Messier 107

Last updated
Messier 107
Messier 107 Hubble WikiSky.jpg
M107 from Hubble Space Telescope; 3.5′ view
Observation data (J2000 epoch)
Class X [1]
Right ascension 16h 32m 31.86s [2]
Declination –13° 03′ 13.6″ [2]
Distance 20.9  kly (6.4  kpc) [3]
Apparent magnitude (V)7.9 [4]
Apparent dimensions (V)10′ [5]
Physical characteristics
Mass1.82×105 [3]   M☉
Radius30 ly [6]
Metallicity  = –0.95 [7] dex
Estimated age13.95  Gyr [7]
Other designationsC 1629-129, GCl 44, M 107, NGC  6171 [8]
See also: Globular cluster, List of globular clusters

Messier 107 or M107, also known as NGC 6171 or the Crucifix Cluster, is a very loose globular cluster in a very mildly southern part of the sky close to the equator in Ophiuchus, and is the last such object in the Messier Catalogue.

Contents

Observational history, namings and guide

It was discovered by Pierre Méchain in April 1782, then independently by William Herschel in 1793. Herschel's son, John, in his 1864 General Catalogue, described it as a "globular cluster of stars, large, very rich, very much compressed, round, well resolved, clearly consisting of stars". [5] It was not until 1947 that Helen Sawyer Hogg added it and three other objects found by Méchain to the modern Catalogue, the latter having contributed several of the suggested observation objects which Messier had verified and added. [9] The cluster is to be found 2.5° south and slightly west of the star Zeta Ophiuchi. [5]

Properties

M107 is close to the galactic plane and about 20,900 light-years from Earth [3] and 9,800 ly (3,000 pc) from the Galactic Center. [10] Its orbit is partly as far out as the galactic halo, as is between 9,200–12,400 ly (2,820–3,790 pc) from the Galactic Center, the lower figure, the "perigalactic distance" sees it enter and leave the galactic bar. [11]

It is an Oosterhoff type I [12] cluster with a metallicity of −0.95 [7] [lower-alpha 1] and it conforms with the bulk of the halo population. [10] There are 22 known RR Lyrae variable stars in this cluster and a probable SX Phoenicis variable. [13]

See also

References and footnotes

  1. ↑ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin, 849 (849): 11–14, Bibcode:1927BHarO.849...11S.
  2. 1 2 Goldsbury, Ryan; et al. (December 2010), "The ACS Survey of Galactic Globular Clusters. X. New Determinations of Centers for 65 Clusters", The Astronomical Journal, 140 (6): 1830–1837, arXiv: 1008.2755 , Bibcode:2010AJ....140.1830G, doi:10.1088/0004-6256/140/6/1830, S2CID   119183070.
  3. 1 2 3 Boyles, J.; et al. (November 2011), "Young Radio Pulsars in Galactic Globular Clusters", The Astrophysical Journal, 742 (1): 51, arXiv: 1108.4402 , Bibcode:2011ApJ...742...51B, doi:10.1088/0004-637X/742/1/51, S2CID   118649860.
  4. ↑ "Messier 107". SEDS Messier Catalog. Retrieved 30 April 2022.
  5. 1 2 3 Mullaney, James (2007), The Herschel Objects and How to Observe Them, Astronomers' Observing Guides, Springer Science & Business Media, p. 94, Bibcode:2007hoho.book.....M, ISBN   978-0387681252.
  6. ↑ From trigonometry: distance × sin( diameter_angle / 2 ) = 39.5 ly. radius
  7. 1 2 3 Forbes, Duncan A.; Bridges, Terry (May 2010), "Accreted versus in situ Milky Way globular clusters", Monthly Notices of the Royal Astronomical Society , 404 (3): 1203–1214, arXiv: 1001.4289 , Bibcode:2010MNRAS.404.1203F, doi: 10.1111/j.1365-2966.2010.16373.x , S2CID   51825384.
  8. ↑ "NGC 6171". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2006-11-16.
  9. ↑ Frommert, Hartmut; Kronberg, Christine (August 30, 2007), "Messier 107", SEDS Messier pages, Students for the Exploration and Development of Space (SEDS), retrieved 2018-12-07.
  10. 1 2 Zinn, R. (June 15, 1985), "The globular cluster system of the galaxy. IV - The halo and disk subsystems", Astrophysical Journal, Part 1, 293: 424–444, Bibcode:1985ApJ...293..424Z, doi:10.1086/163249.
  11. ↑ Pichardo, Bárbara; et al. (July 2004), "Models for the Gravitational Field of the Galactic Bar: An Application to Stellar Orbits in the Galactic Plane and Orbits of Some Globular Clusters", The Astrophysical Journal, 609 (1): 144–165, arXiv: astro-ph/0402340 , Bibcode:2004ApJ...609..144P, doi:10.1086/421008, S2CID   16356464.
  12. ↑ Olech, A.; et al. (March 2001), "The Clusters AgeS Experiment (CASE): RR Lyrae variables in the globular cluster NGC 6362", Monthly Notices of the Royal Astronomical Society, 321 (3): 421–432, arXiv: astro-ph/0005589 , Bibcode:2001MNRAS.321..421O, doi: 10.1046/j.1365-8711.2001.04010.x , S2CID   14453719.
  13. ↑ McCombs, Thayne; et al. (January 2013), "Variable Stars in the Globular Cluster M107: The Discovery of a Probable SX Phoenicis", AAS Meeting #221, vol. 221, American Astronomical Society, p. 250.22, Bibcode:2013AAS...22125022M, 250.22.
  1. ↑ Where minus 1 would be 10 times less iron-to-hydrogen metallicity than the Sun

Related Research Articles

<span class="mw-page-title-main">Messier 5</span> Globular cluster in the constellation Serpens

Messier 5 or M5 is a globular cluster in the constellation Serpens. It was discovered by Gottfried Kirch in 1702.

<span class="mw-page-title-main">Messier 72</span> Globular cluster in the constellation Aquarius

Messier 72 is a globular cluster in the south west of the very mildly southern constellation of Aquarius.

<span class="mw-page-title-main">Messier 2</span> Globular cluster in the constellation Aquarius

Messier 2 or M2 is a globular cluster in the constellation Aquarius, five degrees north of the star Beta Aquarii. It was discovered by Jean-Dominique Maraldi in 1746, and is one of the largest known globular clusters.

<span class="mw-page-title-main">Messier 9</span> Globular cluster in Ophiuchus

Messier 9 or M9 is a globular cluster in the constellation of Ophiuchus. It is positioned in the southern part of the constellation to the southwest of Eta Ophiuchi, and lies atop a dark cloud of dust designated Barnard 64. The cluster was discovered by French astronomer Charles Messier on June 3, 1764, who described it as a "nebula without stars". In 1783, English astronomer William Herschel was able to use his reflector to resolve individual stars within the cluster. He estimated the cluster to be 7–8′ in diameter with stars densely packed near the center.

<span class="mw-page-title-main">Messier 15</span> Globular cluster in the constellation Pegasus

Messier 15 or M15 is a globular cluster in the constellation Pegasus. It was discovered by Jean-Dominique Maraldi in 1746 and included in Charles Messier's catalogue of comet-like objects in 1764. At an estimated 12.5±1.3 billion years old, it is one of the oldest known globular clusters.

<span class="mw-page-title-main">Messier 19</span> Globular cluster in Ophiuchus

Messier 19 or M19 is a globular cluster in the constellation Ophiuchus. It was discovered by Charles Messier on June 5, 1764 and added to his catalogue of comet-like objects that same year. It was resolved into individual stars by William Herschel in 1784. His son, John Herschel, described it as "a superb cluster resolvable into countless stars". The cluster is located 4.5° WSW of Theta Ophiuchi and is just visible as a fuzzy point of light using 50 mm (2.0 in) binoculars. Using a telescope with a 25.4 cm (10.0 in) aperture, the cluster shows an oval appearance with a 3′ × 4′ core and a 5′ × 7′ halo.

<span class="mw-page-title-main">Messier 28</span> Globular cluster in the constellation of Sagittarius

Messier 28 or M28, also known as NGC 6626, is a globular cluster of stars in the center-west of Sagittarius. It was discovered by French astronomer Charles Messier in 1764. He briefly described it as a "nebula containing no star... round, seen with difficulty in 31⁄2-foot telescope; Diam 2′."

<span class="mw-page-title-main">Messier 53</span> Globular cluster in the constellation Coma Berenices

Messier 53 is a globular cluster in the Coma Berenices constellation. It was discovered by Johann Elert Bode in 1775. M53 is one of the more outlying globular clusters, being about 60,000 light-years (18.4 kpc) light-years away from the Galactic Center, and almost the same distance from the Solar System. The cluster has a core radius (rc) of 2.18 pc, a half-light radius (rh) of 5.84 pc, and a tidal radius (rtr) of 239.9 pc.

<span class="mw-page-title-main">Messier 55</span> Globular cluster in the constellation Sagittarius

Messier 55 is a globular cluster in the south of the constellation Sagittarius. It was discovered by Nicolas Louis de Lacaille in 1752 while observing from what today is South Africa. Starting in 1754, Charles Messier made several attempts to find this object from Paris but its low declination meant from there it rises daily very little above the horizon, hampering observation. He observed and catalogued it in 1778. The cluster can be seen with 50 mm binoculars; resolving individual stars needs a medium-sized telescope.

<span class="mw-page-title-main">Messier 56</span> Globular cluster in the constellation Lyra

Messier 56 is a globular cluster in the constellation Lyra. It was discovered by Charles Messier in 1779. It is angularly found about midway between Albireo and Sulafat. In a good night sky it is tricky to find with large (50–80 mm) binoculars, appearing as a slightly fuzzy star. The cluster can be resolved using a telescope with an aperture of 8 in (20 cm) or larger.

<span class="mw-page-title-main">Messier 62</span> Globular cluster in the constellation Ophiuchus

Messier 62 or M62, also known as NGC 6266 or the Flickering Globular Cluster, is a globular cluster of stars in the south of the equatorial constellation of Ophiuchus. It was discovered in 1771 by Charles Messier, then added to his catalogue eight years later.

<span class="mw-page-title-main">Messier 68</span> Globular cluster in the constellation Hydra

Messier 68 is a globular cluster found in the east south-east of Hydra, away from its precisely equatorial part. It was discovered by Charles Messier in 1780. William Herschel described it as "a beautiful cluster of stars, extremely rich, and so compressed that most of the stars are blended together". His son John noted that it was "all clearly resolved into stars of 12th magnitude, very loose and ragged at the borders".

<span class="mw-page-title-main">Messier 70</span> Globular cluster in the constellation Sagittarius

Messier 70 or M70, also known as NGC 6681, is a globular cluster of stars to be found in the south of Sagittarius. It was discovered by Charles Messier in 1780. The famous comet Hale–Bopp was discovered near this cluster in 1995.

<span class="mw-page-title-main">Messier 71</span> Globular cluster in the constellation Sagitta

Messier 71 is a globular cluster in the small northern constellation Sagitta. It was discovered by Philippe Loys de Chéseaux in 1745 and included by Charles Messier in his catalog of non-comet-like objects in 1780. It was also noted by Koehler at Dresden around 1775.

<span class="mw-page-title-main">Messier 75</span> Globular cluster in the constellation Sagittarius

Messier 75 or M75, also known as NGC 6864, is a giant globular cluster of stars in the southern constellation Sagittarius. It was discovered by Pierre Méchain in 1780 and included in Charles Messier's catalog of comet-like objects that same year.

<span class="mw-page-title-main">Messier 92</span> Globular cluster in the constellation Hercules

Messier 92 is a globular cluster of stars in the northern constellation of Hercules.

<span class="mw-page-title-main">NGC 2419</span> Globular cluster in the constellation Lynx

NGC 2419 is a globular cluster in the constellation Lynx. It was discovered by William Herschel on December 31, 1788. NGC 2419 is at a distance of about 300,000 light years from the Solar System and at the same distance from the Galactic Center.

<span class="mw-page-title-main">NGC 5466</span> Class XII globular cluster in the constellation Boötes

NGC 5466 is a class XII globular cluster in the constellation Boötes. Located 51,800 light years from Earth and 52,800 light years from the Galactic Center, it was discovered by William Herschel on May 17, 1784, as H VI.9. This globular cluster is unusual insofar as it contains a certain blue horizontal branch of stars, as well as being unusually metal poor like ordinary globular clusters. It is thought to be the source of a stellar stream discovered in 2006, called the 45 Degree Tidal Stream. This star stream is an approximately 1.4° wide star lane extending from Boötes to Ursa Major.

<span class="mw-page-title-main">NGC 6934</span> Globular cluster in the constellation Delphinus

NGC 6934 is a globular cluster of stars in the northern constellation of Delphinus, about 52 kilolight-years distant from the Sun. It was discovered by the German-born astronomer William Herschel on 24 September 1785. The cluster is following a highly eccentric orbit through the Milky Way along an orbital plane that is inclined by 73° to the galactic plane. It may share a common dynamic origin with NGC 5466. As of 2018, it has been poorly studied.

<span class="mw-page-title-main">NGC 1261</span> Globular cluster in the constellation Horologium

NGC 1261 is a globular cluster of stars in the southern constellation of Horologium, first discovered by Scottish astronomer James Dunlop in 1826. The cluster is located at a distance of 53 kilolight-years from the Sun, and 59 kilolight-years from the Galactic Center. It is about 10.24 billion years old with 341,000 times the mass of the Sun. The cluster does not display the normal indications of core collapse, but evidence suggests it may have instead passed through a post core-collapse bounce state within the past two billion years. The central luminosity density is 2.22 L☉·pc−3, which is low for a globular cluster. Despite this, it has a Shapley–Sawyer Concentration Class of II, indicating a dense central concentration.

This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.