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Trifid Nebula

Coordinates: Sky map 18h 02m 23s, −23° 01′ 48″
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Trifid Nebula
Emission nebula
H II region
reflection nebula and dark nebula
Trifid Nebula by the Hubble Space Telescope
Observation data: J2000 epoch
Right ascension18h 02m 23s[1]
Declination−23° 01′ 48″[1]
Distance4100±200[2] ly   (1,260±70 pc)
Apparent magnitude (V)+6.3[1]
Apparent dimensions (V)28 arcmins
ConstellationSagittarius
Physical characteristics
Radius21 ly
Notable featuresa
DesignationsM20, NGC 6514,[1] Sharpless 30, RCW 147, Gum 76
See also: Lists of nebulae

The Trifid Nebula (catalogued as Messier 20 or M20 and as NGC 6514) is an H II region in the north-west of Sagittarius in a star-forming region in a nearby spiral arm's Scutum-centered part.[3] It was discovered by Charles Messier on June 5, 1764.[4] Its name means 'three-lobe'. The object is an unusual combination of an open cluster of stars, an emission nebula (a relatively dense, red-yellow portion), a reflection nebula (the mainly NNE blue portion), and a dark nebula (the apparent 'gaps' in the former that cause the trifurcated appearance also designated Barnard 85). Viewed through a small telescope, the Trifid Nebula is a bright and peculiar object, and is thus a perennial favorite of amateur astronomers.[5]

The most massive star that has formed in this region is HD 164492A, an O7.5III star with a mass more than 20 times the mass of the Sun.[6] This star is surrounded by a cluster of approximately 3100 young stars.[7]

Characteristics

The Trifid Nebula was the subject of an investigation by astronomers using the Hubble Space Telescope in 1997, using filters that isolate emission from hydrogen atoms, ionized sulfur atoms, and doubly ionized oxygen atoms. The images were combined into a false-color composite picture to suggest how the nebula might look to the eye.

The close-up images show a dense cloud of dust and gas, which is a stellar nursery full of embryonic stars. This cloud is about 8 ly away from the nebula's central star. A stellar jet protrudes from the head of the cloud and is about 0.75 ly long. The jet's source is a young stellar object deep within the cloud. Jets are the exhaust gasses of star formation and radiation from the nebula's central star makes the jet glow.

The images also showed a finger-like stalk to the right of the jet. It points from the head of the dense cloud directly toward the star that powers the Trifid nebula. This stalk is a prominent example of evaporating gaseous globules, or 'EGGs'. The stalk has survived because its tip is a knot of gas that is dense enough to resist being eaten away by the powerful radiation from the star.

In January 2005, NASA's Spitzer Space Telescope discovered 30 embryonic stars and 120 newborn stars not seen in visible light images.

It is centered about 4100 ly away from Earth. Its apparent magnitude is 6.3.

  • M20 with amateur telescope
    M20 with amateur telescope
  • The Trifid nebula. The outlined area is enlarged right.
    The Trifid nebula. The outlined area is enlarged right.
  • Hubble image of a stellar jet in the Trifid nebula.
    Hubble image of a stellar jet in the Trifid nebula.
  • Hubble image, a closer detail of last.
    Hubble image, a closer detail of last.
  • The Trifid Nebula in infrared as seen by the Spitzer Space Telescope. These visible colors show 3.6, 8.0, and 24 micron light
    The Trifid Nebula in infrared as seen by the Spitzer Space Telescope. These visible colors show 3.6, 8.0, and 24 micron light
  • The Trifid Nebula is a rare combination of three nebulae types that reveal the fury of freshly formed stars and point to more star birth in the future.
    The Trifid Nebula is a rare combination of three nebulae types that reveal the fury of freshly formed stars and point to more star birth in the future.
  • This video sequence compares a new view of the Trifid Nebula in infrared light, from the VVV VISTA survey with a more familiar visible-light view from a small telescope.

See also

References

  1. ^ a b c d "NGC 6514". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-16.
  2. ^ Kuhn, Michael A.; Hillenbrand, Lynne A.; Sills, Alison; Feigelson, Eric D.; Getman, Konstantin V. (2018). "Kinematics in Young Star Clusters and Associations with Gaia DR2". The Astrophysical Journal. 870 (1): 32. arXiv:1807.02115. Bibcode:2019ApJ...870...32K. doi:10.3847/1538-4357/aaef8c.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  3. ^ Cambrésy, L.; et al. (2011). "Variation of the extinction law in the Trifid nebula". Astronomy & Astrophysics. 527: A141. arXiv:1101.1089. Bibcode:2011A&A...527A.141C. doi:10.1051/0004-6361/201015863.
  4. ^ Messier 20
  5. ^ "Science Daily". Science Daily article on Trifid Nebula. Retrieved 2010-07-06.
  6. ^ Rho, J.; et al. (2004). "Chandra Observation of the Trifid Nebula: X-Ray Emission from the O Star Complex and Actively Forming Pre-Main-Sequence Stars". Astrophysical Journal. 607 (2): 904–912. arXiv:astro-ph/0401377. Bibcode:2004ApJ...607..904R. doi:10.1086/383081.
  7. ^ Kuhn, M. A.; et al. (2015). "The Spatial Structure of Young Stellar Clusters. II. Total Young Stellar Populations". Astrophysical Journal. 802 (1): 60. arXiv:1501.05300. Bibcode:2015ApJ...802...60K. doi:10.1088/0004-637X/802/1/60.
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