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We present updated radial-velocity (RV) analyses of the AU Mic system. AU Micis a young (22 Myr) early M dwarf known to host two transiting planets -$P_{b}\sim8.46$ days, $R_{b}=4.38_{-0.18}^{+0.18}\ R_{\oplus}$,$P_{c}\sim18.86$ days, $R_{c}=3.51_{-0.16}^{+0.16}\ R_{\oplus}$. With visibleRVs from CARMENES-VIS, CHIRON, HARPS, HIRES, {\sc{\textsc{Minerva}}}-Australis, and TRES, as well as near-infrared (NIR) RVsfrom CARMENES-NIR, CSHELL, IRD, iSHELL, NIRSPEC, and SPIRou, we provide a$5\sigma$ upper limit to the mass of AU Mic c of $M_{c}\leq20.13\ M_{\oplus}$and present a refined mass of AU Mic b of $M_{b}=20.12_{-1.57}^{+1.72}\M_{\oplus}$. Used in our analyses is a new RV modeling toolkit to exploit thewavelength dependence of stellar activity present in our RVs viawavelength-dependent Gaussian processes. By obtaining near-simultaneous visibleand near-infrared RVs, we also compute the temporal evolution of RV-``color''and introduce a regressional method to aid in isolating Keplerian from stellaractivity signals when modeling RVs in future works. Using a multi-wavelengthGaussian process model, we demonstrate the ability to recover injected planetsat $5\sigma$ significance with semi-amplitudes down to $\approx$10\,m\,s$^{-1}$ with a known ephemeris, more than an order of magnitude belowthe stellar activity amplitude. However, we find that the accuracy of therecovered semi-amplitudes is $\sim$50\% for such signals with our model.

Diving Beneath the Sea of Stellar Activity: Chromatic Radial Velocities of the Young AU Mic Planetary System