Arches Cluster

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Arches Cluster
ESO-Arches Cluster.jpg
Arches Cluster in J, H, and K infrared bands (NACO adaptive optics on ESO’s Very Large Telescope)
Observation data (J2000 epoch)
Right ascension 17h 45m 50.5s
Declination –28° 49′ 28″
Distance 25 kly (8.5 kpc)
Physical characteristics
Optically obscured
Associations
Constellation Sagittarius
See also: Open cluster, List of open clusters
Arches Cluster in infrared (NASA/ESA Hubble Space Telescope) Arches Cluster hubble friday 05292015.jpg
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]

Contents

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☉)
B1102bcWN8-9h891,00031,70050 - 6032
F1102adWN8-9h2,000,00033,200101 - 11943
F2102aaWN8-9h
O5-6 Ia+		1,000,00033,50080 [4]
60 [4] 		30
F3102bbWN8-9h1,260,00029,60052 - 6343
F4102alWN7-8h2,000,00036,80066 - 7635
F5102aiWN8-9h891,00032,10031 - 3631
F6102ahWN8-9h2,240,00033,900101 - 11944
F7102ajWN8-9h2,000,00032,90086 - 10244
F8102agWN8-9h1,260,00032,90043 - 5135
F9102aeWN8-9h2,240,00036,600111 - 13138
F10102abO7-8 Ia+891,00032,20055 - 6924
F12102afWN7-8h1,580,00036,90070 - 8231
F14102baWN8-9h1,000,00034,50054 - 6528
F15O6-7 Ia+1,410,00035,60080 - 9732
F16102akWN8-9h794,00032,20046 - 5629
F17102acO5-6 Ia+
F18O4-5 Ia+1,120,00036,90067 - 8226
F20O4-5 Ia794,00038,20047 - 5721
F21O4-6I891,00035,80056 - 7025
F22O4-6I630,00035,80041 - 5321
F23O4-6I630,00035,80041 - 5221
F25 [13] O4-5I851,00040,00019
F26O4-6I707,00039,80045 - 5718
F28O4-6I891,00039,80057 - 7220
F29O4-6I562,00035,70036 - 4520
F32O4-6I707,00040,80047 - 5917
F33O4-6I707,00039,80045 - 5718
F34O4-6I562,00038,10036 - 4618
F35O4-6I501,00033,80034 - 4321
F40O4-5 Ia+562,00039,50057 - 7216

See also

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References

  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. 1 2 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. 1 2 3 4 5 6 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. 1 2 3 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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