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Title:
Timing the Young Pulsar at the Centre of SNR 3C 58
Authors:
Livingstone, Margaret A.; Ransom, Scott M.; Camilo, Fernando; Kaspi, Victoria M.; Lyne, Andrew G.; Kramer, Michael; Stairs, Ingrid H.
Affiliation:
AA(Rutherford Physics Building, McGill University, 3600 University Street, Montreal, Qc, H3A 2T8, Canada), AB(National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA), AC(Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY, USA), AD(Rutherford Physics Building, McGill University, 3600 University Street, Montreal, Qc, H3A 2T8, Canada), AE(University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL), AF(University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL), AG(Department of Physics of Astronomy, UBC, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada)
Publication:
40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP Conference Proceedings, Volume 983, pp. 160-162 (2008). (AIPC Homepage)
Publication Date:
02/2008
Origin:
AIP
PACS Keywords:
Pulsars, Neutron stars, Supernova remnants, X-ray sources; X-ray bursts, Astronomical and space-research instrumentation
DOI:
10.1063/1.2900135
Bibliographic Code:
2008AIPC..983..160L

Abstract

PSR J0205+6449 is a young, rotation-powered pulsar located at the centre of the SNR 3C 58, widely believed to be the remnant of the historical supernova SN 1181. The neutron star is cooler than expected from standard cooling models [1] and the pulsar, though it has a very high spin-down luminosity of E = 2.6×1037 ergs/s, has very low radio (L1400~0.5 mJy kpc2 [2]) and X-ray luminosities (LX = 2.06×1032 ergs/s [3]). We present 4 yrs of timing data spanning 5 yrs obtained with the Rossi X-ray Timing Explorer, the Jodrell Bank Observatory and the Green Bank Telescope. We present phase-coherent timing analyses showing significant timing noise that prevents a measurement of the `braking index'. In addition, we present two glitches observed in the source and discuss implications for the age and temperature of the neutron star.
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