2006/01/25 by K. Torii, Ken’ichi Torii, H. Uchida +8
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Brightness #Cosmic ray #Electron #Galaxy #Gamma ray #Gamma-ray bursts and supernovae #Interstellar medium #Neutrino Physics Research #Optics #Photon #Physics #Supernova #Supernova remnant #Surface brightness #Synchrotron radiation #astro-ph
paper · pdf · doi:10.1093/pasj/58.1.l11
PASJ, in press
arxiv created 2006/01/25 · openalex publication_date 2006/02/25 · arxiv updated 2015/06/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We report here on the first pointed X-ray observation of the supernova remnant (SNR) G330.2+1.0. The X-ray morphology is characterized by an extended shell. Its X-ray spectrum is well represented by a single power-law function with a photon index of γ ≃ 2.8 and interstellar absorption of nH ≃ 2.6 × 1022 [cm-2]. We interpret this emission as synchrotron radiation from accelerated electrons at the SNR shock, as seen in SN 1006. The surface brightness of the X-ray emission is anti-correlated with the radio emission, and the power-law spectrum is dominated at the western shell where the radio emission is weak. The co-existence of two distinct (radio bright/X-ray faint and radio faint/X-ray bright) shells in a single supernova remnant challenges our understanding of the particle acceleration and radiation mechanisms in different interstellar environments. The object may be a good target for searching TeV gamma-rays and molecular gas surrounding the blast shock. We also report on the nature of a bright point-like source (AX J1601-5143) to the south of the SNR.