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The Korean Astronomical Society (한국천문학회)
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HYPER SUPRIME-CAMERA SURVEY OF THE AKARI NEP WIDE FIELD

  • Goto, Tomotsugu (Institute of Astronomy, National Tsing Hua University) ;
  • Toba, Yoshiki (Research Center for Space and Cosmic Evolution, Ehime University) ;
  • Utsumi, Yousuke (Hiroshima University) ;
  • Oi, Nagisa (Institute of Space and Astronautical Science, JAXA) ;
  • Takagi, Toshinobu (Institute of Space and Astronautical Science, JAXA) ;
  • Malkan, Matt (Department of Physics and Astronomy, UCLA) ;
  • Ohayma, Youichi (Institute of Astronomy and Astrophysics Academia Sinica) ;
  • Murata, Kazumi (Institute of Space and Astronautical Science, JAXA) ;
  • Price, Paul (Princeton University, Department of Astrophysical Sciences,) ;
  • Karouzos, Marios (Department of Physics & Astronomy, FPRD, Seoul National University) ;
  • Matsuhara, Hideo (Institute of Space and Astronautical Science, JAXA) ;
  • Nakagawa, Takao (Institute of Space and Astronautical Science, JAXA) ;
  • Wada, Takehiko (Institute of Space and Astronautical Science, JAXA) ;
  • Serjeant, Steve (Department of Physical Sciences, The Open University) ;
  • Burgarella, Denis (Aix-Marseille Universite, CNRS, LAM (Laboratoire d'Astrophysique de Marseille)) ;
  • Buat, Veronique (Aix-Marseille Universite, CNRS, LAM (Laboratoire d'Astrophysique de Marseille)) ;
  • Takada, Masahiro (Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo) ;
  • Miyazaki, Satoshi (National Astronomical Observatory of Japan) ;
  • Oguri, Masamune (Department of Physics, University of Tokyo) ;
  • Miyaji, Takamitsu (Instituto de Astronoma, Universidad Nacional Autnoma de Mxico) ;
  • Oyabu, Shinki (Institute of Astronomy, National Tsing Hua University) ;
  • White, Glenn (Department of Physical Sciences, The Open University) ;
  • Takeuchi, Tsutomu (Division of Particle and Astrophysical Science, Nagoya University) ;
  • Inami, Hanae (Institute of Astronomy, National Tsing Hua University) ;
  • Perason, Chris (Department of Physical Sciences, The Open University) ;
  • Malek, Katarzyna (Division of Particle and Astrophysical Science, Nagoya University) ;
  • Marchetti, Lucia (Division of Particle and Astrophysical Science, Nagoya University) ;
  • Lee, HyungMoK (Department of Physics & Astronomy, FPRD, Seoul National University) ;
  • Im, Myung (Department of Physics & Astronomy, FPRD, Seoul National University) ;
  • Kim, Seong Jin (Department of Physics & Astronomy, FPRD, Seoul National University) ;
  • Koptelova, Ekaterina (Institute of Astronomy, National Tsing Hua University) ;
  • Chao, Dani (Institute of Astronomy, National Tsing Hua University) ;
  • Wu, Yi-Han (Institute of Astronomy, National Tsing Hua University) ;
  • AKARI NEP Survey team (Institute of Space and Astronautical Science, JAXA) ;
  • AKARIAll Sky Survey Team (Institute of Space and Astronautical Science, JAXA)
  • Received : 2015.09.03
  • Accepted : 2016.10.20
  • Published : 2017.03.31
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Abstract

The extragalactic background suggests half the energy generated by stars was reprocessed into the infrared (IR) by dust. At z~1.3, 90% of star formation is obscured by dust. To fully understand the cosmic star formation history, it is critical to investigate infrared emission. AKARI has made deep mid-IR observation using its continuous 9-band filters in the NEP field ($5.4deg^2$), using ~10% of the entire pointed observations available throughout its lifetime. However, there remain 11,000 AKARI infrared sources undetected with the previous CFHT/Megacam imaging (r ~25.9ABmag). Redshift and IR luminosity of these sources are unknown. These sources may contribute significantly to the cosmic star-formation rate density (CSFRD). For example, if they all lie at 1< z <2, the CSFRD will be twice as high at the epoch. We are carrying out deep imaging of the NEP field in 5 broad bands (g, r, i, z, and y) using Hyper Suprime-Camera (HSC), which has 1.5 deg field of view in diameter on Subaru 8m telescope. This will provide photometric redshift information, and thereby IR luminosity for the previously-undetected 11,000 faint AKARI IR sources. Combined with AKARI's mid-IR AGN/SF diagnosis, and accurate midIR luminosity measurement, this will allow a complete census of cosmic star-formation/AGN accretion history obscured by dust.

Keywords

References

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