paper

Identifying and Characterizing the Most Heavily Dust-Obscured Galaxies at

arXiv:2211.12662 · doi:10.1093/mnras/stac3455

Abstract

We present 65 extremely dust-obscured galaxies from the UltraVISTA DR3 survey of the COSMOS field at . In contrast to other studies of dusty galaxies, we select our sample based on dust attenuation measured by UV-MIR spectral energy distribution (SED) modeling that allows for extreme attenuation levels. We construct our sample by making cuts at , A, and log(M/M). This method reliably selects galaxies exhibiting independent indicators of significant dust content, including FIR detection rates. We perform panchromatic SED modeling with matched photometry and find stellar and dust properties that differ from typical sub-millimeter galaxy (SMG) samples as well as sources matched in redshift and stellar mass. Our sources have lower star formation rates and higher A than SMGs, but comparable total IR luminosities. Most of our sample falls on or near the star-forming main sequence for this redshift range. Finally, we perform a morphological analysis with GALFIT using the -band images and and imaging when available. Typical axis ratios of suggest disk-like morphology for the majority of our sources, and we note only three apparent merging systems. Our sample generally agrees with the size-mass relation for star-forming galaxies, with a tail extending to smaller sizes. We conclude that the most heavily obscured galaxies in this redshift range share many characteristics with typical star-forming galaxies, forming a population of dusty galaxies that overlaps, but is not encompassed by, those selected through dust emission.

arXiv commentAccepted for publication in MNRAS

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