Apply to be<br> considered for a student <br> award (Yes / No)?
Level for award<br> (Hons, MSc, <br> PhD)?
Main supervisor (name and email)<br>and his / her institution
Cecilia Lunardini, Cecilia.Lunardini@asu.edu, Arizona State University
Would you like to <br> submit a short paper <br> for the Conference <br> Proceedings (Yes / No)?
Abstract content <br> (Max 300 words)<br><a href="http://events.saip.org.za/getFile.py/access?resId=0&materialId=0&confId=34" target="_blank">Formatting &<br>Special chars</a>
The IceCube Collaboration recently announced twenty-eight events were observed with energies above ~ 30 TeV, more than expected from atmospheric backgrounds. We discuss the detectability of the Fermi Bubbles at IceCube and show that up to 4 − 5 of the 28 events could originate from the Fermi Bubbles (FB). If the observed gamma rays from the FB are created due to the baryonic mechanism, high-energy (> GeV) neutrinos should be emitted as a counterpart. These neutrinos should be detectable as shower or track-like events at a Km3 neutrino detector. For a hard primary cosmic-ray proton spectrum E-2.1 and cutoff energy at or above 10 PeV, the Fermi Bubble flux substantially exceeds the atmospheric backgrounds. For a steeper spectrum E-2.3 and/or lower cutoff energy, to observe the neutrino flux at high significance, longer running time will be required.