Sannadkii 1611 kii, cirbixiyeenkii Jarmalka ahaa ee Kepler wuxuu qaatay laba xabbo oo lens lenticular ah ujeeddada iyo muraayadda indhaha, weynaynta si cad ayaa loo wanaajiyey, markii dambe dadku waxay u arkeen nidaamkan indhaha sida 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 taajka iyo muraayadaha dhagaxa ah ee soo saarista 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 caliber weyn ee telescope refracting ayaa suurtagal ah, ka dibna waxaa jira soo saarida dhexroor weyn oo ah Refractor 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 markaana ultraviolet, nuugista shucaaca infrared waa mid aad u xoog badan. In kasta oo nidaamka shubitaanka muraayadaha indhaha ee weyni uu adag yahay, telescope-ka Yerkes telescope-ka soo celinaya ee la dhisay 1897-kii, horumarku waa uu soo dhammaaday, tan iyo boqolkii sano ee la soo dhaafay ma muuqan telescope ka weyn.