We analyze the gamma-ray sky at energies of 0.5 to 50 GeV using the undecimated wavelet transform on the sphere. Focusing on the inner $60°\times 60°$ of the sky, we identify and characterize four separate residuals beyond the expected Milky Way diffuse emission. We detect the Fermi bubbles, finding compelling evidence that they are diffuse in nature and contain very little small-scale structure. We detect the “cocoon” inside the southern bubble, and we also identify its northern counterpart above 2 GeV. The northern cocoon lies along the same axis but is $\sim 30\%$ dimmer than the southern one. We characterize the Galactic center excess, which we find extends up to 20° in $|b|$. At latitudes $|b|\le 5°$ we find evidence for power in small angular scales that could be the result of point-source contributions, but for $|b|\ge 5°$ the Galactic center excess is dominantly diffuse in its nature. Our findings show either that the Galactic center excess and Fermi bubbles connect smoothly or that the bubbles brighten significantly below 15° in latitude. We find that the Galactic center excess appears off-center toward negative $\ell$. Additionally, we find and characterize two emissions along the Galactic disk centered at $\ell \simeq +25°$ and $-20°$. These emissions are significantly more elongated along the Galactic disk than the Galactic center excess.

• Received 14 March 2018

DOI:https://doi.org/10.1103/PhysRevD.98.043009