Near-infrared views of dust in planetary nebulae: AKARI/IRC NIR spectral atlas of Galactic PNe

11th Pacific Rim Conference on Stellar Astrophysics: Physics and Chemistry of the Late Stages of Stellar Evolution

物理学;天文学

Ohsawa, Ryou^1 ; Onaka, Takashi^2 ; Sakon, Itsuki^2 ; Mori, Tamami^2 ; Matsuura, Mikako^3 ; Yamamura, Issei^4 ; Kaneda, Hidehiro^5

Institute of Astronomy, Graduate School of Science, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo

181-0015, Japan^1

Department of Astronomy, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo

113-0033, Japan^2

School of Physics and Astronomy, Cardiff University, Queen's Buildings, 5 The Parade, Roath, Cardiff

CF24 3AA, United Kingdom^3

Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Chuo-ku, Kanagawa. Sagamihara

252-5210, Japan^4

Division of Particle and Astrophysical Science, Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Aichi, Nagoya

464-8602, Japan^5

关键词: Asymptotic giant branch stars;    Carbonaceous dust;    Emission bands;    Emission features;    Emission lines;    High sensitivity;    Interstellar mediums;    Planetary nebulae;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/728/7/072010/pdf
DOI  :  10.1088/1742-6596/728/7/072010

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

Asymptotic Giant Branch (AGB) stars and post-AGB stars are thought to be major dust sources in galaxies. Investigation of dust in planetary nebulae (PNe), their successors, reveals properties of dust grains injected into the interstellar medium. The near-infrared (2.5-5.0 μm) emission of PNe consists of hot dust continuum, emission lines of ionized gases, and emission bands of carbonaceous dust grains. This wave range, however, has not been well investigated due to the lack of instruments with a high sensitivity. We conducted spectroscopic observations of PNe with the AKARI, obtaining 2.5-5.0 μm spectra of 72 Galactic PNe with a sensitivity of a few mJy. The spectra and the intensities of emission features are compiled as a catalog. The characteristics of the catalog are described.