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We observed eclipses of the transiting brown dwarf CWW 89Ab at 3.6um and4.5um using Spitzer/IRAC. The CWW 89 binary system is a member of the$3.0\pm0.25$ Gyr-old open cluster Ruprecht 147, and is composed of a Sun-likeprimary and an early M-dwarf secondary separated by a projected distance of 25AU. CWW 89Ab has a radius of $0.937\pm0.042$ RJ and a mass of $36.5\pm0.1$ MJ,and is on a 5.3 day orbit about CWW 89A with a non-zero eccentricity of$e=0.19$ (Curtis et al. 2016). We strongly detect the eclipses of CWW 89Ab inboth Spitzer channels as $\delta_{3.6}=1147\pm213$ ppm and$\delta_{4.5}=1097\pm225$ ppm after correcting for the dilution from CWW 89B.After accounting for the irradiation that CWW 89Ab receives from its host star,these measurements imply that the brown dwarf has an internal luminosity of$\log(\mathrm{L_{bol}/\mathrm{L}_\odot})=-4.19\pm0.14$. This is 16 times, or$9.3\,\sigma$, higher than model predictions given the known mass, radius, andage of CWW 89Ab. As we discuss, this over-luminosity is not explainable by aninaccurate age determination, additional stellar heating, nor tidal heating.Instead, we suggest that the anomalous luminosity of CWW 89Ab is caused by adayside temperature inversion -- though a significant error in the evolutionarymodels is also a possibility. Importantly, a temperature inversion wouldrequire a super-stellar C/O ratio in CWW 89Ab's atmosphere. If this is indeedthe case, it implies that CWW 89Ab is a 36.5 MJ object that formed via coreaccretion processes. Finally, we use our measurement of CWW 89Ab's orbitaleccentricity, improved via these observations, to constrain the tidal qualityfactors of the brown dwarf and the host star CWW 89A to be $Q_{BD}>10^{4.15}$and $Q_*>10^{9}$, respectively.

A Significant Over-Luminosity in the Transiting Brown Dwarf CWW 89Ab