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000619039 1001_ $$00000-0001-8583-6429$$aPope, I.$$b0
000619039 245__ $$aA Multiwavelength Investigation of PSR J2229+6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands
000619039 260__ $$aLondon$$bInstitute of Physics Publ.$$c2024
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000619039 520__ $$aG106.3+2.7, commonly considered to be a composite supernova remnant (SNR), is characterized by a boomerang-shaped pulsar wind nebula (PWN) and two distinct (“head” and “tail”) regions in the radio band. A discovery of very-high-energy gamma-ray emission (E$_{γ}$ > 100 GeV) followed by the recent detection of ultrahigh-energy gamma-ray emission (E$_{γ}$ > 100 TeV) from the tail region suggests that G106.3+2.7 is a PeVatron candidate. We present a comprehensive multiwavelength study of the Boomerang PWN (100″ around PSR J2229+6114) using archival radio and Chandra data obtained two decades ago, a new NuSTAR X-ray observation from 2020, and upper limits on gamma-ray fluxes obtained by Fermi-LAT and VERITAS observatories. The NuSTAR observation allowed us to detect a 51.67 ms spin period from the pulsar PSR J2229+6114 and the PWN emission characterized by a power-law model with Γ = 1.52 ± 0.06 up to 20 keV. Contrary to the previous radio study by Kothes et al., we prefer a much lower PWN B-field (B ∼ 3 μG) and larger distance (d ∼ 8 kpc) based on (1) the nonvarying X-ray flux over the last two decades, (2) the energy-dependent X-ray size of the PWN resulting from synchrotron burn-off, and (3) the multiwavelength spectral energy distribution (SED) data. Our SED model suggests that the PWN is currently re-expanding after being compressed by the SNR reverse shock ∼1000 yr ago. In this case, the head region should be formed by GeV–TeV electrons injected earlier by the pulsar propagating into the low-density environment.
000619039 536__ $$0G:(DE-HGF)POF4-613$$a613 - Matter and Radiation from the Universe (POF4-613)$$cPOF4-613$$fPOF IV$$x0
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000619039 542__ $$2Crossref$$i2023-12-27$$uhttps://iopscience.iop.org/info/page/text-and-data-mining
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000619039 7001_ $$00000-0002-5365-5444$$aReynolds, S. P.$$b4
000619039 7001_ $$00000-0001-6189-7665$$aSafi-Harb, S.$$b5
000619039 7001_ $$00000-0002-3681-145X$$aHailey, C. J.$$b6
000619039 7001_ $$aAn, H.$$b7
000619039 7001_ $$aBangale, P.$$b8
000619039 7001_ $$00000-0001-8138-1391$$aBatista, P.$$b9
000619039 7001_ $$00000-0003-2098-170X$$aBenbow, W.$$b10
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000619039 7001_ $$00000-0002-8136-9461$$aCapasso, M.$$b12
000619039 7001_ $$aChristiansen, J. L.$$b13
000619039 7001_ $$aChromey, A. J.$$b14
000619039 7001_ $$00000-0002-5068-7344$$aFalcone, A.$$b15
000619039 7001_ $$aFeng, Q.$$b16
000619039 7001_ $$aFinley, J. P.$$b17
000619039 7001_ $$00000-0002-2944-6060$$aFoote, G. M.$$b18
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000619039 7001_ $$aOng, R. A.$$b40
000619039 7001_ $$aPark, N.$$b41
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000619039 7001_ $$0P:(DE-H253)PIP1006066$$aSadeh, I.$$b50
000619039 7001_ $$aSaha, L.$$b51
000619039 7001_ $$aSembroski, G. H.$$b52
000619039 7001_ $$aTak, D.$$b53
000619039 7001_ $$aTucci, J. V.$$b54
000619039 7001_ $$aWeinstein, A.$$b55
000619039 7001_ $$00000-0003-2740-9714$$aWilliams, D. A.$$b56
000619039 7001_ $$00009-0001-6471-1405$$aWoo, J.$$b57
000619039 7001_ $$aNuSTAR Collaboration$$b58$$eCollaboration Author
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