2009/12/10 by Takayasu Anada, Aya Bamba, Ken Ebisawa +1
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Emission spectrum #Nebula #Optics #Photon #Physics #Pulsar #Pulsar wind nebula #Pulsars and Gravitational Waves Research #Spectral index #Spectral line #Stars #Synchrotron #astro-ph.HE
paper · pdf · doi:10.1093/pasj/62.1.179
12 pages, 25 figures, PASJ, in press
arxiv created 2009/12/10 · openalex publication_date 2010/02/25 · arxiv updated 2015/05/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Suzaku observed the region including HESS J1809-193, a TeV unidentified source, and confirmed the existence of extended hard X-ray emission previously reported by ASCA, as well as hard X-ray emission from PSR J1809-1917 in this region. A one-dimensional profile of the diffuse emission is represented along with a Gaussian model with a best-fit σ of 7^′ ± 1^′. The diffuse emission extends for at least 21 pc (at the 3σ level, assuming a distance of 3.5 kpc), and has a hard spectrum with a photon index of Γ ∼ 1.7. The hard spectrum suggests a pulsar wind nebula origin, which is also strengthened by the hard X-ray emission from PSR J1809-1917, itself. Thanks to the low background of Suzaku XIS, we were able to investigate the spatial variation of the energy spectrum, but no systematic spectral change in the extended emission was found. These results imply that the X-ray emitting pulsar wind electrons can travel up to 21 pc from the pulsar without any noticeable energy loss via synchrotron emission.