20\% of
the sample surprisingly resides in the quiescent region of the UVJ diagram,
while $\sim50$\% at $3<z<4$ fall in the unobscured star-forming region. The
median SED of massive dusty galaxies exhibits weaker MIR and UV emission, and
redder UV slopes with increasing cosmic time. The IR emission for our sample
has a significant contribution ($>20\%$) from dust heated by evolved stellar
populations rather than star formation, demonstrating the need for panchromatic
SED modeling. The local relation between dust mass and SFR is followed only by
a sub-sample with cooler dust temperatures, while warmer objects have reduced
dust masses at a given SFR. Most star-forming galaxies in our sample do not
follow local IRX-$\beta$ relations, though IRX does strongly correlate with
A$_V$. Our sample follows local relations, albeit with large scatter, between
ISM diagnostics and sSFR. We show that FIR-detected sources represent the
extreme of a continuous population of dusty galaxies rather than a
fundamentally different population. Finally, using commonly adopted relations
to derive SFRs from the combination of the rest-frame UV and the observed
24$\mu$m is found to overestimate the SFR by a factor of 3-5 for the galaxies
in our sample.
