HD 97950

HD 97950, is a multiple star system and part of a super star cluster within the NGC 3603 H II region. It was catalogued as a single star although it was always known to be a compact cluster. It is now resolved into a massive multiple star at the centre of one of the densest clusters in the galaxy.

HD 97950
HST image of the HD 97950 cluster
Observation data (J2000 epoch)
ConstellationCarina
Right ascension11h 15m 07.346s[1]
Declination−61° 15 38.52[1]
Distance25 kly (7.6 kpc[2])
Apparent magnitude (V)9.03[3]
Physical characteristics
Mass19,000[4] M
Radius120"[4]
Notable featuresMain cluster in NGC 3603
Other designationsHD 97950, NGC 3603YC, CD-60°3452, CPD-60° 2732, HIP 54948, MR 38, WR 43

Only the six lettered stars A-F at the core of the cluster are typically referred to as components of HD 97950, while the remaining stars of the cluster and surrounding area are usually numbered as members of NGC 3603. The cluster itself is still called the HD 97950 cluster as well as the NGC 3603 young cluster (NGC 3603YC). There are no other notable groupings of stars in NGC 3603 and the HD 97950 cluster is often loosely referred to as simply NGC 3603.

Members

The core of the cluster, with A1/2/3 at the very centre, and B and C to its left

The main components are designated A1, A2, A3, B, and C, of which A1 and C are known to be spectroscopic binaries. A1a, A1b, and C are all WN6h Wolf–Rayet stars, amongst the most massive and luminous known.[5]

There are several dozen early O class stars (O3 and O4) in the cluster, mostly main sequence stars. There are just a handful of giants and supergiants including: one prominent early B supergiant, Sher 25; a highly luminous O3.5 supergiant, Sher 18; and an interesting carbon-rich O9.7 supergiant, Sher 23.

Over 7,500 stars have been identified in the cluster, with the least massive being smaller than the sun and the most massive over 100 M. Stars less than about 4 M have not yet reached the main sequence.[6]

Prominent stars, ordered by distance from the cluster centre[7]
[8] [7] Other names Spectral type[6] mV[2] MV[7] Temperature (K)[2][9] Luminosity (L)[2]
A1a[5]30WR 43aWN6h11.187.842,0002,500,000
A1b[5]WN6h40,0001,500,000
A231O3V12.536.946,500
A326O3III13.096.446,500
29O4V13.68[7]5.244,000
27O4V13.07[7]5.844,000
25O4V13.01[7]5.944,000
B[5]23WR 43bWN6h11.337.942,0002,900,000
40O3V13.335.746,500780,000
33O5V+OB?[2]13.695.8
41O4V14.245.144,000236,000
42O3III12.996.146,5001,030,000
37O6.5V+?14.165.0
C[5]18WR 43cWN6h11.897.344,0002,200,000
D49O4V12.64[7]6.344,000
50O5V12.74[7]6.241,000
52O4V13.68[7]5.244,000
38O3V13.215.946,500540,000
E19O5.5III(f)12.83[7]6.141,000
F39O5V11.86[7]6.141,000
16O3V13.535.446,500711,000
43O4V13.87[7]5.044,000
14O4V13.88[7]5.044,000
59O4V13.65[7]5.344,000
60O4V13.60[7]5.344,000
62O4V13.095.644,000
58O5.5V13.095.139,500
G61O5V12.74[7]6.041,000
51O4V(f)13.33[7]5.644,000
9O4V13.715.244,000
7O4V13.58[10]5.444,000
22O5III(f)13.23[10]5.841,000
1Sher 23OC9.7Ia[2]12.706.330,250449,000
2Sher 22O3III(f)[2]13.215.646,500863,000
5Sher 25B1Iab[2]12.236.522,000649,000
48Sher 18O3.5If[2]12.656.439,5001,790,000
24O4V[2]12.726.244,000
MTT 25O3V[2]12.61[10]6.246,500
20O4V13.98[7]44,000
17O4V14.1044,000
45O8V-III14.144.7[2]33,750124,000
57O4V13.98[7]44,000
10O4V14.175.1[2]44,000258,000
MTT 58[11] O2If*/WN614.765.7855,000
WR 42e[12] O2If*/WN614.536.31,300,000

The number of WNh and early O stars exceeds any known cluster in the galaxy. The Quintuplet and Arches clusters each have around 20 young massive stars and may have masses comparable to the HD 97950 cluster, but they contain no O3 or WN6 stars at all. The rich red supergiant clusters such as Westerlund 1 are too old to contain such stars, although may be even more massive. R136 in the Large Magellanic Cloud contains stars more massive than any in HD 97950, as well as large numbers of early O stars, and the cluster as a whole may be ten times as massive.[13]

It has been proposed that the star WR 42e, found 2.6 arcmin from the centre of the cluster, and J1117−6120, an O6V runaway a quarter of a degree away on the other side of the cluster, were both ejected in a 3-body interaction. Two of the stars then merged to form the extremely massive and luminous WR 42e.[14]

Mass

The HD 97950 cluster has a total photometric mass of 10,000–16,000 M,[6] and a dynamical mass of 19,000 M.[4] The constituent stars have apparently dynamical segregated with the more massive stars predominantly found at the centre of the cluster.[4] The centre of the cluster has a density of 60,000 M pc−3, ten times the Orion Nebula and comparable to R136.[6]

Age

Fitting the main sequence, and pre-main sequence gives a cluster age of 1 million years or less. There is no clear main sequence turnoff, although the most massive stars are modelled best with an age of 2.5 million years, but are compatible with an age around one million years.[6] A small number of stars, for example Sher 25, apparently show much greater ages and it has been suggested that there is either ongoing star formation, or an earlier burst of star formation.[2] Other studies have estimated ages up to 2 million years, but the existence of the most massive and luminous stars provide a hard upper limit of 2.5 million years on the possible age.[15]

This is one of the youngest clusters in the galaxy. The Arches Cluster is around 2.5 million years old, the Quintuplet cluster nearly double that, and the various red supergiant clusters obviously even older. Even R136 is thought to be near to 2 million years old. Trumpler 14 in the Carina Nebula is thought to be as little as 300,000 - 500,000 years old, but is much less massive.[13]

References

  1. Zacharias, N.; et al. (2003). "The Second U.S. Naval Observatory CCD Astrograph Catalog (UCAC2)". CDS/ADC Collection of Electronic Catalogues. 1289. Bibcode:2003yCat.1289....0Z.
  2. Melena, Nicholas W.; Massey, Philip; Morrell, Nidia I.; Zangari, Amanda M. (2008). "The Massive Star Content of NGC 3603". The Astronomical Journal. 135 (3): 878–891. arXiv:0712.2621. Bibcode:2008AJ....135..878M. doi:10.1088/0004-6256/135/3/878. S2CID 16765414.
  3. Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  4. Pang, Xiaoying; Grebel, Eva K.; Allison, Richard J.; Goodwin, Simon P.; Altmann, Martin; Harbeck, Daniel; Moffat, Anthony F. J.; Drissen, Laurent (2013). "On the Origin of Mass Segregation in NGC 3603". The Astrophysical Journal. 764 (1): 73. arXiv:1212.4566. Bibcode:2013ApJ...764...73P. doi:10.1088/0004-637X/764/1/73. S2CID 119199840.
  5. Crowther, P. A.; Schnurr, O.; Hirschi, R.; Yusof, N.; Parker, R. J.; Goodwin, S. P.; Kassim, H. A. (2010). "The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M stellar mass limit". Monthly Notices of the Royal Astronomical Society. 408 (2): 731–751. arXiv:1007.3284. Bibcode:2010MNRAS.408..731C. doi:10.1111/j.1365-2966.2010.17167.x. S2CID 53001712.
  6. Harayama, Y.; Eisenhauer, F.; Martins, F. (2008). "The Initial Mass Function of the Massive Star-forming Region NGC 3603 from Near-Infrared Adaptive Optics Observations". The Astrophysical Journal. 675 (2): 1319–1342. arXiv:0710.2882. Bibcode:2008ApJ...675.1319H. doi:10.1086/524650. S2CID 17905999.
  7. Moffat, Anthony F. J.; Drissen, Laurent; Shara, Michael M. (1994). "NGC 3603 and its Wolf-Rayet stars: Galactic clone of R136 at the core of 30 Doradus, but without the massive surrounding cluster halo". Astrophysical Journal. 436: 183. Bibcode:1994ApJ...436..183M. doi:10.1086/174891.
  8. Van Den Bos, W. H. (1928). "Another nebulous multiple star". Bulletin of the Astronomical Institutes of the Netherlands. 4: 261. Bibcode:1928BAN.....4..261V.
  9. Massey, Philip; Puls, Joachim; Pauldrach, A. W. A.; Bresolin, Fabio; Kudritzki, Rolf P.; Simon, Theodore (2005). "The Physical Properties and Effective Temperature Scale of O-Type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars and Results from the Complete Sample". The Astrophysical Journal. 627 (1): 477–519. arXiv:astro-ph/0503464. Bibcode:2005ApJ...627..477M. doi:10.1086/430417. S2CID 18172086.
  10. Melnick, J.; Tapia, M.; Terlevich, R. (1989). "The galactic giant H II region NGC 3603". Astronomy and Astrophysics. 213: 89. Bibcode:1989A&A...213...89M.
  11. Roman-Lopes, A. (2013). "An O2 If*/WN6 star caught in the act in a compact H II region in the starburst cluster NGC 3603". Monthly Notices of the Royal Astronomical Society. 433 (1): 712–718. arXiv:1305.0851. Bibcode:2013MNRAS.433..712R. doi:10.1093/mnras/stt762. S2CID 118367798.
  12. Roman-Lopes, A. (2012). "A Galactic O2 If*/WN6 star possibly ejected from its birthplace in NGC 3603". Monthly Notices of the Royal Astronomical Society: Letters. 427 (1): L65. arXiv:1209.1598. Bibcode:2012MNRAS.427L..65R. doi:10.1111/j.1745-3933.2012.01346.x. S2CID 118453639.
  13. Portegies Zwart, Simon F.; McMillan, Stephen L. W.; Gieles, Mark (2010). "Young Massive Star Clusters". Annual Review of Astronomy and Astrophysics. 48: 431–493. arXiv:1002.1961. Bibcode:2010ARA&A..48..431P. doi:10.1146/annurev-astro-081309-130834. S2CID 119207843.
  14. Gvaramadze, V. V.; Kniazev, A. V.; Chené, A. -N.; Schnurr, O. (2012). "Two massive stars possibly ejected from NGC 3603 via a three-body encounter". Monthly Notices of the Royal Astronomical Society: Letters. 430: L20–L24. arXiv:1211.5926. Bibcode:2013MNRAS.430L..20G. doi:10.1093/mnrasl/sls041. S2CID 56103308.
  15. Kudryavtseva, Natalia; Brandner, Wolfgang; Gennaro, Mario; Rochau, Boyke; Stolte, Andrea; Andersen, Morten; Da Rio, Nicola; Henning, Thomas; Tognelli, Emanuele; Hogg, David; Clark, Simon; Waters, Rens (2012). "Instantaneous Starburst of the Massive Clusters Westerlund 1 and NGC 3603 YC". The Astrophysical Journal Letters. 750 (2): L44. arXiv:1204.5481. Bibcode:2012ApJ...750L..44K. doi:10.1088/2041-8205/750/2/L44. S2CID 5520745.

Further reading

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