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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 $60^{\circ} \times 60^{\circ}$ of the sky, we identify and characterize four separate residuals beyond the expected Milky Way diffuse emission. We detect the \textit{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 $20^{\circ}$ in $|b|$. At latitudes $|b| \leq 5^{\circ}$ we find evidence for power in small angular scales that could be the result of point-source contributions, but for $|b| \geq 5^{\circ}$ the Galactic center excess is dominantly diffuse in its nature. Our findings show that either the Galactic center excess and {\it Fermi} Bubbles connect smoothly or that the Bubbles brighten significantly below $15^\circ$ in latitude. We find that the Galactic center excess appears off-center by a few degrees towards negative $\ell$. Additionally, we find and characterize two emissions along the Galactic disk centered at $\ell \simeq +25^{\circ}$ and $-20^{\circ}$. These emissions are significantly more elongated along the Galactic disk than the Galactic center excess., Comment: 23 pages, 25 figures, 4 tables, 3 appendices

We report on a new method for tracking the phases of the orbital modulations in very short-period, near-contact, and contact binary systems systems in order to follow starspots. We apply this technique to Kepler light curves for 414 binary systems that were identified as having anticorrelated O-C curves for the midtimes of the primary and secondary eclipses, or in the case of non-eclipsing systems, their light-curve minima. This phase tracking approach extracts more information about starspot and binary system behavior than may be easily obtained from the O-C curves. We confirm the hypothesis of Tran et al. (2013) that we can successfully follow the rotational motions of spots on the surfaces of the stars in these binaries. In ~34% of the systems, the spot rotation is retrograde as viewed in the frame rotating with the orbital motion, while ~13% show significant prograde spot rotation. The remaining systems show either little spot rotation or erratic behavior, or sometimes include intervals of both types of behavior. We discuss the possibility that the relative motions of spots are related to differential rotation of the stars. It is clear from this study that the motions of the starspots in at least 50% of these short-period binaries are not exactly synchronized with the orbits., Comment: 16 pages, 14 figures, 2 tables; submitted to MNRAS