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NGC 3603

From Wikipedia, the free encyclopedia
Open cluster in the constellation Carina
NGC 3603
Molecular cloud
Giant molecular cloud
H II region
NGC 3603 in visible and near infrared light
Observation data:J2000epoch
Right ascension11h 15m 23s[1]
Declination−61° 15′ 00″[1]
Distance6,900[2] pc
Apparent magnitude (V)9.1[3]
Apparent diameter12.0'[3]
ConstellationCarina
DesignationsGum 38b,Collinder 244, RCW 57
See also:Lists of nebulae

NGC 3603 is anebula situated in theCarina–Sagittarius Arm of theMilky Way around 20,000light-years away from theSolar System. It is a massiveH II region containing a very compactopen cluster (probably asuper star cluster)HD 97950.

Observations

[edit]
NGC 3603 (left) andNGC 3576 are star formation regions in the southernMilky Way.

NGC 3603 was observed byJohn Herschel on 14 March 1834 during hisvisit to South Africa, who remarked that it was "a very remarkable object...perhaps aglobular cluster". Herschel catalogued it asnebula 3334 in hisResults of Astronomical Observations made at the Cape of Good Hope, published in 1847. In 1864 theRoyal Society published hisGeneral Catalogue of Nebulae and Clusters, where he listed it as number 2354. It was subsequently incorporated into theNew General Catalogue as byJ. L. E. Dreyer as NGC 3603.[4]

The central cluster was catalogued as the starHD 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 theHenry Draper Catalogue. This was later refined to WN5 + O as the emission was recognised as characteristic of aWolf–Rayet star.[4] Eventually, the cluster would be resolved and found to contain three of themost massive andmost luminous stars known, as well as a number of luminous O class stars and many fainter stars.[5]

Features

[edit]
Image of the NGC 3603 region were obtained in three near-IR filter bands (Js, H and Ks) with theISAAC instrument at the ANTU telescope

NGC 3603 is the most massive visible cloud of glowinggas andplasma, known as aH II region, in the Milky Way.[6] The centralstar cluster is the densest concentration of very massive stars known in the galaxy. Strongultravioletradiation andstellar winds have cleared the gas and dust, giving an unobscured view of the cluster.[7]

Three prominentWolf–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 apair 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 designatedHD 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 ofstarburst regions, in some cases wholegalaxies, 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 cluster30 Doradus, in theLarge Magellanic Cloud.[9]

Sher 25, a B class supergiant, has long been thought to be a member of NGC 3603, but turns out to be a foreground star.[10] 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.[11]

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.[12]

Prominent stars
MDS numberMTT numberOther namesSpectral typemVMVTemperature

(K)

Luminosity

(L☉)

Reference
30(A1)WR 43a (HSW 1)WN6h/WN6h11.18-7.842,000/40,0002,455,000/1,514,000[8][13][5]
31(A2)HSW 4O3V12.53-6.946,5001,500,000[13][5]
26(A3)HSW 5O3III13.09-6.446,500863,000[13][5]
23(B)WR 43b (HSW 2)WN6h11.33-7.942,0002,884,000[8][5]
18(C)WR 43c (HSW 3)WN6h11.89-7.344,0002,239,000[8][5]
49(D1)O4V12.64-6.344,000[14][13][5]
50(D2)O5V12.74-6.241,000[14][13][5]
52(D3)O4V13.68-5.244,000[14][13][5]
19(E)MMM 104O5.5III(f)12.83-6.141,0001,038,000[15][14][13]
39(F)6O5V11.86-6.141,000[14][13][5]
61(G)10O5V12.74-641,000[14][13][5]
58WR 43-2O2If*/WN614.76-5.7855,000[15][12]
WR 42eO2If*/WN614.53-6.31,300,000[15][16]
29O4V13.68-5.244,000[14][13][5]
27O4V13.07-5.844,000[14][13][5]
25O4V13.01-5.944,000[14][13][5]
40O3V13.33-5.746,500718,000[15]
33O5V+OB?13.69-5.8[15][14]
41O4V14.24-5.144,000217,000[15]
42O3III12.99-6.146,500946,000[15]
37O6.5V+?14.16-5[14][5]
38O3V13.21-5.946,500497,000[15]
16O3V13.53-5.446,500655,000[15]
43MMM 111O4V13.87-544,000[14][13][5]
14O4V13.88-544,000[14][13][5]
59O4V13.65-5.344,000[14][13][5]
60O4V13.6-5.344,000[14][13][5]
62O4V13.09-5.644,000[14][13][5]
58MMM 101O6.5V((f))14.02-5.137,000238,000[15]
5123Sher 56O4V(f)13.33-5.644,000[14][13][5]
9MMM 108O5.5V13.71-5.539,500377,000[15]
726Sher 64O4V13.58-5.444,000863,000[15][9]
2217Sher 57O5III(f)13.23-5.841,000787,000[15][9]
112Sher 23OC9.7Ia12.7-6.330,250413,000[15]
218Sher 22O3III(f)13.21-5.646,500863,000[15]
4814Sher 18O3.5If12.65-6.439,5001,644,000[15]
2411Sher 47O4V12.72-6.244,0001,644,000[15]
20O4V13.9844,000[14][13][5]
7639Sher 54O6V14.57-4.638,300150,000[15]
17MMM 116O4V14.144,000[14][5]
36O6V14.52-4.238,300114,000[15]
45O8V-III14.14-4.733,700114,000[15]
441Sher 49O7.5V14.67-4.634,800114,000[15]
57O4V13.9844,000[14][13][5]
10MMM 117O6V14.17-5.138,300238,000[15]
332Sher 24O6V14.27-538,300217,000[15]
51Sher 27O7.5V15.04-434,80065,000[15]
15Sher 63O3.5III(f)13.41-5.645,000597,000[15]
6340Sher 53O8.5V14.47-4.832,700125,000[15]
73MMM 102O8.5V15.32-3.932,70050,000[15]
47Sher 21O6V((f))14.75-4.638,300150,000[15]
25Sher 19O3V12.61-6.246,500497,000[15][9]
MMM 103O3V((f))13.09-5.746,500718,000[15]
MMM 109O7V13.85-4.936,000180,000[15]

References

[edit]
  1. ^abKharchenko, 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.
  2. ^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.
  3. ^abSinnott, 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.
  4. ^abcSher, D. (1965). "The Curious History of NGC 3603".Journal of the Royal Astronomical Society of Canada.59:67–70.Bibcode:1965JRASC..59...67S.
  5. ^abcdefghijklmnopqrstuvwxHarayama, 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.
  6. ^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.
  7. ^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.
  8. ^abcdCrowther, 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.
  9. ^abcdMelnick, J.; Tapia, M.; Terlevich, R. (1989). "The galactic giant H II region NGC 3603".Astronomy and Astrophysics.213: 89.Bibcode:1989A&A...213...89M.
  10. ^Weßmayer, D.; Przybilla, N.; Ebenbichler, A.; Aschenbrenner, P.; Butler, K. (2023-09-01)."The blue supergiant Sher 25 revisited in the Gaia era".Astronomy and Astrophysics.677: A175.arXiv:2308.06164.Bibcode:2023A&A...677A.175W.doi:10.1051/0004-6361/202347253.ISSN 0004-6361.
  11. ^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.
  12. ^abRoman-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.
  13. ^abcdefghijklmnopqrstMoffat, 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.
  14. ^abcdefghijklmnopqrstMassey, 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.
  15. ^abcdefghijklmnopqrstuvwxyzaaabacadaeMelena, 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.
  16. ^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.

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