사용자:Astor/작업장3: 두 판 사이의 차이
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이를 이용하여 처음으로 지구의 [[세차운동]]을 발견하였다. 이러한 작업을 하는 중에 그는 별의 밝기를 나타내는 척도인 [[겉보기등급|등급]]을 고안하였는데, 이는 지금도 쓰이고 있다. 히파르쿠스의 뒤를 이은 [[프톨레미]]는 총 1022개의 별들의 위치와 밝기를 수록한 [[알마게스트]]({{lang||Almagest}})를 발간하였다.<ref name="Kanas2007" />
In the 10th century, [[:en:Abd al-Rahman al-Sufi|Abd al-Rahman al-Sufi]] carried out observations on the stars and described their positions, [[:en:apparent magnitude|magnitude]]s and [[:en:star color|star color]], and gave drawings for each constellation, in his ''[[:en:Book of Fixed Stars|Book of Fixed Stars]]''. [[:en:Ibn Yunus|Ibn Yunus]] observed more than 10,000 entries for the sun's position for many years using a large [[:en:astrolabe|astrolabe]] with a diameter of nearly 1.4 metres. His observations on [[:en:eclipse|eclipse]]s were still used centuries later in [[:en:Simon Newcomb|Simon Newcomb]]'s investigations on the motion of the moon, while his other observations inspired [[:en:Laplace|Laplace]]'s ''Obliquity of the Ecliptic'' and ''Inequalities of Jupiter and Saturn''.{{Clarify|date=August 2009}}<ref>[http://adsabs.harvard.edu/full/1895AJ.....15..113L Great Inequalities of Jupiter and Saturn]</ref> In the 15th century, the [[:en:Timurid dynasty|Timurid]] astronomer [[:en:Ulugh Beg|Ulugh Beg]] compiled the ''[[:en:Zij-i-Sultani|Zij-i-Sultani]]'', in which he catalogued 1,019 stars. Like the earlier catalogs of Hipparchus and Ptolemy, Ulugh Beg's catalogue is estimated to have been precise to within approximately 20 [[:en:minutes of arc|minutes of arc]].<ref>
p. 49, "Astrometry", ''History of astronomy: an encyclopedia'', John Lankford, Taylor & Francis, 1997, ISBN 0-8153-0322-X.</ref> 16세기에 들어와서 티코 브라헤는 [[:en:mural instrument|mural instrument]]같은 발전된 기기들을 이용하여 별들의 위치를 약 15–35[[각초|초]]의 정확도로 측정하였다.
In the 16th century, [[:en:Tycho Brahe|Tycho Brahe]] used improved instruments, including large [[:en:mural instrument|mural instrument]]s, to measure star positions more accurately than previously, with a precision of 15–35 [[Minute_of_arc#Symbols and abbreviations|arcsec]].
<ref>pp. 2–3, ''Fundamentals of astrometry'', Jean Kovalevsky and P. Kenneth Seidelmann, Cambridge University Press, 2004, ISBN 0-521-64216-7.</ref>
이스탄불 천문대의 [[타끼 앗딘]]{{lang||Taqi al-Din}}은 자신이 발명한 "천문시계"를 이용하여 별들의 위치를 측정하였다.
[[:en:Taqi al-Din Muhammad ibn Ma'ruf|Taqi al-Din]] measured the [[:en:right scension|right ascension]] of the stars at the [[:en:Istanbul observatory of Taqi al-Din|Istanbul observatory of Taqi al-Din]] using the "observational clock" he invented.
<ref name=Tekeli>{{cite encyclopedia | first = Sevim | last = Tekeli | title = Taqi al-Din | year = 1997 | encyclopedia = Encyclopaedia of the History of Science, Technology, and Medicine in Non-Western Cultures | publisher = [[:en:Kluwer Academic Publishers|Kluwer Academic Publishers]] | isbn = 0-7923-4066-3 | url = http://www.springer.com/philosophy/philosophy+of+sciences/book/978-1-4020-4425-0 }}</ref>
When [[:en:telescope|telescope]]s became commonplace, [[:en:setting circles|setting circles]] sped measurements
[[:en:James Bradley|James Bradley]] first tried to measure [[:en:stellar parallax|stellar parallax]]es in 1729. The stellar movement proved too insignificant for his [[:en:telescope|telescope]], but he instead discovered the 광행차[[:en:aberration of light|aberration of light]] and the [[:en:nutation|nutation]] of the Earth’s axis. His cataloguing of 3222 stars was refined in 1807 by [[:en:Friedrich Bessel|Friedrich Bessel]], the father of modern astrometry. He made the first measurement of stellar parallax: 0.3 [[Minute_of_arc#Symbols and abbreviations|arcsec]] for the [[:en:binary star|binary star]] [[:en:61 Cygni|61 Cygni]].
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Being very difficult to measure, only about 60 stellar parallaxes had been obtained by the end of the 19th century, mostly by use of the [[:en:filar micrometer|filar micrometer]]. [[:en:Astrograph|Astrograph]]s using astronomical [[:en:photographic plate|photographic plate]]s sped the process in the early 20th century. Automated plate-measuring machines<ref>[http://cdsweb.cern.ch/record/1107461 CERN paper on plate measuring machine] USNO StarScan</ref> and more sophisticated computer technology of the 1960s allowed more efficient compilation of [[:en:star catalogue|star catalogue]]s. In the 1980s, [[:en:charge-coupled device|charge-coupled device]]s (CCDs) replaced photographic plates and reduced optical uncertainties to one milliarcsecond. This technology made astrometry less expensive, opening the field to an amateur audience.
최초로 시차 측정을 발표한 사람은 독일의 프리드리히 베셀로, 1838년에 발표하였다. 그는 백조자리 61번 별의 시차를 0.3136초로 측정하였고, 별까지의 거리가 10.6광년이라는 것을 알아내었다. 이 측정은 현대의 측정치인 11.2광년과 매우 근사한 측정치이다.
In 1989, the [[:en:European Space Agency|European Space Agency]]'s [[:en:Hipparcos|Hipparcos]] satellite took astrometry into orbit, where it could be less affected by mechanical forces of the Earth and optical distortions from its atmosphere. Operated from 1989 to 1993, Hipparcos measured large and small angles on the sky with much greater precision than any previous optical telescopes. During its 4-year run, the positions, parallaxes, and [[:en:proper motions|proper motions]] of 118,218 stars were determined with an unprecedented degree of accuracy. A new “[[:en:Hipparcos Catalogue|Tycho catalog]]” drew together a database of 1,058,332 to within 20-30 [[Minute_of_arc#Symbols and abbreviations|mas]] (milliarcseconds). Additional catalogues were compiled for the 23,882 double/multiple stars and 11,597 [[:en:variable star|variable star]]s also analyzed during the Hipparcos mission.<ref>{{cite web
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