Editing Epsilon Eridani (section)

=== Detection of proximity ===
Based on observations between 1800 and 1880, Epsilon Eridani was found to have a large [[proper motion]] across the [[celestial sphere]], which was estimated at three [[arcsecond]]s per year ([[angular velocity]]).<ref name=mras48_77 /> This movement implied it was relatively close to the Sun,<ref name=belkora2002 /> making it a star of interest for the purpose of [[stellar parallax]] measurements. This process involves recording the position of Epsilon Eridani as Earth moves around the Sun, which allows a star's distance to be estimated.<ref name=mras48_77 /> From 1881 to 1883, American astronomer [[William Lewis Elkin|William L. Elkin]] used a [[heliometer]] at the [[Royal Observatory at the Cape of Good Hope]], South Africa, to compare the position of Epsilon Eridani with two nearby stars. From these observations, a parallax of {{nowrap|0.14 ± 0.02 arcseconds}} was calculated.<ref name=gill1893 /><ref name=gill1884 /> By 1917, observers had refined their parallax estimate to 0.317&nbsp;arcseconds.<ref name=apj46_313 /> The modern value of 0.3109&nbsp;arcseconds is equivalent to a distance of about {{convert|10.50|ly|pc}}.<ref name=aaa474_2_653 />