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We report the discovery of a massive (Mpsini = 13.02 +/- 0.64 Mjup; totalmass 13.25 +/- 0.64 Mjup), large (1.95 +/- 0.16 Rjup) planet in a transiting,eccentric orbit (e = 0.260 +/- 0.017) around a 10th magnitude F5V star in theconstellation Camelopardalis. We designate the planet XO-3b, and the star XO-3,also known as GSC 03727-01064. The orbital period of XO-3b is 3.1915426 +/-0.00014 days. XO-3 lacks a trigonometric distance; we estimate its distance tobe 260 +/- 23 pc. The radius of XO-3 is 2.13 +/- 0.21 Rsun, its mass is 1.41+/- 0.08 Msun, its vsini = 18.54 +/- 0.17 km/s, and its metallicity is [Fe/H] =-0.177 +/- 0.027. This system is unusual for a number of reasons. XO-3b is oneof the most massive planets discovered around any star for which the orbitalperiod is less than 10 days. The mass is near the deuterium burning limit of 13Mjup, which is a proposed boundary between planets and brown dwarfs. AlthoughBurrows et al. (2001) propose that formation in a disk or formation in theinterstellar medium in a manner similar to stars is a more logical way todifferentiate planets and brown dwarfs, our current observations are notadequate to address this distinction. XO-3b is also unusual in that itseccentricity is large given its relatively short orbital period. Both theplanetary radius and the inclination are functions of the spectroscopicallydetermined stellar radius. Analysis of the transit light curve of XO-3bsuggests that the spectroscopically derived parameters may be over estimated.Though relatively noisy, the light curves favor a smaller radius in order tobetter match the steepness of the ingress and egress. The light curve fitsimply a planetary radius of 1.25 +/- 0.15 Rjup, which would correspond to amass of 12.03 +/- 0.46 Mjup.

XO-3b: A Massive Planet in an Eccentric Orbit Transiting an F5V Star