babs/yo_data_for_transcript_cleaned_inter · Datasets at Hugging Face

cleaned_text stringlengths 6 2.09k	source stringclasses 2 values	language stringclasses 1 value
Ohun na lo tun jẹ obinrin akọkọ to jẹ ojogbon ni Yunifasiti ilu Paris.Ìtọ́kasí awon Ọjọ́ìbí ni 1867awon ojoalaisi ni 1934awon elebun Nobel ninu Fisiksiàwọn ẹlẹ́bùn Nobel ninu Kemistri	wikipedia	yo
Telispupu Para Hubble tabi agbewóọ̀kan ofurufu Hubble (Hubble Space Telescope; Hst tàbí toh) jẹ́ Telispu òfúrufú kan tó jẹ́ gbígbé lọ sínú Ònààyípo pẹ̀lú oko àlọ́bo kan ní 1990, tó sì wà níbẹ̀ Látìgbà ná..	wikipedia	yo
Ó jẹ́ Telis tó ní ẹnu-ìwọlé-ìwọlé ìmọ́lẹ̀ , ó sì wà ní Òyípo ìsàlẹ̀ ayé, àwọn irinṣẹ́ mẹ́rẹ̀rin pàtàkì Hubble lè ṣàkíyèsí ní ìtànká etí inúàrò, Aláfojúrí, àti etí inúpupa..	wikipedia	yo
Telis na jẹ́ sí Siru fún Atoràwọ̀ Edwin Hubble.Ọ̀nà-àyípo Hubble tọ́ wa Níwájú ibi Ìdí Ojúàyíká ayé gbà láàyè láti ya àwọn àwòrán tó hàn kedere láì sí iná ẹ̀yìn..	wikipedia	yo
Àwòrán pápá ìkojú dé lé Hubble, fún apẹ̀rẹ̀ ló jẹ́ àwòrán àfojúrí iná tó kúnrẹ́rẹ́ jùlọ fún ohun tó jìnnà tó jẹ́ yíyà ní fọ́tò ní àgbàlá ayé..	wikipedia	yo
Ọ̀pọ̀ àwọn àkíyèsí Hubble ti fa ojutu Ìṣòro nínú sayensi Fisikilràwọ̀, bí ṣíṣe bí àgbàlá ayé ṣe únfẹ́ sí gégé.Bó tilẹ̀jè kí ṣe Telis òfúrufú àkọ́kọ́, Hubble jẹ́ ìkan nínú àwọn tó tóbijùlọ àti tó ṣe é múlò fún oríṣiríṣi iṣẹ́, àti ohun ìwádí tó ṣe pàtàkì àti ohun ìbáṣepọ̀ ìgboro fún itowó-korí..	wikipedia	yo
toh jẹ́ kíkọ́ Látọwọ́ Ilé-iṣẹ́ Ètò Òfurufú Amẹ́ríkà NASA, pẹ̀lú ìfikún látọ̀dọ̀ ilé-iṣẹ́ òfúrufú Europe, ó sì únjẹ mímúṣiṣẹ́ látọwọ́ Space Telescope Science Institute..	wikipedia	yo
teliskopu na jẹ́ ìkan nínu àwọn ibi ìsàkíyèsí gbangba ti NASA, lápapọ̀ mọ́ Compton gamma Ray Observatory, Chandra X-ray Observatory, àti Teliskopu Òfurufú Spigèrè.Àwọn Teliskopu òfurufú jẹ́ dídá lábà láti ọdún 1923..	wikipedia	yo
Owó fún Ikọ̀ Hubble bẹ̀rẹ̀ síní jẹ́ kíkójọ ní ẹ̀wádún 1970s, pẹ̀lú ìrètí pé yíò gbéra ní 1983, ṣùgbọ́n ó kú sẹ́yìn nítorí ìṣòro ìṣiṣẹ́, ìnáwó àti ìjàmbá Challenger..	wikipedia	yo
Nígbà tó ṣakoyin gbéra ní 1990, àwọn onímọ̀ tí ó rí ẹèè iwájú rẹ̀ kò dúró dáada, èyí fa kò mọ̀ ṣiṣẹ́ Bọ́sẹ̀ye..	wikipedia	yo
ÌranOniṣe ṣe àtúnṣe èyí ní 1993.Hubble ni Telispu kan ṣoṣo tó jẹ́ ṣíṣe láti ṣe àtúnṣe rẹ̀ nínú òfúrufú látọwọ́ àwọn arintahati..	wikipedia	yo
Lrin 1993 ati 2002, Iranse mẹrin ṣe àtúnse, isọdọtun ati wọn ṣe obirin awọn siste ninu Teliskopuko na; Iransẹ karun jẹ fífagilé fun abo leyin ijamba Columbia..	wikipedia	yo
Ṣùgbọ́n lẹ́yìn ìfọ̀rọ̀wérọ̀ ìgboro tó wáyé, olùdarí NASA Mike Griffin fàṣẹ sí ìránsẹ̀sẹ̀ àtúnṣe tó gbẹ̀yìn, èyí wáyé ni 2009..	wikipedia	yo
Ìrètí ni pe teliskopu na yio ṣiṣẹ́ titi di 2014 ó kéréjù..	wikipedia	yo
Èyí tí yíò rọ́pò rẹ̀ ni Teliskopù òfúrufú James Webb (jwst), èyí yíò gbéra ní 2018 tàbí lẹ́yìn ìgbà yí.Ìdárò, idà àti àwọn afọ́júsúni àti àwọn aṣíwájú ní 1923, Hermann Oberber — tó jẹ́ gbígbà bí bàbá iṣẹ́ ròkètí ayéòdeòní, lápapọ̀ mọ Robert H..	wikipedia	yo
Goddard àti Konstantin Sitolìpakúpa — Setewe ("ròkètí sínú òfúrufú plánẹ̀tì”; "The Rocket into Planetary Space"), tó fẹnu bá báwo ni Teliskopuko se le je mu Jidejulo sínú ona-Ayika Aye pelu ròkèti.Ìtàn Telispuko ofurufu Hubble se wa sẹ́yìn dé ọdún 1946, nígbàtí atoràwọ̀ Lyman Spidárúkọ kọ iwe-Àyọkà kan to únjẹ “Astronomical Advanls of an ExtraTerre Observatory" (Àwọn àǹfàní itoràwọ̀ Ibi-Isa See Kyun)..	wikipedia	yo
Nínú rẹ̀, ó jíròrò nípa àwọn ànfan pàtàkì méjì ti ibi-ìsàkíyèsí tó bùdó sí òfurufú ní lórí àwọn Teliskòpù tó bùdó sí orí ilẹ̀..	wikipedia	yo
Àkọ́kọ́, igbehan onígun (ẹkúnd kékeréjùlọ níbi tí àwọn ohunkan ṣe le e dámọ) yíò jẹ́ ṣíṣàòṣùpá lásán latọwọ Icasal, kàkà kó jẹ́ látọwọ́ ìjì ní ojú-àyíká, tó únjẹ kí àwọn ìràwọ̀ ó tàn yinrinyinrin, tó jẹ́ mímọ́ bí Ìwó látọwọ́ àwọn Atoràwọ̀..	wikipedia	yo
Lásìkò na àwọn Tẹlifípù ibùdó owó ilẹ̀ igbana ni ìgbéhàn tí kò dín jù 0.5.1.0 Arcscherer lo, tí a bá fìwé mọ́ ìgbé ìgbéhàn 0.05 Arc ti íOrílẹ̀wáyé Saró yíò ní fún Teliskopuko pèlú jígí tí ìdákọjá rẹ̀ jẹ́ 2.5 m..	wikipedia	yo
Èkejì, Telis-kọ́ ibùdó òfúrufú lè ṣàkíyèsí ìmọ́lẹ̀ onínúpupa àti onínúaró, tí wọ́n lé sọnù sójú-àyíká fún Telispupù ibùdó orí ilẹ̀.Spipẹ̀gàn lọ gbogbo àsìkò iṣẹ́ rẹ̀ sí pípẹ́ fún ìgbédìde Telispupù òfúrufú..	wikipedia	yo
Ní 1962, ìjábọ̀ ìwádí ADemi Àwọn sáyẹ́nsì Orílẹ̀-èdè Amẹ́ríkà dá àbá ìgbédìde Teliskopu Òfurufú gẹ́gẹ́ bí apá ètò òfúrufú, àti ní 1965 Spidárúkọ jẹ́ yíyansípò bí olórí Ìgbìmọ̀ tí iṣẹ́ rẹ̀ jẹ́ láti ṣètòka ọ̀nà sáyẹ́nsí fún Telispù Òfurufú níńlá.Ito-Ito ibùdó Òfurufú ti bẹ̀rẹ̀ díẹ̀díẹ̀ lẹ́yìn Ogun Àgbáyé (K, bí àwọn onímọ̀ sáyẹ́nsí lọ ní àwọn ìgbédìde tó ti wáyé nínú ọ̀rọ̀ìṣeọ̀nà ròkè..	wikipedia	yo
ìgbàjà-awo onínúaró àkọ́kọ́ ti ọ̀run jẹ́ rírì ní 1946, NASA sì Sabe orbiting Solar Observatory (ọ̀ṣọ́) láti gba àwọn ìgbájá Uv, ìtànká-X (X-ray), àti ìtànká gamma ní 1962..	wikipedia	yo
Teliskopu Ọ̀nà-àyípo Ọ̀run kan jẹ́ gbígbéra ní 1962 látọwọ́ Ilẹ̀ọba Aṣọ̀kan bíi apá ètò òfúrufú Ariel, bẹ́ẹ̀sìni ní 1966 NASA Sabera ìránsẹ̀ orbiting Astronomical Observatory (OIS) Àkókò..	wikipedia	yo
bátìrì oaọ́-1 kùnà lẹ́yìn ọjọ́ mẹ́ta, èyí fi òpin sí ìranlọ́sẹ̀ náà..	wikipedia	yo
Oineo-2 to rọpo rẹ ṣe akiyesi onínúàro àwọn irawọ ati Galaksì lati igba ìgbéra re ni 1968 titi di 1972, eyi pẹ ju ọdun kan ti wọn gbero fun lọ.Awon iranlose oso ati Obaa fihan bi awon akiyesi ibudo ofurufu se se pataki si ninu itoràwọ̀, bo si se di 1968, NASA ṣàgbẹ̀dìde awon eto gidi fun telispuko Alatanpadà pelu jígí ti idakọja rẹ jẹ 3 M, to je mimo nigba naa bii large orbiting Telescope tabi large space Telescope (L), ti yio gbéra ni 1979..	wikipedia	yo
Àwọn ètò yí tẹnumọ́ bí ó ṣe ṣe pàtàkì fún àwọn ìranlọ́sẹ̀ ìtọ́jú pẹ̀lú àwọn ènìyàn lọ sí Teliskopù nã láti ri pé irú ètò alẹ́wò nã ní ẹ̀mí ọjọ́ pípẹ́, besíni ìgbédìde lásìkò kannã ètò fún and the Conrent Development of plans for the Reuflows oko alobo alátùnmúlò fihàn pé ọ̀rọ̀ìṣeọ̀nà tí yíò gba èyí láyè kò ní pẹ́ wáyé.Ìpèsè owó fún kíkó rẹ̀ ní 1974, Kongṣi jáwọ́ ìnáwó fún ètò Teliskòpù ná..	wikipedia	yo
Nitoriẹ ọpọ awọn Atoràwọ̀ bẹrẹ ipade pẹlu awọn aṣoju ati alàgbà aṣofin lati ri pe owo ko ja lori igbeDídìde rẹ..	wikipedia	yo
Nígbẹ̀yìn Kongrésì pinu láti dá ìnáwó rẹ̀ sí àbọ̀.Nitori aito owó ló fa ti European Space Agency ṣe pinu láti pèsè owó àti irinṣẹ́ fún Telispù nã, àti bátìrì Ọlọ́run tí yíò fún ní agbára, àti àwọn òṣìṣẹ́ láti ṣiṣẹ́ lórí Telis ná ní Amẹ́ríkà, fún èyí wọn yíò fún àwọn àràwọ̀ ará Europe ní 15% àsìkò isà ìsàkíyèsí lórí Telis nã..	wikipedia	yo
Nígbẹ̀yìn Kongrésì fi àṣẹ sí ìpèsè owó tó tó us$36,000,000 fún 1978, bẹ́ síni ìyàẹ̀tọ́ lst bẹ̀rẹ̀, pẹ̀lú èrò láti gbéra ní 1983..	wikipedia	yo
Ní 1983 Teliskopu na jẹ́ Sisoloru fún Edwin Hubble, ẹni tó ṣẹ̀wà ikan nínú àwọn àwárí sáyẹ́ńsì ọ̀rúndún 20k nígbàtó ṣàwárí pé àgbàlá ayé unfesi.Ikọ̀ àti iṣẹ́ẹ̀rọ lẹ́yìn tí iṣẹ́ọwọ́ Telispù òfúrufú nã ti gba àṣẹ, iṣẹ́ bẹ̀rẹ̀ kíákíá lórí rẹ̀, ó sì jẹ́ pínpín lãrín ọ̀pọ̀ àwọn ilé-iṣẹ́..	wikipedia	yo
Marshall Space Flight Center (SHFC) ló gba àṣẹ láti dáetotọ́, ṣàgbẹ̀di àti kọ telispu ná, nígbàtí Goddard Space Flight Center gba àṣẹ iṣẹ́ ìṣèlọ́ Àpapọ̀ àwọn irinṣẹ́ sáyẹ́nsi àti Gbọ̀ngàn Ibi Ìkó orí ilẹ̀ fún Iransẹ nã..	wikipedia	yo
MaFC gbe iṣe fun ile-iṣẹ imọìríran perkin-elmer lati daeto ati ko Optical Telescope Assembly (Ota) ati Fine Guidance Sensors fun telispuko na..	wikipedia	yo
Logheed gba ise lati ko ati searomọ oko-ofurufu ti telispú na yio duro si.2 Telescope Assembly (Ota) fún Ìwòran, toh Unlo Casgrain Reflector ti afowo Ritchey-chrétienne-irúfẹ́, Bó ṣe jẹ́ fún ọ̀pọ̀ àwọn Telispuko ìrun òyáàet..	wikipedia	yo
àfọwọ́dà yí, pẹ̀lú jìgì átẹ́nì méjì (Hyperlic Mirrors), gbajúmọ̀ fún iṣẹ́àwòrán tòdára lórí ibi ìríran tó fẹ́ gidi, pẹ̀lú àìníanfani pé àwọn bi àwọn jìgì nã ṣe rí ṣòro láti dá àti dánwò..	wikipedia	yo
Ed àti Siste onítiwòrán tí Teliskopuko na ní ní wọ́n unṣọ́ bí yíò ṣe ṣiṣẹ́ daradara sí, bẹ́ sí wọ́n jẹ́ tídá ní iye ìkàn.. pàtó	wikipedia	yo
Awon teliskopuko oniwòrán saba ni jìgì to ti je didan to ni isegee bi ti idamẹwa ibuiru ìtànmọ́lẹ̀ afoju afoju, sugbon Telis ofurufu yi on lilo fun isakíyèsí lati ìtànmọ́lẹ̀ afoju de onínúawo (ibu-irin (ibú kere) bẹ síni o gbodo ni deporaction limited pato lati le lo gbogbo anfani ti Aroko ofurufu pese pese..	wikipedia	yo
Nitori eyi, jígí rẹ̀ gbọ́dọ̀ jẹ́ dídán dé ìsegeere 10 Rometers, bí tàbí 1/65 ibú-irú ìtànmọ́lẹ̀ àwọpupa..	wikipedia	yo
Ni apa ibú-iru-ila tógun, Ota na fì fífọwọ́da pẹ̀lú pé Ir rẹ̀ yio ṣiṣẹ́ Bọ́sẹ̀ye dáada — Fún àpẹ, àwọn jìgì ní IgboNásì Toduro laimi (won si loworọ, bi 15 °C)..	wikipedia	yo
Èyí fa àlà sí ise Hubble bi teliskopu onínúawopupa.per-el-me intended to use custom-built and extremely Sophisticated computer-controlled Polanski MacHines to Grind the Mirror to the required shape..	wikipedia	yo
However, in case their cutting-Edge Technology ran into difficulties, NASA demanded that pe sub-contract to kòdàk to construct a back-up Mirror using traditional Mirror-po-ọpọlọ Techniques..	wikipedia	yo
(The team of kódàk and itek also Pired on the original Mirror Polanski Work..	wikipedia	yo
Their Dori called for the two companies to double-Check each other's work, which would have almost certainly caught the poÌyàn Error that later caused such problems.) The kódàk Mirror is now on permanent display at the Smithsonian Institution..	wikipedia	yo
An ìtẹ́k Mirror built as part of the effort is now used in the 2.4 M sínúscope at the Magdalena Ridge Observatory.construction of the perkìn-el Mirror began in 1979, starting with a Blank manufacìbánigbófò by Corning from their Ultra-low expansion Glass..	wikipedia	yo
To keep the Mirror's weight to a minimum it gègéted of inch-Háráck Top and bottom Plates Swihing a Honeyd láttice	wikipedia	yo
perkin-elmer Ṣímùogún Microgravity by Supporting the Mirror on both sides with 138 Rods that Exerted Varying amounts of force..	wikipedia	yo
This ensured that the Mirror's final shape would be correct and to unNígbàọdún When finally Degfàní..	wikipedia	yo
NASA Reports at the time questioned perkìn-elmer's mana'l Structure, and the Polanski began to slip behind schedule and over Budget..	wikipedia	yo
To Save money, NASA Halted work on the back-up Mirror and put the Launch date of the Telescope back to October 1984..	wikipedia	yo
The Mirror was completed by the end of 1981; it was washed using 2,400 gallons (9,100 l) of hot, deionized water and then received a Reflective coating of aluminum 65 Nn-Carter and a say coating of magnesium fluoride 25 N-Doudoubdouts continued to be expressed about perkìn-el's korunance on a project of this importance, as their budget and timescale for producing the rest of the Ota continued to inflate..	wikipedia	yo
In response to a schedule described as "únṣettled and Changing daily", NASA postponed the Launch date of the telescope until April 1985..	wikipedia	yo
perkìn-elmer's schedules continued to slip at a rate of about one month per quarter, and at times Delays reached one day for each day of work..	wikipedia	yo
NASA was forced to postpone the Launch date until March and then September 1986..	wikipedia	yo
By this time, the total project budget had risen to us$1.175 billion.spacecraft systems the spacecraft in which the telescope and instruments were to be housed was another major Engineering challenge..	wikipedia	yo
It would have to withstand frequent passages from Direct sunlight into the darkness of earth's shadow, which would cause major changes in temperature, while being kẹ́tẹ́kẹ́tẹ́ enough to allow extremely accurate pointing of the sínúscope..	wikipedia	yo
A shroud of multi-Atdáyà insulation keeps the temperature within the sínú kẹ́tẹ́kẹ́tẹ́, and surroAmerican a light aluminum shell in which the ráscope and instruments sit..	wikipedia	yo
Within the shell, a Grate-epoxy Frame keeps the working parts of the Telescope firmly Aligned..	wikipedia	yo
Because Grate composites are hygroclusi, there was a risk that water vapor absor by the Truss while in lockheed's clean room would later be expressed in the vacuum of space; the Abẹscope's instruments would be covered in ice..	wikipedia	yo
To Dutace that risk, a nitrogen gas purgé was performed before launhing the òdòdó into space.While construction of the spacecraft in which the telescope and instruments would be housed proorísuneeded somewhat more smoothly than the construction of the ọ̀tá, lock still experienced some budget and schedule slippage, and by the summer of 1985, construction of the spacecraft was 30% over budget and three months behind schedule..	wikipedia	yo
Wf/CDP was a high-solution imaging deVice ] intended for Optical Observations..	wikipedia	yo
It was built by NASA's dispute propulsion Laboratory, and Incorporated a set of 48 filters IBetiBeti gbẹ́kẹ̀leral Lines of Natanias domiphysical interest..	wikipedia	yo
The Inment contained eight charge-coupled deVice (cCD) chips Divided between two Cameras, each using four CCds..	wikipedia	yo
The “Wide field Camera” (WFC) covered a large Angular field at the expense of Resolution, while the "Planetary Camera” (PC) took images at a longer Effect focal length than the w chips, giving it a greater Magàdánwòcation.The GHrs was a yíyàro designed to operate in the ultraviolet..	wikipedia	yo
It was built by the Goddard Space Flight center and could achieve a yíyàral resolution of 90,000..	wikipedia	yo
also Optiẹṣin for nira Observations were the foc and fós, which were capable of the highest spatial resolution of any instruments on Hubble..	wikipedia	yo
Rather than CCds these three instruments used Photon-counting dígícons as their dẹ́tẹ̀ctors..	wikipedia	yo
The fọ́c was constructed by Esa, while the University of California, San Diego and the Martin Mari50 Corporation built the fós.The final instrument was the Hsp, designed and built at the university of Wisconsin-Madison..	wikipedia	yo
It was Optiẹrúsìn for Visible and ultraviolet light Observations of variable stars and other Astronomical objects varying in brightness..	wikipedia	yo
It could take up to 100,000 measurements per second with a photoṢàánú Accuracy of about 2% or better.Hst's guidance system can also be used as a Scientific instrument..	wikipedia	yo
Its three fine guidánce sensors (fgs) are primarily used to keep the Abẹscope accurately pointed during an Observation, but can also be used to carry out extremely raterate lóríRometry; measurements accurate to within 0.2 Arcohùnds have been achieved.Ground support the space telescope science Institute (STScI) is responsible for the Scientific operation of the Abẹscope and delivery of ọwọ́ products to Astronomers..	wikipedia	yo
STScI Is operated by the Association of Universities for research in Astronomy (AURA) and is physically located in Baltimore, Maryland on the homewood Campus of Johns Hopkins University, one of the 33 us Universities and seven international Affiliates that make up the AURA conSoṣíọ́lọ́jì..	wikipedia	yo
STScI was established in 1981 After something of a power struggle between NASA and the Scientific community at large..	wikipedia	yo
NASA had wanted to keep this function “in-house”, but Scientists wanted it to be based in an academic establishment..	wikipedia	yo
The space telescope European Coordinating fatragic (St-ECf), established at Garching èkínní München near Munich in 1984, provides similar support for European Astronomers.One rather Complex task that falls to STScI is scheduling observations for the Telescope..	wikipedia	yo
Hubble is in a low-earth orbit so that it can be reached by the space shuttle for Servicing missions, but this means that most astronomical targets are Occulted by the earth for slightly less than half of each orbit..	wikipedia	yo
Observations cannot take place when the telescope passes through the south Atlantic anotacles due to Jeremaya radiation àfonífojì, and there are also Sicasal exClusion Zones around the sun (preCluding observations of Mercury), moon and earth..	wikipedia	yo
The Solar gugucece ANG is about 50°, which is únfied to keep sunlight from olùgbàgbọminating any part of the ọ̀tá..	wikipedia	yo
Earth and moon gugucece is to keep Bright light out of the FGss and to keep scattered light from entering the instruments..	wikipedia	yo
If the FGss are turned off, however, the moon and earth can be observed..	wikipedia	yo
Earth Observations were used very early in the program to generate Flat-Fields for the WFPc1 Inedment..	wikipedia	yo
There is a so-called continuous viewing Zone (SEcz), at ughly 90 degrees to the plane of Hubble's orbit, in which targets are not culculted for long Periods..	wikipedia	yo
due to the pregbígbà of the orbit, the Location of the Veboz moves slowly over a period of eight weeks..	wikipedia	yo
Because the Lẹ̀hìn of the earth is always within about 30° of rẹ́gíons within the tẹnumọ́z, the brightness of scattered earthshine may be alòdìsí for long Periods during Veboz observations.Because Hubble orts in the upper ."*, its orbit changes over time in a way that is not accurately thereaftertable..	wikipedia	yo
The denọ̀kọ̀ọ̀kan of the upper okoomi vari according to many factors, and this means that Hubble's predicted position for six weeks' time could be in Error by up to 4,000 km..	wikipedia	yo
Observation schedules are typícally finalized only a few days in advance, as a longer lead time would mean there was a Chance that the get would be unobjìyàable by the time it was due to be observed.Engineering support for Hst is provided by NASA and inhabictor perSosórí at the Goddard Space Flight center in greenbelt, Maryland, 48km South South of the STScI..	wikipedia	yo
Hubble's operation is monitored 24 hours per day by four Teams of flight controllers who make up Hubble's flight operations team.Challenger disaster, Delays, and eventistic Launch by early 1986, the lẹ́wà Launch date of October that year sedate feásìble, but the Challenger accident brought the u.S..	wikipedia	yo
Space program to a halt, grounding the space shuttle Fleet and forcing the Launch of Hubble to be postponed for several years..	wikipedia	yo
The Telescope had to be kept in a clean room, lérí up and purged with nitrogen, until a Launch could be reschedu!	wikipedia	yo
This costly situation (about $6 million per month) pushed the rii costs of the project even higher..	wikipedia	yo
This delay did allow time for survi537 to perform extensive tests, Swap out a possibly failure-prone would, and make other improvements..	wikipedia	yo
furthermore, the ground software needed to control Hubble was not ready in 1986, and in fact was barely ready by the 1990 Launch.eventually, following the re.)” of shuttle flights in 1988, the Launch of the òdòdó was scheduled for 1990..	wikipedia	yo
On April 24, 1990, shuttle mission sts-31 saw Discovery Launch the Telescope successfully into its lẹ́wà orbit.From its original total cost estimate of about us$400 million, the sínúscope had by now cost over $2.5billion to construct ..	wikipedia	yo
Hubble'S Cumúlátive costs up to this day are estimated to be several times higher still, with us corpsediture estimated at between $4.5 and $6 billion, and Europe's financial contribution at €593 million (1999 estimate).flawed Mirror within weeks of the Launch of the òdòdó, the returned images indicated a serious problem with the seasoned system..	wikipedia	yo
Although the first images appeared to be Sharper than those of ground-based Telescope, Hubble treaty to achieve a final sharp Focus and the best image quality obtained was drastically lower than expected..	wikipedia	yo
Images of point Sources Spread out over a rakéde of more than one Arcsecond, instead of having a point JJad function (psf) concentrated within a circle 0.1 Arctistic in diameter as had been unùnfied in the design pọ̀.Analysis of the flawed images showed that the cause of the problem was that the Primary Mirror had been ground to the wrong shape..	wikipedia	yo
Although it was probably the most preGígùnly Wàyíred Mirror ever made, with variations from the prescribed curve of only 10 Rìnters, at the perimeter it was too Flat by about 2,200 fagbáraters (2.2 Micrometres)..	wikipedia	yo
This difference was catastrophic, Influcing severe spherical aberration, a lárugẹ in which light artistscting off the Edge of a Mirror focuses on a different point from the light artistscting off its center.The effect of the Mirror ògo on Scientific observations Oníbọnded on the ), Observation—the Core of the aberrated psf was sharp enough to permit high-re alàgbà observations of Bright, and loavesro] was largely unly un..	wikipedia	yo
However, the loss of light to the large, out of Focus Halo severely reduced the usefulness of the telescope for faint objects or high-pinpin imaging..	wikipedia	yo
This meant that nearly all of the coswẹ̀ programs were essẹntially impossible, since they required Observation of exceptiapànìyàn faint objects..	wikipedia	yo
NASA and the Telescope became the butt of many jokes, and the project was popularly regarded as a white elephant..	wikipedia	yo
Nonetheless, during the first three years of the Hubble mission, before the seasoned olókoctions, the òdòdó still carried out a large number of inhabitctive Observations..	wikipedia	yo

Ohun na lo tun jẹ obinrin akọkọ to jẹ ojogbon ni Yunifasiti ilu Paris.Ìtọ́kasí awon Ọjọ́ìbí ni 1867awon ojoalaisi ni 1934awon elebun Nobel ninu Fisiksiàwọn ẹlẹ́bùn Nobel ninu Kemistri

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Telispupu Para Hubble tabi agbewóọ̀kan ofurufu Hubble (Hubble Space Telescope; Hst tàbí toh) jẹ́ Telispu òfúrufú kan tó jẹ́ gbígbé lọ sínú Ònààyípo pẹ̀lú oko àlọ́bo kan ní 1990, tó sì wà níbẹ̀ Látìgbà ná..

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Ó jẹ́ Telis tó ní ẹnu-ìwọlé-ìwọlé ìmọ́lẹ̀ , ó sì wà ní Òyípo ìsàlẹ̀ ayé, àwọn irinṣẹ́ mẹ́rẹ̀rin pàtàkì Hubble lè ṣàkíyèsí ní ìtànká etí inúàrò, Aláfojúrí, àti etí inúpupa..

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Telis na jẹ́ sí Siru fún Atoràwọ̀ Edwin Hubble.Ọ̀nà-àyípo Hubble tọ́ wa Níwájú ibi Ìdí Ojúàyíká ayé gbà láàyè láti ya àwọn àwòrán tó hàn kedere láì sí iná ẹ̀yìn..

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Àwòrán pápá ìkojú dé lé Hubble, fún apẹ̀rẹ̀ ló jẹ́ àwòrán àfojúrí iná tó kúnrẹ́rẹ́ jùlọ fún ohun tó jìnnà tó jẹ́ yíyà ní fọ́tò ní àgbàlá ayé..

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Ọ̀pọ̀ àwọn àkíyèsí Hubble ti fa ojutu Ìṣòro nínú sayensi Fisikilràwọ̀, bí ṣíṣe bí àgbàlá ayé ṣe únfẹ́ sí gégé.Bó tilẹ̀jè kí ṣe Telis òfúrufú àkọ́kọ́, Hubble jẹ́ ìkan nínú àwọn tó tóbijùlọ àti tó ṣe é múlò fún oríṣiríṣi iṣẹ́, àti ohun ìwádí tó ṣe pàtàkì àti ohun ìbáṣepọ̀ ìgboro fún itowó-korí..

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toh jẹ́ kíkọ́ Látọwọ́ Ilé-iṣẹ́ Ètò Òfurufú Amẹ́ríkà NASA, pẹ̀lú ìfikún látọ̀dọ̀ ilé-iṣẹ́ òfúrufú Europe, ó sì únjẹ mímúṣiṣẹ́ látọwọ́ Space Telescope Science Institute..

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teliskopu na jẹ́ ìkan nínu àwọn ibi ìsàkíyèsí gbangba ti NASA, lápapọ̀ mọ́ Compton gamma Ray Observatory, Chandra X-ray Observatory, àti Teliskopu Òfurufú Spigèrè.Àwọn Teliskopu òfurufú jẹ́ dídá lábà láti ọdún 1923..

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Owó fún Ikọ̀ Hubble bẹ̀rẹ̀ síní jẹ́ kíkójọ ní ẹ̀wádún 1970s, pẹ̀lú ìrètí pé yíò gbéra ní 1983, ṣùgbọ́n ó kú sẹ́yìn nítorí ìṣòro ìṣiṣẹ́, ìnáwó àti ìjàmbá Challenger..

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Nígbà tó ṣakoyin gbéra ní 1990, àwọn onímọ̀ tí ó rí ẹèè iwájú rẹ̀ kò dúró dáada, èyí fa kò mọ̀ ṣiṣẹ́ Bọ́sẹ̀ye..

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ÌranOniṣe ṣe àtúnṣe èyí ní 1993.Hubble ni Telispu kan ṣoṣo tó jẹ́ ṣíṣe láti ṣe àtúnṣe rẹ̀ nínú òfúrufú látọwọ́ àwọn arintahati..

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Lrin 1993 ati 2002, Iranse mẹrin ṣe àtúnse, isọdọtun ati wọn ṣe obirin awọn siste ninu Teliskopuko na; Iransẹ karun jẹ fífagilé fun abo leyin ijamba Columbia..

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Ṣùgbọ́n lẹ́yìn ìfọ̀rọ̀wérọ̀ ìgboro tó wáyé, olùdarí NASA Mike Griffin fàṣẹ sí ìránsẹ̀sẹ̀ àtúnṣe tó gbẹ̀yìn, èyí wáyé ni 2009..

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Ìrètí ni pe teliskopu na yio ṣiṣẹ́ titi di 2014 ó kéréjù..

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Èyí tí yíò rọ́pò rẹ̀ ni Teliskopù òfúrufú James Webb (jwst), èyí yíò gbéra ní 2018 tàbí lẹ́yìn ìgbà yí.Ìdárò, idà àti àwọn afọ́júsúni àti àwọn aṣíwájú ní 1923, Hermann Oberber — tó jẹ́ gbígbà bí bàbá iṣẹ́ ròkètí ayéòdeòní, lápapọ̀ mọ Robert H..

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Goddard àti Konstantin Sitolìpakúpa — Setewe ("ròkètí sínú òfúrufú plánẹ̀tì”; "The Rocket into Planetary Space"), tó fẹnu bá báwo ni Teliskopuko se le je mu Jidejulo sínú ona-Ayika Aye pelu ròkèti.Ìtàn Telispuko ofurufu Hubble se wa sẹ́yìn dé ọdún 1946, nígbàtí atoràwọ̀ Lyman Spidárúkọ kọ iwe-Àyọkà kan to únjẹ “Astronomical Advanls of an ExtraTerre Observatory" (Àwọn àǹfàní itoràwọ̀ Ibi-Isa See Kyun)..

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Nínú rẹ̀, ó jíròrò nípa àwọn ànfan pàtàkì méjì ti ibi-ìsàkíyèsí tó bùdó sí òfurufú ní lórí àwọn Teliskòpù tó bùdó sí orí ilẹ̀..

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Àkọ́kọ́, igbehan onígun (ẹkúnd kékeréjùlọ níbi tí àwọn ohunkan ṣe le e dámọ) yíò jẹ́ ṣíṣàòṣùpá lásán latọwọ Icasal, kàkà kó jẹ́ látọwọ́ ìjì ní ojú-àyíká, tó únjẹ kí àwọn ìràwọ̀ ó tàn yinrinyinrin, tó jẹ́ mímọ́ bí Ìwó látọwọ́ àwọn Atoràwọ̀..

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Lásìkò na àwọn Tẹlifípù ibùdó owó ilẹ̀ igbana ni ìgbéhàn tí kò dín jù 0.5.1.0 Arcscherer lo, tí a bá fìwé mọ́ ìgbé ìgbéhàn 0.05 Arc ti íOrílẹ̀wáyé Saró yíò ní fún Teliskopuko pèlú jígí tí ìdákọjá rẹ̀ jẹ́ 2.5 m..

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Èkejì, Telis-kọ́ ibùdó òfúrufú lè ṣàkíyèsí ìmọ́lẹ̀ onínúpupa àti onínúaró, tí wọ́n lé sọnù sójú-àyíká fún Telispupù ibùdó orí ilẹ̀.Spipẹ̀gàn lọ gbogbo àsìkò iṣẹ́ rẹ̀ sí pípẹ́ fún ìgbédìde Telispupù òfúrufú..

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Ní 1962, ìjábọ̀ ìwádí ADemi Àwọn sáyẹ́nsì Orílẹ̀-èdè Amẹ́ríkà dá àbá ìgbédìde Teliskopu Òfurufú gẹ́gẹ́ bí apá ètò òfúrufú, àti ní 1965 Spidárúkọ jẹ́ yíyansípò bí olórí Ìgbìmọ̀ tí iṣẹ́ rẹ̀ jẹ́ láti ṣètòka ọ̀nà sáyẹ́nsí fún Telispù Òfurufú níńlá.Ito-Ito ibùdó Òfurufú ti bẹ̀rẹ̀ díẹ̀díẹ̀ lẹ́yìn Ogun Àgbáyé (K, bí àwọn onímọ̀ sáyẹ́nsí lọ ní àwọn ìgbédìde tó ti wáyé nínú ọ̀rọ̀ìṣeọ̀nà ròkè..

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ìgbàjà-awo onínúaró àkọ́kọ́ ti ọ̀run jẹ́ rírì ní 1946, NASA sì Sabe orbiting Solar Observatory (ọ̀ṣọ́) láti gba àwọn ìgbájá Uv, ìtànká-X (X-ray), àti ìtànká gamma ní 1962..

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Teliskopu Ọ̀nà-àyípo Ọ̀run kan jẹ́ gbígbéra ní 1962 látọwọ́ Ilẹ̀ọba Aṣọ̀kan bíi apá ètò òfúrufú Ariel, bẹ́ẹ̀sìni ní 1966 NASA Sabera ìránsẹ̀ orbiting Astronomical Observatory (OIS) Àkókò..

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bátìrì oaọ́-1 kùnà lẹ́yìn ọjọ́ mẹ́ta, èyí fi òpin sí ìranlọ́sẹ̀ náà..

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Oineo-2 to rọpo rẹ ṣe akiyesi onínúàro àwọn irawọ ati Galaksì lati igba ìgbéra re ni 1968 titi di 1972, eyi pẹ ju ọdun kan ti wọn gbero fun lọ.Awon iranlose oso ati Obaa fihan bi awon akiyesi ibudo ofurufu se se pataki si ninu itoràwọ̀, bo si se di 1968, NASA ṣàgbẹ̀dìde awon eto gidi fun telispuko Alatanpadà pelu jígí ti idakọja rẹ jẹ 3 M, to je mimo nigba naa bii large orbiting Telescope tabi large space Telescope (L), ti yio gbéra ni 1979..

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Àwọn ètò yí tẹnumọ́ bí ó ṣe ṣe pàtàkì fún àwọn ìranlọ́sẹ̀ ìtọ́jú pẹ̀lú àwọn ènìyàn lọ sí Teliskopù nã láti ri pé irú ètò alẹ́wò nã ní ẹ̀mí ọjọ́ pípẹ́, besíni ìgbédìde lásìkò kannã ètò fún and the Conrent Development of plans for the Reuflows oko alobo alátùnmúlò fihàn pé ọ̀rọ̀ìṣeọ̀nà tí yíò gba èyí láyè kò ní pẹ́ wáyé.Ìpèsè owó fún kíkó rẹ̀ ní 1974, Kongṣi jáwọ́ ìnáwó fún ètò Teliskòpù ná..

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Nitoriẹ ọpọ awọn Atoràwọ̀ bẹrẹ ipade pẹlu awọn aṣoju ati alàgbà aṣofin lati ri pe owo ko ja lori igbeDídìde rẹ..

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Nígbẹ̀yìn Kongrésì pinu láti dá ìnáwó rẹ̀ sí àbọ̀.Nitori aito owó ló fa ti European Space Agency ṣe pinu láti pèsè owó àti irinṣẹ́ fún Telispù nã, àti bátìrì Ọlọ́run tí yíò fún ní agbára, àti àwọn òṣìṣẹ́ láti ṣiṣẹ́ lórí Telis ná ní Amẹ́ríkà, fún èyí wọn yíò fún àwọn àràwọ̀ ará Europe ní 15% àsìkò isà ìsàkíyèsí lórí Telis nã..

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Nígbẹ̀yìn Kongrésì fi àṣẹ sí ìpèsè owó tó tó us$36,000,000 fún 1978, bẹ́ síni ìyàẹ̀tọ́ lst bẹ̀rẹ̀, pẹ̀lú èrò láti gbéra ní 1983..

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Ní 1983 Teliskopu na jẹ́ Sisoloru fún Edwin Hubble, ẹni tó ṣẹ̀wà ikan nínú àwọn àwárí sáyẹ́ńsì ọ̀rúndún 20k nígbàtó ṣàwárí pé àgbàlá ayé unfesi.Ikọ̀ àti iṣẹ́ẹ̀rọ lẹ́yìn tí iṣẹ́ọwọ́ Telispù òfúrufú nã ti gba àṣẹ, iṣẹ́ bẹ̀rẹ̀ kíákíá lórí rẹ̀, ó sì jẹ́ pínpín lãrín ọ̀pọ̀ àwọn ilé-iṣẹ́..

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Marshall Space Flight Center (SHFC) ló gba àṣẹ láti dáetotọ́, ṣàgbẹ̀di àti kọ telispu ná, nígbàtí Goddard Space Flight Center gba àṣẹ iṣẹ́ ìṣèlọ́ Àpapọ̀ àwọn irinṣẹ́ sáyẹ́nsi àti Gbọ̀ngàn Ibi Ìkó orí ilẹ̀ fún Iransẹ nã..

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MaFC gbe iṣe fun ile-iṣẹ imọìríran perkin-elmer lati daeto ati ko Optical Telescope Assembly (Ota) ati Fine Guidance Sensors fun telispuko na..

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Logheed gba ise lati ko ati searomọ oko-ofurufu ti telispú na yio duro si.2 Telescope Assembly (Ota) fún Ìwòran, toh Unlo Casgrain Reflector ti afowo Ritchey-chrétienne-irúfẹ́, Bó ṣe jẹ́ fún ọ̀pọ̀ àwọn Telispuko ìrun òyáàet..

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àfọwọ́dà yí, pẹ̀lú jìgì átẹ́nì méjì (Hyperlic Mirrors), gbajúmọ̀ fún iṣẹ́àwòrán tòdára lórí ibi ìríran tó fẹ́ gidi, pẹ̀lú àìníanfani pé àwọn bi àwọn jìgì nã ṣe rí ṣòro láti dá àti dánwò..

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Ed àti Siste onítiwòrán tí Teliskopuko na ní ní wọ́n unṣọ́ bí yíò ṣe ṣiṣẹ́ daradara sí, bẹ́ sí wọ́n jẹ́ tídá ní iye ìkàn.. pàtó

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Awon teliskopuko oniwòrán saba ni jìgì to ti je didan to ni isegee bi ti idamẹwa ibuiru ìtànmọ́lẹ̀ afoju afoju, sugbon Telis ofurufu yi on lilo fun isakíyèsí lati ìtànmọ́lẹ̀ afoju de onínúawo (ibu-irin (ibú kere) bẹ síni o gbodo ni deporaction limited pato lati le lo gbogbo anfani ti Aroko ofurufu pese pese..

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Nitori eyi, jígí rẹ̀ gbọ́dọ̀ jẹ́ dídán dé ìsegeere 10 Rometers, bí tàbí 1/65 ibú-irú ìtànmọ́lẹ̀ àwọpupa..

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Ni apa ibú-iru-ila tógun, Ota na fì fífọwọ́da pẹ̀lú pé Ir rẹ̀ yio ṣiṣẹ́ Bọ́sẹ̀ye dáada — Fún àpẹ, àwọn jìgì ní IgboNásì Toduro laimi (won si loworọ, bi 15 °C)..

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Èyí fa àlà sí ise Hubble bi teliskopu onínúawopupa.per-el-me intended to use custom-built and extremely Sophisticated computer-controlled Polanski MacHines to Grind the Mirror to the required shape..

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However, in case their cutting-Edge Technology ran into difficulties, NASA demanded that pe sub-contract to kòdàk to construct a back-up Mirror using traditional Mirror-po-ọpọlọ Techniques..

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(The team of kódàk and itek also Pired on the original Mirror Polanski Work..

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Their Dori called for the two companies to double-Check each other's work, which would have almost certainly caught the poÌyàn Error that later caused such problems.) The kódàk Mirror is now on permanent display at the Smithsonian Institution..

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An ìtẹ́k Mirror built as part of the effort is now used in the 2.4 M sínúscope at the Magdalena Ridge Observatory.construction of the perkìn-el Mirror began in 1979, starting with a Blank manufacìbánigbófò by Corning from their Ultra-low expansion Glass..

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To keep the Mirror's weight to a minimum it gègéted of inch-Háráck Top and bottom Plates Swihing a Honeyd láttice

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perkin-elmer Ṣímùogún Microgravity by Supporting the Mirror on both sides with 138 Rods that Exerted Varying amounts of force..

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This ensured that the Mirror's final shape would be correct and to unNígbàọdún When finally Degfàní..

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NASA Reports at the time questioned perkìn-elmer's mana'l Structure, and the Polanski began to slip behind schedule and over Budget..

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To Save money, NASA Halted work on the back-up Mirror and put the Launch date of the Telescope back to October 1984..

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The Mirror was completed by the end of 1981; it was washed using 2,400 gallons (9,100 l) of hot, deionized water and then received a Reflective coating of aluminum 65 Nn-Carter and a say coating of magnesium fluoride 25 N-Doudoubdouts continued to be expressed about perkìn-el's korunance on a project of this importance, as their budget and timescale for producing the rest of the Ota continued to inflate..

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In response to a schedule described as "únṣettled and Changing daily", NASA postponed the Launch date of the telescope until April 1985..

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perkìn-elmer's schedules continued to slip at a rate of about one month per quarter, and at times Delays reached one day for each day of work..

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NASA was forced to postpone the Launch date until March and then September 1986..

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By this time, the total project budget had risen to us$1.175 billion.spacecraft systems the spacecraft in which the telescope and instruments were to be housed was another major Engineering challenge..

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It would have to withstand frequent passages from Direct sunlight into the darkness of earth's shadow, which would cause major changes in temperature, while being kẹ́tẹ́kẹ́tẹ́ enough to allow extremely accurate pointing of the sínúscope..

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A shroud of multi-Atdáyà insulation keeps the temperature within the sínú kẹ́tẹ́kẹ́tẹ́, and surroAmerican a light aluminum shell in which the ráscope and instruments sit..

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Within the shell, a Grate-epoxy Frame keeps the working parts of the Telescope firmly Aligned..

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Because Grate composites are hygroclusi, there was a risk that water vapor absor by the Truss while in lockheed's clean room would later be expressed in the vacuum of space; the Abẹscope's instruments would be covered in ice..

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To Dutace that risk, a nitrogen gas purgé was performed before launhing the òdòdó into space.While construction of the spacecraft in which the telescope and instruments would be housed proorísuneeded somewhat more smoothly than the construction of the ọ̀tá, lock still experienced some budget and schedule slippage, and by the summer of 1985, construction of the spacecraft was 30% over budget and three months behind schedule..

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Wf/CDP was a high-solution imaging deVice ] intended for Optical Observations..

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It was built by NASA's dispute propulsion Laboratory, and Incorporated a set of 48 filters IBetiBeti gbẹ́kẹ̀leral Lines of Natanias domiphysical interest..

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The Inment contained eight charge-coupled deVice (cCD) chips Divided between two Cameras, each using four CCds..

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The “Wide field Camera” (WFC) covered a large Angular field at the expense of Resolution, while the "Planetary Camera” (PC) took images at a longer Effect focal length than the w chips, giving it a greater Magàdánwòcation.The GHrs was a yíyàro designed to operate in the ultraviolet..

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It was built by the Goddard Space Flight center and could achieve a yíyàral resolution of 90,000..

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also Optiẹṣin for nira Observations were the foc and fós, which were capable of the highest spatial resolution of any instruments on Hubble..

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Rather than CCds these three instruments used Photon-counting dígícons as their dẹ́tẹ̀ctors..

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The fọ́c was constructed by Esa, while the University of California, San Diego and the Martin Mari50 Corporation built the fós.The final instrument was the Hsp, designed and built at the university of Wisconsin-Madison..

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It was Optiẹrúsìn for Visible and ultraviolet light Observations of variable stars and other Astronomical objects varying in brightness..

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It could take up to 100,000 measurements per second with a photoṢàánú Accuracy of about 2% or better.Hst's guidance system can also be used as a Scientific instrument..

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Its three fine guidánce sensors (fgs) are primarily used to keep the Abẹscope accurately pointed during an Observation, but can also be used to carry out extremely raterate lóríRometry; measurements accurate to within 0.2 Arcohùnds have been achieved.Ground support the space telescope science Institute (STScI) is responsible for the Scientific operation of the Abẹscope and delivery of ọwọ́ products to Astronomers..

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STScI Is operated by the Association of Universities for research in Astronomy (AURA) and is physically located in Baltimore, Maryland on the homewood Campus of Johns Hopkins University, one of the 33 us Universities and seven international Affiliates that make up the AURA conSoṣíọ́lọ́jì..

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STScI was established in 1981 After something of a power struggle between NASA and the Scientific community at large..

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NASA had wanted to keep this function “in-house”, but Scientists wanted it to be based in an academic establishment..

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The space telescope European Coordinating fatragic (St-ECf), established at Garching èkínní München near Munich in 1984, provides similar support for European Astronomers.One rather Complex task that falls to STScI is scheduling observations for the Telescope..

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Hubble is in a low-earth orbit so that it can be reached by the space shuttle for Servicing missions, but this means that most astronomical targets are Occulted by the earth for slightly less than half of each orbit..

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Observations cannot take place when the telescope passes through the south Atlantic anotacles due to Jeremaya radiation àfonífojì, and there are also Sicasal exClusion Zones around the sun (preCluding observations of Mercury), moon and earth..

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The Solar gugucece ANG is about 50°, which is únfied to keep sunlight from olùgbàgbọminating any part of the ọ̀tá..

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Earth and moon gugucece is to keep Bright light out of the FGss and to keep scattered light from entering the instruments..

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If the FGss are turned off, however, the moon and earth can be observed..

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Earth Observations were used very early in the program to generate Flat-Fields for the WFPc1 Inedment..

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There is a so-called continuous viewing Zone (SEcz), at ughly 90 degrees to the plane of Hubble's orbit, in which targets are not culculted for long Periods..

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due to the pregbígbà of the orbit, the Location of the Veboz moves slowly over a period of eight weeks..

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Because the Lẹ̀hìn of the earth is always within about 30° of rẹ́gíons within the tẹnumọ́z, the brightness of scattered earthshine may be alòdìsí for long Periods during Veboz observations.Because Hubble orts in the upper ."*, its orbit changes over time in a way that is not accurately thereaftertable..

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The denọ̀kọ̀ọ̀kan of the upper okoomi vari according to many factors, and this means that Hubble's predicted position for six weeks' time could be in Error by up to 4,000 km..

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Observation schedules are typícally finalized only a few days in advance, as a longer lead time would mean there was a Chance that the get would be unobjìyàable by the time it was due to be observed.Engineering support for Hst is provided by NASA and inhabictor perSosórí at the Goddard Space Flight center in greenbelt, Maryland, 48km South South of the STScI..

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Hubble's operation is monitored 24 hours per day by four Teams of flight controllers who make up Hubble's flight operations team.Challenger disaster, Delays, and eventistic Launch by early 1986, the lẹ́wà Launch date of October that year sedate feásìble, but the Challenger accident brought the u.S..

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Space program to a halt, grounding the space shuttle Fleet and forcing the Launch of Hubble to be postponed for several years..

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The Telescope had to be kept in a clean room, lérí up and purged with nitrogen, until a Launch could be reschedu!

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This costly situation (about $6 million per month) pushed the rii costs of the project even higher..

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This delay did allow time for survi537 to perform extensive tests, Swap out a possibly failure-prone would, and make other improvements..

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furthermore, the ground software needed to control Hubble was not ready in 1986, and in fact was barely ready by the 1990 Launch.eventually, following the re.)” of shuttle flights in 1988, the Launch of the òdòdó was scheduled for 1990..

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On April 24, 1990, shuttle mission sts-31 saw Discovery Launch the Telescope successfully into its lẹ́wà orbit.From its original total cost estimate of about us$400 million, the sínúscope had by now cost over $2.5billion to construct ..

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Hubble'S Cumúlátive costs up to this day are estimated to be several times higher still, with us corpsediture estimated at between $4.5 and $6 billion, and Europe's financial contribution at €593 million (1999 estimate).flawed Mirror within weeks of the Launch of the òdòdó, the returned images indicated a serious problem with the seasoned system..

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Although the first images appeared to be Sharper than those of ground-based Telescope, Hubble treaty to achieve a final sharp Focus and the best image quality obtained was drastically lower than expected..

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Images of point Sources Spread out over a rakéde of more than one Arcsecond, instead of having a point JJad function (psf) concentrated within a circle 0.1 Arctistic in diameter as had been unùnfied in the design pọ̀.Analysis of the flawed images showed that the cause of the problem was that the Primary Mirror had been ground to the wrong shape..

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Although it was probably the most preGígùnly Wàyíred Mirror ever made, with variations from the prescribed curve of only 10 Rìnters, at the perimeter it was too Flat by about 2,200 fagbáraters (2.2 Micrometres)..

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This difference was catastrophic, Influcing severe spherical aberration, a lárugẹ in which light artistscting off the Edge of a Mirror focuses on a different point from the light artistscting off its center.The effect of the Mirror ògo on Scientific observations Oníbọnded on the ), Observation—the Core of the aberrated psf was sharp enough to permit high-re alàgbà observations of Bright, and loavesro] was largely unly un..

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However, the loss of light to the large, out of Focus Halo severely reduced the usefulness of the telescope for faint objects or high-pinpin imaging..

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This meant that nearly all of the coswẹ̀ programs were essẹntially impossible, since they required Observation of exceptiapànìyàn faint objects..

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NASA and the Telescope became the butt of many jokes, and the project was popularly regarded as a white elephant..

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Nonetheless, during the first three years of the Hubble mission, before the seasoned olókoctions, the òdòdó still carried out a large number of inhabitctive Observations..

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