2006/12/31 by W. W. Tian, M. Haverkorn, H. Y. Zhang · 1 citation
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Gamma-ray bursts and supernovae #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.11613.x
published as Mon.Not.Roy.Astron.Soc.378:1283-1286,2007 · 9 pages, 3 figures, accepted by MNRAS
arxiv created 2007/02/13 · openalex publication_date 2007/06/16 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
New images of the supernova remnant (SNR) G351.7+0.8 are presented based on 21-cm H i-line emission and continuum emission data from the Southern Galactic Plane Survey. SNR G351.7+0.8 has a flux density of 8.4 ± 0.7 Jy at 1420 MHz. Its spectral index is 0.52 ± 0.25 (S=v−α) between 1420 and 843 MHz, typical of adiabatically expanding shell-like remnants. H i observations show structures possibly associated with the SNR in the radial velocity range of −10 to −18 km s−1, and suggest a distance of 13.2 kpc and a radius of 30.7 pc. The estimated Sedov age for G351.7+0.8 is less than 6.8×104 yr. A young radio pulsar PSR J1721−3532 lies close to SNR G351.7+0.8 on the sky. The new distance and age of G351.7+0.8 and recent proper motion measurements of the pulsar strongly argue against an association between SNR G351.7+0.8 and PSR J1721−3532. There is an unidentified, faint X-ray point source 1RXS J172055.3−353937 which is close to G351.7+0.8. This may be a neutron star potentially associated with G351.7+0.8.