English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

While the GeV $\gamma$-ray emission of starburst galaxies (SBG) is commonlythought to arise from hadronic interactions between accelerated cosmic rays andinterstellar gas, the origin of the TeV $\gamma$-ray emission is moreuncertain. One possibility is that a population of pulsar wind nebulae (PWNe)in these galaxies could be responsible for the TeV $\gamma$-ray emission. Inthis work, we first synthesize a PWNe population in the Milky Way, and assessedtheir contribution to the $\gamma$-ray emission of the Galaxy, using atime-dependent model to calculate the evolution of the PWN population. Suchsynthetic PWN population can reproduce the flux distribution of identified PWNein the Milky Way given a distribution of the initial state of the pulsarpopulation. We then apply it to starburst galaxies and quantitatively calculatethe spectral energy distribution of all PWNe in the SBG NGC 253 and M82. Wepropose that TeV $\gamma$-ray emission in starburst galaxies can be dominatedby PWNe for a wide range of parameter space. The energetic argument requiresthat $\eta_e \times v_{\rm SN} > 0.01 {\rm yr}^{-1}$, where $\eta_e$ is thefraction the spin-down energy going to electrons and $v_{\rm SN}$ is thesupernova rate. By requiring the synchrotron emission flux of all PWNe in thegalaxy not exceeding the hard X-ray measurement of NGC 253, we constrain theinitial magnetic field strength of PWNe to be $< 400 \mu$G. Future observationsat higher energies with LHAASO or next-generation neutrino observatoryIceCube-Gen2 will help us to understand better the origin of the TeV$\gamma$-ray emission in SBGs.

Could the TeV emission of starburst galaxies originate from pulsar wind nebulae?