Fronefield Crawford et al. 2001 ApJ 554 152 doi:10.1086/321328
Fronefield Crawford1,2, B. M. Gaensler1,3, V. M. Kaspi1,4,5, R. N. Manchester6, F. Camilo7, A. G. Lyne8 and M. J. Pivovaroff1,9
Show affiliationsWe report on Australia Telescope Compact Array observations in the direction of the young high magnetic-field pulsar J1119-6127. In the resulting images we identify a nonthermal radio shell of diameter 15', which we classify as a previously uncataloged young supernova remnant, G292.2-0.5. This supernova remnant is positionally coincident with PSR J1119-6127, and we conclude that the two objects are physically associated. No radio emission is detected from any pulsar wind nebula (PWN) associated with the pulsar; our observed upper limits are consistent with the expectation that high magnetic-field pulsars produce radio nebulae that fade rapidly. This system suggests a possible explanation for the lack of an associated radio pulsar and/or PWN in many supernova remnants.
ISM: individual (G292.2–0.5); pulsars: individual (PSR J1119–6127); radio continuum: ISM; stars: neutron; supernova remnants
Issue 1 (2001 June 10)
Received 2000 September 15, accepted for publication 2000 December 11
Fronefield Crawford et al. 2001 ApJ 554 152
F Delduc and L Feher 1995 J. Phys. A: Math. Gen. 28 5843
Nicolae Cotfas 1998 J. Phys. A: Math. Gen. 31 7273
Katsuhiro Nishinari 2001 J. Phys. A: Math. Gen. 34 10727
Ronald W Hellings 2001 Class. Quantum Grav. 18 4075
M. J. Pivovaroff et al. 2000 ApJ 535 379
J. E. Chiar et al. 2006 ApJ 651 268
P. Caselli et al 1995 ApJ 455 L77
Hsiao-Wen Chen et al. 2007 ApJ 663 420
Iwan Jensen 2005 J. Phys. A: Math. Gen. 38 L769