1. GOODS-ALMA 2.0: Source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies
- Author
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Gómez-Guijarro, C., Elbaz, D., Xiao, M., Béthermin, M., Franco, M., Magnelli, B., Daddi, E., Dickinson, M., Demarco, R., Inami, H., Rujopakarn, W., Magdis, G.E., Shu, X., Chary, R., Zhou, L., Alexander, D.M., Bournaud, F., Ciesla, L., Ferguson, H.C., Finkelstein, S.L., Finlez, C., Giavalisco, M., Iono, D., Juneau, S., Kartaltepe, J.S., Lagache, G., Le Floc'H, E., Leiton, R., Lin, L., Messias, H., Motohara, K., Mullaney, J., Nagar, N.M., Okumura, K., Pannella, M., Papovich, C., Pope, A., Sargent, M.T., Silverman, J.D., Treister, E., Wang, T., Le Floc’h, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Hertfordshire [Hatfield] (UH), NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), Universidad de Concepción - University of Concepcion [Chile], Hiroshima University, Chulalongkorn University [Bangkok], Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Anhui Normal University, California Institute of Technology (CALTECH), Nanjing University (NJU), Durham University, Space Telescope Science Institute (STSci), University of Texas at Austin [Austin], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), National Astronomical Observatory of Japan (NAOJ), Rochester Institute of Technology, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Academia Sinica, The University of Tokyo (UTokyo), University of Sheffield [Sheffield], Università degli studi di Trieste = University of Trieste, Texas A&M University System, University of Sussex, Pontificia Universidad Católica de Chile (UC), Univ New South Wales, MERLin Sch Chem Engn, Sydney, NSW 2052, Australia, and We thank G. Pöpping, C. del P. Lagos, and J. A.Zavala for providing the predicted number counts from their models plotted in Fig. 11. M.F. acknowledges the support from STFC (grant number ST/R000905/1). G.E.M. acknowledges the Villum Fonden research grant 13160 ‘Gas to stars, stars to dust: tracing star formation across cosmic time’ and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant No. 140. H.I. acknowledges support from JSPS KAKENHI Grant Number JP19K23462 and JP21H01129. M.T.S. acknowledges support from a Scientific Exchanges visitor fellowship (IZSEZO_202357) from the Swiss National Science Foundation. This papermakes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00543.S and ADS/JAO.ALMA#2017.1.00755.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We are grateful to the anonymous referee, whose comments have been very useful to improving our work
- Subjects
submillimeter: galaxies ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,structure [Galaxies] ,PHYSICAL-PROPERTIES ,FOS: Physical sciences ,Flux ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,star formation [Galaxies] ,01 natural sciences ,GMASS ULTRADEEP SPECTROSCOPY ,high-redshift [Galaxies] ,galaxies [Submillimeter] ,galaxies: high-redshift ,0103 physical sciences ,STAR-FORMING GALAXIES ,Sensitivity (control systems) ,Continuum (set theory) ,DEEP FIELD-SOUTH ,MAIN-SEQUENCE ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Effective radius ,Physics ,DEGREE EXTRAGALACTIC SURVEY ,SUBMILLIMETER GALAXIES ,010308 nuclear & particles physics ,photometry [Galaxies] ,Homogeneity (statistics) ,MASSIVE GALAXIES ,Astronomy and Astrophysics ,evolution [Galaxies] ,FAR-INFRARED PROPERTIES ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,galaxies: photometry ,LUMINOSITY FUNCTION ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,galaxies: star formation ,galaxies: structure ,Astrophysics::Earth and Planetary Astrophysics ,galaxies: evolution ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Submillimeter/millimeter observations of dusty star-forming galaxies with the Atacama Large Millimeter/submillimeter Array (ALMA) have shown that dust continuum emission generally occurs in compact regions smaller than the stellar distribution. However, it remains to be understood how systematic these findings are. Studies often lack homogeneity in the sample selection, target discontinuous areas with inhomogeneous sensitivities, and suffer from modest $uv$ coverage coming from single array configurations. GOODS-ALMA is a 1.1mm galaxy survey over a continuous area of 72.42arcmin$^2$ at a homogeneous sensitivity. In this version 2.0, we present a new low resolution dataset and its combination with the previous high resolution dataset from the survey, improving the $uv$ coverage and sensitivity reaching an average of $��= 68.4��$Jy beam$^{-1}$. A total of 88 galaxies are detected in a blind search (compared to 35 in the high resolution dataset alone), 50% at $S/N_{peak} \geq 5$ and 50% at $3.5 \leq S/N_{peak} \leq 5$ aided by priors. Among them, 13 out of the 88 are optically dark or faint sources ($H$- or $K$-band dropouts). The sample dust continuum sizes at 1.1mm are generally compact, with a median effective radius of $R_{e} = 0"10 \pm 0"05$ (a physical size of $R_{e} = 0.73 \pm 0.29$kpc at the redshift of each source). Dust continuum sizes evolve with redshift and stellar mass resembling the trends of the stellar sizes measured at optical wavelengths, albeit a lower normalization compared to those of late-type galaxies. We conclude that for sources with flux densities $S_{1.1mm} > 1$mJy, compact dust continuum emission at 1.1mm prevails, and sizes as extended as typical star-forming stellar disks are rare. The $S_{1.1mm} < 1$mJy sources appear slightly more extended at 1.1mm, although they are still generally compact below the sizes of typical star-forming stellar disks., Accepted by A&A. 30 pages, 18 figures
- Published
- 2022
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