Characteristics of the supernova remnant G351.7+0.8 and a distance argument against its association with PSR J1721−3532 |
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| Authors: | W W Tian M Haverkorn † H Y Zhang |
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| Institution: | National Astronomical Observatories, CAS, Beijing 100012, China;Department of Physics &Astronomy, University of Calgary, Calgary, Alberta T2N 1N4, Canada;Astronomy Department, University of California-Berkeley, 601 Campbell Hall, Berkeley, CA 94720, USA |
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| Abstract: | 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. |
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| Keywords: | pulsars: individual: PSR J1721?3532 supernovae: individual: G351 7+0 8 supernova remnants |
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