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Title: X- And γ-Ray Pulsations Of The Nearby Radio-Faint PSR J1741–2054

Journal Article · · The Astrophysical Journal
 [1];  [2];  [3];  [4];  [4];  [5];  [6];  [7];  [8]
  1. Istituto Nazionale di Astrofisica (INAF), Milano (Italy)
  2. Istituto Nazionale di Astrofisica (INAF), Milano (Italy); Univ. of California, Santa Cruz, CA (United States). Santa Cruz Inst. for Particle Physics
  3. Univ. of California, Santa Cruz, CA (United States). Santa Cruz Inst. for Particle Physics; City Univ. of Hong Kong (China)
  4. Istituto Nazionale di Astrofisica (INAF), Milano (Italy); Istituto Nazionale di Fisica Nucleare (INFN), Pavia (Italy)
  5. Univ. of Virginia, Charlottesville, VA (United States)
  6. Istituto Nazionale di Astrofisica (INAF), Milano (Italy); Istituto Nazionale di Fisica Nucleare (INFN), Pavia (Italy); Univ. degli Studi di Pavia (Italy)
  7. Univ. of Virginia, Charlottesville, VA (United States); Univ. of Alberta, Edmonton, AB (Canada)
  8. Columbia Univ., New York, NY (United States). Columbia Astrophysics Lab.; Arecibo Observatory, PR (United States)

The results of a deep XMM-Newton observation of the radio-faint γ-ray pulsar J1741–2054 and its nebula together with the analysis of five years of Fermi Large Area Telescope (LAT) data are reported. The X-ray spectrum of the pulsar is consistent with an absorbed power law plus a blackbody, originating at least partly from the neutron star cooling. The nebular emission is consistent with that of a synchrotron pulsar wind nebula, with hints of spatial spectral variation. We extended the available Fermi LAT ephemeris and folded the γ-ray and X-ray data. We detected X-ray pulsations from the neutron star: both the thermal and non-thermal components are ~35%-40% pulsed, with phase-aligned maxima. A sinusoid fits the thermal-folded profile well. A 10 bin phase-resolved analysis of the X-ray emission shows softening of the non-thermal spectrum during the on-pulse phases. The radio, X-ray, and γ-ray light curves are single-peaked, not phase-aligned, with the X-ray peak trailing the γ-ray peak by more than half a rotation. Spectral considerations suggest that the most probable pulsar distance is in the 0.3-1.0 kpc range, in agreement with the radio dispersion measure.

Research Organization:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Organization:
USDOE
Grant/Contract Number:
AC02-76SF00515
OSTI ID:
1356463
Journal Information:
The Astrophysical Journal, Vol. 790, Issue 1; ISSN 0004-637X
Publisher:
Institute of Physics (IOP)Copyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 8 works
Citation information provided by
Web of Science

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RADIO DETECTION OF LAT PSRs J1741-2054 AND J2032+4127: NO LONGER JUST GAMMA-RAY PULSARS journal October 2009
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Cited By (8)

Magnetic neutron star cooling and microphysics journal January 2018
The two tails of PSR J2055+2539 as seen by Chandra : Analysis of the nebular morphology and pulsar proper motion journal April 2019
Synchrocurvature modelling of the multifrequency non-thermal emission of pulsars journal September 2019
Spectral characterization of the non-thermal X-ray emission of gamma-ray pulsars journal December 2019
Synchro-curvature modelling of the multi-frequency non-thermal emission of pulsars text January 2019
The tale of the two tails of the oldish PSR J2055+2539 text January 2015
Magnetic neutron star cooling and microphysics text January 2017
Synchro-curvature modelling of the multi-frequency non-thermal emission of pulsars text January 2019

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