Abstract
Abstract We make use of the ALMA twenty-Six Arcmin2 survey of GOODS-S At One-millimeter (ASAGAO), deep 1.2 mm continuum observations of a 26-arcmin2 region in the Great Observatories Origins Deep Survey-South (GOODS-S) obtained with Atacama Large Millimeter/sub-millimeter Array (ALMA), to probe dust-enshrouded star formation in K-band selected (i.e., stellar mass selected) galaxies, which are drawn from the FourStar Galaxy Evolution Survey (ZFOURGE) catalog. Based on the ASAGAO combined map, which was created by combining ASAGAO and ALMA archival data in the GOODS-South field, we find that 24 ZFOURGE sources have 1.2 mm counterparts with a signal-to-noise ratio >4.5 (1σ ≃ 30–70 μJy beam−1 at 1.2 mm). Their median redshift is estimated to be $z$median = 2.38 ± 0.14. They generally follow the tight relationship of the stellar mass versus star formation rate (i.e., the main sequence of star-forming galaxies). ALMA-detected ZFOURGE sources exhibit systematically larger infrared (IR) excess (IRX ≡ LIR/LUV) compared to ZFOURGE galaxies without ALMA detections even though they have similar redshifts, stellar masses, and star formation rates. This implies the consensus stellar-mass versus IRX relation, which is known to be tight among rest-frame-ultraviolet-selected galaxies, cannot fully predict the ALMA detectability of stellar-mass-selected galaxies. We find that ALMA-detected ZFOURGE sources are the main contributors to the cosmic IR star formation rate density at $z$ = 2–3.
Highlights
Recent studies have revealed the evolution of the cosmic star formation rate density (SFRD) as a function of redshift based on various wavelengths (e.g., Madau & Dickinson 2014; Bouwens et al 2015; Bouwens et al 2016, and references therein)
We report results of multi-wavelength analysis of ALMA 1.2-mm detected ZFOURGE sources using ASAGAO data
We find that 24 ZFOURGE sources are detected by ALMA with S/N > 4.5
Summary
Recent studies have revealed the evolution of the cosmic star formation rate density (SFRD) as a function of redshift based on various wavelengths (e.g., Madau & Dickinson 2014; Bouwens et al 2015; Bouwens et al 2016, and references therein). The fact that (sub-)millimeter flux densities are almost constant at z > 1 for galaxies with a given infrared (IR) luminosity (i.e., the negative k-correction – e.g., Blain & Longair 1996) makes it efficient to study dust-obscured star-formation activity at high redshift and the extreme star-formation rates (SFRs) of SMGs [a few 100-1000 M⊙ yr−1, modulo expectations for and observations of the stellar initial mass function (IMF) in starburst environments – Papadopoulos et al 2011; Zhang et al 2018] make them nonnegligible contributors to the cosmic SFRD (e.g., Hughes et al 1998; Casey et al 2013; Wardlow et al 2011; Swinbank et al 2014). We adopt the Chabrier IMF (Chabrier 2003) in this paper
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