Hostname: page-component-586b7cd67f-l7hp2 Total loading time: 0 Render date: 2024-11-22T18:18:27.227Z Has data issue: false hasContentIssue false
  • English
  • Français

The GeV Gamma-Ray Emission Detected by Fermi-LAT Adjacent to SNR Kesteven 41

Published online by Cambridge University Press:  17 October 2017

Bing Liu ,
Yang Chen ,
Xiao Zhang ,
Gao-Yuan Zhang ,
Yi Xing  and
Thomas G. Pannuti
Bing Liu
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China
Yang Chen
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing 210093, China
Xiao Zhang
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China
Gao-Yuan Zhang
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China
Yi Xing
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
Thomas G. Pannuti
Affiliation:
Space Science Center, Department of Earth and Space Sciences, Morehead State University, 235 Martindale Drive, Morehead, KY 40351, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Gamma-ray observations for Supernova remnant (SNR)-molecular cloud (MC) association systems play an important role in the research on the acceleration and propagation of cosmic-ray protons. Through the analysis of 5.6 years of Fermi-Large Area Telescope observation data, here we report on the detection of a gamma-ray emission source near the SNR Kesteven 41 with a significance of 24σ in 0.2–300 GeV. The best-fit location of the gamma-ray source is consistent with the MC with which the SNR interacts. Several hypotheses including both leptonic and hadronic scenarios are considered to investigate the origin of these gamma-rays. The gamma-ray emission can be naturally explained by the decay of neutral pions produced via the collision between high energy protons accelerated by the shock of Kesteven 41 and the adjacent MC. The electron energy budget would be too high for the SNR if the gamma-rays were produced via inverse Compton (IC) scattering off the Cosmic Microwave Background (CMB) photons.

Keywords

acceleration of particlesgamma rays: observationssupernova remnantsISM: individual (Kes 41)
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. 310 - 315
Copyright
Copyright © International Astronomical Union 2017 

References

Abdo, A. A., Ackermann, M., Ajello, M., et al. 2009, ApJ (Letters), 706, L1 Google Scholar
Abdo, A. A., Ackermann, M., Ajello, M., et al. 2010a, ApJ, 718, 348 Google Scholar
Abdo, A. A., Ackermann, M., Ajello, M., et al. 2010b, Science, 327, 1103 CrossRefGoogle Scholar
Abdo, A. A., Ackermann, M., Ajello, M., et al. 2010c, ApJ, 712, 459 Google Scholar
Abdo, A. A., Ackermann, M., Ajello, M., et al. 2013, ApJS, 208, 17 Google Scholar
Ackermann, M., Ajello, M., Allafort, A., et al. 2013, Science, 339, 807 Google Scholar
Aharonian, F. A. & Atoyan, A. M. 1996, A&A, 309, 917 Google Scholar
Atwood, W. B., et al. 2009, ApJ, 697, 1071 Google Scholar
Blandford, R. D. & Cowie, L. L. 1982, ApJ, 260, 625 Google Scholar
Castro, D., Slane, P., Carlton, A., & Figueroa-Feliciano, E. 2013, ApJ, 774, 36 Google Scholar
Caswell, J. L. 2004, MNRAS, 349, 99 Google Scholar
Gabici, S., Aharonian, F. A., & Casanova, S. 2009, MNRAS, 396, 1629 Google Scholar
Ginzburg, V. L. & Syrovatskii, S. I. 1969, The origin of cosmic rays (New York: Gordon and Breach)Google Scholar
Koralesky, B., Frail, D. A., Goss, W. M., Claussen, M. J., & Green, A. J. 1998, AJ, 116, 1323 Google Scholar
Li, H. & Chen, Y. 2010, MNRAS, 409, L35 Google Scholar
Li, H. & Chen, Y. 2012, MNRAS, 421, 935 Google Scholar
Nolan, P. L., Abdo, A. A., Ackermann, M., et al. 2012, ApJS, 199, 31 Google Scholar
Ohira, Y., Murase, K., & Yamazaki, R. 2011, MNRAS, 410, 1577 Google Scholar
Tang, X. & Chevalier, R. A. 2014, ApJ (Letters), 784, L35 Google Scholar
Uchiyama, Y., Blandford, R. D., Funk, S., Tajima, H., & Tanaka, T. 2010, ApJ (Letters), 723, L122 Google Scholar
Wenger, M., Ochsenbein, F., Egret, D., et al. 2000, A&AS, 143, 9 Google Scholar
Whiteoak, J. B. Z. & Green, A. J. 1996, A&AS, 118, 329 Google Scholar
Xing, Y., Wang, Z., Zhang, X., & Chen, Y. 2014, ApJ, 781, 64 Google Scholar
Zhang, G.-Y., Chen, Y., Su, Y., Zhou, X., Pannuti, T. G., & Zhou, P. 2015, ApJ, 799, 103 CrossRefGoogle Scholar