cket - bor ne ▁teles cope . ▁On ▁April ▁ 1 9 , ▁ 1 9 6 0 ▁the ▁very ▁first ▁X - ray ▁image ▁of ▁the ▁sun ▁was ▁taken ▁using ▁a ▁pin hole ▁camera ▁on ▁an ▁Aer ob ee - Hi ▁ro cket . ▁ ▁The ▁util ization ▁of ▁X - ray ▁mirror s ▁for ▁ex tras olar ▁X - ray ▁astronom y ▁simultaneously ▁requires : ▁ ▁the ▁ability ▁to ▁determine ▁the ▁location ▁at ▁the ▁arrival ▁of ▁an ▁X - ray ▁phot on ▁in ▁two ▁dimensions ▁and ▁ ▁a ▁reasonable ▁detection ▁efficiency . ▁ ▁X - ray ▁astronom y ▁detect ors ▁ ▁X - ray ▁astronom y ▁detect ors ▁have ▁been ▁designed ▁and ▁configured ▁primarily ▁for ▁energy ▁and ▁occasionally ▁for ▁w avel ength ▁detection ▁using ▁a ▁variety ▁of ▁techniques ▁usually ▁limited ▁to ▁the ▁technology ▁of ▁the ▁time . ▁ ▁X - ray ▁detect ors ▁collect ▁individual ▁X - ray s ▁( ph ot ons ▁of ▁X - ray ▁elect romagnet ic ▁radiation ) ▁and ▁count ▁the ▁number ▁of ▁phot ons ▁collected ▁( int ens ity ), ▁the ▁energy ▁( 0 . 1 2 ▁to ▁ 1 2 0 ▁ke V ) ▁of ▁the ▁phot ons ▁collected , ▁w avel ength ▁( c . ▁ 0 . 0 0 8 – 8   nm ), ▁or ▁how ▁fast ▁the ▁phot ons ▁are ▁detected ▁( count s ▁per ▁hour ), ▁to ▁tell ▁us ▁about ▁the ▁object ▁that ▁is ▁em itting ▁them . ▁ ▁Ast ro phys ical ▁sources ▁of ▁X - ray s ▁