itudes ▁can ▁also ▁be ▁calculated ▁for ▁objects ▁far ▁br ighter ▁than ▁stars ▁( such ▁as ▁the ▁Sun ▁and ▁Moon ), ▁and ▁for ▁objects ▁too ▁faint ▁for ▁the ▁human ▁eye ▁to ▁see ▁( such ▁as ▁Pl uto ). ▁ ▁Ab solute ▁magnitude ▁ ▁O ften , ▁only ▁apparent ▁magnitude ▁is ▁mentioned ▁since ▁it ▁can ▁be ▁measured ▁directly . ▁Ab solute ▁magnitude ▁can ▁be ▁calculated ▁from ▁apparent ▁magnitude ▁and ▁distance ▁from : ▁ ▁This ▁is ▁known ▁as ▁the ▁distance ▁mod ulus , ▁where ▁ ▁is ▁the ▁distance ▁to ▁the ▁star ▁measured ▁in ▁parse cs , ▁ ▁is ▁the ▁apparent ▁magnitude , ▁and ▁ ▁is ▁the ▁absolute ▁magnitude . ▁ ▁If ▁the ▁line ▁of ▁sight ▁between ▁the ▁object ▁and ▁observer ▁is ▁affected ▁by ▁ext inction ▁due ▁to ▁absor ption ▁of ▁light ▁by ▁inter stell ar ▁dust ▁particles , ▁then ▁the ▁object ' s ▁apparent ▁magnitude ▁will ▁be ▁corresponding ly ▁f ain ter . ▁For ▁ ▁magn itudes ▁of ▁ext inction , ▁the ▁relationship ▁between ▁apparent ▁and ▁absolute ▁magn itudes ▁becomes ▁ ▁St ell ar ▁absolute ▁magn itudes ▁are ▁usually ▁designated ▁with ▁a ▁capital ▁M ▁with ▁a ▁sub script ▁to ▁indicate ▁the ▁pass band . ▁ ▁For ▁example , ▁M V ▁is ▁the ▁magnitude ▁at ▁ 1 0 ▁parse cs ▁in ▁the ▁V ▁pass band . ▁ ▁A ▁bol ometric ▁magnitude ▁( M bol ) ▁is ▁an ▁absolute ▁magnitude ▁adjust ed ▁to ▁take ▁account ▁of ▁radiation ▁across ▁all ▁w avel ength s ; ▁it ▁is ▁typically ▁smaller ▁( i . e . ▁br ighter ) ▁than ▁an