New X-ray observations towards PSR J1826-1256

DUVIDOVICH, L.; PETRIELLA, A.; GIACANI, E.; SUPAN, L.; GIACANI, E.; SUPAN, L.; CASTELLETTI, G.; CASTELLETTI, G.; DUVIDOVICH, L.; PETRIELLA, A.

Chania

Congreso; Supernova Remnants II: An Odyssey In Space After Stellar Death; 2019

The pulsar PSR J1826-1256, one of the brightest radio-quiet gamma-ray pulsars, is surrounded by diffuse and weak X-ray emission of non-thermal origin. It was suggested that this emission detected with Chandra could come from the pulsar wind nebula (PWN) powered by PSR J1826-1256, named G18.5-0.4 or ?Eel? PWN (Roberts et al. 2007, BAAS, 39, 997 ). PSR J1826-1256 is seen projected 5.4 ʹ away from the centroid of the TeV source HESS J1826-130, which is a newly-unidentified extended TeV source, previously hidden within the emission from the bright nearby PWN HESS J1825−137 (H.E.S.S. Collaboration 2018, A&A 612, A1).Aims: Confirm the nature of the X-ray emission around PSR J1826-1256 and investigate its connection with the very-high-energy source HESS J1826-130, in order to unveil the origin of the gamma-ray emission.