Deep X-ray and radio observations of the first outburst of the young magnetar Swift J1818.0-1607

TL;DR

This study presents comprehensive X-ray and radio observations of the young magnetar Swift J1818.0-1607, revealing its spectral properties, timing variability, and surrounding diffuse emission, providing insights into its early evolution and environment.

Contribution

First long-term multi-wavelength monitoring of Swift J1818.0-1607, detailing its spectral, timing, and environmental characteristics, and suggesting associations with a supernova remnant.

Findings

X-ray spectrum well modeled by an absorbed blackbody with temperature ~1.1 keV.

Detected radio counterpart with flux density ~4.38 mJy at 3 GHz.

Observed large torque variability with decreasing spin-down rate over time.

Abstract

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~3E14 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 March 2020 until October 2021, 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 nudot~-2.3E-11 Hz^2 that appears to decrease in magnitude over time. We also observed Swift J1818.0-1607 with the Karl G. Jansky Very Large Array (VLA) on 2021 March 22. We detected the radio counterpart to Swift J1818.0-1607 measuring a flux density of S_v = 4.38+/-0.05 mJy at 3 GHz, and a half ring-like 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.