TY  - JOUR
AU  - Pope, I.
AU  - Mori, K.
AU  - Abdelmaguid, M.
AU  - Gelfand, J. D.
AU  - Reynolds, S. P.
AU  - Safi-Harb, S.
AU  - Hailey, C. J.
AU  - An, H.
AU  - Bangale, P.
AU  - Batista, P.
AU  - Benbow, W.
AU  - Buckley, J. H.
AU  - Capasso, M.
AU  - Christiansen, J. L.
AU  - Chromey, A. J.
AU  - Falcone, A.
AU  - Feng, Q.
AU  - Finley, J. P.
AU  - Foote, G. M.
AU  - Gallagher, G.
AU  - Hanlon, W. F.
AU  - Hanna, D.
AU  - Hervet, O.
AU  - Holder, J.
AU  - Humensky, T. B.
AU  - Jin, W.
AU  - Kaaret, P.
AU  - Kertzman, M.
AU  - Kieda, D.
AU  - Kleiner, T. K.
AU  - Korzoun, N.
AU  - Krennrich, F.
AU  - Kumar, S.
AU  - Lang, M. J.
AU  - Maier, G.
AU  - McGrath, C. E.
AU  - Mooney, C. L.
AU  - Moriarty, P.
AU  - Mukherjee, R.
AU  - O'Brien, S.
AU  - Ong, R. A.
AU  - Park, N.
AU  - Patel, S. R.
AU  - Pfrang, K.
AU  - Pohl, M.
AU  - Pueschel, E.
AU  - Quinn, J.
AU  - Ragan, K.
AU  - Reynolds, P. T.
AU  - Roache, E.
AU  - Sadeh, I.
AU  - Saha, L.
AU  - Sembroski, G. H.
AU  - Tak, D.
AU  - Tucci, J. V.
AU  - Weinstein, A.
AU  - Williams, D. A.
AU  - Woo, J.
TI  - A Multiwavelength Investigation of PSR J2229+6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands
JO  - The astrophysical journal / Part 1
VL  - 960
IS  - 1
SN  - 0004-637X
CY  - London
PB  - Institute of Physics Publ.
M1  - PUBDB-2024-07339
M1  - arXiv:2310.04512
SP  - 75
PY  - 2024
AB  - 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<sub>γ</sub> > 100 GeV) followed by the recent detection of ultrahigh-energy gamma-ray emission (E<sub>γ</sub> > 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.
LB  - PUB:(DE-HGF)16
UR  - <Go to ISI:>//WOS:001136394600001
DO  - DOI:10.3847/1538-4357/ad0120
UR  - https://bib-pubdb1.desy.de/record/619039
ER  -