0 ▁might ▁appear ▁vis ibly ▁similar , ▁but ▁would ▁appear ▁different ▁in ▁the ▁inf ra red . ▁ ▁The ▁W I Y N ▁Observ atory ' s ▁ 3 . 5 m ▁teles cope ▁was ▁used ▁for ▁spe ck le ▁imag ing ▁on ▁June ▁ 1 8 , ▁ 2 0 1 0 ; ▁in ▁addition , ▁the ▁P HA RO ▁camera ▁on ▁the ▁Pal om ar ▁Observ atory ' s ▁ 5 m ▁teles cope ▁was ▁used ▁for ▁its ▁adapt ive ▁opt ics ▁capabilities . ▁These ▁observations , ▁combined ▁with ▁observations ▁of ▁Ke pler - 1 0 ' s ▁spectrum ▁taken ▁from ▁the ▁W . M . ▁Ke ck ▁Observ atory , ▁ruled ▁out ▁the ▁possibility ▁that ▁a ▁nearby ▁star ' s ▁light ▁was ▁cor rupt ing ▁the ▁observed ▁spectrum ▁of ▁Ke pler - 1 0 ▁and ▁creating ▁the ▁results ▁that ▁had ▁led ▁astronom ers ▁to ▁believe ▁that ▁a ▁second ▁planet ▁existed ▁in ▁Ke pler - 1 0 ' s ▁orbit . ▁All ▁of ▁these ▁possibilities , ▁with ▁the ▁exception ▁of ▁if ▁such ▁a ▁star ▁existed ▁exactly ▁behind ▁or ▁in ▁front ▁of ▁Ke pler - 1 0 , ▁were ▁effectively ▁ruled ▁out ; ▁even ▁with ▁this , ▁the ▁Ke pler ▁team ▁found ▁that ▁if ▁a ▁star ▁was ▁indeed ▁aligned ▁with ▁Ke pler - 1 0 ▁as ▁seen ▁from ▁Earth , ▁such ▁a ▁star ▁would ▁probably ▁not ▁be ▁a ▁giant ▁star . ▁ ▁With ▁a ▁greater ▁degree ▁of ▁certain ty ▁established , ▁the ▁Ke pler ▁team ▁compared ▁the ▁models ▁formed ▁using ▁B LE