G0.173−0.42: an X-ray and radio magnetized filament near the galactic centre

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https://academic.oup.com/mnras/article/500/3/3142/5936657

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https://doi.org/10.1093/mnras/staa3257
 http://hdl.handle.net/11603/24094

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UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
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https://orcid.org/0000-0001-8403-8548

Date

2020-10-23

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journal articles
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Citation of Original Publication

F Yusef-Zadeh, M Wardle, C Heinke, I Heywood, R Arendt, M Royster, W Cotton, F Camilo, J Michail, G0.173−0.42: an X-ray and radio magnetized filament near the galactic centre, Monthly Notices of the Royal Astronomical Society, Volume 500, Issue 3, January 2021, Pages 3142–3150, https://doi.org/10.1093/mnras/staa3257

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This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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Abstract

The detection of an X-ray filament associated with the radio filament G0.173–0.42 adds to four other non-thermal radio filaments with X-ray counterparts, amongst the more than 100 elongated radio structures that have been identified as synchrotron-emitting radio filaments in the inner couple of degrees of the Galactic centre. The synchrotron mechanism has also been proposed to explain the emission from X-ray filaments. However, the origin of radio filaments and the acceleration sites of energetic particles to produce synchrotron emission in radio and X-rays remain mysterious. Using MeerKAT, VLA, Chandra, WISE, and Spitzer, we present structural details of G0.173–0.42 which consists of multiple radio filaments, one of which has an X-ray counterpart. A faint oblique radio filament crosses the radio and X-ray filaments. Based on the morphology, brightening of radio and X-ray intensities, and radio spectral index variation, we argue that a physical interaction is taking place between two magnetized filaments. We consider that the reconnection of the magnetic field lines at the interaction site leads to the acceleration of particles to GeV energies. We also argue against the synchrotron mechanism for the X-ray emission due to the short ∼30 yr lifetime of TeV relativistic particles. Instead, we propose that the inverse Compton scattering mechanism is more likely to explain the X-ray emission by upscattering of seed photons emitted from a 106 L star located at the northern tip of the X-ray filament.