Dusty Star Forming Galaxies at High Redshift

By C. Casey, D. Narayanan, A. Cooray. 2014

641 citations recorded by the source corpus.

Abstract Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L ⊙ with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both space-based and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the best-understood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al., 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c00893d1c6b6f5456b3f3d2b1356ea13315fbe76

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Citations in the corpus

• Characterization of Scuba-2 450 μm and 850 μm selected galaxies in the COSMOS field (2013, background): “Submillimeter galaxies (SMGs, canonically selected at 850µm with S850 >∼ 2– 5 mJy; Smail et al. 1997; Barger et al. 1998; Hughes et al. 1998; Eales et al. 1999) have since been shown to have a peak volume density at z ≈ 2.2− 2.5 (Chapman et al. 2003, 2005; Yun et al. 2012).”
• FORMING COMPACT MASSIVE GALAXIES (2015, background): “Many other studies have found extreme star forming galaxies by selecting them on the basis of their far-infrared, submm, or radio emission instead (e.g., Kormendy & Sanders 1992; Sanders & Mirabel 1996; Barger et al. 1998; Smail et al. 2000; Barger et al. 2001; Casey et al. 2012).”
• A deep ALMA image of the Hubble Ultra Deep Field (2016, background): “…observations are unable to uncover the most extreme star-forming galaxies, which, following the breakthroughs in far-IR/sub-mm astronomy at the end of the last century, are known to be enshrouded in dust (Smail, Ivison & Blain 1997; Hughes et al. 1998; Barger et al. 1998; Eales et al. 1999).”
• THE EVOLUTION OF GALAXY NUMBER DENSITY AT z < 8 AND ITS IMPLICATIONS (2016, background): “Using the number densities from Casey et al. (2014), we find that between 0.1-1 mJy there are 6.2±0.05× 108 extra galaxies across the sky not matched to optical or near-infrared detections.”
• The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, background): “They belong to the subsample of dusty galaxies; more than 80% of them have E(B − V) > 0.3, and an uncertain photometric redshift as mentioned above (see Spitler et al. 2014; Casey et al. 2014a; Martis et al. 2016, for further insight into massive passive galaxies at high z).”
• An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, methodology): “…(SMGs) with 850-μm flux densities of S850 1–10 mJy were first uncovered over 20 years ago using the atmospheric window around 850 μm with the SCUBA instrument on the James Clerk Maxwell Telescope (JCMT) (Smail, Ivison & Blain 1997; Barger et al. 1998; Hughes et al. 1998; Eales et al. 1999).”
• AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, background): “The first sensitive sub-millimeter bolometer camera (the SCUBA) unveiled a new population of galaxies over a decade ago (Smail et al. 1997; Barger et al. 1998; Hughes et al. 1998) with very large sub-millimeter fluxes (>1mJy at 850 μm), which were named sub-millimeter galaxies (SMGs).14 These…”
• The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, background): “As discussed in a number of studies (Reddy et al. 2006b, 2010; Penner et al. 2012; Casey et al. 2014b; Koprowski et al. 2016), dusty galaxies in general can exhibit a wide range in β (from very blue to very red) depending on the particular spatial configuration of the dust and UV-emitting stars.”
• KILOPARSEC-SCALE DUST DISKS IN HIGH-REDSHIFT LUMINOUS SUBMILLIMETER GALAXIES (2016, background): “The most luminous galaxies at high–redshift are the dusty star–forming galaxies originally detected in the submillimeter and known as submillimeter galaxies (SMG; e.g., Blain et al. 2002; Solomon & Vanden Bout 2005; Carilli & Walter 2013; Casey et al. 2014).”
• Cosmic X-ray surveys of distant active galaxies (2015, background): “4 of Casey et al 2014).”
• A Redshift-independent Efficiency Model: Star Formation and Stellar Masses in Dark Matter Halos at z ≳ 4 (2018, background): “However, the results deviate from it for more IR-luminous, highly obscured galaxies, such as high-z sub-millimeter sources with SFR of up to 1000 M yr −1 (Casey et al. 2014).”
• An Extreme Protocluster of Luminous Dusty Starbursts in the Early Universe (2017, background): “The bulk of their star formation occurred at >z 2, over relatively short periods, in a phase compatible with luminous dusty star-forming galaxies (DSFGs —e.g., Casey et al. 2014) at > –z 3 4 (Collins et al. 2009; Thomas et al. 2010; Gobat et al. 2011; Zeimann et al. 2012).”