Kepler-62f (also known by its Kepler Object of Interest designation KOI-701.04) is a super-Earth exoplanet orbiting within the habitable zone of the star Kepler-62, the outermost of five such planets discovered around the star by NASA's Kepler space telescope. It is located about 982 light-years (301 parsecs) from Earth in the constellation of Lyra.

Kepler-62f orbits its parent star at a distance of 0.718 AU (107,400,000 km; 66,700,000 mi) from its host star with an orbital period of roughly 267 days, and has a radius of around 1.41 times that of Earth. It is one of the more promising candidates for potential habitability, as its parent star is a relatively quiet star, and has less mass than the Sun – thus it can live up to a span of about 30 billion years or so. Based on its size, Kepler-62f is likely a terrestrial or ocean-covered planet. However, key components of the exoplanet still need to be assessed to determine habitability; such as its atmosphere if one exists, since it lies within the outer part of its host star's habitable zone.

The discovery of the exoplanet–along with Kepler-62e–was announced in April 2013 by NASA as part of the Kepler space telescope data release. The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. According to scientists, it is a potential candidate to search for extraterrestrial life, and was chosen as one of the targets to study by the Search for Extraterrestrial Intelligence (SETI) program.

Kepler-62f is a super-Earth, placing it within the class of exoplanets with a radius and mass bigger than Earth, but smaller than that of the ice giants Neptune and Uranus. It has an equilibrium temperature of 208 K (−65 °C; −85 °F), close to that of Mars’s temperature. It has a radius of 1.46 R_🜨, placing it below the radius of ≥1.6 R_🜨 where it would otherwise be a mini-Neptune with a volatile composition, with no solid surface. Due to its radius, it is likely a rocky planet. However, the mass isn't constrained yet, estimates place an upper limit of <35 M_🜨, the real mass is expected to be significantly lower than this. The Planetary Habitability Laboratory estimated a mass of around 2.6 M_🜨, assuming a rocky Earth-like composition.

The planet orbits a (K-type) star named Kepler-62, orbited by a total of five known planets. The star has a mass of 0.69 M_☉ and a radius of 0.64 R_☉. It has a temperature of 4925 K and is 7 billion years old. In comparison, the Sun is 4.6 billion years old and has a temperature of 5778 K. The star is somewhat metal-poor, with a metallicity ([Fe/H]) of −0.37, or 42% of the solar amount. Its luminosity (L_☉) is 21% that of the Sun.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.65. Therefore, it is too dim to be seen with the naked eye.

Kepler-62f orbits its host star every 267.29 days at a semi-major axis distance of about 0.718 astronomical units (107,400,000 km, 66,700,000 mi), which is roughly the same as Venus's semi-major axis from the Sun. Compared to Earth, this is about seven-tenths of the distance from it to the Sun. Kepler-62f is estimated to receive about 41% of the amount of sunlight that Earth does from the Sun, which is comparable to Mars, which receives 43%.

Given the planet's age (7 ± 4 billion years), irradiance (0.41 ± 0.05 times Earth's) and radius (1.46 ± 0.07 times Earth's), a rocky (silicate-iron) composition with the addition of a possibly substantial amount of water is considered plausible. A modeling study indicates it is likely that a great majority of planets in its size range are completely covered by ocean. If its density is the same as Earth's, its mass would be 1.41³ or 2.80 times Earth's. The planet has the potential for hosting a moon according to a study of tidal effects on potentially habitable planets. The planet may be the only habitable-zone candidate which would avoid desiccation by irradiation from the host star at its current location.