Volume 620, December 2018
|Number of page(s)||26|
|Published online||11 December 2018|
GOODS-ALMA: 1.1 mm galaxy survey
I. Source catalog and optically dark galaxies
AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, France
2 Aix-Marseille Univ., CNRS, LAM, Laboratoire d’Astrophysique de Marseille, Marseille, France
3 Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
4 Leiden Observatory, Leiden University, 2300 RA Leiden, The Netherlands
5 National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA
6 Department of Astronomy, Universidad de Concepción, Casilla 160-C, Concepción, Chile
7 Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
8 Center for Extragalactic Astronomy, Department of Physics, Durham University, Durham DH1 3LE, UK
9 Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
10 Fakultät für Physik der Ludwig-Maximilians-Universität, 81679 München, Germany
11 Astronomy Department, University of Massachusetts, Amherst, MA 01003, USA
12 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
13 Infrared Processing and Analysis Center, MS314-6, California Institute of Technology, Pasadena, CA 91125, USA
14 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
15 Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA
16 Univ. Lyon, Univ. Lyon1, ENS de Lyon, CNRS, Center de Recherche Astrophysique de Lyon (CRAL) UMR5574, 69230 Saint-Genis-Laval, France
17 National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
18 SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
19 Instituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretaña 1111, Valparaiso, Chile
20 Institute of Astronomy & Astrophysics, Academia Sinica, Taipei 10617, Taiwan
21 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Mariesvej 30, 2100 Copenhagen, Denmark
22 Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, 15236 Athens, Greece
23 Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura 763-0355, Santiago, Chile
24 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, 19 Santiago, Chile
25 Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
26 Department of Physics and Astronomy, The University of Sheffield, Hounsfield Road, Sheffield S3 7RH, UK
27 Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843-4242, USA
28 George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, College Station, TX 77843-4242, USA
29 Scientific Support Office, ESA/ESTEC, Noordwijk, The Netherlands
30 Department of Physics, Faculty of Science, Chulalongkorn University, 254 Phayathai Road, Pathumwan, Bangkok 10330, Thailand
31 National Astronomical Research Institute of Thailand (Public Organization), Donkaew, Maerim, Chiangmai 50180, Thailand
32 Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
33 Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UK
34 Department of Physics, Anhui Normal University, Wuhu Anhui 241000, PR China
35 School of Astronomy and Space Science, Nanjing University, Nanjing 210093, PR China
Accepted: 30 July 2018
Aims. We present a 69 arcmin2 ALMA survey at 1.1 mm, GOODS-ALMA, matching the deepest HST-WFC3 H-band part of the GOODS-South field.
Methods. We tapered the 0″24 original image with a homogeneous and circular synthesized beam of 0″60 to reduce the number of independent beams – thus reducing the number of purely statistical spurious detections – and optimize the sensitivity to point sources. We extracted a catalog of galaxies purely selected by ALMA and identified sources with and without HST counterparts down to a 5σ limiting depth of H = 28.2 AB (HST/WFC3 F160W).
Results. ALMA detects 20 sources brighter than 0.7 mJy at 1.1 mm in the 0″60 tapered mosaic (rms sensitivity σ ≃ 0.18 mJy beam−1) with a purity greater than 80%. Among these detections, we identify three sources with no HST nor Spitzer-IRAC counterpart, consistent with the expected number of spurious galaxies from the analysis of the inverted image; their definitive status will require additional investigation. We detect additional three sources with HST counterparts either at high significance in the higher resolution map, or with different detection-algorithm parameters ensuring a purity greater than 80%. Hence we identify in total 20 robust detections.
Conclusions. Our wide contiguous survey allows us to push further in redshift the blind detection of massive galaxies with ALMA with a median redshift of z = 2.92 and a median stellar mass of M⋆ = 1.1 × 1011 M⊙. Our sample includes 20% HST-dark galaxies (4 out of 20), all detected in the mid-infrared with Spitzer-IRAC. The near-infrared based photometric redshifts of two of them (z ∼ 4.3 and 4.8) suggest that these sources have redshifts z > 4. At least 40% of the ALMA sources host an X-ray AGN, compared to ∼14% for other galaxies of similar mass and redshift. The wide area of our ALMA survey provides lower values at the bright end of number counts than single-dish telescopes affected by confusion.
Key words: galaxies: high-redshift / galaxies: evolution / galaxies: star formation / galaxies: active / galaxies: photometry / submillimeter: galaxies
© ESO 2018
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