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Large pristine samples of red clump stars are highly sought after given thatthey are standard candles and give precise distances even at large distances.However, it is difficult to cleanly select red clumps stars because they canhave the same T$_{\mathrm{eff}}$ and log $g$ as red giant branch stars.Recently, it was shown that the asteroseismic parameters, $\rm{\Delta}$P and$\rm{\Delta\nu}$, which are used to accurately select red clump stars, can bederived from spectra using the change in the surface carbon to nitrogen ratio([C/N]) caused by mixing during the red giant branch. This change in [C/N] canalso impact the spectral energy distribution. In this study, we predict the$\rm{\Delta}$P, $\rm{\Delta\nu}$, T$_{\mathrm{eff}}$ and log $g$ using 2MASS,AllWISE, \gaia, and Pan-STARRS data in order to select a clean sample of redclump stars. We achieve a contamination rate of $\sim$20\%, equivalent to whatis achieved when selecting from T$_{\mathrm{eff}}$ and log $g$ derived from lowresolution spectra. Finally, we present two red clump samples. One sample has acontamination rate of $\sim$ 20\% and $\sim$ 405,000 red clump stars. The otherhas a contamination of $\sim$ 33\% and $\sim$ 2.6 million red clump stars whichincludes $\sim$ 75,000 stars at distances $>$ 10 kpc. For |b|>30 degrees wefind $\sim$ 15,000 stars with contamination rate of $\sim$ 9\%. The scientificpotential of this catalog for studying the structure and formation history ofthe Galaxy is vast given that it includes millions of precise distances tostars in the inner bulge and distant halo where astrometric distances areimprecise.

From the Inner to Outer Milky Way: A Photometric Sample of 2.6 Million Red Clump Stars