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Title:
Supernova 185 its Associated Remnant and PSR:1509-58
Authors:
Strom, R. G.
Publication:
R.A.S. MONTHLY NOTICES V.268, NO. 1/MAY1, P. L5, 1994 (MNRAS Homepage)
Publication Date:
05/1994
Origin:
KNUDSEN; MNRAS
MNRAS Keywords:
pulsars: individual: PSR 1509-58 - supernovae: individual: SN 185 - ISM: individual: G315.4-2.3 - ISM: individual: G 320.4 - 1.2 - ISM: supernova remnants
Bibliographic Code:
1994MNRAS.268L...5S

Abstract

A recent suggestion that the identification of SN 185 with the shell remnant G 315.4-2.3 should be rejected in favour of the young pulsar PSR 1509-58 and its presumed remnant G 320.4-1.2 is critically re-appraised. It is shown that interstellar absorption of low-energy X-rays from G 315.4-2.3 indicates a distance of about 1 kpc, and that modelling of the X-ray spectrum independently confirms this value. The X-ray models, moreover, favour an age consistent with the event of AD 185, with which the kinematics derived from the Balmer spectrum also roughly agree. An additional piece of evidence suggesting that G 315.4-2.3 is young is its radially directed magnetic field. The usually adopted distance to G 320.4-1.2 of 4.2 kpc is based upon H 1 absorption toward the brightest radio emission associated with the nebulosity RCW 89. Recent X-ray spectra suggest that the extended emission surrounding PSR 1509-58 suffers greater absorption than does RCW 89, and is hence more distant, in agreement with the pulsar's dispersion measure distance of 5.9 kpc. At this distance, the event that produced PSR 1509-58 is very unlikely to have been visually observable. Previous investigations of the Chinese record had already indicated that the discrepancy in date of disappearance can be accounted for; G 315.4-2.3 is certainly to be preferred over PSR 1509-58 on the basis of the positional description. Since RCW 89 and PSR 1509-58 cannot be physically associated, it is suggested that the old G 320.4-1.2 complex comprises at least two unrelated supernova remnants.

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