Ohsawa, Ryou, Onaka, Takashi, Sakon, Itsuki, Mori, Tamami I., Miyata, Takashi, Asano, Kentaro, Matsuura, Mikako ![]() |
Abstract
We investigate the polycyclic aromatic hydrocarbon (PAH) features in the young Galactic planetary nebula PN G095.2+00.7 based on mid-infrared observations. The near- to mid-infrared spectra obtained with the AKARI/IRC and the Spitzer/IRS show the PAH features as well as the broad emission feature at 12 μm usually seen in proto-planetary nebulae (pPNe). The spatially resolved spectra obtained with Subaru/COMICS suggest that the broad emission around 12 μm is distributed in a shell-like structure, but the unidentified infrared band at 11.3 μm is selectively enhanced at the southern part of the nebula. The variation can be explained by a difference in the amount of the UV radiation to excite PAHs, and does not necessarily require the chemical processing of dust grains and PAHs. It suggests that the UV self-extinction is important to understand the mid-infrared spectral features. We propose a mechanism which accounts for the evolutionary sequence of the mid-infrared dust features seen in a transition from pPNe to PNe.
Item Type: | Article |
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Date Type: | Publication |
Status: | Published |
Schools: | Physics and Astronomy |
Publisher: | American Astronomical Society |
ISSN: | 2041-8205 |
Date of Acceptance: | 29 October 2012 |
Last Modified: | 15 May 2024 09:15 |
URI: | https://orca.cardiff.ac.uk/id/eprint/168114 |
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