Henize 70

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Henize 70
Emission nebula
Superbubble
Henize N70 Superbubble Nebula.jpg
Amateur photograph of Henize 70
Observation data: J2000 epoch
Right ascension 05h 43m 17.5s [1]
Declination −67° 50′ 48″ [1]
Distance~50,000 [2]   pc
Apparent dimensions (V)7′ × 8′ [3]
Constellation Dorado
Physical characteristics
Dimensions346 × 396 ly [4] [lower-alpha 1]
Notable features Superbubble
DesignationsHenize 70, [5] N70, [3] LHA 120-N 70, [3] [6] DEM L 301, MCELS L-373 [6]
See also: Lists of nebulae

Henize 70 (N70) is a faint [7] emission nebula [8] and superbubble [5] [4] [9] [10] [11] [12] [13] [14] [15] [16] [17] [18] [19] [20] [21] [ excessive citations ] located in the Large Magellanic Cloud in the constellation of Dorado.

Contents

Observation history

Henize 70 was first observed in 1950 in a survey of bright planetary nebulae. Based on appearance it was proposed that it might be a supernova remnant. [7] In 1956, it was added to a catalogue of Hα emission stars and nebulae by Karl Gordon Henize, where it was described as an emission nebula rather than a planetary nebula. [8]

Origins

ESO image of Henize 70 Superbubble N70 in LMC.jpg
ESO image of Henize 70

A paper published in 1978 proposed that the formations of Henize 70 and other emission nebulae could be due to stellar winds. [22] Later in 1981, a scientific article mentioned a higher likeliness of a supernova explosion forming the nebula instead of stellar winds. [23] A 2014 study measured that Henize 70 featured high SII and Hα ratios, indicating that it is not a supernova remnant. [24]

Henize 70 has spectral line ratios relatively similar to that of supernova remnants due to having similar SII/Hα line ratios although most supernova remnants have higher NII/Hα line ratios. [25]

Notes

  1. ↑ Using angular dimensions of 7’ × 8’ and a distance of ~170 kly.

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The Large Magellanic Cloud (LMC) is a dwarf galaxy and satellite galaxy of the Milky Way. At a distance of around 50 kiloparsecs (163,000 light-years), the LMC is the second- or third-closest galaxy to the Milky Way, after the Sagittarius Dwarf Spheroidal (c. 16 kiloparsecs (52,000 light-years) away) and the possible dwarf irregular galaxy called the Canis Major Overdensity. Based on the D25 isophote at the B-band (445 nm wavelength of light), the Large Magellanic Cloud is about 9.86 kiloparsecs (32,200 light-years) across. It is roughly one-hundredth the mass of the Milky Way and is the fourth-largest galaxy in the Local Group, after the Andromeda Galaxy (M31), the Milky Way, and the Triangulum Galaxy (M33).

<span class="mw-page-title-main">H II region</span> Large, low-density interstellar cloud of partially ionized gas

An H II region or HII region is a region of interstellar atomic hydrogen that is ionized. It is typically in a molecular cloud of partially ionized gas in which star formation has recently taken place, with a size ranging from one to hundreds of light years, and density from a few to about a million particles per cubic centimetre. The Orion Nebula, now known to be an H II region, was observed in 1610 by Nicolas-Claude Fabri de Peiresc by telescope, the first such object discovered.

<span class="mw-page-title-main">Wolf–Rayet star</span> Heterogeneous class of stars with unusual spectra

Wolf–Rayet stars, often abbreviated as WR stars, are a rare heterogeneous set of stars with unusual spectra showing prominent broad emission lines of ionised helium and highly ionised nitrogen or carbon. The spectra indicate very high surface enhancement of heavy elements, depletion of hydrogen, and strong stellar winds. The surface temperatures of known Wolf–Rayet stars range from 20,000 K to around 210,000 K, hotter than almost all other kinds of stars. They were previously called W-type stars referring to their spectral classification.

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The Tarantula Nebula is a large H II region in the Large Magellanic Cloud (LMC), forming its south-east corner.

<span class="mw-page-title-main">Extinction (astronomy)</span> Interstellar absorption and scattering of light

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<span class="mw-page-title-main">Yellow hypergiant</span> Class of massive star with a spectral type of A to K

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R136a1 is one of the most massive and luminous stars known, at nearly 200 M☉ and nearly 4.7 million L☉, and is also one of the hottest, at around 46,000 K. It is a Wolf–Rayet star at the center of R136, the central concentration of stars of the large NGC 2070 open cluster in the Tarantula Nebula in the Large Magellanic Cloud. The cluster can be seen in the far southern celestial hemisphere with binoculars or a small telescope, at magnitude 7.25. R136a1 itself is 100 times fainter than the cluster and can only be resolved using speckle interferometry.

<span class="mw-page-title-main">AB7</span> Binary star in the Small Magellanic Cloud in the constellation Tucana

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<span class="mw-page-title-main">WR 31a</span> Wolf Rayet star in the constellation Carina

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<span class="mw-page-title-main">LH 41-1042</span> Wolf Rayet star in the constellation Dorado

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<span class="mw-page-title-main">LHA 120-N 55</span> Nebula in the constellation Dorado

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<span class="mw-page-title-main">N41 (nebula)</span> Nebula in the constellation Dorado

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<span class="mw-page-title-main">Hen 2-131</span> Planetary nebula in the constellation Apus

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References

  1. 1 2 Pellegrini, E. W.; Oey, M. S.; Winkler, P. F.; Points, S. D.; Smith, R. C.; Jaskot, A. E.; Zastrow, J. (13 February 2012). "The Optical Depth of H II Regions in the Magellanic Clouds". The Astrophysical Journal. 755 (1): 30. arXiv: 1202.3334 . Bibcode:2012ApJ...755...40P. doi: 10.1088/0004-637X/755/1/40 . ISSN   0004-637X. S2CID   51059889.
  2. ↑ Schneiter, E. M.; Reyes-Iturbide, J.; Velàzquez, P. F.; Esquivel, A. (2 February 2022). "X-ray and optical emission from large superbubbles including the stellar photoionization". Monthly Notices of the Royal Astronomical Society. 511 (3): 3420–3427. Bibcode:2022MNRAS.511.3420S. doi: 10.1093/mnras/stac292 . ISSN   1365-2966.
  3. 1 2 3 Davies, R. D.; Elliott, K. H.; Meaburn, J. (1976). "The nebular complexes of the Large and Small Magellanic Clouds". Memoirs of the Royal Astronomical Society. 81: 89. Bibcode:1976MmRAS..81...89D.
  4. 1 2 "N70. Henize 70". Astrodrudis. Retrieved 14 April 2023.
  5. 1 2 "Henize 70: A SuperBubble In The LMC". Astronomy Picture of the Day . Retrieved 14 April 2023.
  6. 1 2 "LHA 120-N 70". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 14 April 2023.
  7. 1 2 Evans, D. S.; Thackeray, A. D. (1950). "A photographic survey of bright southern planetary nebulae". Monthly Notices of the Royal Astronomical Society. 110 (5): 429–439. Bibcode:1950MNRAS.110..429E. doi: 10.1093/mnras/110.5.429 . ISSN   1365-2966.
  8. 1 2 Henize, Karl G. (September 1956). "Catalogues of Hα-emission Stars and Nebulae in the Magellanic Clouds". Astrophysical Journal Supplement. 2: 315. Bibcode:1956ApJS....2..315H. doi:10.1086/190025. ISSN   0067-0049.
  9. ↑ "N70 Nebula in the Large Magellanic Cloud". European Southern Observatory. 14 April 2023.
  10. ↑ "Henize 70: A Superbubble in the LMC". NASA. 14 April 2023.
  11. ↑ Ambrocio-Cruz, P.; Le Coarer, E.; Rosado, M.; Russeil, D.; Amram, P.; Laval, A.; Epinat, B.; Ramírez, M.; Odonne, M.; Goldes, G. (1 April 2016). "The kinematical properties of superbubbles and H II regions of the Large Magellanic Cloud derived from the 3D Hα Survey". Monthly Notices of the Royal Astronomical Society. 457 (2): 2048–2067. Bibcode:2016MNRAS.457.2048A. doi: 10.1093/mnras/stw054 . ISSN   0035-8711. S2CID   123722565.
  12. ↑ De Horta, A. Y.; et al. (14 May 2014). "Multi-frequency Observations of a Superbubble in the LMC: The Case of LHA 120-N 70". The Astronomical Journal. 147 (6): 8. arXiv: 1404.3823 . Bibcode:2014AJ....147..162D. doi:10.1088/0004-6256/147/6/162. ISSN   0004-6256. S2CID   118458341.
  13. ↑ Reyes-Iturbide, J.; et al. (17 October 2014). "Diffuse X-Ray Emission from the Superbubbles N70 and N185 in the Large Magellanic Cloud". The Astronomical Journal. 148 (5): 8. arXiv: 1407.7586 . Bibcode:2014AJ....148..102R. doi:10.1088/0004-6256/148/5/102. ISSN   0004-6256. S2CID   119225213.
  14. ↑ Rodríguez-González, A.; et al. (2 May 2011). "X-Ray Emission and Dynamics from Large Diameter Superbubbles: The Case of the N70 Superbubble". The Astrophysical Journal. 733 (1): 8. arXiv: 1102.2938 . Bibcode:2011ApJ...733...34R. doi:10.1088/0004-637X/733/1/34. ISSN   0004-637X. S2CID   119210133.
  15. ↑ Reyes-Iturbide, J.; et al. (October 2011). "Diffuse X-ray emission from the superbubble N70" (PDF). XIII Latin American Regional IAU Meeting (Eds. W. J. Henney & S. Torres-Peimbert) Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias). 40: 199. Bibcode:2011RMxAC..40..199R. S2CID   117750676.
  16. ↑ Sankrit, Ravi; Dixon, W. Van Dyke (13 February 2007). "O VI Emission from Superbubbles in the Large Magellanic Cloud". The Publications of the Astronomical Society of the Pacific. 119 (853): 284–291. Bibcode:2007PASP..119..284S. doi:10.1086/513288. ISSN   0004-6280. S2CID   116757625.
  17. ↑ Danforth, Charles W.; Blair, William P. (July 2006). "Possible Detection of O VI from the Large Magellanic Cloud Superbubble N70". The Astrophysical Journal. 646 (1): 205–212. arXiv: astro-ph/0603809 . Bibcode:2006ApJ...646..205D. doi:10.1086/504706. ISSN   0004-637X. S2CID   18990945.
  18. ↑ Oey, M. S.; García-Segura, G. (September 2004). "Ambient Interstellar Pressure and Superbubble Evolution". The Astrophysical Journal. 613 (1): 302–311. arXiv: astro-ph/0403713 . Bibcode:2004ApJ...613..302O. doi:10.1086/421483. ISSN   0004-637X. S2CID   9404310.
  19. ↑ Oey, M. S. (August 1996). "The Dynamics of Superbubbles in the Large Magellanic Cloud". The Astrophysical Journal. 467: 666. Bibcode:1996ApJ...467..666O. doi:10.1086/177642. ISSN   0004-637X. S2CID   122079386.
  20. ↑ Oey, M. S. (May 1996). "UBV Photometry of OB Associations within Superbubbles of the Large Magellanic Cloud". Astrophysical Journal Supplement. 104: 71. Bibcode:1996ApJS..104...71O. doi:10.1086/192292. ISSN   0067-0049. S2CID   122528550.
  21. ↑ Chu, You-Hua; Mac Low, Mordecai-Mark (December 1990). "X-Rays from Superbubbles in the Large Magellanic Cloud". The Astrophysical Journal. 365: 510. Bibcode:1990ApJ...365..510C. doi:10.1086/169505. ISSN   0004-637X.
  22. ↑ Meaburn, J. (November 1978). "H I, Molecular/H II Shells from 1 to 2000 pc Diameter: Wind-Driven or Supernova Remnants?" . Astrophysics and Space Science. 59 (1): 193–214. Bibcode:1978Ap&SS..59..193M. doi:10.1007/BF00651050. ISSN   1572-946X. S2CID   121072103.
  23. ↑ Rosado, M.; Georgelin, Y. P.; Georgelin, Y. M.; Laval, A.; Monnet, G. (April 1981). "Kinematics of ring-shaped nebulae in the LMC. I - The radial velocity field of N70". Astronomy and Astrophysics. 97 (2): 342–346. Bibcode:1981A&A....97..342R. eISSN   1432-0746. ISSN   0004-6361.
  24. ↑ Zhang, Ning-Xiao; Chu, You-Hua; Williams, R. M.; Jiang, Bing; Chen, Yang; Gruendl, R. A. (24 July 2014). "Physical Nature of the [S II]-bright Shell Nebulae N70 and N185". The Astrophysical Journal. 792 (1): 9. arXiv: 1407.6718 . Bibcode:2014ApJ...792...58Z. doi: 10.1088/0004-637X/792/1/58 . ISSN   0004-637X. S2CID   118666688.
  25. ↑ Skelton, Brooke P.; Waller, William H.; Gelderman, Richard F.; Brown, Larry; Woodgate, Bruce; Caulet, Adeline; Schommer, Robert A. (27 February 1999). "Emission-Line Properties of the Large Magellanic Cloud Bubble N70". The Publications of the Astronomical Society of the Pacific. 111 (758): 465–481. arXiv: astro-ph/9903001 . Bibcode:1999PASP..111..465S. doi:10.1086/316346. ISSN   1538-3873. S2CID   120179184.
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