X-ray studies of the gamma-ray pulsar J1826-1256 and its pulsar wind nebula with Chandra and XMM-Newton

Abstract

We have analyzed archival XMM-Newton and Chandra observations of the gamma-ray radio-quiet pulsar J1826-1256 and its pulsar wind nebula. The pulsar spectrum can be described by a power-law model with a photon index $\Gamma \approx 1$. We find that the nebular spectrum softens with increasing distance from the pulsar, implying synchrotron cooling. The empirical interstellar absorption-distance relation gives a distance of $\approx 3.5$ kpc to J1826-1256. We also discuss the nebula geometry and association between the pulsar, the very high energy source HESS J1826-130, the supernova remnant candidate G18.45-0.42 and the open star cluster Bica 3.

Accepted for publication in MNRAS

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Cited by in corpus (6)

• An extreme particle accelerator in the Galactic plane: HESS J1826$-$130
• The LHAASO PeVatron bright sky: what we learned
• Broadband X-ray Spectroscopy of the Pulsar Wind Nebula in HESS J1640-465
• Observational connection of non-thermal X-ray emission from pulsars with their timing properties and thermal emission
• The Eel Pulsar Wind Nebula: a PeVatron-Candidate Origin for HAWC J1826-128 and HESS J1826-130
• Chandra Proper Motions and Milliarcsecond Astrometry of Nineteen Pulsars