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Planets in highly eccentric orbits form a class of objects not seen withinour Solar System. The most extreme case known amongst these objects is theplanet orbiting HD~20782, with an orbital period of 597~days and aneccentricity of 0.96. Here we present new data and analysis for this system aspart of the Transit Ephemeris Refinement and Monitoring Survey (TERMS). Weobtained CHIRON spectra to perform an independent estimation of the fundamentalstellar parameters. New radial velocities from AAT and PARAS observationsduring periastron passage greatly improve our knowledge of the eccentric natureof the orbit. The combined analysis of our Keplerian orbital and Hipparcosastrometry show that the inclination of the planetary orbit is $> 1.22\degr$,ruling out stellar masses for the companion. Our long-term robotic photometryshow that the star is extremely stable over long timescales. Photometricmonitoring of the star during predicted transit and periastron times using MOSTrule out a transit of the planet and reveal evidence of phase variations duringperiastron. These possible photometric phase variations may be caused byreflected light from the planet's atmosphere and the dramatic change instar--planet separation surrounding the periastron passage.

Evidence for Reflected Light from the Most Eccentric Exoplanet Known