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Coldz: a High Space Density of Massive Dusty Starburst Galaxies 1 Billion Years After the Big Bang ∼ DRAFT VERSION MAY 7, 2020 Preprint typeset using LATEX style AASTeX6 v. 1.0 COLDZ: A HIGH SPACE DENSITY OF MASSIVE DUSTY STARBURST GALAXIES 1 BILLION YEARS AFTER THE BIG BANG ∼ DOMINIK A. RIECHERS1,2 ,JACQUELINE A. HODGE3 ,RICCARDO PAVESI1 ,EMANUELE DADDI4 ,ROBERTO DECARLI5 , ROB J. IVISON6 ,CHELSEA E. SHARON7 ,IAN SMAIL8 ,FABIAN WALTER2,9 ,MANUEL ARAVENA10 ,PETER L. CAPAK11 , CHRISTOPHER L. CARILLI9,12 ,PIERRE COX13 ,ELISABETE DA CUNHA14,15,16 ,HELMUT DANNERBAUER17,18 , MARK DICKINSON19 ,ROBERTO NERI20 , AND JEFF WAGG21 (Received 20/01/2020; Revised 17/04/2020; Accepted 21/04/2020) 1Department of Astronomy, Cornell University, Space Sciences Building, Ithaca, NY 14853, USA 2Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany 3Leiden Observatory, Leiden University, P.O. Box 9513, NL2300 RA Leiden, The Netherlands 4Laboratoire AIM, CEA/DSM-CNRS-Univ. Paris Diderot, Irfu/Service d’Astrophysique, CEA Saclay, Orme des Merisiers, F-91191 Gif-sur-Yvette cedex, France 5INAF - Osservatorio di Astrofisica e Scienza dello Spazio, via Gobetti 93/3, I-40129, Bologna, Italy 6European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching, Germany 7Yale-NUS College, #01-220, 16 College Avenue West, Singapore 138527 8Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK 9National Radio Astronomy Observatory, Pete V. Domenici Array Science Center, P.O. Box O, Socorro, NM 87801, USA 10Núcleo de Astronomía, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile 11Spitzer Science Center, California Institute of Technology, MC 220-6, 1200 East California Boulevard, Pasadena, CA 91125, USA 12Cavendish Astrophysics Group, University of Cambridge, Cambridge, CB3 0HE, UK 13Sorbonne Université, UPMC Université Paris 6 and CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France 14Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia 15International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia 16ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) 17Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain 18Universidad de La Laguna, Departamento de Astrofísica, E-38206 La Laguna, Tenerife, Spain 19NSF’s National Optical-Infrared Astronomy Research Laboratory, 950 North Cherry Avenue, Tucson, AZ 85719, USA 20Institut de RadioAstronomie Millimétrique, 300 Rue de la Piscine, Domaine Universitaire, F-38406 Saint Martin d’Héres, France 21SKA Organization, Lower Withington, Macclesfield, Cheshire SK11 9DL, UK ABSTRACT We report the detection of CO(J=2 1) emission from three massive dusty starburst galaxies at z>5 through ! molecular line scans in the NSF’s Karl G. Jansky Very Large Array (VLA) CO Luminosity Density at High Redshift (COLDz) survey. Redshifts for two of the sources, HDF 850.1 (z=5.183) and AzTEC-3 (z=5.298), were previously known. We revise a previous redshift estimate for the third source GN10 (z=5.303), which we have independently confirmed through detections of CO J=1 0, 5 4, 6 5, and [CII] 158 µm emission with ! ! ! the VLA and the NOrthern Extended Milllimeter Array (NOEMA). We find that two currently independently confirmed CO sources in COLDz are “optically dark”, and that three of them are dust-obscured galaxies at z>5. arXiv:2004.10204v2 [astro-ph.GA] 5 May 2020 Given our survey area of 60 arcmin2, our results appear to imply a 6–55 times higher space density of such ∼ ∼ distant dusty systems within the first billion years after the Big Bang than previously thought. At least two of these z>5 galaxies show star-formation rate surface densities consistent with so-called “maximum” starbursts, but we find significant differences in CO excitation between them. This result may suggest that different frac- tions of the massive gas reservoirs are located in the dense, star-forming nuclear regions – consistent with the more extended sizes of the [CII] emission compared to the dust continuum and higher [CII]-to-far-infrared lu- minosity ratios in those galaxies with lower gas excitation. We thus find substantial variations in the conditions for star formation between z>5 dusty starbursts, which typically have dust temperatures 57% 25% warmer ∼ ± than starbursts at z=2–3 due to their enhanced star formation activity. Keywords: cosmology: observations — galaxies: active — galaxies: formation — galaxies: high-redshift — galaxies: starburst — radio lines: galaxies [email protected] 2 RIECHERS ET AL. 1. INTRODUCTION nous DSFGs appear to contain large molecular gas reservoirs Luminous dusty star-forming galaxies (DSFGs) represent that fuel their star formation, and to be significantly metal- the most intense episodes of star formation throughout cos- enriched, leading to bright CO line emission. As such, these mic history (see, e.g., Blain et al. 2002; Casey et al. 2014 for systems are preferentially picked up by panoramic molecular reviews). While the bulk of the population likely existed at line scan surveys, and they may even dominate among detec- redshifts z 1 to 3.5 (e.g., Greve et al. 2005; Bothwell et al. tions at the highest redshifts, where most other galaxy pop- ∼ 2013), a tail in their redshift distribution has been discovered ulations may exhibit only weak CO emission (e.g., Pavesi et over the past decade (e.g., Capak et al. 2008; Daddi et al. al. 2019) due to a combination of lower characteristic galaxy 2009b; Coppin et al. 2010; Smolciˇ c´ et al. 2012), found to be masses at earlier epochs, lower metallicity (which is thought reaching out to z>5 (Riechers et al. 2010; Capak et al. 2011), to lead to an increase in the αCO conversion factor, i.e., a and subsequently, z>6 (Riechers et al. 2013). Dust emission lower CO luminosity per unit molecular gas mass; see Bo- in moderately luminous galaxies1 has now been detected at latto et al. 2013 for a review), and possibly lower CO line z>8 (Tamura et al. 2019), but no luminous DSFG is currently excitation (e.g., Daddi et al. 2015). Support for this idea was 2 known at z 7 (e.g., Strandet et al. 2017). provided by the detection of the “optically-dark” z=5.183 ≥ DSFGs in the z>5 tail are thought to be rare, but their level DSFG HDF 850.1 in a molecular line scan in the Hubble of rarity is subject to debate (e.g., Asboth et al. 2016; Ivison Deep Field North (Walter et al. 2012), but the survey area of 0.5 arcmin2 was too small to make more quantitative state- et al. 2016; Bethermin et al. 2015; 2017; see also Simpson et ∼ al. 2014; 2020; Dudzeviciute et al. 2020). A significant chal- ments regarding the broader properties and space density of 3 lenge in determining the space density of such sources is the such sources. difficulty in finding them in the first place. Given their dis- To build upon this encouraging finding, and to provide a tance, classical techniques combining optical and radio iden- better understanding of the true space densities of the most tifications have been largely unsuccessful due to the faintess distant DSFGs, we here study the properties of dusty star- or lack of detection at these wavelengths, commonly lead- bursts at z>5 found in sensitive molecular line scans, based 2 ing to misidentifications given the significant positional un- on the 60 arcmin VLA COLDz survey data (Pavesi et al. ∼ 4 certainties of the classical sub/millimeter single-dish surveys 2018b; Riechers et al. 2019, hereafter P18, R19). We re- port the detection of CO(J=2 1) emission from three sys- in which they are the most easily seen (e.g., Chapman et al. ! 2005; Cowie et al. 2009, and references therein). Also, due tems initially detected in 850 µm and 1.1 mm continuum to the strong negative K correction at sub/millimeter wave- surveys, HDF 850.1, AzTEC-3, and GN10 (Hughes et al. lengths (e.g., Blain et al. 2002), it remained challenging to 1998; Pope et al. 2005; Scott et al. 2008), two of which pick out the most distant DSFGs among the much more nu- had previous correct redshift identifications through CO mea- merous specimen at z<3.5. Over the past decade, many of surements (AzTEC-3 and HDF 850.1; Riechers et al. 2010; these challenges were overcome through new observational Capak et al. 2011; Walter et al. 2012). We also report capabilities and selection techniques, such as direct identi- higher-resolution observations of AzTEC-3 and HDF 850.1, fications based on interferometric observations of the dust and detailed follow-up observations of the third system, the continuum emission (e.g., Younger et al. 2007; Smolciˇ c´ et al. “optically-dark” galaxy GN10, as well as CO line excita- 2012; Simpson et al. 2014; 2015; Brisbin et al. 2017; Stach et tion modeling for the sample. Our analysis is used to con- al. 2018; see also earlier works by, e.g., Downes et al. 1999; strain the evolution of dust temperature with redshift, and Dannerbauer et al. 2002), redshift identifications through tar- the space density of z>5 DSFGs. In Section 2, we de- geted molecular line scans (e.g., Weiß et al. 2009; Riechers scribe all observations, the results of which are given in Sec- 2011), and target selection based on sub/millimeter colors or tion 3. Section 4 provides a detailed analysis of our find- flux limits (e.g., Cox et al. 2011; Riechers et al. 2013; 2017; ings for the COLDz z>5 DSFG sample, which are discussed Dowell et al. 2014; Vieira et al. 2010; Weiß et al. 2013). Nev- in the context of all currently known z>5 DSFGs in Sec- ertheless, all of the current studies only provide incomplete tion 5.
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