English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

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 modelingtheir spectral energy distributions (SEDs) obtained from the combination ofUltraVISTA 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-formationrates (SFR) and dust obscuration (A$_V$) out to $z \sim 3$, $\sim$15-20\% ofthe sample surprisingly resides in the quiescent region of the UVJ diagram,while $\sim50$\% at $3<z<4$ fall in the unobscured star-forming region. Themedian SED of massive dusty galaxies exhibits weaker MIR and UV emission, andredder UV slopes with increasing cosmic time. The IR emission for our samplehas a significant contribution ($>20\%$) from dust heated by evolved stellarpopulations rather than star formation, demonstrating the need for panchromaticSED modeling. The local relation between dust mass and SFR is followed only bya sub-sample with cooler dust temperatures, while warmer objects have reduceddust masses at a given SFR. Most star-forming galaxies in our sample do notfollow local IRX-$\beta$ relations, though IRX does strongly correlate withA$_V$. Our sample follows local relations, albeit with large scatter, betweenISM diagnostics and sSFR. We show that FIR-detected sources represent theextreme of a continuous population of dusty galaxies rather than afundamentally different population. Finally, using commonly adopted relationsto derive SFRs from the combination of the rest-frame UV and the observed24$\mu$m is found to overestimate the SFR by a factor of 3-5 for the galaxiesin our sample.

astrophysical journal/the astrophysical journal

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