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Arches Cluster

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Arches Cluster
Arches Cluster in J, H, and K infrared bands (NACO adaptive optics on ESO’s Very Large Telescope)
Observation data (J2000 epoch)
Right ascension17h 45m 50.5s
Declination–28° 49′ 28″
Distance25 kly (8.5 kpc)
Physical characteristics
Estimated age2.5 million years
Optically obscured
Associations
ConstellationSagittarius
See also: Open cluster, List of open clusters
Arches Cluster in infrared (NASA/ESA Hubble Space Telescope)

The Arches Cluster is the densest known star cluster in the Milky Way, about 100 light-years from its center in the constellation Sagittarius (The Archer), 25,000 light-years from Earth. Its discovery was reported by Nagata et al. in 1995,[1] and independently by Cotera et al. in 1996.[2] Due to extremely heavy optical extinction by dust in this region, the cluster is obscured in the visual bands, and is observed in the X-ray, infrared and radio bands. It contains approximately 135 young, very hot stars that are many times larger and more massive than the Sun, plus many thousands of less massive stars.[3]

The star cluster is estimated to be around two and a half million years old.[3][4] Although larger and denser than the nearby Quintuplet Cluster, it appears to be slightly younger. Only stars earlier and more massive than O5 have evolved away from the main sequence while the Quintuplet Cluster includes a number of hot supergiants as well as a red supergiant and three luminous blue variables.[4]

The most prominent members of the Arches Cluster are hot emission line stars: thirteen Wolf–Rayet stars, all massive hydrogen-rich types; and eight class O hypergiants. One of these is an eclipsing binary with a Wolf–Rayet primary and a class O supergiant secondary. X-ray emission from the cluster suggests that many other members are also in close binary systems with two hot luminous members, but there is little evidence of the evolution of these stars being affected by binary mass exchange. The spectral classes and their properties merge smoothly from the main sequence to normal class O giants and supergiants, to class O hypergiants, to the presumed most evolved Wolf–Rayets. One star is intermediate between WN8–9h and O4–6 Ia . There are no cooler evolved stars.[4]

Work by Donald Figer, an astronomer at the Rochester Institute of Technology suggests that 150 solar masses (M☉) is the upper limit of stellar mass in the current era of the universe. He used the Hubble Space Telescope to observe about a thousand stars in the Arches cluster and found no stars over that limit despite a statistical expectation that there should be several.[5] However, later research demonstrated a very high sensitivity of the calculated star masses upon the extinction laws used for mass derivation, which can affect the upper mass limit by about 30% using different extinction laws[6] (possibly from 150 M☉ to about 100 M☉). The limit of 150 solar masses was previously deduced by Carsten Weidner & Pavel Kroupa[7] using observations of the cluster R136.

Prominent stars
B=Blum[8] F=Figer[9] WR#[10] Spectral type[4] Luminosity[11] (L☉) Temperature[11] (effective, K) Mass[12] (M☉) Radius[11] (R☉)
B1 102bc WN8–9h 891,000 31,700 50–60 32
F1 102ad WN8–9h 2,000,000 33,200 101–119 43
F2 102aa WN8–9h
O5–6 Ia 		1,000,000 33,500 80[4]
60[4]		 30
F3 102bb WN8–9h 1,260,000 29,600 52–63 43
F4 102al WN7–8h 2,000,000 36,800 66–76 35
F5 102ai WN8–9h 891,000 32,100 31–36 31
F6 102ah WN8–9h 2,240,000 33,900 101–119 44
F7 102aj WN8–9h 2,000,000 32,900 86–102 44
F8 102ag WN8–9h 1,260,000 32,900 43–51 35
F9 102ae WN8–9h 2,240,000 36,600 111–131 38
F10 102ab O7–8 Ia 891,000 32,200 55–69 24
F12 102af WN7–8h 1,580,000 36,900 70–82 31
F14 102ba WN8–9h 1,000,000 34,500 54–65 28
F15 O6–7 Ia 1,410,000 35,600 80–97 32
F16 102ak WN8–9h 794,000 32,200 46–56 29
F17 102ac O5–6 Ia
F18 O4–5 Ia 1,120,000 36,900 67–82 26
F20 O4–5 Ia 794,000 38,200 47–57 21
F21 O4–6I 891,000 35,800 56–70 25
F22 O4–6I 630,000 35,800 41–53 21
F23 O4–6I 630,000 35,800 41–52 21
F25[13] O4–5I 851,000 40,000 19
F26 O4–6I 707,000 39,800 45–57 18
F28 O4–6I 891,000 39,800 57–72 20
F29 O4–6I 562,000 35,700 36–45 20
F32 O4–6I 707,000 40,800 47–59 17
F33 O4–6I 707,000 39,800 45–57 18
F34 O4–6I 562,000 38,100 36–46 18
F35 O4–6I 501,000 33,800 34–43 21
F40 O4–5 Ia 562,000 39,500 57–72 16

See also

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References

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  1. ^ Nagata, T.; Woodward, C.; Shure, M.; Kobayashi, N. (April 1995). "Object 17: Another cluster of emission-line stars near the Galactic center". Astronomical Journal. 109 (4): 1676. Bibcode:1995AJ....109.1676N. doi:10.1086/117395.
  2. ^ Cotera, A.; Erickson, E.; Colgan, S.; Simpson, J.; Allen, D.; Burton, M. (April 1996). "The discovery of hot stars near the Galactic center thermal radio filaments". Astrophysical Journal. 461 (750): 750. Bibcode:1996ApJ...461..750C. doi:10.1086/177099.
  3. ^ a b Espinoza, P.; Selman, F. J.; Melnick, J. (July 2009). "The massive star initial mass function of the Arches cluster". Astronomy and Astrophysics. 504 (2): 563–583. arXiv:0903.2222. Bibcode:2009A&A...501..563E. doi:10.1051/0004-6361/20078597. S2CID 14412034.
  4. ^ a b c d e f Clark, J. S; Lohr, M. E; Najarro, F; Dong, H; Martins, F (2018). "The Arches cluster revisited: I. Data presentation and stellar census". Astronomy & Astrophysics. A65: 617. arXiv:1803.09567. Bibcode:2018A&A...617A..65C. doi:10.1051/0004-6361/201832826. S2CID 53362252.
  5. ^ Figer (2005). "An upper limit to the masses of stars". Nature. 434 (7030): 192–194. arXiv:astro-ph/0503193. Bibcode:2005Natur.434..192F. doi:10.1038/nature03293. ISSN 0028-0836. PMID 15758993. S2CID 4417561.
  6. ^ Habibi, M.; Stolte, A.; Brandner, W.; Hußmann, B.; Motohara, K. (August 2013). "The Arches cluster out to its tidal radius: dynamical mass segregation and the effect of the extinction law on the stellar mass function". Astronomy and Astrophysics. 556 (A26): A26. arXiv:1212.3355. Bibcode:2013A&A...556A..26H. doi:10.1051/0004-6361/201220556. S2CID 118475820.
  7. ^ Weidner, Carsten; Kroupa, Pavel (2005). "Evidence for a fundamental stellar upper mass limit from clustered star formation". MNRAS. 348 (1): 187–191. arXiv:astro-ph/0310860. Bibcode:2004MNRAS.348..187W. doi:10.1111/j.1365-2966.2004.07340.x.
  8. ^ Blum, R. D.; Schaerer, D.; Pasquali, A.; Heydari-Malayeri, M.; Conti, P. S.; Schmutz, W. (2001). "2 Micron Narrowband Adaptive Optics Imaging in the Arches Cluster" (PDF). The Astronomical Journal. 122 (4): 1875. arXiv:astro-ph/0106496. Bibcode:2001AJ....122.1875B. doi:10.1086/323096. S2CID 2957272.
  9. ^ Figer, D. F.; Najarro, F.; Gilmore, D.; Morris, M.; Kim, S. S.; Serabyn, E.; McLean, I. S.; Gilbert, A. M.; Graham, J. R.; Larkin, J. E.; Levenson, N. A.; Teplitz, H. I. (2002). "Massive Stars in the Arches Cluster". The Astrophysical Journal. 581 (1): 258–275. arXiv:astro-ph/0208145. Bibcode:2002ApJ...581..258F. doi:10.1086/344154. S2CID 119002004.
  10. ^ Van Der Hucht, K. A. (2006). "New Galactic Wolf–Rayet stars, and candidates. An annex to the VIIth Catalogue of Galactic Wolf–Rayet Stars". Astronomy and Astrophysics. 458 (2): 453. arXiv:astro-ph/0609008. Bibcode:2006A&A...458..453V. doi:10.1051/0004-6361:20065819. S2CID 119104786.
  11. ^ a b c Martins, F.; Hillier, D. J.; Paumard, T.; Eisenhauer, F.; Ott, T.; Genzel, R. (2008). "The most massive stars in the Arches cluster". Astronomy and Astrophysics. 478 (1): 219–233. arXiv:0711.0657. Bibcode:2008A&A...478..219M. doi:10.1051/0004-6361:20078469. S2CID 7509876.
  12. ^ Gräfener, G.; Vink, J. S.; de Koter, A.; Langer, N. (2011). "The Eddington factor as the key to understand the winds of the most massive stars". Astronomy & Astrophysics. 535: A56. arXiv:1106.5361. Bibcode:2011A&A...535A..56G. doi:10.1051/0004-6361/201116701. ISSN 0004-6361. S2CID 59396651.
  13. ^ Clark, J. S.; Lohr, M. E.; Najarro, F.; Patrick, L. R.; Ritchie, B. W. (2023). "The Arches cluster revisited: IV. Observational constraints on the binary properties of very massive stars". Monthly Notices of the Royal Astronomical Society. 521 (3): 4473–4489. arXiv:2302.04008. Bibcode:2023MNRAS.521.4473C. doi:10.1093/mnras/stad449.
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