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SXDF-UDS-CANDELS-ALMA 1.5 arcmin2 deep survey

Published online by Cambridge University Press:  17 August 2016

K. Kohno ,
Y. Yamaguchi ,
Y. Tamura ,
K. Tadaki ,
B. Hatsukade ,
S. Ikarashi ,
K.I. Caputi ,
W. Rujopakarn ,
R.J. Ivison  and
J.S. Dunlop
...Show all authors
K. Kohno
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan email: kkohno@ioa.s.u-tokyo.ac.jp
Y. Yamaguchi
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan email: kkohno@ioa.s.u-tokyo.ac.jp
Y. Tamura
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan email: kkohno@ioa.s.u-tokyo.ac.jp
K. Tadaki
Affiliation:
Max-Planck-Institut für extraterrestrische Physik (MPE), Garching, Germany
B. Hatsukade
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
S. Ikarashi
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, The Netherlands
K.I. Caputi
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, The Netherlands
W. Rujopakarn
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo, Chiba, Japan Department of Physics, Faculty of Science, Chulalongkorn University, Bangkok, Thailand
R.J. Ivison
Affiliation:
European Southern Observatory, Garching, Germany Institute for Astronomy, University of Edinburgh, Royal Observatory, UK
J.S. Dunlop
Affiliation:
Institute for Astronomy, University of Edinburgh, Royal Observatory, UK
K. Motohara
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan email: kkohno@ioa.s.u-tokyo.ac.jp
H. Umehata
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan email: kkohno@ioa.s.u-tokyo.ac.jp European Southern Observatory, Garching, Germany
K. Yabe
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo, Chiba, Japan
W.H. Wang
Affiliation:
Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Taipei, Taiwan
T. Kodama
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
Y. Koyama
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
M. Hayashi
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
Y. Matsuda
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
D. Hughes
Affiliation:
Instituto Nacional de Astrofsica, Óptica y Electrónica (INAOE), Puebla, Mexico
I. Aretxaga
Affiliation:
Instituto Nacional de Astrofsica, Óptica y Electrónica (INAOE), Puebla, Mexico
G.W. Wilson
Affiliation:
Department of Astronomy, University of Massachusetts, Amherst, USA
M.S. Yun
Affiliation:
Department of Astronomy, University of Massachusetts, Amherst, USA
K. Ohta
Affiliation:
Department of Astronomy, Kyoto University, Kyoto, Japan
M. Akiyama
Affiliation:
Astronomical Institute, Tohoku University, Sendai, Japan
R. Kawabe
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
D. Iono
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
K. Nakanishi
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
M. Lee
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
R. Makiya
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan email: kkohno@ioa.s.u-tokyo.ac.jp
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Abstract

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We have conducted 1.1 mm ALMA observations of a contiguous 105” × 50” or 1.5 arcmin2 window in the SXDF-UDS-CANDELS. We achieved a 5σ sensitivity of 0.28 mJy, giving a flat sensus of dusty star-forming galaxies with LIR ~6×1011L⊙ (if Tdust=40K) up to z ~ 10 thanks to the negative K-correction at this wavelength. We detected 5 brightest sources (S/N>6) and 18 low-significant sources (5>S/N>4; they may contain spurious detections, though). One of the 5 brightest ALMA sources (S1.1mm = 0.84 ± 0.09 mJy) is extremely faint in the WFC3 and VLT/HAWK-I images, demonstrating that a contiguous ALMA imaging survey uncovers a faint dust-obscured population invisible in the deep optical/near-infrared surveys. We find a possible [CII]-line emitter at z=5.955 or a low-z CO emitting galaxy within the field, allowing us to constrain the [CII] and/or CO luminosity functions across the history of the universe.

Keywords

galaxies: starburst – galaxies: high-redshift – submillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S319: Galaxies at High Redshift and Their Evolution Over Cosmic Time , August 2015 , pp. 92 - 95
Copyright
Copyright © International Astronomical Union 2016 

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