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We present photometric and spectroscopic observations of the nearby($D\approx28$ Mpc) interacting supernova (SN) 2019esa, discovered within hoursof explosion and serendipitously observed by the Transiting Exoplanet SurveySatellite (TESS). Early, high cadence light curves from both TESS and the DLT40survey tightly constrain the time of explosion, and show a 30 day rise tomaximum light followed by a near constant linear decline in luminosity. Opticalspectroscopy over the first 40 days revealed a highly reddened object withnarrow Balmer emission lines seen in Type IIn supernovae. The slow rise tomaximum in the optical lightcurve combined with the lack of broad H$\alpha$emission suggest the presence of very optically thick and close circumstellarmaterial (CSM) that quickly decelerated the supernova ejecta. This CSM waslikely created from a massive star progenitor with an $\dot{M}$ $\sim$ 0.3M$_{\odot}$ yr$^{-1}$ lost in a previous eruptive episode 3--4 years beforeeruption, similar to giant eruptions of luminous blue variable stars. At latetimes, strong intermediate-width Ca II, Fe I, and Fe II lines are seen in theoptical spectra, identical to those seen in the superluminous interacting SN2006gy. The strong CSM interaction masks the underlying explosion mechanism inSN 2019esa, but the combination of the luminosity, strength of the H$\alpha$lines, and mass loss rate of the progenitor all point to a core collapseorigin.

High Cadence TESS and ground-based data of SN 2019esa, the less energetic sibling of SN 2006gy