Orion Molecular Cloud Complex

The Orion Molecular Cloud Complex (or, simply, the Orion Complex) is a star forming region with stellar ages ranging up to 12 Myr. Two giant molecular clouds are a part of it, Orion A and Orion B. The stars currently forming within the Complex are located within these clouds. A number of other somewhat older stars no longer associated with the molecular gas are also part of the Complex, most notably the Orion's Belt (Orion OB1b), as well as the dispersed population north of it (Orion OB1a). Near the head of Orion there is also a population of young stars that is centered on Meissa. The Complex is between 1 000 and 1 400 light-years away, and hundreds of light-years across.

Orion Molecular Cloud Complex
Molecular cloud
Molecular cloud complex
Orion Head to Toe.jpg
Part of the Orion Molecular Cloud Complex, with the Great Nebula in Orion near the center, along with the Belt of Orion, and Barnard's Loop curling around the image
Observation data: J2000.0[1] epoch
Right ascension05h 35.3m [1]
Declination−05° 23′[1]
DesignationsOrion Complex, Orion Cloud Complex, Orion Molecular Cloud Complex
See also: Lists of nebulae

The Orion Complex is one of the most active regions of nearby stellar formation visible in the night sky, and is home to both protoplanetary discs and very young stars. Much of it is bright in infrared wavelengths due to the heat-intensive processes involved in stellar formation, though the complex contains dark nebulae, emission nebulae, reflection nebulae, and H II regions. The presence of ripples on the surface of Orion's Molecular Clouds was discovered in 2010. The ripples are a result of the expansion of the nebulae gas over pre-existing molecular gas.[2]

The Orion Complex includes a large group of bright nebulae, dark clouds in the Orion constellation. Several nebulae can be observed through binoculars and small telescopes, and some parts (such as the Orion Nebula) are visible to the naked eye.

Nebulae within the complexEdit

A labeled map of the Orion Molecular Cloud, with the images taken by IRAS and various telescopes that mapped CO in this part of the sky

The following is a list of notable regions within the larger Complex:

A more complete list can be found for example in Maddalena et al. (1986) Table 1[5]

Individual componentsEdit

Young stars in Orion A and Orion B molecular clouds. The clouds were imaged by Herschel and the newborn stars were imaged by ALMA and the VLA.

Orion AEdit

The giant molecular cloud Orion A is the most active star-forming region in the local neighbourhood of the sun. In the last few million years about 3000 young stellar objects were formed in this region, including about 190 protostars and about 2600 pre-main sequence stars.[6] The Orion A cloud has a mass in the order of 105 M.[7] The stars in Orion A do not have the same distance to us. The "head" of the cloud, which also contains the Orion Nebula is about 1300 light-years (400 parsec) away from the sun. The "tail" however is up to 1530 light-years (470 parsec) away from the sun. The Orion A cloud is therefore longer than the projected length of 130 light-years (40 parsec) and has a true length of 290 light-years (90 parsec).[8]

Orion BEdit

Orion B is about 1370 light-years (420 parsec) distant to Earth.[9] It has a size of about 1.5 kpc² and a mass in the order of 105 M. It contains several star forming regions with the star cluster inside the Flame Nebula being the largest cluster.[10][7]

Orion OB1 associationEdit

The Orion OB1 association represents different stellar populations that are superimposed along our line of sight. The oldest group with 8-10 million years is Orion OB1a, northwest of Orion's Belt, and the youngest group with less than 2 million years is Orion OB1d, which contains the Orion Nebula cluster and NGC 2024.[7]

Lambda Orionis molecular ringEdit

The Lambda Orionis ring is a large molecular ring, centered around Lambda Orioinis (Meissa). It was suggested that this ring formed after a supernova happened inside the central star-forming region that once surrounded the Lambda Orionis Cluster, dispersing the material into the ring seen today. Star-formation is still continuing in regions of the ring.[11]


Parts of the Orion-Eridanus superbubble were first seen as Barnard's Loop in Hydrogen-alpha images that warp around the eastern portion of Orion. The other part of the superbubble that is seen in H-alpha is the Eridanus Loop. The walls of the entire bubble are seen in far-infrared and HI. Some features of the Eridanus Loop might be as close as 590 light-years (180 parsec) to the sun.[7]


See alsoEdit


  1. ^ a b c "NAME ORI COMPLEX". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2014-03-14.
  2. ^ Berné, Olivier; Marcelino, Núria; Cernicharo, José (2010). "Waves on the surface of the Orion molecular cloud". Nature. 466 (7309): 947–949. arXiv:1011.0295. Bibcode:2010Natur.466..947B. doi:10.1038/nature09289. PMID 20725034.
  3. ^ Bally, John; Heathcote, Steve; Reipurth, Bo; Morse, Jon; Hartigan, Patrick; Schwartz, Richard (May 2002). "Hubble Space Telescope Observations of Proper Motions in Herbig-Haro Objects 1 and 2". AJ. 123 (5): 2627–2657. Bibcode:2002AJ....123.2627B. doi:10.1086/339837. ISSN 0004-6256.
  4. ^ "Orion's Big Head Revealed in Infrared". www.nasa.gov. NASA. Retrieved 24 February 2015.
  5. ^ Maddalena, R. J.; Morris, M.; Moscowitz, J.; Thaddeus, P. (April 1986). "The Large System of Molecular Clouds in Orion and Monoceros". Astrophysical Journal. 303: 375. Bibcode:1986ApJ...303..375M. doi:10.1086/164083. ISSN 0004-637X.
  6. ^ Großschedl, Josefa Elisabeth; Alves, João; Teixeira, Paula S.; Bouy, Hervé; Forbrich, Jan; Lada, Charles J.; Meingast, Stefan; Hacar, Álvaro; Ascenso, Joana; Ackerl, Christine; Hasenberger, Birgit (February 2019). "VISION - Vienna survey in Orion. III. Young stellar objects in Orion A". A&A. 622: A149. arXiv:1810.00878. Bibcode:2019A&A...622A.149G. doi:10.1051/0004-6361/201832577. ISSN 0004-6361.
  7. ^ a b c d Bally, J. (December 2008). "Overview of the Orion Complex". Hsf1. 4: 459. Bibcode:2008hsf1.book..459B.
  8. ^ Großschedl, Josefa E.; Alves, João; Meingast, Stefan; Ackerl, Christine; Ascenso, Joana; Bouy, Hervé; Burkert, Andreas; Forbrich, Jan; Fürnkranz, Verena; Goodman, Alyssa; Hacar, Álvaro (November 2018). "3D shape of Orion A from Gaia DR2". A&A. 619: A106. arXiv:1808.05952. Bibcode:2018A&A...619A.106G. doi:10.1051/0004-6361/201833901. ISSN 0004-6361.
  9. ^ Zucker, Catherine; Speagle, Joshua S.; Schlafly, Edward F.; Green, Gregory M.; Finkbeiner, Douglas P.; Goodman, Alyssa A.; Alves, João (July 2019). "A Large Catalog of Accurate Distances to Local Molecular Clouds: The Gaia DR2 Edition". Astrophysical Journal. 879 (2): 125. arXiv:1902.01425. Bibcode:2019ApJ...879..125Z. doi:10.3847/1538-4357/ab2388. ISSN 0004-637X.
  10. ^ Buckle, J. V.; Curtis, E. I.; Roberts, J. F.; White, G. J.; Hatchell, J.; Brunt, C.; Butner, H. M.; Cavanagh, B.; Chrysostomou, A.; Davis, C. J.; Duarte-Cabral, A. (January 2010). "The JCMT Legacy Survey of the Gould Belt: a first look at Orion B with HARP". MNRAS. 401 (1): 204–222. arXiv:0908.4162. Bibcode:2010MNRAS.401..204B. doi:10.1111/j.1365-2966.2009.15619.x. ISSN 0035-8711.
  11. ^ Dolan, Christopher J.; Mathieu, Robert D. (January 2002). "A Photometric Study of the Young Stellar Population throughout the λ Orionis Star-Forming Region". AJ. 123 (1): 387–403. arXiv:astro-ph/0110160. Bibcode:2002AJ....123..387D. doi:10.1086/324631. ISSN 0004-6256.

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