Astronomy:Taurus Molecular Cloud

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Taurus Molecular Cloud
Molecular cloud
Giant molecular cloud
File:300px
Taurus molecular cloud (Herschel Space Observatory)
Observation data: J2000.0[1] epoch
Right ascension 04h 41.0m [1]
Declination+25° 52′ [1]
ConstellationTaurus
DesignationsHCL 2, Heiles's cloud 2, TMC, Taurus Molecular Cloud 1 [1]
See also: Lists of nebulae
File:APEX Turns its Eye to Dark Clouds in Taurus (zoom).ogv
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.
File:APEX Turns its Eye to Dark Clouds in Taurus (pan).ogv
This video pans over part of the Taurus Molecular Cloud region.

The Taurus Molecular Cloud is a 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 also reveals characteristics that make it ideal for detailed physical studies. It has been important in star formation studies at all wavelengths.[3]

The cloud is notable for containing many complex molecules, including cyanopolyynes HCnN for n=3,5,7,9.[4]

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.[5] 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.[6] The many young stars and the close proximity to earth is an ideal condition to search for protoplanetary disks around members of the association, to search for exoplanets around these stars or to identify brown dwarfs that are part of the association. Members of this region are suited for direct imaging of exoplanets, because young planets glow brightly in infrared wavelengths.

Members[6][7] 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.
Close up on the Orion Arm, with major stellar associations (yellow), nebulae (red) and dark nebulae (grey) around the Local Bubble, with the Taurus Molecular Cloud above the midfle (Sol).

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 "TMC-1 -- Molecular Cloud". SIMBAD. http://simbad.u-strasbg.fr/simbad/sim-id?submit=display&bibdisplay=refsum&bibyear1=1850&bibyear2=%24currentYear&Ident=%40732625&Name=TMC-1#lab_bib. 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. doi:10.1088/0067-0049/186/1/111. ISSN 0067-0049. Bibcode: 2010ApJS..186..111L. 
  3. ↑ Guedel, M.; Briggs, K. R.; Arzner, K.; Audard, M. et al. (2007). "The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST)". Astronomy and Astrophysics 468 (2): 353–377. doi:10.1051/0004-6361:20065724. Bibcode: 2007A&A...468..353G. 
  4. ↑ A. Freeman and T. J. Millar (1983), Formation of complex molecules in TMC-1. Nature, volume 301, 402-404 doi:10.1038/301402a0
  5. ↑ Kenyon, Scott J.; Hartmann, Lee (November 1995). "Pre-Main-Sequence Evolution in the Taurus-Auriga Molecular Cloud" (in en). Astrophysical Journal Supplement Series 101: 117. doi:10.1086/192235. ISSN 0067-0049. Bibcode: 1995ApJS..101..117K. 
  6. ↑ 6.0 6.1 Gagné, Jonathan; Mamajek, Eric E.; Malo, Lison; Riedel, Adric; Rodriguez, David; Lafrenière, David; Faherty, Jacqueline K.; Roy-Loubier, Olivier et al. (March 2018). "BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc" (in en). Astrophysical Journal 856 (1): 23. doi:10.3847/1538-4357/aaae09. ISSN 0004-637X. Bibcode: 2018ApJ...856...23G. 
  7. ↑ Kwon, Woojin; Looney, Leslie W.; Mundy, Lee G. (October 2011). "Resolving the Circumstellar Disk of Hl Tauri at Millimeter Wavelengths" (in en). The Astrophysical Journal 741 (1): 3. doi:10.1088/0004-637X/741/1/3. ISSN 0004-637X. Bibcode: 2011ApJ...741....3K. 
  8. ↑ "V1298 Tau". https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=V1298%20Tau&type=PLANET_HOST. 
  9. ↑ 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" (in en). Astrophysical Journal Letters 885 (1): L12. doi:10.3847/2041-8213/ab4c99. ISSN 0004-637X. Bibcode: 2019ApJ...885L..12D. 

Coordinates: Sky map 04h 41m 00s, +25° 52′ 00″




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