Messier 62

Nowadays, Messier 62 has become a topic of great relevance and interest to a wide range of people. Its impact and relevance range from the personal to the professional sphere, influencing decisions, behaviors and ways of thinking. Messier 62 is not only a current phenomenon, but has been present throughout history, evolving and adapting to the changing circumstances of society. In this article we will explore different aspects of Messier 62, from its origin to its influence today, in order to better understand its importance and scope in our daily lives.

Messier 62
Messier 62 by the Hubble Space Telescope
Observation data (J2000 epoch)
ClassIV[1]
ConstellationOphiuchus
Right ascension17h 01m 12.60s[2]
Declination–30° 06′ 44.5″[2]
Distance21.5 ± 1.3 kly (6.6 ± 0.4 kpc)[3]
Apparent magnitude (V)6.5[4]
Apparent dimensions (V)15′
Physical characteristics
Absolute magnitude−9.18.[5]
Mass1.22×106[6] M☉
Radius48 ly[7]
Tidal radius59 ly.[8]
Metallicity = –1.02[9] dex
Estimated age11.78 Gyr[9]
Other designationsC 1658-300, GCl 51, M62, NGC 6266[10]
See also: Globular cluster, List of globular clusters

Messier 62 or M62, also known as NGC 6266 or the Flickering Globular Cluster, is a globular cluster of stars in the south[a] of the equatorial constellation of Ophiuchus. It was discovered in 1771 by Charles Messier,[b] then added to his catalogue eight years later.[11]

M62 is about 21.5 kly[3] from Earth and 5.5 kly from the Galactic Center.[2] It is among the ten most massive and luminous globular clusters in the Milky Way, showing an integrated absolute magnitude of −9.18.[5] It has an estimated mass of 1.22×106 M☉[6] and a mass-to-light ratio of 2.05±0.04 in the core visible light band, the V band.[12] It has a projected ellipticity of 0.01, meaning it is essentially spherical.[13] The density profile of its member stars suggests it has not yet undergone core collapse.[14] It has a core radius of 1.3 ly (0.39 pc), a half-mass radius of 9.6 ly (2.95 pc), and a half-light radius of 6.0 ly (1.83 pc). The stellar density at the core is 5.13 M☉ per cubic parsec.[15] It has a tidal radius of 59 ly (18.0 pc).[8]

The cluster shows at least two distinct populations of stars, which most likely represent two separate episodes of star formation. Of the main sequence stars in the cluster, 79%±1% are from the first generation and 21%±1% from the second. The second is enriched by elements released by the first. In particular, abundances of helium, carbon, magnesium, aluminium, and sodium differ between these two.[5]

Indications are this is an Oosterhoff type I, or "metal-rich" system. A 2010 study identified 245 variable stars in the cluster's field, of which 209 are RR Lyrae variables, four are Type II Cepheids, 25 are long period variables, and one is an eclipsing binary. The cluster may prove to be the galaxy's richest in terms of RR Lyrae variables.[16] It has ten binary millisecond pulsars, including one (M62B) that is displaying eclipsing behavior from gas streaming off its companion,[17] and one (M62H) with an orbiting exoplanet about three times the mass of Jupiter.[18] There are multiple X-ray sources, including 50 within the half-mass radius.[14] 47 blue straggler candidates have been identified, formed from the merger of two stars in a binary system, and these are preferentially concentrated near the core region.[14]

It is hypothesized that this cluster may be host to an intermediate mass black hole (IMBH) – it is considered well-suited for searching for such an object. A brief study, before 2013, of the proper motion of stars within 17″ of the core did not require an IMBH to explain. However, simulations can not rule out one with a mass of a few thousand M☉ in M62's core. For example, based upon radial velocity measurements within an arcsecond of the core, Kiselev et al. (2008) made the claim of an IMBH in M15, likewise with mass of (1–9)×103 M☉.[12]

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. ^ a b c Di Criscienzo, M.; et al. (February 2006), "RR Lyrae-based calibration of the Globular Cluster Luminosity Function", Monthly Notices of the Royal Astronomical Society, 365 (4): 1357–1366, arXiv:astro-ph/0511128, Bibcode:2006MNRAS.365.1357D, doi:10.1111/j.1365-2966.2005.09819.x, S2CID 17838243.
  3. ^ a b Oliveira, R. A. P.; Ortolani, S.; Barbuy, B.; Kerber, L. O.; Maia, F. F. S.; Bica, E.; Cassisi, S.; Souza, S. O.; Pérez-Villegas, A. (2022). "Precise distances from OGLE-IV member RR Lyrae stars in six bulge globular clusters". Astronomy & Astrophysics. 657: A123. arXiv:2110.13943. Bibcode:2022A&A...657A.123O. doi:10.1051/0004-6361/202141596. S2CID 239998638.
  4. ^ "Messier 62". SEDS Messier Catalog. Retrieved 29 April 2022.
  5. ^ a b c Milone, A. P. (January 2015), "Helium and multiple populations in the massive globular cluster NGC 6266 (M 62)", Monthly Notices of the Royal Astronomical Society, 446 (2): 1672–1684, arXiv:1409.7230, Bibcode:2015MNRAS.446.1672M, doi:10.1093/mnras/stu2198.
  6. ^ a b 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.
  7. ^ distance × sin( diameter_angle / 2 ) = 48 ly. radius
  8. ^ a b Mackey, A. D.; van den Bergh, Sidney (June 2005), "The properties of Galactic globular cluster subsystems", Monthly Notices of the Royal Astronomical Society, 360 (2): 631–645, arXiv:astro-ph/0504142, Bibcode:2005MNRAS.360..631M, doi:10.1111/j.1365-2966.2005.09080.x, S2CID 15709239.
  9. ^ a b 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.
  10. ^ "M 62". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved November 27, 2018.
  11. ^ Thompson, Robert; Thompson, Barbara (2007), Illustrated Guide to Astronomical Wonders: From Novice to Master Observer, DIY science, O'Reilly Media, Inc, p. 332, ISBN 978-0596526856.
  12. ^ a b McNamara, Bernard J.; et al. (February 2012), "A Search for an Intermediate-mass Black Hole in the Core of the Globular Cluster NGC 6266" (PDF), The Astrophysical Journal, 745 (2): 7, Bibcode:2012ApJ...745..175M, doi:10.1088/0004-637X/745/2/175, S2CID 119528711, 175.
  13. ^ McNamara, Bernard J.; McKeever, Jean (November 2011), "The Dynamical Distance, RR Lyrae Absolute Magnitude, and Age of the Globular Cluster NGC 6266", The Astronomical Journal, 142 (5): 4, Bibcode:2011AJ....142..163M, doi:10.1088/0004-6256/142/5/163, 163.
  14. ^ a b c Beccari, G.; et al. (May 2006), "The Dynamical State and Blue Straggler Population of the Globular Cluster NGC 6266 (M62)", The Astronomical Journal, 131 (5): 2551–2560, arXiv:astro-ph/0601187, Bibcode:2006AJ....131.2551B, doi:10.1086/500643, S2CID 8259349.
  15. ^ Baumgardt, H.; Hilker, M. (August 2018), "A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters", Monthly Notices of the Royal Astronomical Society, 478 (2): 1520–1557, arXiv:1804.08359, Bibcode:2018MNRAS.478.1520B, doi:10.1093/mnras/sty1057.
  16. ^ Contreras, R.; et al. (December 2010), "Time-series Photometry of Globular Clusters: M62 (NGC 6266), the Most RR Lyrae-rich Globular Cluster in the Galaxy?", The Astronomical Journal, 140 (6): 1766–1786, arXiv:1009.4206, Bibcode:2010AJ....140.1766C, doi:10.1088/0004-6256/140/6/1766, S2CID 118515997
  17. ^ Cocozza, G.; et al. (June 2008), "A Puzzling Millisecond Pulsar Companion in NGC 6266", The Astrophysical Journal Letters, 679 (2): L105, arXiv:0804.3574, Bibcode:2008ApJ...679L.105C, doi:10.1086/589557, S2CID 16826859.
  18. ^ Vleeschower, L.; Corongiu, A.; et al. (March 2024). "Discoveries and timing of pulsars in M62". Monthly Notices of the Royal Astronomical Society. 530 (2): 1436–1456. arXiv:2403.12137. Bibcode:2024MNRAS.530.1436V. doi:10.1093/mnras/stae816.
  1. ^ In daily rising of this star, whether in day- or nighttime, it will reach 15° above the due southern horizon, at the 90°−30°−15° parallel thus the 45th parallel north, the furthest north for very detailed observation for this object
  2. ^ On June 7
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