Pope, I.Mori, K.Abdelmaguid, M.Gelfand, J. D.Reynolds, S. P.Safi-Harb, S.Hailey, C. J.An, H.(NuSTAR Collaboration)Bangale, P.Batista, P.Benbow, W.Buckley, J. H.Capasso, M.Christiansen, J. L.Chromey, A. J.Falcone, A.Feng, Q.Finley, J. P.Foote, G. M.Gallagher, G.Hanlon, W. F.Hanna, D.Hervet, O.Holder, J.Humensky, T. B.Jin, W.Kaaret, P.Kertzman, M.Kieda, D.Kleiner, T. K.Korzoun, N.Krennrich, F.Kumar, S.Lang, M. J.Maier, G.McGrath, C. E.Mooney, C. L.Moriarty, P.Mukherjee, R.O'Brien, S.Ong, R. A.Park, N.Patel, S. R.Pfrang, K.Pohl, M.Pueschel, E.Quinn, J.Ragan, K.Reynolds, P. T.Roache, E.Sadeh, I.Saha, L.Sembroski, G. H.Tak, D.Tucci, J. V.Weinstein, A.Williams, D. A.Woo, J.(VERITAS Collaboration)2024-12-132024-12-132024-01Pope, I., Mori, K., Abdelmaguid, M., Gelfand, J. D., Reynolds, S. P., Safi-Harb, S., ... & VERITAS Collaboration. (2024). A Multiwavelength Investigation of PSR J2229+ 6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands. The Astrophysical Journal, 960(1), 75. https://doi.org/10.3847/1538-4357/ad0120https://hdl.handle.net/1805/45062G106.3+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 (Eγ > 100 GeV) followed by the recent detection of ultrahigh-energy gamma-ray emission (Eγ > 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.enAttribution 4.0 Internationalpulsar wind nebulaex-ray astronomygamma-ray astronomyArticle