Kepler-395 c is a planet about 1.3 times Earth's width orbiting an orange dwarf star about 1,400 light-years away. It crosses in front of its star every 35 days and is the outer of two known planets in the system, after Kepler-395 b.
NASA's Kepler space telescope found both by the small dips in starlight as they pass across the star. They were confirmed in 2014 in a study led by Jason Rowe that validated hundreds of Kepler planets at once. When a star shows more than one transit signal, it is very unlikely that they are all false alarms from something else in view, so such planets can be confirmed statistically without weighing them. In 2017 a team led by Guillermo Torres re-examined Kepler-395 c, listed as candidate KOI-2650.01, with a separate statistical method called BLENDER plus spectra and high-resolution imaging, and validated it at about 99.92 percent confidence.
Torres's team was studying small planets in or near the habitable zone, the range of distances where liquid water could last on a surface. They calculated that Kepler-395 c receives about 2.1 times the light Earth gets from the Sun, with an equilibrium temperature, set by starlight alone, of about 341 kelvin, warmer than Earth. Its imaging also showed a faint star about three arcseconds away. At about 1.3 Earth radii it is small enough that it could be rocky, but its mass has not been measured.