We detected bright mid- to far-infrared emission from the helium nova V445 Puppis in the AKARI all-sky survey data taken in 2006. Assuming an optically thin condition, we decomposed the spectral energy distribution (SED) of V445 Puppis in October 2006 by model tting and found that the SED can be explained by a combination of cold amorphous carbon (125 K and the mass of 4:5+6:6 2:7 X 10-4 M⊙) and warm amorphous carbon (250 K and the mass of 1:8+1:0 -0:5 X 10-5 M⊙). Assuming that the former is pre-existing dust formed in the past nova outbursts and the latter is newly formed dust in December 2000's nova wind, this result suggests that the amount of dust formed around V445 Puppis in a single outburst is larger than 10-5 M⊙, which is larger than those in any other classical novae ever reported.

ABSTRACT
1. INTRODUCTION
2. OBSERVATIONS
3. RESULTS OF PHOTOMETRY
4. DUST MODEL FITTING
REFERENCES

• Sayaka Shimamoto(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Itsuki Sakon(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Takashi Onaka(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Fumihiko Usui(Department of Astronomy, Graduate School of Science, The University of Tokyo)
• Takafumi Ootsubo(Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo)
• Yasuo Doi(Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, 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)
• Daisuke Ishihara(Graduate School of Science, Nagoya University)