M 107 (звёздное скопление)

У этого термина существуют и другие значения, см. M107.
М 107
Шаровое скопление
M107; Телескоп Хаббл / STScI / WikiSky
M107; Телескоп Хаббл / STScI / WikiSky
История исследования
Открыватель Пьер Мешен
Дата открытия 1782
Наблюдательные данные
(Эпоха J2000.0)
Прямое восхождение 16ч 32м 31,86с
Склонение −13° 03′ 13,60″
Расстояние 20 900 св. лет (6400 пк)
Видимая звёздная величина (V) +8,85
Видимые размеры 13,0′
Лучевая скорость (Rv) −33,8 ± 0,3 км/с[2]
Собственное движение
 • прямое восхождение −0,43 ± 0,34 mas/год[1]
 • склонение −11,52 ± 0,34 mas/год[1]
Созвездие Змееносец
Физические характеристики
Класс X
Часть от Млечный Путь
Радиус 39,5 св. года
Абсолютная звёздная величина (V) −7,08[2]
Металличность [Fe/H] −1,06[3]
Информация в базах данных
SIMBAD M 107
Коды в каталогах
NGC 6171, M 107
Логотип Викиданных Информация в Викиданных ?
Логотип Викисклада Медиафайлы на Викискладе

Messier 107 (англ. M 107, NGC 6171, рус. Мессье 107) — шаровое звёздное скопление в созвездии Змееносца.

История открытия

Было открыто сотрудником Мессье Пьером Мешеном в 1782 году и независимо Уильямом Гершелем в 1793 году. В первые редакции каталога Мессье оно не вошло и было добавлено в него под номером 107 лишь в 1947.

Интересные характеристики

М107 в Созвездии Змееносца

Расположенное на расстоянии 20 900 световых лет, М107 близко к галактической плоскости, в отличие от большинства шаровых скоплений, которые не проявляют тенденцию группировки к плоскости Галактики. В скоплении известно 25 переменных звёзд.

См. также

Примечания

  1. ↑ 1 2 Kharchenko N. V., Piskunov A. E., Schilbach E., Röser S., R.-D. Scholz Global survey of star clusters in the Milky Way (англ.) // Astronomy and Astrophysics / T. Forveille — EDP Sciences, 2013. — Vol. 558. — P. 53–53. — ISSN 0004-6361; 0365-0138; 1432-0746; 1286-4846 — doi:10.1051/0004-6361/201322302 — arXiv:1308.5822
  2. ↑ 1 2 Harris W. E. A catalog of parameters for globular clusters in the Milky Way (англ.) // The Astronomical Journal / J. G. III, E. Vishniac — New York City: IOP Publishing, AAS, University of Chicago Press, AIP, 1996. — Vol. 112, Iss. 4. — P. 1487. — ISSN 0004-6256; 1538-3881 — doi:10.1086/118116
  3. ↑ Leaman R. Insights into pre-enrichment of star clusters and self-enrichment of dwarf galaxies from their intrinsic metallicity dispersions (англ.) // The Astronomical Journal / J. G. III, E. Vishniac — New York City: IOP Publishing, AAS, University of Chicago Press, AIP, 2012. — Vol. 144, Iss. 6. — P. 183. — ISSN 0004-6256; 1538-3881 — doi:10.1088/0004-6256/144/6/183 — arXiv:1209.4648

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