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Transiting hot Jupiters present a unique opportunity to measure absoluteplanetary masses due to the magnitude of their radial velocity signals andknown orbital inclination. Measuring planet mass is critical to understandingatmospheric dynamics and escape under extreme stellar irradiation. Here, wepresent the ultra-hot Jupiter system, KELT-9, as a double-lined spectroscopicbinary. This allows us to directly and empirically constrain the mass of thestar and its planetary companion, without reference to any theoretical stellarevolutionary models or empirical stellar scaling relations. Using data from thePEPSI, HARPS-N, and TRES spectrographs across multiple epochs, we applyleast-squares deconvolution to measure out-of-transit stellar radialvelocities. With the PEPSI and HARPS-N datasets, we measure in-transit planetradial velocities using transmission spectroscopy. By fitting the circularorbital solution that captures these Keplerian motions, we recover a planetarydynamical mass of 2.17 $\pm$ 0.56 $\mathrm{M_J}$ and stellar dynamical mass of2.11 $\pm$ 0.78 $\mathrm{M_\odot}$, both of which agree with the discoverypaper. Furthermore, we argue that this system, as well as systems like it, arehighly overconstrained, providing multiple independent avenues for empiricallycross-validating model-independent solutions to the system parameters. We alsodiscuss the implications of this revised mass for studies of atmosphericescape.

KELT-9 as an eclipsing double-lined spectroscopic binary: a unique and self-consistent solution to the system