2013/07/13 by D. A. Frail, M. J. Claussen, J. Méhault +1 · 1 citation
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Cosmic ray #Gamma-ray bursts and supernovae #Hadron #Line (geometry) #Line-of-sight #Maser #Molecular cloud #Neutron star #Nuclear physics #Physics #Stars #Supernova #Supernova remnant #astro-ph.HE
paper · pdf · doi:10.1088/2041-8205/773/2/l19
4 pages, 1 figure. ApJ Letters, submitted
arxiv created 2013/07/13 · openalex publication_date 2013/07/31 · arxiv updated 2015/06/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We report on the discovery of compact, narrow OH line emission from the hydroxyl molecule at 1720 MHz toward the extended TeV source J1834−087. The origin of this high energy emission is unknown; it could be powered by one or more candidate neutron stars (leptonic) or by cosmic rays interacting with dense gas (hadronic). The OH emission is detected near the center of J1834−087, coincident with the radio continuum of the supernova remnant W41, and the radial velocity of the line is the same velocity as a giant molecular cloud along the line of sight. We argue that the OH is maser emission stimulated by the interaction of the W41 shock with the molecular cloud. The known correlation between γ-ray bright supernova remnants and OH masers favors a hadronic interpretation for this high energy emission.