NGC 1866
| NGC 1866 | |
|---|---|
 NGC 1866 taken by Hubble Space Telescope[1] | |
| Observation data (J2000 epoch) | |
| Constellation | Dorado |
| Right ascension | 05h 13m 38.92s[2] |
| Declination | −65° 27′ 52.75″[2] |
| Distance | 161.7 kly (49.59 kpc)[3] |
| Apparent magnitude (V) | 9.73 |
| Apparent dimensions (V) | 5.50′ × 5.50′[4] |
| Physical characteristics | |
| Mass | (1.35±0.25)×105[5] M☉ |
| Metallicity | [Fe/H] = −0.43±0.01[6] dex |
| Estimated age | 190+20 −10 Ma[3] |
| Other designations | ESO 85-52, KMHK 664, LW 163, SL63 319, NGC 1866[7] |
NGC 1866 is a young[3] globular cluster of stars near the northern edge of the Large Magellanic Cloud (LMC),[8] located in the southern constellation of Dorado. NGC 1866 was discovered August 3, 1826 by British astronomer James Dunlop.[9] The LMC is located at a distance of 161.7 thousand light-years (49.59 kpc) from the Sun, while NGC 1866 is orbiting 13.0 ± 1.7 thousand light-years (3.98 ± 0.53 kpc) from the LMC core.[3]
An isochrone fit to the cluster members yields an estimated age of approximately 190 million years.[3] Of the objects in the LMC that formed over the last three billion years, NGC 1866 may be one of the most massive, having an estimated 135,000 times the mass of the Sun.[5] The cluster has a core radius of 11.1 ly (3.39 pc) and a 90% light radius of 47.6 ly (14.60 pc).[2]
A. D. Thackeray began a search of NGC 1866 in 1948, finding some Cepheid variables.[8] An independent study by H. Shapley and V. M. Nail in 1951 found 29 variables, of which 23 are Classical Cepheids with a notable lack of older type II Cepheids.[10] Thackeray found both red and blue giants in the cluster, and the integrated color index of the cluster was very blue, suggesting a young age.[8] The rich abundance of cepheids in this cluster, all at the same distance from the Earth, has made them a subject for frequent study.[11]
One of the findings from studying young globular clusters in the Magellenic Clouds is that they exhibit bimodal main sequences on their color-magnitude diagrams. An investigation of NGC 1866 with the Hubble Space Telescope shows both a similar split main sequence and an extended main sequence turnoff (eMSTO).[12] Spectroscopc study of eMSTO stars shows two populations: one older, rapidly rotating and the other younger and rotating more slowly.[13] A study of Cepheid variables in NGC 1866 supports this dichotomy.[14] The cluster contains a high abundance of fast rotating Be stars.[15]
In 2025, a planetary nebula was discovered near the center of the cluster. Its size and expansion rate indicate an age of 18,000 years. The blue central star is visible, and the progenitor likely had an initial mass of 3.9 M☉.[16]
References
- ↑ "Different generations". www.spacetelescope.org. Retrieved 20 November 2018.
- 1 2 3 Werchan, Felicia; Zaritsky, Dennis (2011). "The Star Clusters of the Large Magellanic Cloud: Structural Parameters". The Astronomical Journal. 142 (2): 48. arXiv:1105.1769. Bibcode:2011AJ....142...48W. doi:10.1088/0004-6256/142/2/48. S2CID 118331608.
- 1 2 3 4 5 Niederhofer, F.; et al. (January 2026). "Hubble Space Telescope proper motions of Large Magellanic Cloud star clusters: II. Kinematic structure of young and intermediate-age clusters". Astronomy & Astrophysics. 705. id. A94. arXiv:2511.14351. Bibcode:2026A&A...705A..94N. doi:10.1051/0004-6361/202557397.
- ↑ Bica, E.; et al. (September 2008). "A general catalogue of extended objects in the Magellanic System". Monthly Notices of the Royal Astronomical Society. 389 (2): 678−690. arXiv:0806.3049. Bibcode:2008MNRAS.389..678B. doi:10.1111/j.1365-2966.2008.13612.x. S2CID 1867090.
- 1 2 Fischer, Philippe; et al. (June 2003). "Dynamics of the Young LMC Clusters NGC 1866". The Astronomical Journal. 125 (6): 3111–3121. arXiv:astro-ph/0302458. Bibcode:2003AJ....125.3111B. doi:10.1086/374946.
- ↑ Mucciarelli, A.; et al. (May 2011). "NGC 1866: a milestone for understanding the chemical evolution of stellar populations in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 413 (2): 837–851. arXiv:1012.1476. Bibcode:2011MNRAS.413..837M. doi:10.1111/j.1365-2966.2010.18167.x.
- ↑ "NGC 1866". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-11-21.
- 1 2 3 Arp, Halton; Thackeray, A. D. (July 1967). "The Star Cluster NGC 1866 and its Cepheids". Astrophysical Journal. 149: 73. Bibcode:1967ApJ...149...73A. doi:10.1086/149232.
- ↑ Seligman, Courtney. "NGC 1866". Celestial Atlas. Retrieved 21 November 2018.
- ↑ Shapley, H.; McKibben Nail, V. (February 1951). "NGC 1866 and the Magellanic Cloud variables". Astronomical Journal. 55: 249–251. Bibcode:1951AJ.....55..249S. doi:10.1086/106476.
- ↑ Musella, I.; et al. (April 2016). "The Cepheids of NGC 1866: a precise benchmark for the extragalactic distance scale and stellar evolution from modern UBVI photometry". Monthly Notices of the Royal Astronomical Society. 457 (3): 3084–3095. arXiv:1601.06628. Bibcode:2016MNRAS.457.3084M. doi:10.1093/mnras/stw151.
- ↑ Milone, A. P.; et al. (March 2017). "Multiple stellar populations in Magellanic Cloud clusters - V. The split main sequence of the young cluster NGC 1866". Monthly Notices of the Royal Astronomical Society. 465 (4): 4363–4374. arXiv:1611.06725. Bibcode:2017MNRAS.465.4363M. doi:10.1093/mnras/stw2965.
- ↑ Dupree, A. K.; et al. (September 2017). "NGC 1866: First Spectroscopic Detection of Fast-rotating Stars in a Young LMC Cluster". The Astrophysical Journal Letters. 846 (1). id. L1. arXiv:1708.03386. Bibcode:2017ApJ...846L...1D. doi:10.3847/2041-8213/aa85dd.
- ↑ Costa, Guglielmo; et al. (November 2019). "Multiple stellar populations in NGC 1866. New clues from Cepheids and colour-magnitude diagram". Astronomy & Astrophysics. 631. id. A128. arXiv:1909.01907. Bibcode:2019A&A...631A.128C. doi:10.1051/0004-6361/201936409.
- ↑ Cristofari, Paul I.; et al. (October 2025). "Spectroscopic Confirmation: Fast Rotators in the Young Clusters NGC 1856 and NGC 1953". The Astrophysical Journal. 991 (2). id. 165. arXiv:2508.02599. Bibcode:2025ApJ...991..165C. doi:10.3847/1538-4357/adfb5e.
- ↑ Bond, Howard E.; et al. (November 2025). "Serendipitous Discovery of a Faint Planetary Nebula in the Massive Young LMC Cluster NGC 1866". Publications of the Astronomical Society of the Pacific. 137 (11). id. 114202. arXiv:2510.16630. Bibcode:2025PASP..137k4202B. doi:10.1088/1538-3873/ae1664.
Further reading
- Lemasle, B.; et al. (December 2017). "Detailed chemical composition of classical Cepheids in the LMC cluster NGC 1866 and in the field of the SMC". Astronomy & Astrophysics. 608. id. A85. arXiv:1709.03083. Bibcode:2017A&A...608A..85L. doi:10.1051/0004-6361/201731370.
- Brocato, E.; et al. (October 2004). "Pulsational Evidence for Mass Loss in NGC 1866 Cepheids". The Astronomical Journal. 128 (4): 1597–1605. Bibcode:2004AJ....128.1597B. doi:10.1086/423917.
- Brocato, E.; et al. (June 2003). "The Luminosity Function of the Large Magellanic Cloud Globular Cluster NGC 1866". The Astronomical Journal. 125 (6): 3111–3121. arXiv:astro-ph/0302458. Bibcode:2003AJ....125.3111B. doi:10.1086/374946.
- Salaris, M.; et al. (May 2003). "The Distance to the Large Magellanic Cloud Cluster NGC 1866 and the Surrounding Field". The Astrophysical Journal. 588 (2): 801–804. arXiv:astro-ph/0301532. Bibcode:2003ApJ...588..801S. doi:10.1086/374260.
- Barmina, R.; et al. (April 2002). "NGC 1866: A workbench for stellar evolution". Astrnomy and Astrophysics. 385: 847–861. arXiv:astro-ph/0202128. Bibcode:2002A&A...385..847B. doi:10.1051/0004-6361:20020197.
- Walker, A. R.; et al. (October 2001). "The Distance of the Large Magellanic Cloud Cluster NGC 1866". The Astrophysical Journal. 560 (2): L139–L142. arXiv:astro-ph/0109147. Bibcode:2001ApJ...560L.139W. doi:10.1086/324224.
- Testa, Vincenzo; et al. (December 1999). "The Large Magellanic Cloud Globular Cluster NGC 1866: New Data, New Models, New Analysis". The Astronomical Journal. 118 (6): 2839–2864. arXiv:astro-ph/9909417. Bibcode:1999AJ....118.2839T. doi:10.1086/301148.
- Stappers, B. W.; et al. (March 1997). "The Star-Formation History in the Vicinity of NGC 1866 in the Large Magellanic Cloud". Publications of the Astronomical Society of the Pacific. 109: 292–296. Bibcode:1997PASP..109..292S. doi:10.1086/133888.
- Welch, Douglas L.; Stetson, Peter B. (May 1993). "Robust Variable Star Detection Techniques Suitable for Automated searches: New Results for NGC 1866". Astronomical Journal. 105: 1813. Bibcode:1993AJ....105.1813W. doi:10.1086/116556.
- Fischer, Philippe; et al. (March 1992). "Dynamics of the Young LMC Clusters NGC 1866". Astronomical Journal. 103: 857. Bibcode:1992AJ....103..857F. doi:10.1086/116107.
- Welch, Douglas L.; et al. (February 1991). "The Variable Stars of NGC 1866". Astronomical Journal. 101: 490. Bibcode:1991AJ....101..490W. doi:10.1086/115700.
- Brocato, E.; et al. (September 1989). "CCD Photometry of the Large Magellanic Cloud Cluster NGC 1866: Observational Results". Astrophysical Journal Supplement. 71: 25. Bibcode:1989ApJS...71...25B. doi:10.1086/191363.
- Chiosi, C.; et al. (July 1989). "Globular clusters in the Large Magellanic Cloud : NGC 1866, a test for convective overshoot". Astronomy and Astrophysics. 219: 167–191. Bibcode:1989A&A...219..167C.
- Meyer-Hofmeister, E. (June 1969). "A theoretical Hertzsprung-Russell-diagram for the star cluster NGC 1866". Astronomy and Astrophysics. 2: 143–150. Bibcode:1969A&A.....2..143M.
- Arp, Halton (July 1967). "Analysis of Stellar Content and Cepheid Evolution in NGC 1866". Astrophysical Journal. 149: 91. Bibcode:1967ApJ...149...91A. doi:10.1086/149233.
External links
Media related to NGC 1866 at Wikimedia Commons
