Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1

J. W T Hessels, Mallory Roberts, S. M. Ransom, V. M. Kaspi, R. W. Roman, C. Y. Ng, P. C C Freire, B. M. Gaensler

Research output: Contribution to journalArticle

Abstract

We present the results from X-ray and radio observations of the recently discovered young Vela-like pulsar PSR J2021+3651, which is coincident with the EGRET γ-ray source GeV 2020+3658. A 19.0 ks Chandra ACIS-S observation has revealed a ∼20″ × 10″ pulsar wind nebula that is reminiscent of the equatorial tori seen around some young pulsars, along with thermal emission from an embedded point source (kT = 0.15 ± 0.02 keV). We have named the nebula G75.2+0.1. Its spectrum is well fitted by an absorbed power-law model with a photon index of Γ = 1.7 -0.2 -0.3, a hydrogen column density of NH = (7.8-1.4 +1.7) × 1021 cm-2, and an unabsorbed 0.5-10.0 keV flux of (1.7 ± 0.1) × 10-12 ergs cm-2 s-1. We have spatially fitted G75.2+0.1 with a model that assumes a toroidal morphology, and from this we infer that the axis of the torus is highly inclined to the line of sight. A 20.8 ks Chandra observation in continuous-clocking mode reveals a possible pulse detection, with a pulsed fraction of ∼65% and an H-test probability of occurring by chance of 8.9 × 10-5. Timing observations with the Arecibo radio telescope spanning 2 yr show that PSR J2021+3651 glitched sometime between MJD 52,616 and 52,645 with parameters Δν/ν = (2.587 ± 0.002) × 10-6 and Δν̇/ν̇ = (6.2 ± 0.3) × 10-3, similar to those of the largest glitches observed in the Vela pulsar. PSR J2021+3651 is heavily scattered (τscsc = 17.7 ± 0.9 ms at 1 GHz) and exhibits a significant amount of timing noise.

Original languageEnglish (US)
Pages (from-to)389-397
Number of pages9
JournalAstrophysical Journal
Volume612
Issue number1 I
DOIs
StatePublished - Sep 1 2004

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nebulae
pulsars
radio
erg
point source
power law
x rays
time measurement
hydrogen
radio observation
radio telescopes
thermal emission
line of sight
point sources
rays
young
photons
pulses
test
detection

ASJC Scopus subject areas

  • Space and Planetary Science
  • Nuclear and High Energy Physics
  • Astronomy and Astrophysics

Cite this

Hessels, J. W. T., Roberts, M., Ransom, S. M., Kaspi, V. M., Roman, R. W., Ng, C. Y., ... Gaensler, B. M. (2004). Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1. Astrophysical Journal, 612(1 I), 389-397. https://doi.org/10.1086/422408

Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1. / Hessels, J. W T; Roberts, Mallory; Ransom, S. M.; Kaspi, V. M.; Roman, R. W.; Ng, C. Y.; Freire, P. C C; Gaensler, B. M.

In: Astrophysical Journal, Vol. 612, No. 1 I, 01.09.2004, p. 389-397.

Research output: Contribution to journalArticle

Hessels, JWT, Roberts, M, Ransom, SM, Kaspi, VM, Roman, RW, Ng, CY, Freire, PCC & Gaensler, BM 2004, 'Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1', Astrophysical Journal, vol. 612, no. 1 I, pp. 389-397. https://doi.org/10.1086/422408
Hessels JWT, Roberts M, Ransom SM, Kaspi VM, Roman RW, Ng CY et al. Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1. Astrophysical Journal. 2004 Sep 1;612(1 I):389-397. https://doi.org/10.1086/422408
Hessels, J. W T ; Roberts, Mallory ; Ransom, S. M. ; Kaspi, V. M. ; Roman, R. W. ; Ng, C. Y. ; Freire, P. C C ; Gaensler, B. M. / Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1. In: Astrophysical Journal. 2004 ; Vol. 612, No. 1 I. pp. 389-397.
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abstract = "We present the results from X-ray and radio observations of the recently discovered young Vela-like pulsar PSR J2021+3651, which is coincident with the EGRET γ-ray source GeV 2020+3658. A 19.0 ks Chandra ACIS-S observation has revealed a ∼20″ × 10″ pulsar wind nebula that is reminiscent of the equatorial tori seen around some young pulsars, along with thermal emission from an embedded point source (kT∞ = 0.15 ± 0.02 keV). We have named the nebula G75.2+0.1. Its spectrum is well fitted by an absorbed power-law model with a photon index of Γ = 1.7 -0.2 -0.3, a hydrogen column density of NH = (7.8-1.4 +1.7) × 1021 cm-2, and an unabsorbed 0.5-10.0 keV flux of (1.7 ± 0.1) × 10-12 ergs cm-2 s-1. We have spatially fitted G75.2+0.1 with a model that assumes a toroidal morphology, and from this we infer that the axis of the torus is highly inclined to the line of sight. A 20.8 ks Chandra observation in continuous-clocking mode reveals a possible pulse detection, with a pulsed fraction of ∼65{\%} and an H-test probability of occurring by chance of 8.9 × 10-5. Timing observations with the Arecibo radio telescope spanning 2 yr show that PSR J2021+3651 glitched sometime between MJD 52,616 and 52,645 with parameters Δν/ν = (2.587 ± 0.002) × 10-6 and Δν̇/ν̇ = (6.2 ± 0.3) × 10-3, similar to those of the largest glitches observed in the Vela pulsar. PSR J2021+3651 is heavily scattered (τscsc = 17.7 ± 0.9 ms at 1 GHz) and exhibits a significant amount of timing noise.",
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N2 - We present the results from X-ray and radio observations of the recently discovered young Vela-like pulsar PSR J2021+3651, which is coincident with the EGRET γ-ray source GeV 2020+3658. A 19.0 ks Chandra ACIS-S observation has revealed a ∼20″ × 10″ pulsar wind nebula that is reminiscent of the equatorial tori seen around some young pulsars, along with thermal emission from an embedded point source (kT∞ = 0.15 ± 0.02 keV). We have named the nebula G75.2+0.1. Its spectrum is well fitted by an absorbed power-law model with a photon index of Γ = 1.7 -0.2 -0.3, a hydrogen column density of NH = (7.8-1.4 +1.7) × 1021 cm-2, and an unabsorbed 0.5-10.0 keV flux of (1.7 ± 0.1) × 10-12 ergs cm-2 s-1. We have spatially fitted G75.2+0.1 with a model that assumes a toroidal morphology, and from this we infer that the axis of the torus is highly inclined to the line of sight. A 20.8 ks Chandra observation in continuous-clocking mode reveals a possible pulse detection, with a pulsed fraction of ∼65% and an H-test probability of occurring by chance of 8.9 × 10-5. Timing observations with the Arecibo radio telescope spanning 2 yr show that PSR J2021+3651 glitched sometime between MJD 52,616 and 52,645 with parameters Δν/ν = (2.587 ± 0.002) × 10-6 and Δν̇/ν̇ = (6.2 ± 0.3) × 10-3, similar to those of the largest glitches observed in the Vela pulsar. PSR J2021+3651 is heavily scattered (τscsc = 17.7 ± 0.9 ms at 1 GHz) and exhibits a significant amount of timing noise.

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