Gurwich, Ilya | Search NASA

DOE OSTI2017

IceCube Constraints on the Fermi Bubbles

We analyze the IceCube four-year neutrino data in search of a signal from the Fermi bubbles. No signal is found from the bubbles or from their dense shell, even when taking into account the softer background. This imposes a conservative ξ {sub i} < 8% upper limit on the cosmic-ray ion (CRI) acceleration efficiency, and an η ≡ ξ {sub e} / ξ {sub i} ≳ 0.006 lower limit on the electron-to-ion ratio of acceleration efficiencies (at the 2 σ confidence level). For typical ξ {sub i} , a signal should surface once the number of IceCube neutrinos increases by ∼an order of magnitude, unless there is a <PeV cutoff on the CRI spectrum.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2017

Fermi Bubble Edges: Spectrum and Diffusion Function

Current measurements of the γ-ray Fermi bubbles (FB) are based on model-dependent tracers, carry substantial systematic uncertainties, and contain some discrepancies between each other. We show that gradient filters pick out the FB edges, which are found to smoothly connect to the bipolar X-ray structure emanating from the Galactic center, thus supporting the interpretation of the FBs as a Galactic-scale phenomenon. The sharp edges facilitate a direct, model-free measurement of the peripheral FB spectrum. The result is strikingly similar to the full FB-integrated spectrum, softened by a power law of index η ≃ (0.2–0.3). This is naturally explained, in both hadronic and leptonic models, if cosmic rays are injected at the edge, and diffuse away preferentially at higher energies E. The inferred, averaged diffusion function in the (more plausible) leptonic model, D(E)≃10{sup 29.5}(E/10GeV){sup 0.48±0.02} cm{sup 2} s{sup −1}, is consistent with estimates for Kraichnan-like turbulence. Our results, in particular the minute spatial variations in η, indicate that the FB edge is a strong, Mach ≳5, forward shock.

79 ASTRONOMY AND ASTROPHYSICS↗