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A supernova remnant counterpart for HESS J1832−085

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Haberl,  F.
High Energy Astrophysics, MPI for Extraterrestrial Physics, Max Planck Society;

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Citation

Maxted, N. I., Filipović, M. D., Hurley-Walker, N., Bojičić, I., Rowell, G. P., Haberl, F., et al. (2019). A supernova remnant counterpart for HESS J1832−085. The Astrophysical Journal, 885(2): 129. doi:10.3847/1538-4357/ab3e3f.


Cite as: http://hdl.handle.net/21.11116/0000-0005-79BD-F
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.