▁are ▁still ▁in ▁the ▁process ▁of ▁contra ction ▁before ▁they ▁reach ▁the ▁main ▁sequence , ▁and ▁they ▁may ▁still ▁have ▁gas ▁acc re ting ▁onto ▁them ▁from ▁either ▁a ▁circum stell ar ▁disk ▁or ▁en velope . ▁ ▁Cl uster ▁members ▁in ▁RC W ▁ 3 6 ▁have ▁been ▁identified ▁through ▁both ▁inf ra red ▁and ▁X - ray ▁observations . ▁Bright ▁inf ra red ▁sources , ▁attributed ▁to ▁massive ▁stars , ▁were ▁first ▁identified ▁by ▁the ▁T IF R ▁ 1 0 0 - cm ▁bal lo on - born ▁teles cope ▁from ▁the ▁National ▁Bal lo on ▁Fac ility ▁in ▁Hy der abad , ▁India . ▁In ▁the ▁early ▁ 2 0 0 0 s , ▁inf ra red ▁images ▁in ▁the ▁J , ▁H , ▁and ▁K s ▁bands ▁have ▁suggested ▁at ▁least ▁ 3 5 0 ▁cluster ▁members . ▁Observ ations ▁by ▁NASA ' s ▁Sp itzer ▁Space ▁T eles cope ▁and ▁Ch andra ▁X - ray ▁Observ atory ▁were ▁used ▁to ▁identify ▁cluster ▁members ▁as ▁part ▁of ▁the ▁MY St IX ▁survey ▁of ▁nearby ▁star - form ing ▁regions . ▁In ▁the ▁MY St IX ▁catalog ▁of ▁ 3 8 4 ▁probable ▁young ▁stell ar ▁members ▁of ▁RC W ▁ 3 6 , ▁more ▁than ▁ 3 0 0 ▁of ▁the ▁stars ▁are ▁detected ▁by ▁X - ray ▁sources . ▁Model ing ▁of ▁the ▁bright ness es ▁of ▁stars ▁at ▁various ▁inf ra red ▁w avel ength s ▁has ▁shown ▁ 1 3 2 ▁young ▁stell ar ▁objects