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Fast-Expanding Hi Shells Associated with Supernova Remnants in the I-GALFA Survey

Published online by Cambridge University Press:  29 January 2014

Geumsook Park ,
Bon-Chul Koo ,
Steven J. Gibson  and
Ji-hyun Kang
Geumsook Park
Affiliation:
Department of Physics and Astronomy, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 151-742, Republic of Korea email: [email protected], [email protected]
Bon-Chul Koo
Affiliation:
Department of Physics and Astronomy, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 151-742, Republic of Korea email: [email protected], [email protected]
Steven J. Gibson
Affiliation:
Department of Physics and Astronomy, Western Kentucky University, Bowling Green, KY 42101, USA email: [email protected]
Ji-hyun Kang
Affiliation:
Yonsei University Observatory, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 120-749, Republic of Korea Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 305-348, Republic of Korea email: [email protected]
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Abstract

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We examine excess emission at high positive and negative velocities toward known Galactic supernova remnants (SNRs) in the “Inner-Galaxy Arecibo L-band Feed Array (I-GALFA)” Hi 21-cm survey data. The I-GALFA survey covers ℓ = 32° to 77°, and has a velocity range of ±700 km s−1 with high angular and velocity resolutions (4′ and 0.18 km s−1, respectively) and good sensitivity (0.2 K). The excess emission which is thought to be part of a fast-expanding Hi shell of a SNR is detected from four among 39 SNRs in the I-GALFA area: W44, G54.4–0.3, W51C, and CTB 80. Although the Hi shells of the four SNRs were already reported in low-resolution studies, the first detection of both sides of an expanding Hi shell associated with W44 is very inspiring. We discuss physical properties of these four SNRs and their statistical nature.

Keywords

ISM: supernova remnantsradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S296: Supernova Environmental Impacts , January 2013 , pp. 386 - 387
Copyright
Copyright © International Astronomical Union 2014 

References

Green, D. A. 2009a, Bulletin of the Astronomical Society of India, 37, 45Google Scholar
Green, D. A. 2009b MNRAS, 399, 177CrossRefGoogle Scholar
Koo, B.-C. & Heiles, C. 1991, ApJ, 382, 204CrossRefGoogle Scholar
Koo, B.-C. & Heiles, C. 1995, ApJ, 442, 679Google Scholar
Koo, B.-C. & Moon, D.-S. 1997a, ApJ, 475, 194CrossRefGoogle Scholar
Koo, B.-C. & Moon, D.-S. 1997b, ApJ, 485, 263CrossRefGoogle Scholar
Koo, B.-C., Reach, W. T., Heiles, C., Fesen, R. A., & Shull, J. M. 1990, ApJ, 364, 178Google Scholar
Peek, J. E. G., Begum, A., Douglas, K. A., et al. 2010, Astronomical Society of the Pacific Conference Series, 438, 393Google Scholar
Peek, J. E. G., Heiles, C., Douglas, K. A., et al. 2011, ApJS, 194, 20CrossRefGoogle Scholar