Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan
Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan
National Taiwan Normal University : Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan
出版者
宇宙航空研究開発機構(JAXA)
出版者（英）
Japan Aerospace Exploration Agency (JAXA)
雑誌名
宇宙航空研究開発機構特別資料
雑誌名(英)
JAXA Special Publication: Proceedings of the SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe
巻
JAXA-SP-17-010E
ページ
235 - 238
発行年
2018-03-09
会議概要（会議名, 開催地, 会期, 主催者等）（英）
SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan
抄録（英）
Asymptotic giant branch (AGB) stars are significant contributors to the chemical enrichment of the interstellar medium (ISM) of galaxies. It is therefore essential to constrain the AGB contribution to the dust budget in galaxies. Recent estimates of the total AGB dust injection rate to the Large and Small Magellanic Clouds (LMC and SMC; Riebel et al. 2012; Boyer et al. 2012, Srinivasan et al. in prep) have used data from the Spitzer Space Telescope SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006) and SAGE-SMC (Gordon et al. 2011) surveys. When sorted by dust chemistry, the data allow for a comparison of O-rich and carbonaceous dust production rates. In the LMC, for instance, the rate of dust production from carbon stars is two and a half times that from oxygen-rich AGBs. A reliable determination of the fractional contributions of the two types of dust would serve as input to models of chemical evolution. However, the Spitzer IRAC photometric bands do not sufficiently probe the characteristic mid-infrared spectral features that can distinguish O-rich AGBs from carbon stars - namely, the 9.7 μm silicate feature and 11.3 μm silicon carbide feature. With the continuous spectral coverage in the approximately 4-30 μm range, SPICA has the potential to distinguish these two types of chemistries. In this contribution, synthetic photometry from the model grid of AGB stars, GRAMS (Sargent et al. 2011; Srinivasan et al. 2011), will be used to discuss the science possibilities that SPICA might offer this study.
内容記述
形態: カラー図版あり
内容記述（英）
Physical characteristics: Original contains color illustrations
Identifying the Chemistry of the Dust around AGB Stars in Nearby Galaxies
AA1730027050.pdf
(4.01MB)
