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Title:
X-ray and Radio Timing of the Pulsar in 3C 58
Authors:
Livingstone, Margaret A.; Ransom, Scott M.; Camilo, Fernando; Kaspi, Victoria M.; Lyne, Andrew G.; Kramer, Michael; Stairs, Ingrid H.
Affiliation:
AA(Department of Physics, McGill University, Montréal, QC H3A 2T8, Canada ), AB(National Radio Astronomy Observatory (NRAO), Charlottesville, VA 22903, USA ), AC(Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA ), AD(Department of Physics, McGill University, Montréal, QC H3A 2T8, Canada ), AE(University of Manchester, Jodrell Bank Centre for Astrophysics, Manchester M13 9PL, UK ), AF(University of Manchester, Jodrell Bank Centre for Astrophysics, Manchester M13 9PL, UK ; Max-Planck Institut fuer Radioastronomie, 53121 Bonn, Germany ), AG(Department of Physics of Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada ; Australia Telescope National Facility, CSIRO, Epping, NSW 1710, Australia ; Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia)
Publication:
The Astrophysical Journal, Volume 706, Issue 2, pp. 1163-1173 (2009). (ApJ Homepage)
Publication Date:
12/2009
Origin:
IOP
ApJ Keywords:
pulsars: general, pulsars: individual: PSR J0205+6449, X-rays: stars
DOI:
10.1088/0004-637X/706/2/1163
Bibliographic Code:
2009ApJ...706.1163L

Abstract

We present timing data spanning 6.4 yr for the young and energetic PSR J0205+6449, in the supernova remnant 3C 58. Data were obtained with the Rossi X-ray Timing Explorer, the Jodrell Bank Observatory, and the Robert C. Byrd Green Bank Telescope. We present phase-coherent timing analyses showing timing noise and two spin-up glitches with fractional frequency increases of ~3.4 × 10–7 near MJD 52555 and ~3.8 × 10–6 between MJDs 52777 and 53062. These glitches are unusually large if the pulsar was created in the historical supernova in 1181, as has been suggested. For the X-ray timing, we developed a new unbinned maximum likelihood method for determining pulse arrival times, which performs significantly better than the traditional binned techniques. In addition, we present an X-ray pulse profile analysis of four years of RXTE data showing that the pulsar is detected up to ~40 keV. We also present the first measurement of the phase offset between the radio and X-ray pulse for this source, showing that the radio pulse leads the X-ray pulse by phi = 0.10 ± 0.01 in phase. We compile all known measurements of the phase offsets between radio and X-ray and radio and γ-ray pulses for X-ray and γ-ray pulsars. We show that there is no relationship between pulse period and phase offset, supported by our measurement of the phase offset for PSR J0205+6449.
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