List of open clusters

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The open cluster Messier 6 in the constellation Scorpius is also known as the Butterfly Cluster or NGC 6405 M6a.jpg
The open cluster Messier 6 in the constellation Scorpius is also known as the Butterfly Cluster or NGC 6405

This is a list of open clusters located in the Milky Way. An open cluster is an association of up to a few thousand stars that all formed from the same giant molecular cloud. There are over 1,000 known open clusters in the Milky Way galaxy, but the actual total may be up to ten times higher. [1] The estimated half-lives of clusters, after which half the original cluster members will have been lost, range from 150 million to 800 million years, depending on the original density. [2]

Cluster
identifier		 Constellation Distance
(parsecs)		Age
(Myr)		Diameter Apparent
magnitude 		Notes
Epoch J2000
R. A. Dec.
Hyades 04h 26.9m+15° 52′ Taurus 47625330'0.5 [3]
Coma Star Cluster 12h 22.5m+25° 51′ Coma Berenices 86400-500120'1.8 [4]
Trapezium Cluster 5h 35.4m−05° 27′ Orion 4120.30.783'4.0 [5]
Messier 6, Butterfly Cluster 17h 40.1m−32° 13′Scorpius4879420'4.2 [1]
Messier 7 17h 53.8m−34° 47′ Scorpius 28022480'3.3 [6] [7]
Messier 11, Wild Duck Cluster 18h 51.1m−06° 16′Scutum1,90025013'5.8 [1] [7] [8]
Messier 16, Eagle Nebula 18h 18.8m−13° 49′Serpens1,8001.36'6.0 [1]
Messier 18 18h 20.0m−17° 06′Sagittarius1,296175'6.9 [1]
Messier 21 18h 04.2m−22° 29′Sagittarius1,2051214'5.9 [1]
Messier 23 17h 57.0m−18° 59′Sagittarius62830030'5.5 [1] [7]
Messier 24 18h 17.0m−18° 29′Sagittarius3,07022090'2.5 [1] [7]
Messier 25 18h 31.7m−19° 07′ Sagittarius 6209230'4.6 [1]
Messier 26 18h 45.3m−09° 23′ Scutum 1,600857'8.0 [1]
Messier 34 02h 42.1m+42° 46′Perseus49918036'5.2 [1] [7]
Messier 35 06h 09.1m+24° 21′ Gemini 91218025'5.0 [9]
Messier 36 05h 36.2m+34° 08′ Auriga 1,3302510'6.0 [1]
Messier 37 05h 52.3m+32° 33′Auriga1,40034714'5.6 [1]
Messier 38 05h 28.7m+35° 51′Auriga1,40031620'6.4 [1]
Messier 39 21h 31.8m+48° 27′ Cygnus 31128030'4.6 [1] [6]
Messier 41 06h 46.0m−20° 46′Canis Major71024040'4.5 [1] [7]
Messier 44, Beehive Cluster 08h 40.4m+19° 41′ Cancer 18783070'3.1 [10] [11]
Messier 45, Pleiades 03h 47.4m+24° 07′Taurus136125120'1.2 [12]
Messier 46 07h 41.7m−14° 49′Puppis1,51025020'6.1 [1]
Messier 47 07h 36.6m−14° 30′Puppis4907325'4.4 [1]
Messier 48 08h 13.7m−05° 45′ Hydra 77040030'5.8 [1]
Messier 50 07h 02.6m−08° 23′Monoceros1,00013014'5.9 [9]
Messier 52 23h 24.8m+61° 35′Cassiopeia1,400160156.9 [1]
Messier 67 08h 51.3m+11° 48′ Cancer 9084,00025'6.9 [1] [7]
Messier 93 07h 44.6m−23° 52′Puppis103739010'6.2 [1]
Messier 103 01h 33.4m+60° 39′Cassiopeia3,000165'7.4 [13]
IC 2602, Southern Pleiades10h 43.2m−64° 24′ Carina 16730100'1.9 [14]
IC 2391, Omicron Velorum Cluster08h 40.6m−53° 02′ Vela 1763060'2.5 [14]
NGC 2451 A 07h 45.4m−37° 58′ Puppis 1895045'2.8 [6] [15]
Alpha Persei Cluster 03h 26.0m+49° 07′ Perseus 17250300'1.2 [16]
Arp-Madore 2 07h 38.8m−33° 51′Puppis8,8705,0001.3' [17]
Blanco 1 00h 04.3m−29° 56′ Sculptor 25310090'4.5 [14]
Hodge 301 05h 38.5m−69° 04′ Dorado 51,400250.5'11 [18] [19]
Lambda Orionis Cluster 05h 35m+09° 56′ Orion 43852.8 [20]
Pi Puppis Cluster 07h 08m−37° 10′ Puppis 31950'2.1 [21]
Melotte 186 18h 01.1m+02° 54′ Ophiuchus 200100240'3.0 [22]
NGC 2070 05h 38.7m−69° 06′ Dorado 48,5001.53.5'7.25 [23] [24]
NGC 2232 06h 26.4m−04° 45′ Monoceros 3255345'3.9 [1] [6]
IC 4756 18h 39.0m−05° 27′ Serpens 33050040'4.6 [1] [6]
NGC 2516, Southern Beehive Cluster07h 58.0m−60° 48′Carina34614130'3.8 [6] [7]
IC 4665 17h 46.3m+05° 43′ Ophiuchus 3524370'4.2 [1]
Trumpler 10 08h 47.8m−42° 29′Vela3653514'4.6 [1] [6]
NGC 6633 18h 27.7m+06° 34′ Ophiuchus 37566020'4.6 [25]
IC 348 03h 44.6m+32° 10′Perseus385447'7.3 [1]
NGC 752 01h 57.7m+37° 47′ Andromeda 4001,700–2,00075'5.7 [26]
NGC 3532, Wishing Well Cluster11h 06.4m−58° 40′Carina40531650'3.0 [6] [7]
Collinder 12107h 08m−37° 10′ Canis Major 60050'2.6 [27]
Collinder 140 07h 24.5m−31° 51′ Canis Major 4103542'3.5 [1] [6]
Collinder 26112h 38.0m−68° 22′ Musca 2,5008,0009'10.7 [28] [29]
NGC 2547 08h 10.8m−49° 18′Vela4333825'4.7 [6]
NGC 6281 17h 04.7m−37° 59′Scorpius4792208'5.4 [1]
NGC 225 00h 43.6m+61° 46′ Cassiopeia 65713012'7.0 [1]
NGC 5662 14h 35.6m−56° 37′ Centaurus 6667030'5.5 [1] [7]
NGC 5460 14h 07.4m−48° 20′ Centaurus 67816036'5.6 [1] [7]
NGC 189 00h 39.7m+61° 04′Cassiopeia752103.7'8.8 [1]
NGC 6025 16h 03.3m−60° 26′ Triangulum Australe 75613014'5.1 [1] [7]
IC 5146 21h 53.5m+47° 16′Cygnus85219'7.2 [1]
NGC 2301 06h 51.75m+00° 28′Monoceros85816512'6.0 [30]
IC 4651 17h 24.8m−49° 56′Ara8881,90010'6.9 [1] [7]
NGC 6087, S Normae Cluster16h 18.8m−57° 56′ Norma 8917014'5.4 [1] [7]
NGC 3114 10h 02.7m−60° 07′Carina91112436'4.2 [1]
NGC 2509 08h 00.7m−19° 04′Puppis912Uncertain [31] 10'9.3 [32]
NGC 2264 06h 41.0m+09° 53′ Monoceros 9131.540'3.9 [33]
NGC 1502 04h 07.8m+62° 20′ Camelopardalis 1,000108'5.7 [1]
Berkeley 59 00h 04.0m+68° 35′ Cepheus 1,0002180' [34]
NGC 2169 06h 08.4m+13° 58′ Orion 1,052125'5.9 [1]
NGC 6242 16h 55.6m−39° 28′Scorpius1,131509'6.4 [1] [7]
NGC 381 01h 08.3m+61° 35′Cassiopeia1,1483207'9.3 [1]
NGC 6204 16h 46.1m−47° 01′ Ara 1,200796'8.2 [1]
NGC 6231 16h 54.1m−41° 50′Scorpius1,243614'2.6 [1] [7]
NGC 2439 07h 40.8m−31° 41′Puppis1,300259'6.9 [1] [7]
NGC 6067 16h 13.2m−54° 13′Norma1,41717014'5.6 [1] [7]
NGC 2362, Tau Canis Majoris Cluster07h 18.6m−24° 59′Canis Major1,4804–55'4.1 [35]
NGC 6756 19h 08.7m+04° 42′ Aquila 1,507624'4.5 [1]
NGC 6031 16h 07.9m−54° 03′Norma1,5101173'8.5 [1] [36]
NGC 2175 06h 09.7m+20° 29′Orion1,6278.95'6.8 [1]
NGC 188 00h 48.4m+85° 15′Cepheus1,6606,60017'8.1 [7] [37]
NGC 2244 06h 31.9m+04° 56′Monoceros1,6601.930'4.8 [1]
NGC 129 00h 30.0m+60° 13′Cassiopeia1,6707621′6.5 [38]
NGC 2360, Caroline's Cluster07h 17.7m−15° 38′Canis Major1,8871,00013'7.2 [1] [7]
NGC 6834 19h 52.2m+29° 25′Cygnus1,930765'7.8 [1] [36]
NGC 659 01h 44.4m+60° 40′Cassiopeia1,938355'7.9 [1]
NGC 4755, Jewel Box 12h 53.6m−60° 22′ Crux 1,9761410'4.2 [1] [7]
NGC 6200 16h 44.1m−47° 28′Ara2,0568.512'7.4 [39]
NGC 869 02h 19.1m+57° 09′Perseus2,0791218'3.7 [1]
NGC 637 01h 43.0m+64° 02′Cassiopeia2,160104.2'8.2 [1]
NGC 2355 07h 17.0m+13° 47′Gemini2,2009555'9.7 [1] [7]
NGC 2129 06h 01.1m+23° 19′Gemini2,200105'6.7 [1] [40]
NGC 663 01h 46.1m+61° 14′Cassiopeia2,4202514'7.1 [1]
NGC 457 01h 19.1m+58° 17′Cassiopeia2,4292120'6.4 [41]
NGC 2204 06h 15.5m−18° 40′Canis Major2,62978713'8.6 [1]
NGC 884 02h 22.0m+57° 08′Perseus2,9401418'3.8 [1] [7]
NGC 1931 05h 31.0m+34° 15′Auriga3,086103'10.1 [1]
NGC 1980 5h 25.43m−05° 54′ Orion 5504.714'2.5 [42]
NGC 2158 06h 07.4m+24° 06′Gemini5,0711,0545'8.6 [1]
Teutsch 205h 41.4m+39° 14′Auriga5,7009002'11 [43]
NGC 6791 19h 20.9m+37° 46′ Lyra 5,8538,90016'9.5 [1] [7]
NGC 3293 10h 35.8m−58° 13′ Carina 2,75088'4.7
NGC 3766, Pearl Cluster11h 36.2m−61° 37′ Centaurus 17451412'5.3
NGC 7419 22h 54.3m+60° 48.9′ Cepheus 2,8002'13
NGC 7789, White Rose Cluster23h 57.4m+56° 43′ Cassiopeia 2,3371,70016'6.7 [44]
Gaia 1 06h 45.9m−16° 45′Canis Major4,6006,30013'8.3
Ru 7 06h 58.9m−13° 15′Canis Major[ citation needed ]

See also

Related Research Articles

<span class="mw-page-title-main">Wild Duck Cluster</span> Open cluster in the constellation Scutum

The Wild Duck Cluster is an open cluster of stars in the constellation Scutum. It was discovered by Gottfried Kirch in 1681. Charles Messier included it in his catalogue of diffuse objects in 1764. Its popular name derives from the brighter stars forming a triangle which could resemble a flying flock of ducks. The cluster is located just to the east of the Scutum Star Cloud midpoint.

<span class="mw-page-title-main">Messier 21</span> Open cluster in the constellation Sagittarius

Messier 21 or M21, also designated NGC 6531 or Webb's Cross, is an open cluster of stars located to the north-east of Sagittarius in the night sky, close to the Messier objects M20 to M25. It was discovered and catalogued by Charles Messier on June 5, 1764. This cluster is relatively young and tightly packed. A few blue giant stars have been identified in the cluster, but Messier 21 is composed mainly of small dim stars. With a magnitude of 6.5, M21 is not visible to the naked eye; however, with the smallest binoculars it can be easily spotted on a dark night. The cluster is positioned near the Trifid nebula, but is not associated with that nebulosity. It forms part of the Sagittarius OB1 association.

<span class="mw-page-title-main">Messier 23</span> Open cluster in Sagittarius

Messier 23, also known as NGC 6494, is an open cluster of stars in the northwest of the southern constellation of Sagittarius. It was discovered by Charles Messier in 1764. It can be found in good conditions with binoculars or a modestly sized telescope. It is in front of "an extensive gas and dust network", which there may be no inter-association. It is within 5° the sun's position so can be occulted by the moon.

<span class="mw-page-title-main">Messier 26</span> Open cluster in the constellation Scutum

Messier 26, also known as NGC 6694, is an open cluster of stars in the southern constellation of Scutum. It was discovered by Charles Messier in 1764. This 8th magnitude cluster is a challenge to find in ideal skies with typical binoculars, where it can be, with any modern minimum 3-inch (76 mm) aperture device. It is south-southwest of the open cluster Messier 11 and is 14′ across. About 25 stars are visible in a telescope with a 150–200 mm (6–8 in) aperture.

<span class="mw-page-title-main">Messier 18</span> Open cluster in the constellation Sagittarius

Messier 18 or M18, also designated NGC 6613 and sometimes known as the Black Swan Cluster, is an open cluster of stars in the constellation Sagittarius. It was discovered by Charles Messier in 1764 and included in his list of comet-like objects. From the perspective of Earth, M18 is situated between the Omega Nebula (M17) and the Small Sagittarius Star Cloud (M24).

<span class="mw-page-title-main">NGC 381</span> Open cluster in the constellation Cassiopeia

NGC 381 is an open cluster of stars in the northern constellation of Cassiopeia, located at a distance of approximately 3,120 light-years from the Sun. Credit for the discovery of this cluster was given to Caroline Herschel by her brother William in 1787, although she may never have actually seen it.

<span class="mw-page-title-main">NGC 2204</span> Open cluster in the constellation Canis Major

NGC 2204 is an open cluster of stars in the Canis Major constellation. It was discovered by the German-English astronomer William Herschel on 6 February 1785. The cluster has an integrated visual magnitude of 8.6 and spans a diameter of 10.0′. Resolving the individual member stars is a challenge with a 10 to 12-inch amateur telescope. It is located at a distance of approximately 13,400 light years from the Sun. The cluster shows a mean radial velocity of +91.38±0.30 km/s relative to the Sun, and is orbiting the inner galactic disk region about 1 kpc below the galactic plane.

56 Andromedae, abbreviated 56 And, is a probable binary star system in the northern constellation of Andromeda. 56 Andromedae is the Flamsteed designation. It has a combined apparent visual magnitude of 5.69, which is just bright enough to be dimly visible to the naked eye under good seeing conditions. The distance to this system can be ascertained from its annual parallax shift, measured at 9.9 mas with the Gaia space observatory, which yields a separation of 330 light years. It is moving further from the Earth with a heliocentric radial velocity of +62 km/s and is traversing the celestial sphere at a relatively high rate of 0.183″ per year. This pair is positioned near the line of sight to the open cluster NGC 752, located 1,490 light-years away.

<span class="mw-page-title-main">NGC 346</span> Open cluster in the constellation Tucana

NGC 346 is a young open cluster of stars with associated nebula located in the Small Magellanic Cloud (SMC) that appears in the southern constellation of Tucana. It was discovered August 1, 1826 by Scottish astronomer James Dunlop. J. L. E. Dreyer described it as, "bright, large, very irregular figure, much brighter middle similar to double star, mottled but not resolved". On the outskirts of the cluster is the multiple star system HD 5980, one of the brightest stars in the SMC.

NGC 6738 is an astronomical feature that is catalogued as an NGC object. Although listed as an open cluster in some astronomical databases, it may be merely an asterism; a 2003 paper in the journal Astronomy and Astrophysics describes it as being an "apparent concentration of a few bright stars on patchy background absorption".

<span class="mw-page-title-main">NGC 6208</span> Open star cluster in the constellation Ara

NGC 6208 is an open cluster in the southern constellation of Ara. With an age of 1.17 Gigayears, it is one of the oldest known open clusters.

<span class="mw-page-title-main">S Monocerotis</span> Star in the constellation Monoceros

S Monocerotis, also known as 15 Monocerotis, is a massive multiple and variable star system located in the constellation Monoceros. It is the brightest star in the Christmas Tree open cluster in the area catalogued as NGC 2264.

<span class="mw-page-title-main">NGC 2506</span> Open cluster in the constellation Monoceros

NGC 2506 is a mildly-elongated open cluster of stars in the equatorial constellation of Monoceros, located at a distance of 12.7 kly from the Sun near the Galactic anti-center. It was discovered by William Herschel in 1791. The cluster lies around 10,000 ly from the Galactic Center and about 1,600 ly above the Galactic plane. It is of intermediate age, estimated at around two billion years. The cluster has an angular radius of 12′ and a core radius of 4.8′.

<span class="mw-page-title-main">NGC 6388</span> Globular cluster in the constellation Scorpius

NGC 6388 is a globular cluster of stars located in the southern constellation of Scorpius. The cluster was discovered by Scottish astronomer James Dunlop on May 13, 1826 using a 20 cm (9 in) reflector telescope. It was later determined to be a globular cluster by English astronomer John Herschel, who was able to resolve it into individual stars. NGC 6388 is located at a distance of approximately 35,600 light-years (10.90 kpc) from the Sun. Due to its apparent visual magnitude of +6.8, binoculars or a small telescope are required to view it.

<span class="mw-page-title-main">NGC 1792</span> Galaxy in the constellation Columba

NGC 1792 is a spiral galaxy located in the southern Columba constellation. It was discovered by Scottish astronomer James Dunlop on October 4, 1826. This galaxy is located at a distance of about 36.4 million light-years and is receding from the Milky Way with a heliocentric radial velocity of 1,208 km/s. NGC 1792 is a member of the NGC 1808 cluster of galaxies.

<span class="mw-page-title-main">NGC 433</span> Open cluster in the constellation Cassiopeia

NGC 433 is an open cluster in the northern constellation of Cassiopeia, located at a distance of 6,500 light years from the Sun. It was discovered on September 29, 1829, by John Herschel, and was described by John Dreyer as "cluster, small, a little compressed." The cluster is considered on the poor side, with only 12 stars above magnitude 16. It has a linear diameter of 26.3 ly, with around 479 times the mass of the Sun and an age of 65 million years.

<span class="mw-page-title-main">NGC 4103</span> Open cluster in the constellation Crux

NGC 4103 is an open cluster in the constellation Crux. It was discovered by James Dunlop in 1826. It is located approximately 5,000 light years away from Earth, in the Carina-Sagittarius arm.

<span class="mw-page-title-main">Collinder 228</span>

Collinder 228 is an open cluster within the southern part of the Carina Nebula NGC 3372, about 25' south of η Carinae. It is probably composed of stars which recently formed from the material in the nebula. QZ Carinae is the brightest member of Collinder 228 with an apparent magnitude between 6.16–6.49 .

<span class="mw-page-title-main">NGC 4123</span> Galaxy in the constellation Virgo

NGC 4123 is a modest-sized, strongly-barred spiral galaxy located 75 million light-years away in the equatorial constellation of Virgo. It was discovered February 25, 1784 by William Herschel. This is a member of the Virgo cluster, and it belongs to a group of three galaxies. A companion galaxy, NGC 4116, lies at an angular separation of 14′ to the southwest. There is no indication of an interaction between the two galaxies. The third member of the group is NGC 4179.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 Dias W.S.; Alessi B.S.; Moitinho A.; Lepine J.R.D. (July 2002). "New catalog of optically visible open clusters and candidates". Astronomy and Astrophysics. 389 (3): 871–873. arXiv: astro-ph/0203351 . Bibcode:2002A&A...389..871D. doi:10.1051/0004-6361:20020668. S2CID   18502004. Note: see the VizieR catalogue B/ocl.
  2. ↑ de La Fuente, M. R. (1998). "Dynamical Evolution of Open Star Clusters". Publications of the Astronomical Society of the Pacific. 110 (751): 1117. Bibcode:1998PASP..110.1117D. doi: 10.1086/316220 .
  3. ↑ Perryman, M.A.C.; et al. (1998). "The Hyades: distance, structure, dynamics, and age". Astronomy & Astrophysics. 331: 81–120. arXiv: astro-ph/9707253 . Bibcode:1998A&A...331...81P.
  4. ↑ Casewell, S. L.; Jameson, R. F.; Dobbie, P. D. (January 2006). "New stellar members of the Coma Berenices open star cluster". Monthly Notices of the Royal Astronomical Society . 365 (2): 447–453. arXiv: astro-ph/0510133 . Bibcode:2006MNRAS.365..447C. doi: 10.1111/j.1365-2966.2005.09689.x .
  5. ↑ Reid, M. J.; et al. (2009). "Trigonometric Parallaxes of Massive Star Forming Regions: VI. Galactic Structure, Fundamental Parameters and Non-Circular Motions". Astrophysical Journal . 700 (1): 137–148. arXiv: 0902.3913 . Bibcode:2009ApJ...700..137R. doi:10.1088/0004-637X/700/1/137. S2CID   11347166.
  6. 1 2 3 4 5 6 7 8 9 10 Robichon, N.; et al. (2005). "Open clusters with Hipparcos. I. Mean astrometric parameters". Astronomy and Astrophysics. 345: 471–484. arXiv: astro-ph/9903131 . Bibcode:1999A&A...345..471R.
  7. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 Meynet, G.; Mermilliod, J.-C.; Maeder, A. (May 1993). "New dating of galactic open clusters". Astronomy and Astrophysics Supplement Series. 98 (3): 477–504. Bibcode:1993A&AS...98..477M.
  8. ↑ Paunzen, E.; Pintado, O. I.; Maitzen, H. M. (December 2003). "CCD photometric search for peculiar stars in open clusters. V. NGC 2099, NGC 3114, NGC 6204, NGC 6705 and NGC 6756". Astronomy and Astrophysics. 412 (3): 721–725. arXiv: astro-ph/0310069 . Bibcode:2003A&A...412..721P. doi:10.1051/0004-6361:20031065. S2CID   6381138.
  9. 1 2 Kalirai, Jasonjot Singh; Fahlman, Gregory G.; Richer, Harvey B.; Ventura, Paolo (September 2003). "The CFHT Open Star Cluster Survey. IV. Two Rich, Young Open Star Clusters: NGC 2168 (M35) and NGC 2323 (M50)". The Astronomical Journal. 126 (3): 1402–1414. arXiv: astro-ph/0306241 . Bibcode:2003AJ....126.1402K. doi:10.1086/377320. S2CID   17018911.
  10. ↑ Pinfield, D. J.; et al. (July 2003). "Brown dwarfs and low-mass stars in the Pleiades and Praesepe: membership and binarity". Monthly Notices of the Royal Astronomical Society. 342 (4): 1241–1259. arXiv: astro-ph/0303600 . Bibcode:2003MNRAS.342.1241P. doi: 10.1046/j.1365-8711.2003.06630.x . S2CID   285922.
  11. ↑ "NGC 2632". sim-id. Retrieved 2020-06-11.
  12. ↑ Percival, S. M.; Salaris, M.; Groenewegen, M. A. T. (2005). "The distance to the Pleiades. Main sequence fitting in the near infrared". Astronomy and Astrophysics. 429 (3): 887–894. arXiv: astro-ph/0409362 . Bibcode:2005A&A...429..887P. doi:10.1051/0004-6361:20041694. S2CID   14842664.
  13. ↑ Sanner, J.; et al. (September 1999). "Photometric and kinematic studies of open star clusters. I. NGC 581 (M 103)". Astronomy and Astrophysics. 349: 448–456. arXiv: astro-ph/9908059 . Bibcode:1999A&A...349..448S.
  14. 1 2 3 Mermilliod, J.-C.; Turon, C.; Robichon, N.; Arenou, F.; Lebreton, Y. (May 13–16, 1997). "The Distance of the Pleiades and Nearby Clusters". Proceedings of the ESA Symposium 'Hipparcos - Venice '97'. Venice, Italy: ESA. Bibcode:1997ESASP.402..643M.
  15. ↑ Hünsch, M.; Weidner, C. & Schmitt, J. H. M. M. (May 2003). "An X-ray study of the open clusters NGC 2451 A and B". Astronomy and Astrophysics. 402 (2): 571–586. Bibcode:2003A&A...402..571H. doi: 10.1051/0004-6361:20030268 .
  16. ↑ Basri, Gibor; Martín, Eduardo L. (January 1999). "The Mass and Age of Very Low Mass Members of the Open Cluster alpha Persei". The Astrophysical Journal. 510 (1): 266–273. arXiv: astro-ph/9807145 . Bibcode:1999ApJ...510..266B. doi:10.1086/306564. S2CID   2562718.
  17. ↑ Lee, Myung Gyoon (February 1997). "UBVI CCD Photometry of the Remote Old Open Cluster AM-2". Astronomical Journal. 113: 729–739. Bibcode:1997AJ....113..729L. doi: 10.1086/118292 .
  18. ↑ "Hodge 301". The Hubble Heritage Project. NASA. April 1, 1999. Retrieved 2010-03-25.
  19. ↑ Grebel, Eva K.; Chu, You-Hua (February 2000). "Hubble Space Telescope Photometry of Hodge 301: An "Old" Star Cluster in 30 Doradus". The Astronomical Journal. 119 (2): 787–799. arXiv: astro-ph/9910426 . Bibcode:2000AJ....119..787G. doi:10.1086/301218. S2CID   118590210.
  20. ↑ "Cl Collinder 69". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-06-07.
  21. ↑ "Cl Collinder 135". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-06-07.
  22. ↑ "Cl Melotte 186". sim-id. Retrieved 2020-07-13.
  23. ↑ "NGC 2070". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 11 August 2017.
  24. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). The Tycho-2 catalogue of the 2.5 million brightest stars. Vol. 355. pp. L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862. ISBN   978-0333750889.{{cite book}}: |journal= ignored (help)
  25. ↑ van Leeuwen, F. (February 2013), "Parallaxes and proper motions for 20 open clusters as based on the new Hipparcos catalogue", Astronomy and Astrophysics, 497 (1): 209–242, arXiv: 0902.1039 , Bibcode:2009A&A...497..209V, doi:10.1051/0004-6361/200811382, S2CID   16420237.
  26. ↑ Giardino, G.; et al. (October 2008). "The X-ray luminosity of solar-mass stars in the intermediate age open cluster NGC 752". Astronomy and Astrophysics. 490 (1): 113–123. arXiv: 0808.3451 . Bibcode:2008A&A...490..113G. doi:10.1051/0004-6361:200810042. S2CID   18980057.
  27. ↑ "Cl Collinder 121". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-06-07.
  28. ↑ "Cl Collinder 261". sim-id. Retrieved 2020-06-11.
  29. ↑ Salaris, M; Weiss, A; Percival, S. M. (2004). "The age of the oldest Open Clusters" (PDF). Astronomy & Astrophysics: 165–167.
  30. ↑ "SIMBAD Astronomical Database". Results for NGC 2301. Retrieved 2019-04-30.
  31. ↑ Carraro, G.; Costa, E. (March 2007). "Photometry of the five marginally studied open clusters Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen 4". Astronomy and Astrophysics. 464 (2): 573–580. arXiv: astro-ph/0611705 . Bibcode:2007A&A...464..573C. doi:10.1051/0004-6361:20066350. S2CID   1419651.
  32. ↑ Sujatha, S.; Babu, G. S. D. (2003). "Study of open cluster NGC 2509". Bulletin of the Astronomical Society of India. 31: 9–18. Bibcode:2003BASI...31....9S.
  33. ↑ Baxter, Eric J.; et al. (September 2009), "The Distance to NGC 2264", The Astronomical Journal, 138 (3): 963–974, arXiv: 0907.3139 , Bibcode:2009AJ....138..963B, doi:10.1088/0004-6256/138/3/963, S2CID   7940517.
  34. ↑ Pandey, A. K.; et al. (January 2008). "Stellar contents and star formation in the young star cluster Be 59". Monthly Notices of the Royal Astronomical Society. 383 (3): 1241–1258. arXiv: 0710.5429 . Bibcode:2008MNRAS.383.1241P. doi: 10.1111/j.1365-2966.2007.12641.x . S2CID   6776240.
  35. ↑ Currie, Thayne; et al. (June 2009). "The Last Gasp of Gas Giant Planet Formation: A Spitzer Study of the 5 Myr Old Cluster NGC 2362". The Astrophysical Journal. 698 (1): 1–27. arXiv: 0903.2666 . Bibcode:2009ApJ...698....1C. doi:10.1088/0004-637X/698/1/1. S2CID   9207187.
  36. 1 2 Paunzen, E.; et al. (July 2006). "CCD photometric search for peculiar stars in open clusters. VII. Berkeley 11, Berkeley 94, Haffner 15, Lyngå 1, NGC 6031, NGC 6405, NGC 6834 and Ruprecht 130". Astronomy and Astrophysics. 454 (1): 171–178. arXiv: astro-ph/0602567 . Bibcode:2006A&A...454..171P. doi:10.1051/0004-6361:20054628. S2CID   5131254.
  37. ↑ Bonatto, C.; Bica, E.; Santos, J. F. C. Jr. (April 2005). "Spatial dependence of 2MASS luminosity and mass functions in the old open cluster NGC 188". Astronomy and Astrophysics. 433 (3): 917–929. arXiv: astro-ph/0502453 . Bibcode:2005A&A...433..917B. doi:10.1051/0004-6361:20041113. S2CID   5134042.
  38. ↑ Turner, David G.; et al. (September 1992). "Galactic clusters with associated Cepheid variables. II - NGC 129 and DL Cassiopeiae". Astronomical Journal. 104 (3): 1132–1143. Bibcode:1992AJ....104.1132T. doi:10.1086/116302.
  39. ↑ "open cluster NGC 6200". WEBDA. Universität Wien. Retrieved 2011-10-28.
  40. ↑ Carraro, Giovanni; Chaboyer, Brian; Perencevich, James (January 2006). "The young open cluster NGC 2129". Monthly Notices of the Royal Astronomical Society. 365 (8): 867–873. arXiv: astro-ph/0510573 . Bibcode:2006MNRAS.365..867C. doi: 10.1111/j.1365-2966.2005.09762.x . S2CID   15621721.
  41. ↑ Frinchaboy, Peter M.; et al. (2008). "Open Clusters as Galactic Disk Tracers. I. Project Motivation, Cluster Membership, and Bulk Three-Dimensional Kinematics". The Astronomical Journal. 136 (1): 118–145. arXiv: 0804.4630 . Bibcode:2008AJ....136..118F. doi:10.1088/0004-6256/136/1/118. S2CID   16641439. See table I, p. 12.
  42. ↑ "The open cluster NGC 1980". In the Sky. Retrieved 27 November 2017.
  43. ↑ Bonatto, C.; Bica, E. (22 October 2010). "The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters". Astronomy and Astrophysics. 521: A74. Bibcode:2010A&A...521A..74B. doi: 10.1051/0004-6361/201015222 . hdl: 10183/99276 .
  44. ↑ Kharchenko, N. V; Piskunov, A. E; Röser, S; Schilbach, E; Scholz, R.-D (2005). "Astrophysical parameters of Galactic open clusters". Astronomy and Astrophysics. 438 (3): 1163–1173. arXiv: astro-ph/0501674 . Bibcode:2005A&A...438.1163K. doi:10.1051/0004-6361:20042523. S2CID   9079873.
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