2007年11月26日 · Kes 75 is likely at distance of 5.1 to 7.5 kpc because the highest HI absorption velocity is at 95 km/s and no absorption is associated with a nearby HI emission peak at 102 km/s in the direction of Kes 75. This distance to Kes 75 gives a reasonable luminosity of PSR J1846-0258 and its PWN, and also leads to a much smaller radius for Kes 75.

VHE gamma-ray emission from the new source HESS J1846-029 is spatially coincident with G29.7-0.3 (also known as Kes 75), one of the youngest composite SNRs in the Galaxy, which contains the nebula of PSR J1846-0258.

Applying this type of study to PSR J1846 0258 and PWN Kes 75 allows − valuable constraints in understanding why this source exhibits both RPP-like and magnetar properties. From this we can understand whether this is an evolutionary phase of young and energetic NSs or a separate class.

We report the detection of gamma-ray emission from pulsar wind nebula (PWN) Kes 75 and PSR J1846-0258. Through modeling the spectral energy distribution incorporating the new Fermi-LAT data, we find that the observed gamma-ray emission is likely a combination of both the PWN and pulsar magnetosphere.

2022年1月12日 · Kes 75 is a Galactic SNR consisting of a PWN and a partial thermal shell. The PWN is powered by a 0.3 s pulsar (PSR J1846-0258) that has a characteristic age of 723 yr, one of the youngest known (Gotthelf et al. 2000).

We model the dynamical and radiative evolution of the Kes 75 system to estimate the birth properties of the neutron star, the energetics of its progenitor, and properties of the PWN. This suggests that the progenitor of Kes 75 was originally in a binary system which transferred most of its mass to a companion before exploding.

We present the results of detailed spatial and spectral analysis of the pulsar wind nebula (PWN) in supernova remnant Kes 75 (G29.7-0.3) using a deep exposure with Chandra X-Ray Observatory. The PWN shows a complex morphology with clear axisymmetric structure.

2001年12月3日 · We have observed the young Galactic supernova remnant Kes 75 with the Chandra X-ray Observatory. This object is one of an increasing number of examples of a shell-type remnant with a central extended radio core harboring a pulsar. Here we present a preliminary spatially resolved spectroscopic analysis of the Kes~75 system.

We present coeval XMM-Newton and NuSTAR X-ray observations of the pulsar wind nebula (PWN) in the supernova remnant (SNR) Kes 75. The PWN is powered by PSR J1846-0258, a highly energetic (Edot = 8.1×10 36 erg/s) rotation-powered pulsar with the youngest spin-down age (Pdot/2P ∼ 728 yr).

By studying composite supernova remnants (SNRs), remnants which contain a pulsar wind nebula (PWN), it is possible to estimate physical properties of the progenitor explosion, central neutron...