Modeling the {\gamma}-ray Pulsar Wind Nebulae population in our Galaxy

TL;DR

This paper develops a comprehensive, physically motivated model of the Galactic pulsar wind nebulae population to predict their gamma-ray emission, aiding future surveys in source detection and cosmic-ray studies.

Contribution

It introduces a long-term, evolution-based one-zone model incorporating reverberation effects supported by numerical studies, improving spectral evolution predictions of PWNe.

Findings

Approximately 50% of expected PWNe are detectable in current TeV surveys.

CTA is projected to triple the number of detected TeV PWNe.

The model accurately reproduces observed emission properties of known PWNe.

Abstract

Pulsar wind nebulae (PWNe) represent the largest class of sources that upcoming {\gamma}-ray surveys will detect. Therefore, accurate modelling of their global emission properties is one of the most urgent problems in high-energy astrophysics. Correctly characterizing these dominant objects is a needed step to allow {\gamma}-ray surveys to detect fainter sources, investigate the signatures of cosmic-ray propagation and estimate the diffuse emission in the Galaxy. In this paper we present an observationally motivated construction of the Galactic PWNe population. We made use of a modified one-zone model to evolve for a long period of time the entire population. The model provides, for every source, at any age, a simplified description of the dynamical and spectral evolution. The long term effects of the reverberation phase on the spectral evolution are described, for the first time, based on physically motivated prescriptions for the evolution of the nebular radius supported by numerical studies. This effort tries to solve one of the most critical aspects of one-zone modeling, namely the typical overcompression of the nebula during the reverberation phase, resulting in a strong modification of its spectral properties at all frequencies. We compare the emission properties of our synthetic Pulsar Wind Nebulae population with the most updated catalogues of TeV Galactic sources. We find that the firmly identified and candidate PWNe sum up to about 50% of the expected objects in this class above threshold for detection. Finally, we estimate that CTA will increase the number of TeV detected PWNe by a factor$\geq3$.