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ALMA twenty-six arcmin2 survey of GOODS-S at one millimeter (ASAGAO)

Published online by Cambridge University Press:  04 June 2020

B. Hatsukade
Affiliation:
Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo181-0015, Japan email: hatsukade@ioa.s.u-tokyo.ac.jp
K. Kohno
Affiliation:
Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo181-0015, Japan email: hatsukade@ioa.s.u-tokyo.ac.jp Research Center for the Early Universe, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo113-0033, Japan
Y. Yamaguchi
Affiliation:
Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo181-0015, Japan email: hatsukade@ioa.s.u-tokyo.ac.jp
H. Umehata
Affiliation:
Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo181-0015, Japan email: hatsukade@ioa.s.u-tokyo.ac.jp RIKEN Cluster for Pioneering Research, 2-1 Hirosawa, Wako-shi, Saitama351-0198, Japan
Y. Ao
Affiliation:
Purple Mountain Observatory & Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, 8 Yuanhua Road, Nanjing210034, China
I. Aretxaga
Affiliation:
Instituto Nacional de Astrofsica, Óptica y Electrónica (INAOE), Luis Enrique Erro 1, Sta. Ma. Tonantzintla, Puebla, Mexico
K. I. Caputi
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700AV Groningen, The Netherlands
J. S. Dunlop
Affiliation:
Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ UK
E. Egami
Affiliation:
Steward Observatory, University of Arizona, 933 N. Cherry Ave, Tucson, AZ85721, USA
D. Espada
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan
S. Fujimoto
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, Kashiwa, Chiba277-8582, Japan
N. Hayatsu
Affiliation:
Department of Physics, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo, 113-0033, Japan European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany
D. H. Hughes
Affiliation:
Instituto Nacional de Astrofsica, Óptica y Electrónica (INAOE), Luis Enrique Erro 1, Sta. Ma. Tonantzintla, Puebla, Mexico
S. Ikarashi
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700AV Groningen, The Netherlands
D. Iono
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan
R. J. Ivison
Affiliation:
Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ UK European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany
R. Kawabe
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan
T. Kodama
Affiliation:
Astronomical Institute, Tohoku University, Aramaki, Aoba-ku, Sendai, Miyagi980-8578, Japan
M. Lee
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya464-8601, Japan
Y. Matsuda
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan
K. Nakanishi
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan
K. Ohta
Affiliation:
Department of Astronomy, Kyoto University, Kyoto606-8502, Japan
M. Ouchi
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, Kashiwa, Chiba277-8582, Japan Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, Japan277-8583 (Kavli IPMU, WPI)
W. Rujopakarn
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, Japan277-8583 (Kavli IPMU, WPI) Department of Physics, Faculty of Science, Chulalongkorn University, 254 Phayathai Road, Pathumwan, Bangkok10330, Thailand National Astronomical Research Institute of Thailand (Public Organization), Don Kaeo, Mae Rim, Chiang Mai50180, Thailand
T. Suzuki
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan
Y. Tamura
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya464-8601, Japan
Y. Ueda
Affiliation:
Department of Astronomy, Kyoto University, Kyoto606-8502, Japan
T. Wang
Affiliation:
Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo181-0015, Japan email: hatsukade@ioa.s.u-tokyo.ac.jp National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-8588, Japan
W.-H. Wang
Affiliation:
Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan
G. W. Wilson
Affiliation:
Department of astronomy, University of Massachusetts, Amherst, MA01003, USA
Y. Yoshimura
Affiliation:
Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo181-0015, Japan email: hatsukade@ioa.s.u-tokyo.ac.jp
M. S. Yun
Affiliation:
Department of astronomy, University of Massachusetts, Amherst, MA01003, USA
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Abstract

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The ALMA twenty-six arcmin2 survey of GOODS-S at one millimeter (ASAGAO) is a deep (1σ ∼ 61μJy/beam) and wide area (26 arcmin2) survey on a contiguous field at 1.2 mm. By combining with archival data, we obtained a deeper map in the same region (1σ ∼ 30μJy/beam−1, synthesized beam size 0.59″ × 0.53″), providing the largest sample of sources (25 sources at 5σ, 45 sources at 4.5σ) among ALMA blank-field surveys. The median redshift of the 4.5σ sources is 2.4. The number counts shows that 52% of the extragalactic background light at 1.2 mm is resolved into discrete sources. We create IR luminosity functions (LFs) at z = 1–3, and constrain the faintest luminosity of the LF at 2 < z < 3. The LFs are consistent with previous results based on other ALMA and SCUBA-2 observations, which suggests a positive luminosity evolution and negative density evolution.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

References

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