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Dark gas: a new possible link between low and high-energy phenomena

Published online by Cambridge University Press:  17 August 2012

Kazufumi Torii
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan email: torii@a.phys.nagoya-u.ac.jp
Yasuo Fukui
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan email: torii@a.phys.nagoya-u.ac.jp
Hidetoshi Sano
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan email: torii@a.phys.nagoya-u.ac.jp
Junki Sato
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan email: torii@a.phys.nagoya-u.ac.jp
Takeshi Okuda
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan email: torii@a.phys.nagoya-u.ac.jp
Hiroaki Yamamoto
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan email: torii@a.phys.nagoya-u.ac.jp
Akiko Kawamura
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
Norikazu Mizuno
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
Toshikazu Onishi
Affiliation:
Department of Astrophysics, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan
Hideo Ogawa
Affiliation:
Department of Astrophysics, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan
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Abstract

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Galactic-scale studies of γ-rays and sub-mm radiation suggest that a significant amount of neutral interstellar medium is not detectable either in CO or HI (Grenier et al. 2005; Ade et al. 2011). This component is called “dark gas”. Here we argue that cool and dense atomic gas without molecules is responsible for the dark gas. This interpretation is supported by a recent finding of cool HI gas corresponding to the TeV γ-ray shell in the SNR RX J1713.7-3946 (Fukui et al. 2011). Such HI gas is not recognized under a usual assumption of optically thin HI emission but is identified by a careful analysis considering optically thick HI. The typical column density of such HI gas is a few times 1021 cm−2 and is also identified as visual extinction.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

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