TY - JOUR
T1 - Deep X-Ray and Radio Observations of the First Outburst of the Young Magnetar Swift J1818.0−1607
AU - Ibrahim, A. Y.
AU - Borghese, A.
AU - Rea, N.
AU - Zelati, F. Coti
AU - Parent, E.
AU - Russell, T. D.
AU - Ascenzi, S.
AU - Sathyaprakash, R.
AU - Götz, D.
AU - Mereghetti, S.
AU - Topinka, M.
AU - Rigoselli, M.
AU - Savchenko, V.
AU - Campana, S.
AU - Israel, G. L.
AU - Tiengo, A.
AU - Perna, R.
AU - Turolla, R.
AU - Zane, S.
AU - Esposito, P.
AU - Castillo, G. A.Rodríguez
AU - Graber, V.
AU - Possenti, A.
AU - Dehman, C.
AU - Ronchi, M.
AU - Loru, S.
N1 - Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/1/1
Y1 - 2023/1/1
N2 - Swift J1818.0−1607 is a radio-loud magnetar with a spin period of 1.36 s and a dipolar magnetic field strength of B ∼ 3 × 1014 G, which is very young compared to the Galactic pulsar population. We report here on the long-term X-ray monitoring campaign of this young magnetar using XMM-Newton, NuSTAR, and Swift from the activation of its first outburst in 2020 March until 2021 October, as well as INTEGRAL upper limits on its hard X-ray emission. The 1-10 keV magnetar spectrum is well modeled by an absorbed blackbody with a temperature of kT BB ∼ 1.1 keV and apparent reduction in the radius of the emitting region from ∼0.6 to ∼0.2 km. We also confirm the bright diffuse X-ray emission around the source extending between ∼50″ and ∼110″. A timing analysis revealed large torque variability, with an average spin-down rate ν ̇ ∼ −2.3 × 10−11 Hz2 that appears to decrease in magnitude over time. We also observed Swift J1818.0−1607 with the Karl G. Jansky Very Large Array on 2021 March 22. We detected the radio counterpart to Swift J1818 measuring a flux density of S v = 4.38 ± 0.05 mJy at 3 GHz and a half-ringlike structure of bright diffuse radio emission located at ∼90″ to the west of the magnetar. We tentatively suggest that the diffuse X-ray emission is due to a dust-scattering halo and that the radio structure may be associated with the supernova remnant of this young pulsar, based on its morphology.
AB - Swift J1818.0−1607 is a radio-loud magnetar with a spin period of 1.36 s and a dipolar magnetic field strength of B ∼ 3 × 1014 G, which is very young compared to the Galactic pulsar population. We report here on the long-term X-ray monitoring campaign of this young magnetar using XMM-Newton, NuSTAR, and Swift from the activation of its first outburst in 2020 March until 2021 October, as well as INTEGRAL upper limits on its hard X-ray emission. The 1-10 keV magnetar spectrum is well modeled by an absorbed blackbody with a temperature of kT BB ∼ 1.1 keV and apparent reduction in the radius of the emitting region from ∼0.6 to ∼0.2 km. We also confirm the bright diffuse X-ray emission around the source extending between ∼50″ and ∼110″. A timing analysis revealed large torque variability, with an average spin-down rate ν ̇ ∼ −2.3 × 10−11 Hz2 that appears to decrease in magnitude over time. We also observed Swift J1818.0−1607 with the Karl G. Jansky Very Large Array on 2021 March 22. We detected the radio counterpart to Swift J1818 measuring a flux density of S v = 4.38 ± 0.05 mJy at 3 GHz and a half-ringlike structure of bright diffuse radio emission located at ∼90″ to the west of the magnetar. We tentatively suggest that the diffuse X-ray emission is due to a dust-scattering halo and that the radio structure may be associated with the supernova remnant of this young pulsar, based on its morphology.
UR - https://www.scopus.com/pages/publications/85146906607
U2 - 10.3847/1538-4357/aca528
DO - 10.3847/1538-4357/aca528
M3 - Article
SN - 0004-637X
VL - 943
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 20
ER -