▁bl uer ▁than ▁the ▁source ▁light : ▁ ▁where ▁ ▁is ▁the ▁em itted ▁w avel ength , ▁ ▁is ▁the ▁velocity ▁of ▁the ▁object , ▁and ▁ ▁is ▁the ▁observed ▁w avel ength . ▁Note ▁that ▁v < 0 ▁corresponds ▁to ▁ λ < λ 0 , ▁a ▁bl ues h ift ed ▁w avel ength . ▁A ▁red shift ed ▁absor ption ▁or ▁emission ▁line ▁will ▁appear ▁more ▁towards ▁the ▁red ▁end ▁of ▁the ▁spectrum ▁than ▁a ▁station ary ▁line . ▁In ▁ 1 9 1 3 ▁V esto ▁S li pher ▁determined ▁the ▁And rom eda ▁Gal axy ▁was ▁bl ues h ift ed , ▁meaning ▁it ▁was ▁moving ▁towards ▁the ▁Mil ky ▁Way . ▁ ▁He ▁recorded ▁the ▁spect ra ▁of ▁ 2 0 ▁other ▁galaxies ▁— ▁all ▁but ▁ 4 ▁of ▁which ▁were ▁red shift ed ▁— ▁and ▁was ▁able ▁to ▁calculate ▁their ▁veloc ities ▁relative ▁to ▁the ▁Earth . ▁Ed win ▁Hub ble ▁would ▁later ▁use ▁this ▁information , ▁as ▁well ▁as ▁his ▁own ▁observations , ▁to ▁define ▁Hub ble ' s ▁law : ▁The ▁further ▁a ▁galax y ▁is ▁from ▁the ▁Earth , ▁the ▁faster ▁it ▁is ▁moving ▁away ▁from ▁us . ▁Hub ble ' s ▁law ▁can ▁be ▁general ised ▁to ▁ ▁where ▁ ▁is ▁the ▁velocity ▁( or ▁Hub ble ▁Flow ), ▁ ▁is ▁the ▁Hub ble ▁Constant , ▁and ▁ ▁is ▁the ▁distance ▁from ▁Earth . ▁ ▁Red shift ▁( z ) ▁can ▁be ▁expressed ▁by ▁the ▁following ▁equations : ▁ ▁In ▁these