Taurus molecular cloud

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Taurus molecular cloud
Nebula
Herschel's view of the Taurus molecular cloud ESA384012.jpg
Taurus molecular cloud (Herschel Space Observatory)
Observation data: J2000.0 [1] epoch
Right ascension 04h 41.0m [1]
Declination +25° 52′ [1]
Constellation Taurus
DesignationsHCL 2, Heiles's cloud 2, TMC-1, Taurus molecular cloud 1 [1]
See also: Lists of nebulae
This video begins with a wide-field view of the sky, before zooming into the Taurus molecular cloud region, about 450 light-years from Earth. Dark clouds of cosmic dust grains obscure the background stars at visible wavelengths. The submillimetre-wavelength observations from the LABOCA camera on APEX reveal the heat glow of the dust grains, shown here in orange tones. The observations cover two regions in the cloud, which are known as Barnard 211 and Barnard 213. In them, newborn stars are hidden, and dense clouds of gas are on the verge of collapsing to form yet more stars.
This video pans over part of the Taurus molecular cloud region.

The Taurus molecular cloud (TMC-1) is an interstellar molecular cloud in the constellations Taurus and Auriga. This cloud hosts a stellar nursery containing hundreds of newly formed stars. [2] The Taurus molecular cloud is only 140 pc (430 ly) away from Earth, making it possibly the nearest large star formation region. It has been important in star formation studies at all wavelengths. [3]

It is notable for containing many complex molecules, such as cyanopolyynes HCnN for n = 3,5,7,9, [4] and cumulene carbenes H2Cn for n = 3–6. [5]

The Taurus molecular cloud was identified in the past as a part of the Gould Belt, a large structure surrounding the solar system. More recently (January 2020) the Taurus molecular cloud was identified as being part of the much larger Radcliffe wave, a wave-shaped structure in the local arm of the Milky Way.

The newly formed stars in this cloud have an age of 1–2 million years. [6] The Taurus–Auriga association, which is the stellar association of the cloud, contains the variable star T Tauri, which is the prototype of T Tauri stars. [7] The many young stars and the close proximity to earth make it uniquely well-suited to search for protoplanetary disks and exoplanets around stars, and to identify brown dwarfs in the association. Members of this region are suited for direct imaging of young exoplanets, which glow brightly in infrared wavelengths.

Members [7] [8] of the Taurus–Auriga association with a circumstellar disk or exoplanet:

Main dark nebulae of the Solar apex half of the galactic plane, with the Taurus molecular cloud at the left edge. Regioni celesti scelte - Osc A.png
Main dark nebulae of the Solar apex half of the galactic plane, with the Taurus molecular cloud at the left edge.

See also

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<span class="mw-page-title-main">SU Aurigae</span> Star in the constellation Auriga

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<span class="mw-page-title-main">AA Tauri</span> Star in the constellation Taurus

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<span class="mw-page-title-main">AB Aurigae</span> Star in the constellation Auriga

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<span class="mw-page-title-main">HL Tauri</span> Star in constellation Taurus

HL Tauri is a young T Tauri star in the constellation Taurus, approximately 450 light-years (140 pc) from Earth in the Taurus Molecular Cloud. The luminosity and effective temperature of HL Tauri imply that its age is less than 100,000 years. At apparent magnitude 15.1, it is too faint to be seen with the unaided eye. It is surrounded by a protoplanetary disk marked by dark bands visible in submillimeter radiation that may indicate a number of planets in the process of formation. It is accompanied by the Herbig–Haro object HH 150, a jet of gas emitted along the rotational axis of the disk that is colliding with nearby interstellar dust and gas.

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<span class="mw-page-title-main">LkCa 15</span> Star system in the constellation Taurus

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<span class="mw-page-title-main">GG Tauri</span> Star in the constellation Taurus

GG Tauri, often abbreviated as GG Tau, is a quintuple star system in the constellation Taurus. At a distance of about 450 light years away, it is located within the Taurus-Auriga Star Forming Region. The system comprises three stars orbiting each other in a hierarchical triple system, known as GG Tauri A, and another binary star system more distant from the central system, known as GG Tauri B.

<span class="mw-page-title-main">Circumplanetary disk</span> Accumulation of matter around a planet

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<span class="mw-page-title-main">V1298 Tauri</span> Star in the constellation Taurus

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<span class="mw-page-title-main">FU Tauri</span> Brown dwarf binary star system in the constellation Taurus

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<span class="mw-page-title-main">RY Tauri</span> Star in the constellation Taurus

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<span class="mw-page-title-main">GV Tauri</span> Young binary star system in the constellation of Taurus

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<span class="mw-page-title-main">DL Tauri</span> Protostar system with planetary system in the constellation of Taurus

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<span class="mw-page-title-main">LDN 1641</span>

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References

  1. 1 2 3 4 "TMC-1 – Molecular Cloud". SIMBAD . Retrieved 2014-03-14.
  2. ↑ Luhman, K. L.; Allen, P. R.; Espaillat, C.; Hartmann, L.; Calvet, N. (2010). "The Disk Population of the Taurus Star-Forming Region". The Astrophysical Journal Supplement Series. 186 (1): 111–174. arXiv: 0911.5457 . Bibcode:2010ApJS..186..111L. doi:10.1088/0067-0049/186/1/111. ISSN   0067-0049. S2CID   119189843.
  3. ↑ Guedel, M.; Briggs, K. R.; Arzner, K.; et al. (2007). "The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST)". Astronomy and Astrophysics. 468 (2): 353–377. arXiv: astro-ph/0609160 . Bibcode:2007A&A...468..353G. doi:10.1051/0004-6361:20065724. S2CID   8846597.
  4. ↑ Freeman, A.; Millar, T. J. (1983). "Formation of complex molecules in TMC-1". Nature. 301 (5899): 402–404. Bibcode:1983Natur.301..402F. doi:10.1038/301402a0. ISSN   0028-0836. S2CID   26107828.
  5. ↑ Cabezas, C.; Tercero, B.; Agúndez, M.; et al. (2021). "Cumulene carbenes in TMC-1: Astronomical discovery of l-H2C5". Astronomy & Astrophysics. 650: L9. arXiv: 2106.00635 . Bibcode:2021A&A...650L...9C. doi:10.1051/0004-6361/202141274. ISSN   0004-6361. PMC   7611420 . PMID   34334798.
  6. ↑ Kenyon, Scott J.; Hartmann, Lee (November 1995). "Pre-Main-Sequence Evolution in the Taurus–Auriga Molecular Cloud". Astrophysical Journal Supplement Series. 101: 117. Bibcode:1995ApJS..101..117K. doi:10.1086/192235. ISSN   0067-0049.
  7. 1 2 Gagné, Jonathan; Mamajek, Eric E.; Malo, Lison; Riedel, Adric; Rodriguez, David; Lafrenière, David; Faherty, Jacqueline K.; Roy-Loubier, Olivier; Pueyo, Laurent; Robin, Annie C.; Doyon, René (March 2018). "BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc". Astrophysical Journal. 856 (1): 23. arXiv: 1801.09051 . Bibcode:2018ApJ...856...23G. doi: 10.3847/1538-4357/aaae09 . ISSN   0004-637X.
  8. ↑ Kwon, Woojin; Looney, Leslie W.; Mundy, Lee G. (October 2011). "Resolving the Circumstellar Disk of Hl Tauri at Millimeter Wavelengths". The Astrophysical Journal. 741 (1): 3. arXiv: 1107.5275 . Bibcode:2011ApJ...741....3K. doi:10.1088/0004-637X/741/1/3. ISSN   0004-637X. S2CID   118525138.
  9. ↑ "V1298 Tau". exoplanetarchive.ipac.caltech.edu. Retrieved 2020-02-21.
  10. ↑ David, Trevor J.; Petigura, Erik A.; Luger, Rodrigo; Foreman-Mackey, Daniel; Livingston, John H.; Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2019). "Four Newborn Planets Transiting the Young Solar Analog V1298 Tau". Astrophysical Journal Letters. 885 (1): L12. arXiv: 1910.04563 . Bibcode:2019ApJ...885L..12D. doi: 10.3847/2041-8213/ab4c99 . ISSN   0004-637X. S2CID   204008446.
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