A supernova remnant counterpart for HESS J1832-085

Nigel I. Maxted, M. D. Filipović, N. Hurley-Walker, I. Bojičić, G. P. Rowell, F. Haberl, A. J. Ruiter, I. R. Seitenzahl, F. Panther, G. F. Wong, C. Braiding, M. Burton, G. Pühlhofer, H. Sano, Y. Fukui, M. Sasaki, W. Tian, H. Su, X. Cui, D. LeahyP. J. Hancock

Research output: Contribution to journalArticlepeer-review

2 Citations (Scopus)

Abstract

We examine the new Galactic supernova remnant (SNR) candidate, G23.11+0.18, as seen by the Murchison Widefield Array radio telescope. We describe the morphology of the candidate and find a spectral index of -0.63 ± 0.05 in the 70-170 MHz domain. Coincident TeV gamma-ray detection in High Energy Stereoscopic System (HESS) data supports the SNR nature of G23.11+0.18 and suggests that G23.11+0.18 is accelerating particles beyond TeV energies, thus making this object a promising new cosmic-ray hadron source candidate. The remnant cannot be seen in current optical, infrared and X-ray data sets. We do find, however, a dip in CO-traced molecular gas at a line-of-sight velocity of ∼85 km s-1, suggesting the existence of a G23.11+0.18 progenitor wind-blown bubble. Furthermore, the discovery of molecular gas clumps at a neighboring velocity toward HESS J1832-085 adheres to the notion that a hadronic gamma-ray production mechanism is plausible toward the north of the remnant. Based on these morphological arguments, we propose an interstellar medium association for G23.11+0.18 at a kinematic distance of 4.6 ± 0.8 kpc.
Original languageEnglish
Article number129
Number of pages17
JournalAstrophysical Journal
Volume885
Issue number2
DOIs
Publication statusPublished - 2019

Keywords

  • galactic cosmic rays
  • gamma ray sources
  • interstellar matter
  • interstellar molecules
  • supernova remnants

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