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Low frequency radio counterparts of HESS J1731−347 a.k.a SNR G353.6−0.7

Published online by Cambridge University Press:  17 October 2017

A. J. Nayana  and
Poonam Chandra
A. J. Nayana
Affiliation:
National centre for Radio Astrophysics, Tata Institute of Fundamental Research, PO Box 3, Pune 411007 email: nayana@ncra.tifr.res.in; email: poonam@ncra.tifr.res.in
Poonam Chandra
Affiliation:
National centre for Radio Astrophysics, Tata Institute of Fundamental Research, PO Box 3, Pune 411007 email: nayana@ncra.tifr.res.in; email: poonam@ncra.tifr.res.in
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Abstract

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HESS J1731−347 a.k.a. SNR G353.6−0.7 is one of the five known very high energy (VHE, Energy > 0.1 TeV) shell-type supernova remnants. We carried out Giant Metrewave Radio Telescope (GMRT) observations of this TeV SNR in 1390, 610 and 325 MHz bands. We detected the 325 and 610 MHz radio counterparts of the SNR G353.6−0.7 (Nayana et al. 2017). We also determined the spectral indices of individual filaments and our values are consistent with the non-thermal radio emission. We compared the radio morphology with that of VHE emission. The peak in radio emission corresponds to the faintest feature in the VHE emission. We explain this anti-correlated emission in a possible leptonic origin of the VHE γ-rays.

Keywords

acceleration of particles–radiation mechanisms: non-thermal–cosmic rays–ISM: individual objects:SNR G353.6−0.7–ISM: supernova remnants–radio continuum: ISM.
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S331: Supernova 1987A:30 years later - Cosmic Rays and Nuclei from Supernovae and their aftermaths , February 2017 , pp. 201 - 205
Copyright
Copyright © International Astronomical Union 2017 

References

Acero, F., Aharonian, F., Akhperjanian, A. G., et al. 2010, A&A, 516, A62 Google Scholar
Acero, F., Lemoine-Goumard, M., Renaud, M., et al. 2015, A&A, 580, A74 Google Scholar
Aharonian, F. A., Akhperjanian, A. G., Aye, K.-M., et al. 2004, Nature, 432, 75 CrossRefGoogle Scholar
Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2007, ApJ, 661, 236 CrossRefGoogle Scholar
Aharonian, F., Akhperjanian, A. G., Barres de Almeida, U., et al. 2008, A&A, 477, 353 Google Scholar
Aharonian, F., Akhperjanian, A. G., de Almeida, U. B., et al. 2009, ApJ, 692, 1500 CrossRefGoogle Scholar
Bamba, A., Pühlhofer, G., Acero, F., et al. 2012, ApJ, 756, 149 CrossRefGoogle Scholar
Blasi, P. 2013, A&AR, 21, 70 Google Scholar
Condon, J. J., Cotton, W. D., Greisen, E. W., et al. 1998, AJ, 115, 1693 CrossRefGoogle Scholar
Green, A. J., Cram, L. E., Large, M. I., & Ye, T. 1999, ApJS, 122, 207 CrossRefGoogle Scholar
Green, D. A. 2011, Bulletin of the Astronomical Society of India, 39, 289 Google Scholar
Halpern, J. P. & Gotthelf, E. V. 2010, ApJ, 710, 941 CrossRefGoogle Scholar
Haverkorn, M., Gaensler, B. M., McClure-Griffiths, N. M., Dickey, J. M., & Green, A. J. 2006, ApJS, 167, 230 CrossRefGoogle Scholar
H. E. S. S. Collaboration, Abramowski, A., Acero, F., et al. 2011, A&A, 531, A81 Google Scholar
Jones, T. W., Rudnick, L., Jun, B.-I., et al. 1998, PASP, 110, 125 CrossRefGoogle Scholar
Nayana, A. J., Chandra, P., Roy, S., et al. 2017, MNRAS, 467, 155 Google Scholar
Neugebauer, G., Habing, H. J., van Duinen, R., et al. 1984, ApJ (Letters), 278, L1 CrossRefGoogle Scholar
Tian, W. W., Leahy, D. A., Haverkorn, M., & Jiang, B. 2008, ApJ (Letters), 679, L85 CrossRefGoogle Scholar
Tian, W. W., Li, Z., Leahy, D. A., et al. 2010, ApJ, 712, 790 CrossRefGoogle Scholar
Wright, E. L., Eisenhardt, P. R. M., Mainzer, A. K., et al. 2010, AJ, 140, 1868 CrossRefGoogle Scholar