Ponente
Descripción
A point-like gamma-ray source (HESS J1745–290) has been detected in the inner Galactic Center, spatially coincident with Sagittarius A (Sgr A). However, the currently quiescent state of Sgr A challenges its interpretation as the origin of the emission. An alternative explanation is that a single pulsar wind nebula (PWN) accounts for the observed signal. However, X-ray observations have identified dozens of PWN candidates within the angular resolution of the gamma-ray instrument. Our goal is to determine whether the point-like gamma-ray emission observed toward Sgr A can be attributed to a population of PWNe. We develop a PWN evolutionary model that is consistent with the observed properties of pulsars in the Galaxy and with interstellar medium conditions representative of the Galactic Center. We compute the cumulative gamma-ray emission from $\sim 10^{35}$ synthetic PWN populations and compare the results with current observations. Although the observed spectrum can be reproduced by several hundred different PWN populations, the rapid evolution of all PWNe in the GC environment prevents their simultaneous presence. At most, two PWNe can coexist within the central 30 pc, in contrast with X-ray observations. In conclusion, the observed gamma-ray spectrum could be explained by one or two PWNe embedded in an intense ambient photon field. The remaining X-ray sources are likely bow shocks from pulsars, with negligible gamma-ray emission.
