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

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

doi:10.1086/422408

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

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

Physics

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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 N_H = (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 (τ_scsc = 17.7 ± 0.9 ms at 1 GHz) and exhibits a significant amount of timing noise.

Original language	English (US)
Pages (from-to)	389-397
Number of pages	9
Journal	Astrophysical Journal
Volume	612
Issue number	1 I
DOIs	https://doi.org/10.1086/422408
State	Published - Sep 1 2004

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/422408

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@article{998714ac1d754d4c88ad1428b7d5c5c1,

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

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 Δ{\.ν}/{\.ν} = (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.",

author = "Hessels, {J. W.T.} and Roberts, {M. S.E.} and Ransom, {S. M.} and Kaspi, {V. M.} and Roman, {R. W.} and Ng, {C. Y.} and Freire, {P. C.C.} and Gaensler, {B. M.}",

year = "2004",

month = sep,

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doi = "10.1086/422408",

language = "English (US)",

volume = "612",

pages = "389--397",

journal = "Astrophysical Journal",

issn = "0004-637X",

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T1 - Observations of PSR J2021+3651 and its X-ray pulsar wind nebula G75.2+0.1

AU - Hessels, J. W.T.

AU - Roberts, M. S.E.

AU - Ransom, S. M.

AU - Kaspi, V. M.

AU - Roman, R. W.

AU - Ng, C. Y.

AU - Freire, P. C.C.

AU - Gaensler, B. M.

PY - 2004/9/1

Y1 - 2004/9/1

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.

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

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