Sannadkii 1611 kii, cirbixiyeenkii Jarmalka ahaa ee Kepler waxa uu qaatay laba xabbo oo lens lenticular ah ujeeddada iyo muraayadda indhaha, weynayntu si cad ayaa loo wanaajiyey, markii dambe dadku waxay u arkeen in nidaamkan indhaha uu yahay telescope Kepler.

Sannadkii 1757, Du Grand iyada oo loo marayo daraasadda dhalooyinka iyo dib-u-soo-celinta biyaha iyo kala-firdhinta, ayaa aasaasay aasaaska aragtida muraayadda achromatic, waxayna adeegsatay muraayadaha muraayadaha iyo muraayadaha muraayadaha muraayadaha achromatic.Wixii markaas ka dambeeyay, Telescope Refractor achromatic ayaa si buuxda u beddelay jidhkii muraayadda dheer ee muraayadda.

Dhammaadkii qarnigii sagaal iyo tobnaad, oo ay weheliso tignoolajiyada wax-soo-saarka ayaa la hagaajiyay, samaynta cabbirka weyn ee telescope-ka dib-u-celinta ayaa suurtagal ah, ka dibna waxaa jira soo saarista dhexroorka weyn ee Telescope climax.Mid ka mid ah kuwa ugu caansan ayaa ahaa Telescope Ekes oo ah dhexroor 102 cm 1897 iyo Rick telescope 91 cm dhexroor 1886.

Telescope-ka dib-u-celinta waxay leedahay faa'iidooyinka dhererka focal, miisaanka saxanka waa weyn yahay, leexinta tuubada waa mid aan dareen lahayn, oo ku habboon shaqada cabbirka astronomical.Laakiin had iyo jeer waxay leedahay midab haraaga ah, isla markaaba ultraviolet, nuugista shucaaca infrared waa mid aad u xoog badan.In kasta oo nidaamka shubitaanka muraayadda indhaha ee weyn uu adag yahay, telescope-ka Yerkes ee dib-u-celinta telescope-ka ee la dhisay 1897, horumarku wuxuu gaadhay heerkii ugu sarreeyay, tan iyo boqolkii sano ee la soo dhaafay ma muuqan telescope weyn.