Searching for High Energy Neutrino counterpart signals; The case of the Fermi Bubbles signal and of Dark Matter annihilation in the inner Galaxy

TL;DR

This paper evaluates various theoretical models explaining the Fermi Bubbles and WMAP haze through their predicted high-energy neutrino signals, assessing the potential of current and future neutrino detectors to distinguish these models and probe dark matter annihilation.

Contribution

It compares neutrino signals from different models of the Fermi Bubbles and dark matter, highlighting the capabilities of IceCube DeepCore and km$^3$ telescopes to discriminate among them.

Findings

Some models will be tested by IceCube DeepCore.

Future km$^3$ telescopes can distinguish hadronic, leptonic, and dark matter models.

Neutrino spectra can probe TeV-scale dark matter annihilation.

Abstract

The recent uncovering of the \textit{Fermi} Bubbles/haze in the \textit{Fermi} gamma-ray data has generated theoretical work to explain such a signal of hard $\gamma$-rays in combination with the \textit{WMAP} haze signal. Many of these theoretical models can have distinctively different implications with regards to the production of high energy neutrinos. We discuss the neutrino signals from different models proposed for the explanation of the \textit{Fermi} Bubbles/haze, more explicitly, from Dark Matter annihilation in the galactic halo with conditions of preferential CR diffusion, from recent AGN jet activity, from periodic diffusive shock acceleration, from stochastic 2nd order Fermi acceleration and from long time-scale star formation in the galactic center in combination with strong galactic winds. We find that some of these models will be probed by the IceCube DeepCore detector. Moreover, with a km$^3$ telescope located at the north hemisphere, we will be able to discriminate between the hadronic, leptonic and the DM models. Additionally using the reconstructed neutrino spectra we will probe annihilation of TeV scale dark matter towards the galactic center.