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American Astronomical Society, Astrophysical Journal, 2(788), p. 155, 2014

DOI: 10.1088/0004-637x/788/2/155

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NuSTAR Discovery of a Young, Energetic Pulsar Associated with the Luminous Gamma-ray Source HESS J1640-465

Journal article published in 2014 by E. V. Gotthelf ORCID, J. A. Tomsick ORCID, J. P. Halpern, J. D. Gelfand ORCID, F. A. Harrison, S. E. Boggs, F. E. Christensen ORCID, W. W. Craig, J. C. Hailey, V. M. Kaspi, D. K. Stern ORCID, W. W. Zhang
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

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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 Ṗ = 9.758(44) × 10^(–13), yielding a spin-down luminosity Ė = 4.4 × 10^(36) erg s^(–1), characteristic age τ_c ≡ P/2Ṗ = 3350 yr, and surface dipole magnetic field strength B_s = 1.4 × 10^(13) 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 Ė. 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.