An overview of the North Ecliptic Pole (NEP) deep multi-wavelength survey covering from X-ray to radio wavelengths is presented. The main science objective of this multi-wavelength project is to unveil the star-formation and AGN activities obscured by dust in the violent epoch of the Universe (z=0.5-2), when the star formation and black-hole evolution activities were much stronger than the present. The NEP deep survey with AKARI/IRC consists of two survey projects: shallow wide (8.2 sq. deg, NEP-Wide) and the deep one (0.6 sq. deg, NEP-Deep). The NEP-Deep provides us with a 15 μm or 18 μm selected sample of several thousands of galaxies, the largest sample ever made at these wavelengths. A continuous filter coverage at mid-IR wavelengths (7, 9, 11, 15, 18, and 24 μ m ) is unique and vital to diagnose the contribution from starbursts and AGNs in the galaxies at the violent epoch. The recent updates of the ancillary data are also provided: optical/near-IR magnitudes (Subaru, CFHT), X-ray (Chandra), FUV/NUV (GALEX), radio (WSRT, GMRT), optical spectra (Keck/DEIMOS etc.), Subaru/FMOS, Herschel/SPIRE, and JCMT/SCUBA-2.

ABSTRACT
1. INTRODUCTION
2. ADVANTAGES OF THE NEP DEEP SURVEY
3. OVERVIEW OF THE ANCILLARY DATA
4. THE CATALOG RELEASE AND SCOPE FOR FUTURE
REFERENCES

• H. MATSUHARA(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)
• T. WADA(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)
• T. TAKAGI(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)
• T. NAKAGAWA(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)
• K. MURATA(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)
• S. CHUREI(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)
• T. GOTO(Institute for Astronomy, University of Hawaii)
• S. OYABU(Graduate School of Science, Nagoya University)
• T.T. TAKEUCHI(Graduate School of Science, Nagoya University)
• Y. OHYAMA(Academia Sinica, Institute of Astronomy and Astrophysics)
• T. MIYAJI(Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, University of California, San Diego, Center for Astrophysics and Space Sciences)
• M. KRUMPE(European Southern Observatory, University of California, San Diego, Center for Astrophysics and Space Sciences)
• H. M. LEE(Department of Physics & Astronomy, FPRD, Seoul National University)
• M. IM(Department of Physics & Astronomy, FPRD, Seoul National University)
• S. SERJEANT(The Open University)
• C. P. PEASON(Rutherford Appleton Laboratory Oxon)
• G. WHITE(The Open University, Rutherford Appleton Laboratory Oxon)
• M. A. MALKAN(University of California)
• H. HANAMI(Iwate University)
• T. ISHIGAKI(Iwate University)
• D. BURGARELLA(LAM, OAMP, Universite Aix-Marseille, CNRS)
• AKARI NEP TEAM