NuSTAR discovery of a young, energetic pulsar associated with the luminous gamma-ray source HESS J1640-465

E. V. Gotthelf; J. A. Tomsick; J. P. Halpern; J. D. Gelfand; F. A. Harrison; S. E. Boggs; F. E. Christensen; W. W. Craig; J. C. Hailey; V. M. Kaspi; D. K. Stern; W. W. Zhang

doi:10.1088/0004-637X/788/2/155

NuSTAR discovery of a young, energetic pulsar associated with the luminous gamma-ray source HESS J1640-465

E. V. Gotthelf, J. A. Tomsick, J. P. Halpern, J. D. Gelfand, F. A. Harrison, S. E. Boggs, F. E. Christensen, W. W. Craig, J. C. Hailey, V. M. Kaspi, D. K. Stern, W. W. Zhang

Physics

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Abstract

We report the discovery of a 206 ms pulsar associated with the TeV γ-ray source HESS J1640-465 using the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray observatory. PSR J1640-4631 lies within the shell-type supernova remnant (SNR) G338.3-0.0, and coincides with an X-ray point source and putative pulsar wind nebula (PWN) previously identified in XMM-Newton and Chandra images. It is spinning down rapidly with period derivative 9.758(44) × 10^-13, yielding a spin-down luminosity 4.4 × 10 ³⁶ erg s^-1, characteristic age 3350 yr, and surface dipole magnetic field strength B_s = 1.4 × 10¹³ G. For the measured distance of 12 kpc to G338.3-0.0, the 0.2-10 TeV luminosity of HESS J1640-465 is 6% of the pulsar's present . The Fermi source 1FHL J1640.5-4634 is marginally coincident with PSR J1640-4631, but we find no γ-ray pulsations in a search using five years of Fermi Large Area Telescope (LAT) data. The pulsar energetics support an evolutionary PWN model for the broadband spectrum of HESS J1640-465, provided that the pulsar's braking index is n 2, and that its initial spin period was P ₀ ∼ 15 ms.

Original language	English (US)
Article number	155
Journal	Astrophysical Journal
Volume	788
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/788/2/155
State	Published - Jun 20 2014

Keywords

ISM: individual objects (G338.3-0.0, HESS J1640-465, 1FHL J1640.5-4634, AX J1640.7-4632, XMMU J164045.4-463131)
ISM: supernova remnants
pulsars: individual (PSR J1640-4631)
stars: neutron

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1088/0004-637X/788/2/155

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Gotthelf, E. V., Tomsick, J. A., Halpern, J. P., Gelfand, J. D., Harrison, F. A., Boggs, S. E., Christensen, F. E., Craig, W. W., Hailey, J. C., Kaspi, V. M., Stern, D. K., & Zhang, W. W. (2014). NuSTAR discovery of a young, energetic pulsar associated with the luminous gamma-ray source HESS J1640-465. Astrophysical Journal, 788(2), Article 155. https://doi.org/10.1088/0004-637X/788/2/155

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title = "NuSTAR discovery of a young, energetic pulsar associated with the luminous gamma-ray source HESS J1640-465",

abstract = "We report the discovery of a 206 ms pulsar associated with the TeV γ-ray source HESS J1640-465 using the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray observatory. PSR J1640-4631 lies within the shell-type supernova remnant (SNR) G338.3-0.0, and coincides with an X-ray point source and putative pulsar wind nebula (PWN) previously identified in XMM-Newton and Chandra images. It is spinning down rapidly with period derivative 9.758(44) × 10-13, yielding a spin-down luminosity 4.4 × 10 36 erg s-1, characteristic age 3350 yr, and surface dipole magnetic field strength Bs = 1.4 × 1013 G. For the measured distance of 12 kpc to G338.3-0.0, the 0.2-10 TeV luminosity of HESS J1640-465 is 6% of the pulsar's present . The Fermi source 1FHL J1640.5-4634 is marginally coincident with PSR J1640-4631, but we find no γ-ray pulsations in a search using five years of Fermi Large Area Telescope (LAT) data. The pulsar energetics support an evolutionary PWN model for the broadband spectrum of HESS J1640-465, provided that the pulsar's braking index is n 2, and that its initial spin period was P 0 ∼ 15 ms.",

keywords = "ISM: individual objects (G338.3-0.0, HESS J1640-465, 1FHL J1640.5-4634, AX J1640.7-4632, XMMU J164045.4-463131), ISM: supernova remnants, pulsars: individual (PSR J1640-4631), stars: neutron",

author = "Gotthelf, {E. V.} and Tomsick, {J. A.} and Halpern, {J. P.} and Gelfand, {J. D.} and Harrison, {F. A.} and Boggs, {S. E.} and Christensen, {F. E.} and Craig, {W. W.} and Hailey, {J. C.} and Kaspi, {V. M.} and Stern, {D. K.} and Zhang, {W. W.}",

year = "2014",

month = jun,

day = "20",

doi = "10.1088/0004-637X/788/2/155",

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T1 - NuSTAR discovery of a young, energetic pulsar associated with the luminous gamma-ray source HESS J1640-465

AU - Gotthelf, E. V.

AU - Tomsick, J. A.

AU - Halpern, J. P.

AU - Gelfand, J. D.

AU - Harrison, F. A.

AU - Boggs, S. E.

AU - Christensen, F. E.

AU - Craig, W. W.

AU - Hailey, J. C.

AU - Kaspi, V. M.

AU - Stern, D. K.

AU - Zhang, W. W.

PY - 2014/6/20

Y1 - 2014/6/20

N2 - We report the discovery of a 206 ms pulsar associated with the TeV γ-ray source HESS J1640-465 using the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray observatory. PSR J1640-4631 lies within the shell-type supernova remnant (SNR) G338.3-0.0, and coincides with an X-ray point source and putative pulsar wind nebula (PWN) previously identified in XMM-Newton and Chandra images. It is spinning down rapidly with period derivative 9.758(44) × 10-13, yielding a spin-down luminosity 4.4 × 10 36 erg s-1, characteristic age 3350 yr, and surface dipole magnetic field strength Bs = 1.4 × 1013 G. For the measured distance of 12 kpc to G338.3-0.0, the 0.2-10 TeV luminosity of HESS J1640-465 is 6% of the pulsar's present . The Fermi source 1FHL J1640.5-4634 is marginally coincident with PSR J1640-4631, but we find no γ-ray pulsations in a search using five years of Fermi Large Area Telescope (LAT) data. The pulsar energetics support an evolutionary PWN model for the broadband spectrum of HESS J1640-465, provided that the pulsar's braking index is n 2, and that its initial spin period was P 0 ∼ 15 ms.

AB - We report the discovery of a 206 ms pulsar associated with the TeV γ-ray source HESS J1640-465 using the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray observatory. PSR J1640-4631 lies within the shell-type supernova remnant (SNR) G338.3-0.0, and coincides with an X-ray point source and putative pulsar wind nebula (PWN) previously identified in XMM-Newton and Chandra images. It is spinning down rapidly with period derivative 9.758(44) × 10-13, yielding a spin-down luminosity 4.4 × 10 36 erg s-1, characteristic age 3350 yr, and surface dipole magnetic field strength Bs = 1.4 × 1013 G. For the measured distance of 12 kpc to G338.3-0.0, the 0.2-10 TeV luminosity of HESS J1640-465 is 6% of the pulsar's present . The Fermi source 1FHL J1640.5-4634 is marginally coincident with PSR J1640-4631, but we find no γ-ray pulsations in a search using five years of Fermi Large Area Telescope (LAT) data. The pulsar energetics support an evolutionary PWN model for the broadband spectrum of HESS J1640-465, provided that the pulsar's braking index is n 2, and that its initial spin period was P 0 ∼ 15 ms.

KW - ISM: individual objects (G338.3-0.0, HESS J1640-465, 1FHL J1640.5-4634, AX J1640.7-4632, XMMU J164045.4-463131)

KW - ISM: supernova remnants

KW - pulsars: individual (PSR J1640-4631)

KW - stars: neutron

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U2 - 10.1088/0004-637X/788/2/155

DO - 10.1088/0004-637X/788/2/155

M3 - Article

AN - SCOPUS:84902214606

SN - 0004-637X

VL - 788

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 155

ER -

NuSTAR discovery of a young, energetic pulsar associated with the luminous gamma-ray source HESS J1640-465

Abstract

Keywords

ASJC Scopus subject areas

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