Using a sample of nearly half million galaxies, intersected by over 7 millionlines of sight from the Sloan Digital Sky Survey Data Release 12, we traceH$\alpha$ + [N{\small II}] emission from a galactocentric projected radius,$r_p$, of 5 kpc to more than 100 kpc. The emission flux surface brightness is$\propto r_p^{-1.9 \pm 0.4}$. We obtain consistent results using only theH$\alpha$ or [N{\small II}] flux. We measure a stronger signal for the bluerhalf of the target sample than for the redder half on small scales, $r_p <$ 20kpc. We obtain a $3\sigma$ detection of H$\alpha$ + [N{\small II}] emission inthe 50 to 100 kpc $r_p$ bin. The mean emission flux within this bin is $(1.10\pm 0.35) \times 10^{-20}$ erg cm$^{-2}$ s$^{-1}$ \AA$^{-1}$, which correspondsto $1.87 \times 10^{-20}$ erg cm$^{-2}$ s$^{-1}$ arcsec$^{-2}$ or 0.0033Rayleigh. This detection is 34 times fainter than a previous strict limitobtained using deep narrow-band imaging. The faintness of the signaldemonstrates why it has been so difficult to trace recombination radiation outto large radii around galaxies. This signal, combined with published estimatesof n$_{\rm H}$, lead us to estimate the temperature of the gas to be 12,000 K,consistent with independent empirical estimates based on metal ion absorptionlines and expectations from numerical simulations.