ND ER ▁to ▁the ▁phot ometric ▁observations ▁collected ▁by ▁the ▁Ke pler ▁satellite . ▁The ▁B LE ND ER ▁technique ▁allowed ▁the ▁Ke pler ▁team ▁to ▁rule ▁out ▁the ▁majority ▁of ▁the ▁alternatives ▁including , ▁not ably , ▁that ▁of ▁triple ▁star ▁systems . ▁B LE ND ER ▁then ▁allowed ▁the ▁Ke pler ▁team ▁to ▁determine ▁that ▁although ▁all ▁models ▁representing ▁hier arch ical ▁triple ▁stars ▁( a ▁binary ▁system ▁between ▁a ▁single ▁star ▁and ▁a ▁double ▁star ) ▁can ▁res emble ▁the ▁light ▁curve ▁of ▁Ke pler - 1 0 , ▁the ▁a for ement ioned ▁follow - up ▁observations ▁would ▁have ▁detected ▁them ▁all . ▁The ▁only ▁possible ▁bl ends ▁remaining ▁after ▁r uling ▁out ▁hier arch ical ▁triple ▁stars ▁was ▁that ▁of ▁determ ining ▁if ▁the ▁curve ▁is ▁caused ▁by ▁inter ference ▁from ▁a ▁background ▁star , ▁or ▁if ▁it ▁is ▁indeed ▁caused ▁by ▁the ▁orbit ▁of ▁a ▁trans iting ▁planet . ▁ ▁Compar isons ▁of ▁K O I ▁ 0 7 2 . 0 2 ▁to ▁the ▁ 1 2 3 5 ▁other ▁Ke pler ▁Object s ▁of ▁Interest ▁in ▁Ke pler ' s ▁field ▁of ▁vision ▁allowed ▁astronom ers ▁to ▁use ▁models ▁that ▁led ▁to ▁the ▁confirm ation ▁of ▁K O I ▁ 0 7 2 . 0 2 ▁as ▁a ▁planet ▁with ▁a ▁high ▁degree ▁of ▁certain ty . ▁K O I ▁ 0 7 2 . 0 2 ▁was ▁then ▁renamed ▁Ke pler - 1 0 c . ▁The ▁planet ' s ▁confirm ation ▁was ▁announced