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

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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.