학술논문
A Multiwavelength Investigation of PSR J2229+6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands
Document Type
article
Author
I. Pope; K. Mori; M. Abdelmaguid; J. D. Gelfand; S. P. Reynolds; S. Safi-Harb; C. J. Hailey; H. An; NuSTAR Collaboration; P. Bangale; P. Batista; W. Benbow; J. H. Buckley; M. Capasso; J. L. Christiansen; A. J. Chromey; A. Falcone; Q. Feng; J. P. Finley; G. M Foote; G. Gallagher; W. F Hanlon; D. Hanna; O. Hervet; J. Holder; T. B. Humensky; W. Jin; P. Kaaret; M. Kertzman; D. Kieda; T. K. Kleiner; N. Korzoun; F. Krennrich; S. Kumar; M. J. Lang; G. Maier; C. E McGrath; C. L. Mooney; P. Moriarty; R. Mukherjee; S. O’Brien; R. A. Ong; N. Park; S. R. Patel; K. Pfrang; M. Pohl; E. Pueschel; J. Quinn; K. Ragan; P. T. Reynolds; E. Roache; I. Sadeh; L. Saha; G. H. Sembroski; D. Tak; J. V. Tucci; A. Weinstein; D. A. Williams; J. Woo; VERITAS Collaboration
Source
The Astrophysical Journal, Vol 960, Iss 1, p 75 (2023)
Subject
Language
English
ISSN
1538-4357
Abstract
G106.3+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 μ G) 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.