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] located in the Large Magellanic Cloud. It is located 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 instead of a planetary nebula. [8]

Origins

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

In a paper published in 1978, it was proposed that stellar winds could be a major part of the formation of Henize 70 and other emission nebulae. [11] Later, in a scientific article 1981 it was mentioned that it was more likely from a supernova explosion rather than stellar winds. [12] Another study in 2014 measured high SII and Hα ratios, indicating that it is not a supernova remnant. [13]

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. [14]

Notes

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

Related Research Articles

<span class="mw-page-title-main">Nebula</span> Body of interstellar clouds

A nebula is a distinct luminescent part of interstellar medium, which can consist of ionized, neutral, or molecular hydrogen and also cosmic dust. Nebulae are often star-forming regions, such as in the "Pillars of Creation" in the Eagle Nebula. In these regions, the formations of gas, dust, and other materials "clump" together to form denser regions, which attract further matter and eventually become dense enough to form stars. The remaining material is then thought to form planets and other planetary system objects.

<span class="mw-page-title-main">SN 1987A</span> 1987 supernova event in the constellation Dorado

SN 1987A was a type II supernova in the Large Magellanic Cloud, a dwarf satellite galaxy of the Milky Way. It occurred approximately 51.4 kiloparsecs from Earth and was the closest observed supernova since Kepler's Supernova in 1604. Light and neutrinos from the explosion reached Earth on February 23, 1987 and was designated "SN 1987A" as the first supernova discovered that year. Its brightness peaked in May of that year, with an apparent magnitude of about 3.

<span class="mw-page-title-main">Large Magellanic Cloud</span> Satellite galaxy of the Milky Way

The Large Magellanic Cloud (LMC) is a spiral 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">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.

<span class="mw-page-title-main">Tarantula Nebula</span> H II region in the constellation Dorado

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<span class="mw-page-title-main">Orion molecular cloud complex</span> Star-forming region in the constellation Orion

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<span class="mw-page-title-main">NGC 2060</span> Star cluster in the constellation Dorado

NGC 2060 is a star cluster within the Tarantula Nebula in the Large Magellanic Cloud, very close to the larger NGC 2070 cluster containing R136. It was discovered by John Herschel in 1836. It is a loose cluster approximately 10 million years old, within one of the Tarantula Nebula's superbubbles formed by the combined stellar winds of the cluster or by old supernovae.

<span class="mw-page-title-main">Henize 206</span> Large Magellanic Cloud nebula in the constellation Mensa

Henize 206 is a nebula in the Large Magellanic Cloud. This luminous cloud of gas and dust houses a cluster of newborn stars. Although Henize 206 was first catalogued in the 1950s, it was reported in NASA press releases in March 2004, for showing several example images generated from the various infrared cameras on the Spitzer Space Telescope launched in August 2003.

<span class="mw-page-title-main">R136a1</span> Wolf–Rayet star with one of the highest mass and luminosity of any known star

R136a1 is one of the most massive and luminous stars known, at around 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

AB7, also known as SMC WR7, is a binary star in the Small Magellanic Cloud. A Wolf–Rayet star and a supergiant companion of spectral type O orbit in a period of 19.56 days. The system is surrounded by a ring-shaped nebula known as a bubble nebula.

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

LH 41-1042 is a Wolf–Rayet star located in the Large Magellanic Cloud (LMC). It is an extremely rare member of the WO oxygen sequence, the second to be discovered in the LMC and one of only three found so far in that galaxy.

<span class="mw-page-title-main">N119</span> Spiral shaped H II region in the constellation Dorado

N119 is a spiral-shaped H II region in the Large Magellanic Cloud. Its dimensions are large, at 131 x 175 pc. It contains several luminous stars including S Doradus, LH41-1042, and LMC195-1. Its peculiar S-shaped structure is difficult to explain with classical models.

<span class="mw-page-title-main">N11 (emission nebula)</span> Emission nebula in the constellation Dorado

N11 is the brightest emission nebula in the north-west part of the Large Magellanic Cloud in the Dorado constellation. The N11 complex is the second largest H II region of that galaxy, the largest being the Tarantula Nebula. It covers an area approximately 6 arc minutes across. It has an elliptical shape and consists of a large bubble, generally clear interstellar area, surrounded by nine large nebulae. It was named by Karl Henize in 1956.

<span class="mw-page-title-main">NGC 3859</span> Spiral galaxy in the constellation Leo

NGC 3859 is a spiral galaxy located about 295 million light-years away in the constellation Leo. It was discovered by astronomer Édouard Stephan on March 23, 1884. The galaxy is a member of the Leo Cluster.

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

LHA 120-N 55 or N55 is an emission nebula located within the Large Magellanic Cloud (LMC). N55 is situated inside a superbubble called LMC 4. It is a glowing clump of gas and dust that gets its light output from the hydrogen atoms shedding electrons within it. It was named in 1956, in a catalogue of H-alpha emission line objects in the LMC.

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

N41 is an emission nebula in the north part of the Large Magellanic Cloud in the Dorado constellation. Originally catalogued in Karl Henize's "Catalogue of H-alpha emission stars and nebulae in the Magellanic Clouds" of 1956, it is approximately 100 light-years wide and 160,000-170,000 light-years distant.

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

Hen 2-131 is a planetary nebula in the southern constellation of Apus. It was discovered by Andrew David Thackeray in 1950 and added to the Catalogues of Hα-emission Stars and Nebulae in the Magellanic Clouds by Karl Gordon Henize in 1967.

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. ↑ 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.
  12. ↑ 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.
  13. ↑ 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.
  14. ↑ 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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