Our understanding of dust emission, interaction, and evolution, is evolving. In recent years, electric dipole emission by spinning dust has been suggested to explain the anomalous microwave excess (AME), appearing between 10 and 90 Ghz. The observed frequencies suggest that spinning grains should be on the order of 10nm in size, hinting at polycyclic aromatic hydrocarbon molecules (PAHs). We present data from the AKARI/Infrared Camera (IRC) due to its high sensitivity to the PAH bands. By inspecting the IRC data for a few AME regions, we nd a preliminary indication that regions well-tted by a spinning- dust model have a higher 9 m than 18 m intensity vs. non-spinning-dust regions. Ongoing eorts to improve the analysis by using DustEM and including data from the AKARI Far Infrared Surveyor (FIS), IRAS, and Planck High Frequency Instrument (HFI) are described.

ABSTRACT
1. INTRODUCTION
2. AN EARLY IRC vs. AMEσ RESULT AND ONGOINGWORK
REFERENCES

• Aaron C. Bell(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Takashi Onaka(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Yasuo Doi(Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo)
• Itsuki Sakon(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Fumihiko Usui(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Itsuki Sakon(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Daisuke Ishihara(Graduate School of Science, Nagoya University)
• Hidehiro Kaneda(Graduate School of Science, Nagoya University)
• Martin Giard(IRAP, Universite'de Toulouse & CNRS; France)
• Ronin Wu(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Ryou Ohsawa(Department of Astronomy, Graduate School of Science, The University of Tokyo/Institute of Astronomy, Graduate School of Science, The University of Tokyo)
• Tamami Mori-Ito(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Mark Hammonds(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Ho-Gyu Lee(Korea Astronomy and Space Institute)