The existence of polycyclic aromatic hydrocarbons (PAHs) astronomically is well accepted, but the specic molecular forms observed remain uncertain. To better understand the molecular structures which may be present along a given sightline, the 3.0 - 3.6 μm region is modelled with careful consideration given to the underlying sub-features arising from specic structures within emitting molecules.

ABSTRACT
1. INTRODUCTION
2. AKARI DATA REDUCTION AND SPECTROSCOPICMODELLING
    2.1. Hydrocarbon Emission Features
    2.2. Ice Absorption Feature
3. CONCLUSIONS
REFERENCES

• Mark Hammonds(Department of Astronomy, The University of Tokyo)
• Tamami Mori(Department of Astronomy, The University of Tokyo)
• Fumihiko Usui(Department of Astronomy, The University of Tokyo)
• Takashi Onaka(Department of Astronomy, The University of Tokyo)