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Messier 36

Messier 36
Open cluster M36 seen in infrared light., courtesy of: [1]
Observation data (J2000.0 epoch)
Right ascension05h 36m 18.0s[1]
Declination+34° 08′ 24″[1]
Distance4.34 ± 0.87 kly (1.330 ± 0.266 kpc)[1]
Apparent magnitude (V)6.3
Apparent dimensions (V)12'[2]
Physical characteristics
Mass746+606
−334 M☉[3] M☉
Radius7 ly
Estimated age25.1 Myr[1]
Other designationsC 0532+341, M 36, NGC 1960, OCl 445[4]
Associations
ConstellationAuriga
See also: Open cluster, List of open clusters

Messier 36 or M36, also known as NGC 1960 or the Pinwheel Cluster, is an open cluster of stars in the somewhat northern Auriga constellation. It was discovered by Giovanni Batista Hodierna before 1654, who described it as a nebulous patch.[5] The cluster was independently re-discovered by Guillaume Le Gentil in 1749, then Charles Messier observed it in 1764 and added it to his catalogue.[6] It is about 1,330 pc (4,340 light years) away from Earth.[1] The cluster is very similar to the Pleiades cluster (M45), and if as far away it would be of similar apparent magnitude.[7]

This cluster has an angular diameter of 10′[8] and a core radius of 3.2′.[9] It has a mass of roughly 746 M☉ and a linear tidal radius of 10.6 ± 1.6 parsecs (34.6 ± 5.2 ly).[3] Based upon photometry, the age of the cluster has been estimated by Wu et al. (2009) as 25.1 Myr[1] and 26.3+3.2
−5.2 Myr by Bell et al. (2013). The luminosity of the stars that have not yet depleted their lithium implies an age of 22±4 Myr, in good agreement with these older estimates.[9]

M36 includes ten stars with a visual magnitude brighter than 10,[9] and 178 down to magnitude 14.[8] 38 members display an infrared excess, with one being particularly high.[10] There is one candidate B-type variable star, of 9th magnitude.[11]

A 2020 study of the variable stars in the cluster estimated a new closer distance of 3,800 light years from Earth.[12]

The YSO Holoea in M36 and the outflow at different wavelengths.

A young stellar object with an outflow, associated with the infrared source IRAS 05327+3404 was discovered in optical observations of M36. The outflow is nicknamed "Holoea", Hawaiian for "flowing gas". Despite appearing close to M36 it is probably not a part of M36 .It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.[13]

Map

Map

See also

References

  1. ^ a b c d e f Wu, Zhen-Yu; et al. (November 2009), "The orbits of open clusters in the Galaxy", Monthly Notices of the Royal Astronomical Society, 399 (4): 2146–2164, arXiv:0909.3737, Bibcode:2009MNRAS.399.2146W, doi:10.1111/j.1365-2966.2009.15416.x, S2CID 6066790.
  2. ^ "Messier 36". SEDS Messier Catalog. Retrieved 23 July 2024.
  3. ^ a b Piskunov, A. E.; et al. (January 2008), "Tidal radii and masses of open clusters", Astronomy and Astrophysics, 477 (1): 165–172, Bibcode:2008A&A...477..165P, doi:10.1051/0004-6361:20078525.
  4. ^ "M 36". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved November 22, 2018.
  5. ^ Fodera-Serio, G.; et al. (February 1985), "Hodierna's Observations of Nebulae and his Cosmology", Journal for the History of Astronomy, 16 (1): 1, Bibcode:1985JHA....16....1F, doi:10.1177/002182868501600101.
  6. ^ Stoyan, Ronald; et al. (2008), Atlas of the Messier Objects: Highlights of the Deep Sky, translated by Schroeder, Klaus-Peter, Cambridge University Press, pp. 530–533, ISBN 978-1139473118
  7. ^ Frommert, Hartmut; Kronberg, Christine (August 25, 2007), "Messier 36", The Messier Catalog, Students for the Exploration and Development of Space (SEDS), retrieved 2018-11-24.
  8. ^ a b Sanner, J.; et al. (May 2000), "Photometric and kinematic studies of open star clusters. II. NGC 1960 (M 36) and NGC 2194", Astronomy and Astrophysics, 357: 471–483, arXiv:astro-ph/0003327, Bibcode:2000A&A...357..471S.
  9. ^ a b c Jeffries, R. D.; et al. (September 2013), "A lithium depletion boundary age of 22 Myr for NGC 1960", Monthly Notices of the Royal Astronomical Society, 434 (3): 2438–2450, arXiv:1306.6339, Bibcode:2013MNRAS.434.2438J, doi:10.1093/mnras/stt1180.
  10. ^ Smith, R.; Jeffries, R. D. (March 2012), "Dust discs around intermediate-mass and Sun-like stars in the 16 Myr old NGC 1960 open cluster", Monthly Notices of the Royal Astronomical Society, 420 (4): 2884–2898, arXiv:1110.4219, Bibcode:2012MNRAS.420.2884S, doi:10.1111/j.1365-2966.2011.20032.x, S2CID 119188688.
  11. ^ Delgado, A. J.; et al. (October 1984), "Search for B-Type Variable Stars in Open Clusters", Information Bulletin on Variable Stars, 2603: 1, Bibcode:1984IBVS.2603....1D.
  12. ^ Nowakowski, Tomasz (21 January 2023). "Astronomers perform a comprehensive study of young open cluster NGC 1960". Phys.org. Retrieved 28 June 2023.
  13. ^ Morata, O.; Kuan, Y. -J.; Ho, P. T. P.; Huang, H. -C.; Magnier, E. A.; Zhao-Geisler, R. (2013-09-01). "Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36". The Astronomical Journal. 146 (3): 49. arXiv:1305.6550. Bibcode:2013AJ....146...49M. doi:10.1088/0004-6256/146/3/49. ISSN 0004-6256.
Quelle: https://en.wikipedia.org/wiki/NGC_1960