2007/10/01 by J. A. Hinton, S. Funk, S. Carrigan +5 · 1 citation
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Galaxy #Luminosity #Nebula #Nuclear physics #Physics #Pulsar #Pulsar wind nebula #Pulsars and Gravitational Waves Research #Stars #Synchrotron #astro-ph
paper · pdf · doi:10.1051/0004-6361:20078775
published as Astron.Astrophys.476:25,2007 · 4 pages, 2 figures, submitted to A&A
arxiv created 2007/10/01 · openalex publication_date 2007/11/12 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Combined X-ray synchrotron and inverse-Compton γ-ray observations of pulsar wind nebulae (PWN) may help to elucidate the processes of acceleration and energy loss in these systems. In particular, such observations provide constraints on the particle injection history and the magnetic field strength in these objects. The newly discovered TeV γ-ray source HESS J1718-385 has been proposed as the likely PWN of the high spin-down luminosity pulsar PSR J1718-3825. The absence of previous, sensitive X-ray measurements of this pulsar, and the unusual energy spectrum of the TeV source, motivated observations of this region with XMM-Newton. The data obtained reveal a hard-spectrum X-ray source at the position of PSR 1718-3825 and evidence of diffuse emission in the vicinity of the pulsar. We derive limits on the keV emission from the centroid of HESS J1718-385 and discuss the implications of these findings for the PWN nature of this object.