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 $\sim 100$ 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 $\sim 0.45$m 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 $v_{\infty }\sim 42.1\pm 5.5\mathrm{km}{\mathrm{s}}^{-1}$ outside of the solar system. Its origin is approximately towards R.A. $49.4\pm 4.1^{\circ }$ and declination $11.2\pm 1.8^{\circ }$, implying that its initial velocity vector was $58\pm 6\mathrm{km}{\mathrm{s}}^{-1}$ 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 $10^{6{}_{-1.5}^{+0.75}}\mathrm{A}{\mathrm{U}}^{-3}$ or $9\times 10^{21{}_{-1.5}^{+0.75}}\mathrm{p}{\mathrm{c}}^{-3}$ (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.