A Population of TeV Pulsar Wind Nebulae in the H.E.S.S. Galactic Plane Survey

Abstract

The nine-year H.E.S.S. Galactic Plane Survey (HGPS) has yielded the most uniform observation scan of the inner Milky Way in the TeV gamma-ray band to date. The sky maps and source catalogue of the HGPS allow for a systematic study of the population of TeV pulsar wind nebulae found throughout the last decade. To investigate the nature and evolution of pulsar wind nebulae, for the first time we also present several upper limits for regions around pulsars without a detected TeV wind nebula. Our data exhibit a correlation of TeV surface brightness with pulsar spin-down powerĖ. This seems to be caused both by an increase of extension with decreasingĖ, and hence with time, compatible with a power law RPWN(Ė) ∼Ė −0.65±0.20 , and by a mild decrease of TeV gamma-ray luminosity with decreasingĖ, compatible with L1−10 TeV ∼Ė 0.59±0.21 . We also find that the offsets of pulsars with respect to the wind nebula centre with ages around 10 kyr are frequently larger than can be plausibly explained by pulsar proper motion and could be due to an asymmetric environment. In the present data, it seems that a large pulsar offset is correlated with a high apparent TeV efficiency L1−10 TeV /Ė. In addition to 14 HGPS sources considered firmly identified pulsar wind nebulae and 5 additional pulsar wind nebulae taken from literature, we find 10 HGPS sources that are likely TeV pulsar wind nebula candidates. Using a model that subsumes the present common understanding of the very high-energy radiative evolution of pulsar wind nebulae, we find that the trends and variations of the TeV observables and limits can be reproduced to a good level, drawing a consistent picture of present-day TeV data and theory.

Ground-based gamma-ray astronomy

“…For instance, all PWNe candidates detected at TeV energies are powered by relatively young pulsars with high spin down power. However, variations between the different systems are also clearly visible and could be due to the differences in the surrounding medium or different starting conditions [15].…”