The interstellar dust grains are formed and supplied to interstellar space from asymptotic giant branch (AGB) stars or supernova remnants, and become constituents of the star- and planet-formation processes that lead to the next generation of stars. Both a qualitative, and a compositional study of this cycle are essential to understanding the origin of the pre-solar grains, the missing sources of the interstellar material, and the chemical evolution of our Galaxy. The AKARI/MIR all-sky survey was performed with two mid-infrared photometric bands centered at 9 and 18 μ m . These data have advantages in detecting carbonaceous and silicate circumstellar dust of AGB stars, and the interstellar polycyclic aromatic hydrocarbons separately from large grains of amorphous silicate. By using the AKARI/MIR All-Sky point source catalogue, we surveyed C-rich and O-rich AGB stars in our Galaxy, which are the dominant suppliers of carbonaceous and silicate grains, respectively. The C-rich stars are uniformly distributed across the Galactic disk, whereas O-rich stars are concentrated toward the Galactic center, following the metallicity gradient of the interstellar medium, and are presumably affected by the environment of their birth place. We will compare the distributions of the dust suppliers with the distributions of the interstellar grains themselves by using the AKARI/MIR All-Sky diffuse maps. To enable discussions on the faint diffuse interstellar radiation, we are developing an accurate AKARI/MIR All-Sky diffuse map by correcting artifacts such as the ionising radiation effects, scattered light from the moon, and stray light from bright sources.

ABSTRACT
1. INTRODUCTION
2. DATA ANALYSIS
    2.1. Selection of C-rich and O-rich AGBs from the AKARI/MIR PSC
    2.2. AKARI/MIR All-Sky Diffuse Map Development
3. RESULTS
    3.1. Galactic Distributions of C-Rich and O-Rich AGBs
    3.2. Improved AKARI/MIR All-Sky Map
4. DISCUSSION
    4.1. Radial Profile of the Density Distribution
    4.2. Mass Budget Analysis
    4.3. Reason of the Difference in the Distributions
    4.4. Comparison with the Distributions of PAHs and Large Grains
5. SUMMARY
REFERENCES

• D. ISHIHARA(Graduate School of Science, Nagoya University)
• H. KANEDA(Graduate School of Science, University of Tokyo)
• A. MOURI(Graduate School of Science, University of Tokyo)
• T. KONDO(Graduate School of Science, University of Tokyo)
• S. SUZUKI(Graduate School of Science, University of Tokyo)
• S. OYABU(Graduate School of Science, University of Tokyo)
• T. ONAKA(Graduate School of Science, University of Tokyo)
• Y. ITA(Astronomical Institute, Tohoku University)
• M. MATSUURA(UCL-Institute of Origins, Department of Physics and Astronomy, University College London, UCL-Institute of Origins, Mullard Space Science Laboratory, University College London)
• N. MATSUNAGA(Kiso Observatory, Institute of Astronomy, University of Tokyo)