Carina Nebula

Carina Nebula
Emission nebula

The Carina Nebula. Eta Carinae and the Keyhole Nebula are just left of center, while NGC 3324 is at upper right.
Credit: Harel Boren
Observation data: J2000.0 epoch
Right ascension 10h 45m 08.5s[1]
Declination −59° 52′ 04″[1]
Distance ~6,500-10,000[2] ly   (~2,000-3,100 pc)
Apparent magnitude (V) +1.0[3]
Constellation Carina
Physical characteristics
Radius ~460[4] ly   (~140 pc)
Notable features
  • Eta Carinae
  • Keyhole Nebula
  • Includes numerous open clusters and dark nebulae
Designations NGC 3372,[5] ESO 128-EN013,[1] GC 2197,[1] h 3295,[1] Caldwell 92[6]

Coordinates: 10h 45m 08.5s, −59° 52′ 04″

The Carina Nebula (catalogued as NGC 3372; also known as the Grand Nebula, Great Nebula in Carina, or Eta Carinae Nebula) is a large, complex area of bright and dark nebulosity in the constellation Carina, and is located in the Carina–Sagittarius Arm. The nebula lies at an estimated distance between 6,500 and 10,000 light-years (2,000 and 3,100 pc) from Earth.

The nebula has within its boundaries the large Carina OB1 association and several related open clusters, including numerous O-type stars and several Wolf–Rayet stars. Carina OB1 encompasses the star clusters Trumpler 14 and Trumpler 16. Trumpler 14 is one of the youngest known star clusters at half a million years old. Trumpler 16 is the home of WR 25, currently the most luminous star known in our Milky Way galaxy, together with the less luminous but more massive and famous Eta Carinae star system and the O2 supergiant HD 93129A. Trumpler 15, Collinder 228, Collinder 232, NGC 3324, and NGC 3293 are also considered members of the association. NGC 3293 is the oldest and furthest from Trumpler 14, indicating sequential and ongoing star formation.

The nebula is one of the largest diffuse nebulae in our skies. Although it is some four times as large and even brighter than the famous Orion Nebula, the Carina Nebula is much less well known due to its location in the southern sky. It was discovered by Nicolas-Louis de Lacaille in 1752 from the Cape of Good Hope.

Discovery and basic info

Nicolas-Louis de Lacaille discovered the nebula on 25 January 1752.[3] Its dimensions are 120×120 arcminutes centered on the coordinates of right ascension 10h 45m 08.5s and declination −59° 52′ 04″.[1] In modern times it is calculated to be around 6,500 to 10,000 light-years (2,000 to 3,100 pc) from Earth.[2]

Objects within the Carina Nebula

Eta Carinae

Main article: Eta Carinae
Eta Carinae observed in different wavelengths

Eta Carinae is a highly luminous hypergiant star. Estimates of its mass range from 100 to 150 times the mass of the Sun, and its luminosity is about four million times that of the Sun.

This object is currently the most massive star that can be studied in great detail, because of its location and size. Several other known stars may be more luminous and more massive, but data on them is far less robust. (Caveat: Since examples such as the Pistol Star have been demoted by improved data, one should be skeptical of most available lists of "most massive stars". In 2006, Eta Carinae still had the highest confirmed luminosity, based on data across a broad range of wavelengths.) Stars with more than 80 times the mass of the Sun produce more than a million times as much light as the Sun. They are quite rare—only a few dozen in a galaxy as big as ours—and they flirt with disaster near the Eddington limit, i.e., the outward pressure of their radiation is almost strong enough to counteract gravity. Stars that are more than 120 solar masses exceed the theoretical Eddington limit, and their gravity is barely strong enough to hold in its radiation and gas, resulting in a possible supernova or hypernova in the near future.

Eta Carinae's effects on the nebula can be seen directly. Dark globules and some other less visible objects have tails pointing directly away from the massive star. The entire nebula would have looked very different before the Great Eruption in the 1840s surrounded Eta Carinae with dust, drastically reducing the amount of ultraviolet light it put into the nebula.

Homunculus Nebula

Main article: Homunculus Nebula
Eta Carinae, surrounded by the Homunculus Nebula

Within the large bright nebula is a much smaller feature, immediately surrounding Eta Carinae itself, known as the Homunculus Nebula (from Latin meaning Little Man). It is believed to have been ejected in an enormous outburst in 1841 which briefly made Eta Carinae the second-brightest star in the sky.

The Homunculus Nebula is a small HII region, with gas shocked into ionised and excited states.[7] It also absorbs much of the light from the extremely luminous central stellar system and re-radiates it as infrared (IR). It is the brightest object in the sky at mid-IR wavelengths.[8]:145-169

Observations of the spectrum of the Homunculus at a particular angular distance from the central star have shown the actual linear distance of that point from the central star, which defines the distance. Values obtained using this method are around 2.3 kiloparsecs (7,500 ly) with a margin of error around 100 parsecs (330 ly).[9][10]

The same calculations also return the inclination of the axis of the Homunculus relative to the line of sight. This turns out to be 41°, or 49° relative to the plane of the sky, which means it is seen from Earth slightly more "end on" than "side on".[9][10]

Keyhole Nebula

The Keyhole Nebula is a dark nebulosity superimposed on the brightest part of the Carina Nebula.

The Keyhole, or Keyhole Nebula, is a small dark cloud of cold molecules and dust within the Carina Nebula, containing bright filaments of hot, fluorescing gas, silhouetted against the much brighter background nebula. John Herschel used the term "lemniscate-oval vacuity" when first describing it,[11] and subsequently referred to it simply as the "oval vacuity".[12] The term lemniscate continued to be used to describe this portion of the nebula[13] until popular astronomy writer Emma Converse described the shape of the nebula as "resembling a keyhole" in an 1873 Appleton's Journal article.[14] The name Keyhole Nebula then came into common use, sometimes for the Keyhole itself, sometimes to describe the whole of the Carina Nebula (signifying "the nebula that contains the Keyhole").[15][16]

The diameter of the Keyhole structure is approximately seven light-years (2.1 pc). Its appearance has changed significantly since it was first observed, possibly due to changes in the ionising radiation from Eta Carinae.[17] The Keyhole does not have its own NGC designation. It is sometimes erroneously called NGC 3324,[18] but that catalogue designation refers to a reflection and emission nebula just northwest of the Carina Nebula (or to its embedded star cluster).[19][20][21]

Trumpler 14

Main article: Trumpler 14
Hubble image of the open cluster Trumpler 14

Trumpler 14 is an open cluster with a diameter of six light-years (1.8 pc), located within the inner regions of the Carina Nebula, approximately 8,000 light-years (2,500 pc) from Earth.[22] It is one of the main clusters of the Carina OB1 stellar association, which is the largest association in the Carina Nebula.[8] About 2,000 stars have been identified in Trumpler 14.[23] and the total mass of the cluster is estimated to be 4,300 M☉.[24]

Trumpler 16

Main article: Trumpler 16

Trumpler 16 is on of the main clusters of the Carina OB1 stellar association, which is the largest association in the Carina Nebula, and it is bigger and more massive than Trumpler 14.[8]

Mystic Mountain

Main article: Mystic Mountain
Mystic Mountain

Mystic Mountain is the term for a dust–gas pillar in the Carina Nebula, a photo of which was taken by Hubble Space Telescope on its 20th anniversary. The area was observed by Hubble's Wide Field Camera 3 on 1–2 February 2010. The pillar measures three light-years (0.92 pc) in height; nascent stars inside the pillar fire off gas jets, that stream from towering peaks.

WR 22

Main article: WR 22

WR 22 is an eclipsing binary. The dynamical masses derived from orbital fitting vary from over 70 M☉ to less than 60 M☉ for the primary and about 21 to 27 M☉ for the secondary.[25] The spectroscopic mass of the primary has been calculated at 74 M☉[26] or 78.1 M☉.[27]

WR 25

Main article: WR 25
The brightest star is WR 25

WR 25 is a binary system in the central portion of the Carina Nebula, a member of the Trumpler 16 cluster. The primary is a Wolf–Rayet star, possibly the most luminous star in the galaxy. The secondary is hard to detect but thought to be a luminous OB star.

HD 93129

Main article: HD 93129

HD 93129 is a triple star system of O-class stars in Carina. All three stars of HD 93129 are among the most luminous in the galaxy;[28] HD 93129 consists of two clearly resolved components, HD 93129 A and HD 93129 B, and HD 93129 A itself is made up of two much closer stars.

HD 93129 A has been resolved into two components. The spectrum is dominated by the brighter component, although the secondary is only 0.9 magnitudes fainter. HD 93129 Aa is an O2 supergiant and Ab is an O3.5 main sequence star.[29] Their separation has decreased from 55 milliarcseconds in 2004 to only 27 mas in 2013, but an accurate orbit is not available.[30]

HD 93129 B is an O3.5 main-sequence star 3 arcseconds away from the closer pair. It is about 1.5 magnitudes fainter than the combined HD 93129 A, and is approximately the same brightness as HD 93129 Ab.[31][32]

HD 93250

Main article: HD 93250

HD 93250 is one of the brightest stars in the region of the Carina Nebula. It is only 7.5 arcminutes from Eta Carinae,[33] and HD 93250 is considered to be a member of the same loose open cluster Trumpler 16, although it appears closer to the more compact Trumpler 14.[34]

HD 93250 is known to be a binary star, however, individual spectra of the two components have never been observed but are thought to be very similar. The spectral type of HD 93250 has variously been given as O5,[35] O6/7,[36] O4,[37] and O3.[38] It has sometimes been classified as a main sequence star and sometimes as a giant star.[37][38] The Galactic O-Star Spectroscopic Survey has used it as the standard star for the newly created O4 subgiant spectral type.[39]

HD 93205

Main article: HD 93205

HD 93205 is a binary system of two large stars.

The more massive member of the pair is an O3.5 main sequence star. The spectrum shows some ionised nitrogen and helium emission lines, indicating some mixing of fusion products to the surface and a strong stellar wind. The mass calculated from apsidal motion of the orbits is 40 to 60 M☉. This is somewhat lower than expected from evolutionary modelling of a star with its observed parameters.[40]

The less massive member is an O8 main sequence star of approximately 20 M☉.[41] It moves in its orbit at a speed of over 300 km/s (190 mi/s) and is considered to be a relativistic binary, which causes the apses of the orbit to change in a predictable way.[42]

Catalogued open clusters in Carina Nebula

As of 1998, there are eight known open clusters in the Carina Nebula:[3]

Annotated map

Annotated map of part of the Carina Nebula showing the location of various objects in the nebula. This view combines multiple ground and Hubble observatory images in a 50-light-year wide (15 pc) view.[44]

Gallery

  1. ^ "Wallpaper: The Caterpillar, a Bok Globule in the Carina Nebula". Hubblesite.org. 2007. Retrieved 29 November 2016. 

See also

References

  1. 1 2 3 4 5 6 "NGC 3372". The NGC/IC Project. Retrieved 29 November 2016.
  2. 1 2 Morison, Ian (25 September 2014). A Journey through the Universe: Gresham Lectures on Astronomy. Cambridge University Press. p. 215. ISBN 978-1-107-07346-3.
  3. 1 2 3 Frommert, Hartmut; Kronberg, Christine (22 March 1998). "NGC 3372". SEDS.org. Retrieved 26 November 2016.
  4. ↑ "NGC 3372 - The Eta Carinae Nebula". Atlas of the Universe. Retrieved 1 October 2013.
  5. ↑ "NGC 3372". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 3 September 2013.
  6. ↑ O'Meara, S. J. (2002). The Caldwell Objects. Cambridge University Press. pp. 361–369. ISBN 0-521-82796-5.
  7. ↑ Teodoro, M.; Damineli, A.; Sharp, R. G.; Groh, J. H.; Barbosa, C. L. (June 2008). "Near-infrared integral field spectroscopy of the Homunculus nebula around η Carinae using Gemini/CIRPASS". Monthly Notices of the Royal Astronomical Society. 387 (2): 564–576. arXiv:0804.0240Freely accessible. Bibcode:2008MNRAS.387..564T. doi:10.1111/j.1365-2966.2008.13264.x.
  8. 1 2 3 Davidson, Kris; Humphreys, Roberta M., eds. (23 January 2012). Eta Carinae and the Supernova Impostors. Astrophysics and Space Science Library, Volume 384. Springer Science+Business Media. Bibcode:2012ASSL..384.....D. doi:10.1007/978-1-4614-2275-4. ISBN 978-1-4614-2274-7.
  9. 1 2 Smith, Nathan (June 2006). "The Structure of the Homunculus. I. Shape and Latitude Dependence from H
    2     and [Fe II] Velocity Maps of η Carinae". The Astrophysical Journal. 644 (2): 1151–1163. arXiv:astro-ph/0602464Freely accessible. Bibcode:2006ApJ...644.1151S. doi:10.1086/503766.
  10. 1 2 Davidson, Kris; Smith, Nathan; Gull, Theodore R.; Ishibashi, Kazunori; Hillier, D. J. (March 2001). "The Shape and Orientation of the Homunculus Nebula Based on Spectroscopic Velocities". The Astronomical Journal. 121 (3): 1569–1577. Bibcode:2001AJ....121.1569D. doi:10.1086/319419.
  11. ↑ Herschel, John Frederick William (1847). Results of astronomical observations made during the years 1834, 5, 6, 7, 8, at the Cape of Good Hope: Being the completion of a telescopic survey of the whole surface of the visible heavens, commenced in 1825. 1. London: Smith, Elder and Co. pp. 33–35. OCLC 5045340.
  12. ↑ Herschel, John Frederick William (1864). "Catalogue of Nebulae and Clusters of Stars". Philosophical Transactions of the Royal Society of London. 154: 1–137. Bibcode:1864RSPT..154....1H. doi:10.1098/rstl.1864.0001.
  13. ↑ Abbott, F. (1873). "Eta Argus". Astronomical Register. 11: 221–224. Bibcode:1873AReg...11..221A.
  14. ↑ Converse, Emma M. (27 December 1873). Eta Argûs. Appletons' Journal. 10. D. Appleton and Company. p. 818.
  15. ↑ Moore, Joseph Haines; Sanford, Roscoe Frank (1914). "The spectrum of η Carinae". Lick Observatory Bulletin. University of California Publications. 8 (252): 55–61. Bibcode:1914LicOB...8...55M. doi:10.5479/ADS/bib/1914LicOB.8.55M.
  16. ↑ See, e.g., Burnham, Jr, Robert (1978). Burnham's Celestial Handbook. New York: Dover. p. 467. ISBN 0-486-23567-X.
  17. ↑ Walborn, N. R.; Ingerson, T. E. (July 1977). "Structure in the Carina Nebula and Eta Carinae". Sky and Telescope. 54: 22–24. Bibcode:1977S&T....54...22W.
  18. ↑ For example, see APOD - NGC 3324.
  19. ↑ Cooper, Ian; Kay, Jenni; Kepple, George Robert (2008). The Night Sky Observer's Guide. Volume 3: The Southern Skies. Willmann-Bell. p. 52. ISBN 978-0-943396-89-7.
  20. ↑ "NGC 3324". The NGC/IC Project. Retrieved 17 May 2014.
  21. ↑ "NGC 3324". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 May 2014.
  22. ↑ Dias, W. S.; Alessi, B. S.; Moitinho, A.; Lépine, J. R. D. (July 2002). "New catalogue of optically visible open clusters and candidates". Astronomy & Astrophysics. 389 (3): 871–873. arXiv:astro-ph/0203351Freely accessible. Bibcode:2002A&A...389..871D. doi:10.1051/0004-6361:20020668.
  23. ↑ "Stellar Family Portrait Takes Imaging Technique to New Extremes". European Southern Observatory. 3 December 2009. Science Release eso0947.
  24. ↑ Sana, H.; Momany, Y.; Gieles, M.; Beletsky, Y.; Ivanov, V. D.; et al. (June 2010). "A MAD view of Trumpler 14". Astronomy & Astrophysics. 515. A26. arXiv:1003.2208Freely accessible. Bibcode:2010A&A...515A..26S. doi:10.1051/0004-6361/200913688.
  25. ↑ Schweickhardt, J.; Schmutz, W.; Stahl, O.; Szeifert, Th.; Wolf, B. (July 1999). "Revised mass determination of the super massive Wolf-Rayet star WR 22". Astronomy & Astrophysics. 347 (1): 127–136. Bibcode:1999A&A...347..127S.
  26. ↑ Hamann, W.-R.; Gräfener, G.; Liermann, A. (October 2006). "The Galactic WN stars. Spectral analyses with line-blanketed model atmospheres versus stellar evolution models with and without rotation". Astronomy & Astrophysics. 457 (3): 1015–1031. arXiv:astro-ph/0608078Freely accessible. Bibcode:2006A&A...457.1015H. doi:10.1051/0004-6361:20065052.
  27. ↑ Gräfener, G.; Hamann, W.-R. (May 2008). "Mass loss from late-type WN stars and its Z-dependence. Very massive stars approaching the Eddington limit". Astronomy & Astrophysics. 482 (3): 945–960. arXiv:0803.0866Freely accessible. Bibcode:2008A&A...482..945G. doi:10.1051/0004-6361:20066176.
  28. ↑ Cohen, D. H.; Gagné, M.; Leutenegger, M. A.; MacArthur, J. P.; Wollman, E. E.; et al. (August 2011). "Chandra X-ray spectroscopy of the very early O supergiant HD 93129A: Constraints on wind shocks and the mass-loss rate". Monthly Notices of the Royal Astronomical Society. 415 (4): 3354–3364. arXiv:1104.4786Freely accessible. Bibcode:2011MNRAS.415.3354C. doi:10.1111/j.1365-2966.2011.18952.x.
  29. ↑ Benaglia, P.; Koribalski, B. (March 2004). "Radio observations of HD 93129A: The earliest O star with the highest mass loss?". Astronomy & Astrophysics. 416 (1): 171–178. arXiv:astro-ph/0312003Freely accessible. Bibcode:2004A&A...416..171B. doi:10.1051/0004-6361:20034138.
  30. ↑ Sana, H.; Le Bouquin, J.-B.; Lacour, S.; Berger, J.-P.; Duvert, G.; et al. (November 2014). "Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection". The Astrophysical Journal Supplement. 215 (1). 15. arXiv:1409.6304Freely accessible. Bibcode:2014ApJS..215...15S. doi:10.1088/0067-0049/215/1/15.
  31. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy & Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  32. ↑ Vazquez, R. A.; Baume, G.; Feinstein, A.; Prado, P. (March 1996). "Investigation on the region of the open cluster TR 14". Astronomy & Astrophysics Supplement. 116: 75–94. Bibcode:1996A&AS..116...75V.
  33. ↑ Sana, H.; Le Bouquin, J.-B.; De Becker, M.; Berger, J.-P.; De Koter, A.; et al. (October 2011). "The Non-thermal Radio Emitter HD 93250 Resolved by Long Baseline Interferometry". The Astrophysical Journal Letters. 740 (2). L43. arXiv:1110.0831Freely accessible. Bibcode:2011ApJ...740L..43S. doi:10.1088/2041-8205/740/2/L43.
  34. ↑ Smith, Nathan (April 2006). "A census of the Carina Nebula. I. Cumulative energy input from massive stars". Monthly Notices of the Royal Astronomical Society. 367 (2): 763–772. arXiv:astro-ph/0601060Freely accessible. Bibcode:2006MNRAS.367..763S. doi:10.1111/j.1365-2966.2006.10007.x.
  35. ↑ Thackeray, A. D.; Tritton, S. B.; Walker, E. N. (1973). "Radial velocities of southern B stars determined at the Radcliffe Observatory—VII". Memoirs of the Royal Astronomical Society. 77: 199. Bibcode:1973MmRAS..77..199T.
  36. ↑ Houk, Nancy; Cowley, Anne P. (1975). University of Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars. Volume 1. Declinations -90° to -53°. Department of Astronomy, University of Michigan. Bibcode:1975MSS...C01....0H. ISBN 978-0-8357-0331-4.
  37. 1 2 Walborn, Nolan R.; Sota, Alfredo; Maíz Apellániz, Jesús; Alfaro, Emilio J.; Morrell, Nidia I.; et al. (March 2010). "Early Results from the Galactic O-Star Spectroscopic Survey: C III Emission Lines in of Spectra". The Astrophysical Journal Letters. 711 (2): L143–L147. Bibcode:2010ApJ...711L.143W. doi:10.1088/2041-8205/711/2/L143.
  38. 1 2 Williams, S. J.; Gies, D. R.; Hillwig, T. C.; McSwain, M. V.; Huang, W. (November 2011). "Radial Velocities of Galactic O-type Stars. I. Short-term Constant Velocity Stars". The Astronomical Journal. 142 (5). 146. Bibcode:2011AJ....142..146W. doi:10.1088/0004-6256/142/5/146.
  39. ↑ Maíz Apellániz, J.; Sota, A.; Arias, J. I.; Barbá, R. H.; Walborn, N. R.; et al. (May 2016). "The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 Additional O-type Systems". The Astrophysical Journal Supplement Series. 224 (1). 4. arXiv:1602.01336Freely accessible. Bibcode:2016ApJS..224....4M. doi:10.3847/0067-0049/224/1/4.
  40. ↑ Benvenuto, O. G.; Serenelli, A. M.; Althaus, L. G.; Barbá, R. H.; Morrell, N. I. (February 2002). "Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion". Monthly Notices of the Royal Astronomical Society. 330 (2): 435–442. arXiv:astro-ph/0110662Freely accessible. Bibcode:2002MNRAS.330..435B. doi:10.1046/j.1365-8711.2002.05083.x.
  41. ↑ Antokhina, Eleonora A.; Moffat, Anthony F. J.; Antokhin, Igor I.; Bertrand, Jean-François; Lamontagne, Robert (January 2000). "Light Curve Solution of HD 93205 (O3 V+O8 V) Containing the Earliest Known Star in a Well-studied Binary". The Astrophysical Journal. 529 (1): 463–476. Bibcode:2000ApJ...529..463A. doi:10.1086/308228.
  42. ↑ Morrell, N. I.; Barbá, R. H.; Niemela, V. S.; Corti, M. A.; Albacete Colombo, J. F.; et al. (September 2001). "Optical spectroscopy of X-Mega targets - II. The massive double-lined O-type binary HD 93205". Monthly Notices of the Royal Astronomical Society. 326 (1): 85–94. arXiv:astro-ph/0105014Freely accessible. Bibcode:2001MNRAS.326...85M. doi:10.1046/j.1365-8711.2001.04500.x.
  43. ↑ Frommert, Hartmut; Kronberg, Christine (6 May 2001). "Collinder 228". SEDS.org. Retrieved 29 November 2016.
  44. ↑ "The Carina Nebula: Star Birth in the Extreme". The Hubble Heritage Project. Space Telescope Science Institute. 24 April 2007. Retrieved 29 November 2016.

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