We selected 47 DOGs at z ~ 1:5 using optical R (or r' ), AKARI 18 μm, and 24 μm color in the AKARI North Ecliptic Pole (NEP) Deep survey field. Using the colors among 3, 4, 7, and 9μm, we classified them into 3 groups; bump DOGs (23 sources), power-law DOGs (16 sources), and unknown DOGs (8 sources). We built spectral energy distributions (SEDs) with optical to far-infrared photometric data and investigated their properties using SED fitting method. We found that AGN activity such as a AGN contribution to the infrared luminosity and a Chandra detection rate for bump and power-law DOGs are signicantly different, while stellar component properties like a stellar mass and a star-formation rate are similar to each other. A specific star-formation rate range of power-law DOGs is slightly higher than that of bump DOGs with wide overlap. Herschel/PACS detection rates are almost the same between bump and power-law DOGs. On the other hand SPIRE detection rates show large differences between bump and power-law DOGs. These results might be explained by differences in dust temperatures. Both groups of DOGs host hot and/or warm dust ( 50 Kelvin), and many bump DOGs contain cooler dust ( < 30 Kelvin).

ABSTRACT
1. INTRODUCTION
2. SAMPLE SELECTION
    2.1. Imaging Data
    2.2. Sample Selection
3. SED FITTING
4. PROPERTIES OF BUMP AND POWER-LAW DOGs
    4.1. Stellar and AGN properties
    4.2. Properties of Dust Temperature
    REFERENCES

• Nagisa Oi(Department of Infrared Astrophysics Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)
• Hideo Matsuhara(Department of Infrared Astrophysics Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency/Department of Space and Astronautical Science, The Graduate University for Advanced Studies)
• Chris Pearson(Department of Physical Sciences, The Open University/Rutherford Appleton Laboratory Oxon/Oxford Astrophysics, Denys Wilkinson Building, University of Oxford)
• Veronique Buat(Aix-Marseille Universite, CNRS, LAM (Laboratoire d'Astrophysique de Marseille))
• Denis Burgarella(Aix-Marseille Universite, CNRS, LAM (Laboratoire d'Astrophysique de Marseille))
• Matt Malkan(Department of Physics and Astronomy, UCLA)
• Takamitsu Miyaji(Universidad Nacional Autonoma de Mexico)
• AKARI-NEP team(Department of Infrared Astrophysics Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)