NGC 3603 is a nebula situated in the Carina–Sagittarius Arm of the Milky Way around 20,000 light-years away from the Solar System. It is a massive H II region containing a very compact open cluster (probably a super star cluster) HD 97950.
| Molecular cloud | |
|---|---|
| Giant molecular cloud | |
| H II region | |
 NGC 3603 in visible and near infrared light | |
| Observation data: J2000 epoch | |
| Right ascension | 11h 15m 23s[1] |
| Declination | −61° 15′ 00″[1] |
| Distance | 6,900[2] pc |
| Apparent magnitude (V) | 9.1[3] |
| Apparent diameter | 12.0'[3] |
| Constellation | Carina |
| Designations | Gum 38b, Collinder 244 |
Observations
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NGC 3603 was observed by John Herschel on 14 March 1834 during his visit to South Africa, who remarked that it was "a very remarkable object...perhaps a globular cluster". Herschel catalogued it as nebula 3334 in his Results of Astronomical Observations made at the Cape of Good Hope, published in 1847. In 1864 the Royal Society published his General Catalogue of Nebulae and Clusters, where he listed it as number 2354. It was subsequently incorporated into the New General Catalogue as by J. L. E. Dreyer as NGC 3603.[4]
The central cluster was catalogued as the star HD 97950, but has long been recognised as nebulous or multiple.[4] It was also noted for having an unusual emission spectrum and the spectral type was given as Oe in the Henry Draper Catalogue. This was later refined to WN5 + O as the emission was recognised as characteristic of a Wolf–Rayet star.[4] Eventually, the cluster would be resolved and found to contain three of the most massive and most luminous stars known, as well as a number of luminous O class stars and many fainter stars.[5]
Features
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NGC 3603 is the most massive visible cloud of glowing gas and plasma, known as a H II region, in the Milky Way.[6] The central star cluster is the densest concentration of very massive stars known in the galaxy. Strong ultraviolet radiation and stellar winds have cleared the gas and dust, giving an unobscured view of the cluster.[7]
Three prominent Wolf–Rayet stars have been detected within the cluster, all originally unresolved and known as the single star HD 97950. The brightest of the three, HD 97950A1 (or NGC 3603-A1) is actually a pair of Wolf–Rayet stars that orbit around each other once every 3.77 days. The primary is an estimated mass 120 M☉, while its companion is 92 M☉. The star designated HD 97950B is a single star more massive and more luminous than either of the individual members of HD 97950A1. It is 2,880,000 times as luminous as the sun and 132 times as massive.[8]
NGC 3603 is visible in the telescope as a small rather insignificant nebulosity with a yellowish tinge due to the effects of interstellar absorption. In the mid-1960s, optical studies combined with radio astronomical observations showed it to be an extremely strong thermal radio source. Later observations of other galaxies introduced the concept of starburst regions, in some cases whole galaxies, of extremely rapid star formation. NGC 3603 is now considered to be such a region, and it has been compared by some authors to the larger cluster 30 Doradus, in the Large Magellanic Cloud.[9]
Sher 25, the B class supergiant on the outskirts of NGC 3603, is surrounded by ejected material in an hourglass shape similar to that found for the supernova 1987A, and this has aroused intense interest in the future evolution of stars such as Sher 25.[10]
Two of the most luminous young stars known are found within NGC 3603, but outside the central cluster. WR 42e and NGC 3603 MTT 58 both have a spectral type of O2If*/WN6 indicating an extremely massive young star. WR 42e is a possible runaway from a three-body encounter, while MTT 58 appears to still be embedded within its parental cocoon and is in a possible binary with an O3If star.[11]
| MDS number | MTT number | Other names | Spectral type | mV | MV | Temperature
(K) |
Luminosity
(L☉) |
Reference |
|---|---|---|---|---|---|---|---|---|
| 30(A1) | WR 43a (HSW 1) | WN6h/WN6h | 11.18 | -7.8 | 42,000/40,000 | 2,455,000/1,514,000 | [8][12][5] | |
| 31(A2) | HSW 4 | O3V | 12.53 | -6.9 | 46,500 | 1,500,000 | [12][5] | |
| 26(A3) | HSW 5 | O3III | 13.09 | -6.4 | 46,500 | 863,000 | [12][5] | |
| 23(B) | WR 43b (HSW 2) | WN6h | 11.33 | -7.9 | 42,000 | 2,884,000 | [8][5] | |
| 18(C) | WR 43c (HSW 3) | WN6h | 11.89 | -7.3 | 44,000 | 2,239,000 | [8][5] | |
| 49(D1) | O4V | 12.64 | -6.3 | 44,000 | [13][12][5] | |||
| 50(D2) | O5V | 12.74 | -6.2 | 41,000 | [13][12][5] | |||
| 52(D3) | O4V | 13.68 | -5.2 | 44,000 | [13][12][5] | |||
| 19(E) | MMM 104 | O5.5III(f) | 12.83 | -6.1 | 41,000 | 1,038,000 | [14][13][12] | |
| 39(F) | 6 | O5V | 11.86 | -6.1 | 41,000 | [13][12][5] | ||
| 61(G) | 10 | O5V | 12.74 | -6 | 41,000 | [13][12][5] | ||
| 58 | WR 43-2 | O2If*/WN6 | 14.76 | -5.7 | 855,000 | [14][11] | ||
| WR 42e | O2If*/WN6 | 14.53 | -6.3 | 1,300,000 | [14][15] | |||
| 29 | O4V | 13.68 | -5.2 | 44,000 | [13][12][5] | |||
| 27 | O4V | 13.07 | -5.8 | 44,000 | [13][12][5] | |||
| 25 | O4V | 13.01 | -5.9 | 44,000 | [13][12][5] | |||
| 40 | O3V | 13.33 | -5.7 | 46,500 | 718,000 | [14] | ||
| 33 | O5V+OB? | 13.69 | -5.8 | [14][13] | ||||
| 41 | O4V | 14.24 | -5.1 | 44,000 | 217,000 | [14] | ||
| 42 | O3III | 12.99 | -6.1 | 46,500 | 946,000 | [14] | ||
| 37 | O6.5V+? | 14.16 | -5 | [13][5] | ||||
| 38 | O3V | 13.21 | -5.9 | 46,500 | 497,000 | [14] | ||
| 16 | O3V | 13.53 | -5.4 | 46,500 | 655,000 | [14] | ||
| 43 | MMM 111 | O4V | 13.87 | -5 | 44,000 | [13][12][5] | ||
| 14 | O4V | 13.88 | -5 | 44,000 | [13][12][5] | |||
| 59 | O4V | 13.65 | -5.3 | 44,000 | [13][12][5] | |||
| 60 | O4V | 13.6 | -5.3 | 44,000 | [13][12][5] | |||
| 62 | O4V | 13.09 | -5.6 | 44,000 | [13][12][5] | |||
| 58 | MMM 101 | O6.5V((f)) | 14.02 | -5.1 | 37,000 | 238,000 | [14] | |
| 51 | 23 | Sher 56 | O4V(f) | 13.33 | -5.6 | 44,000 | [13][12][5] | |
| 9 | MMM 108 | O5.5V | 13.71 | -5.5 | 39,500 | 377,000 | [14] | |
| 7 | 26 | Sher 64 | O4V | 13.58 | -5.4 | 44,000 | 863,000 | [14][9] |
| 22 | 17 | Sher 57 | O5III(f) | 13.23 | -5.8 | 41,000 | 787,000 | [14][9] |
| 1 | 12 | Sher 23 | OC9.7Ia | 12.7 | -6.3 | 30,250 | 413,000 | [14] |
| 2 | 18 | Sher 22 | O3III(f) | 13.21 | -5.6 | 46,500 | 863,000 | [14] |
| 5 | 13 | Sher 25 | B1Iab | 12.23 | -6.5 | 22,000 | 597,000 | [14] |
| 48 | 14 | Sher 18 | O3.5If | 12.65 | -6.4 | 39,500 | 1,644,000 | [14] |
| 24 | 11 | Sher 47 | O4V | 12.72 | -6.2 | 44,000 | 1,644,000 | [14] |
| 20 | O4V | 13.98 | 44,000 | [13][12][5] | ||||
| 76 | 39 | Sher 54 | O6V | 14.57 | -4.6 | 38,300 | 150,000 | [14] |
| 17 | MMM 116 | O4V | 14.1 | 44,000 | [13][5] | |||
| 36 | O6V | 14.52 | -4.2 | 38,300 | 114,000 | [14] | ||
| 45 | O8V-III | 14.14 | -4.7 | 33,700 | 114,000 | [14] | ||
| 4 | 41 | Sher 49 | O7.5V | 14.67 | -4.6 | 34,800 | 114,000 | [14] |
| 57 | O4V | 13.98 | 44,000 | [13][12][5] | ||||
| 10 | MMM 117 | O6V | 14.17 | -5.1 | 38,300 | 238,000 | [14] | |
| 3 | 32 | Sher 24 | O6V | 14.27 | -5 | 38,300 | 217,000 | [14] |
| 51 | Sher 27 | O7.5V | 15.04 | -4 | 34,800 | 65,000 | [14] | |
| 15 | Sher 63 | O3.5III(f) | 13.41 | -5.6 | 45,000 | 597,000 | [14] | |
| 63 | 40 | Sher 53 | O8.5V | 14.47 | -4.8 | 32,700 | 125,000 | [14] |
| 73 | MMM 102 | O8.5V | 15.32 | -3.9 | 32,700 | 50,000 | [14] | |
| 47 | Sher 21 | O6V((f)) | 14.75 | -4.6 | 38,300 | 150,000 | [14] | |
| 25 | Sher 19 | O3V | 12.61 | -6.2 | 46,500 | 497,000 | [14][9] | |
| MMM 103 | O3V((f)) | 13.09 | -5.7 | 46,500 | 718,000 | [14] | ||
| MMM 109 | O7V | 13.85 | -4.9 | 36,000 | 180,000 | [14] |
References
edit- ^ a b Kharchenko, N. V.; Piskunov, A. E.; Schilbach, E.; Röser, S.; Scholz, R.-D. (2013). "Global survey of star clusters in the Milky Way. II. The catalogue of basic parameters". Astronomy & Astrophysics. 558: A53. arXiv:1308.5822. Bibcode:2013A&A...558A..53K. doi:10.1051/0004-6361/201322302. S2CID 118548517.
- ^ 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.
- ^ a b Sinnott, Roger W. (1988). "The complete new general catalogue and index catalogues of nebulae and star clusters by J. L. E. Dreyer". Cambridge: Sky Publishing Corporation and Cambridge University Press. Bibcode:1988cngc.book.....S.
- ^ a b c Sher, D. (1965). "The Curious History of NGC 3603". Journal of the Royal Astronomical Society of Canada. 59: 67–70. Bibcode:1965JRASC..59...67S.
- ^ a b c d e f g h i j k l m n o p q r s t u v w x 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. arXiv:0710.2882. Bibcode:2008ApJ...675.1319H. doi:10.1086/524650. S2CID 17905999.
- ^ Brandl, B.; Brandner, W.; Grebel, E. K.; Zinnecker, H. (1999). "VLT/ISAAC and HST/WFPC2 observations of NGC 3603". The Messenger. 98: 46. Bibcode:1999Msngr..98...46B.
- ^ Drissen, Laurent; Moffat, Anthony F. J.; Walborn, Nolan R.; Shara, Michael M. (1995). "The Dense Galactic Starburst NGC 3603. I. HST/FOS Spectroscopy of Individual Stars in the Core and the source of Ionization and Kinetic Energy". Astronomical Journal. 110: 2235. Bibcode:1995AJ....110.2235D. doi:10.1086/117684.
- ^ a b c d 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. arXiv:1007.3284. Bibcode:2010MNRAS.408..731C. doi:10.1111/j.1365-2966.2010.17167.x. S2CID 53001712.
- ^ a b c d 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.
- ^ Hendry, M. A.; Smartt, S. J.; Skillman, E. D.; Evans, C. J.; Trundle, C.; Lennon, D. J.; Crowther, P. A.; Hunter, I. (2008). "The blue supergiant Sher 25 and its intriguing hourglass nebula". Monthly Notices of the Royal Astronomical Society. 388 (3): 1127. arXiv:0803.4262. Bibcode:2008MNRAS.388.1127H. doi:10.1111/j.1365-2966.2008.13347.x. S2CID 16802111.
- ^ a b 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.
- ^ a b c d e f g h i j k l m n o p q r s t 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.
- ^ a b c d e f g h i j k l m n o p q r s t 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.
- ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af 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.
- ^ 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–L69. arXiv:1209.1598. Bibcode:2012MNRAS.427L..65R. doi:10.1111/j.1745-3933.2012.01346.x. S2CID 118453639.
External links
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