The first interstellar object, 'Oumuamua, was discovered in the Solar System by Pan-STARRS in 2017, allowing for a calibration of the abundance of interstellar objects of its size ∼ 100 m. One would expect a much higher abundance of smaller interstellar objects, with some of them colliding with Earth frequently enough to be noticeable. Based on the CNEOS catalog of bolide events, we identify the ∼ 0.45m meteor detected at 2014-01-08 17:05:34 UTC as originating from an unbound hyperbolic orbit with 99.999% confidence. We infer that the meteor had an asymptotic speed of v ∞ ∼ 42.1±5.5 km s −1 outside of the solar system. Its origin is approximately towards R.A. 49.4±4.1 • and declination 11.2 ± 1.8 • , implying that its initial velocity vector was 58 ± 6 km s −1 away from the velocity of the Local Standard of Rest (LSR). Its high LSR speed implies a possible origin from the deep interior of a planetary system or a star in the thick disk of the Milky Way galaxy. The local number density of its population is 10 6 +0.75 −1.5 AU −3 or 9 × 10 21 +0.75 −1.5 pc −3 (necessitating 0.2 -20 Earth masses of material to be ejected per local star). This discovery enables a new method for studying the composition of interstellar objects, based on spectroscopy of their gaseous debris as they burn up in the Earth's atmosphere.