{{Short description|Interstellar molecular cloud in the constellations Taurus and Auriga}} {{redirect|TMC-1|the gene|TMC1}} {{infobox nebula | type = giant molecular cloud | name = Taurus molecular cloud | constellation = Taurus | epoch = J2000.0<ref name=SIMBAD>{{cite web |url= http://simbad.u-strasbg.fr/simbad/sim-id?submit=display&bibdisplay=refsum&bibyear1=1850&bibyear2=%24currentYear&Ident=%40732625&Name=TMC-1#lab_bib |title= TMC-1 – Molecular Cloud |publisher= SIMBAD |accessdate= 2014-03-14 }}</ref> | ra = {{RA|04|41.0}}<ref name=SIMBAD/> | dec = {{DEC|+25|52}}<ref name=SIMBAD/> | names = HCL&nbsp;2, {{nowrap|Heiles's cloud 2}}, TMC-1, {{nowrap|Taurus molecular cloud 1}}<ref name=SIMBAD/> | image = 300px | caption = Taurus molecular cloud (Herschel Space Observatory) |dist_ly=430|dist_pc=140|notes=Close distance, numerous molecular species}} {{Easy CSS image crop |Image = Emission nebulae behind molecular clouds in Perseus and Taurus.jpg |desired_width = 300 |crop_left_perc = 0 |crop_right_perc = 42 |crop_top_perc = 55 |crop_bottom_perc = 7 |align=right |description=Taurus molecular cloud (green and blue) in front of HII regions (red) as seen by the Northern Sky Narrowband Survey. The Pleiades (bright green nebulae on the right side) appear to be connected in this image. Indeed, they lie at the same distance, making it likely that this object is related.}} {{multiple image | align = right | direction = horizontal | image1 = APEX Turns its Eye to Dark Clouds in Taurus (zoom).ogv | width1 = 300 | alt1 = | caption1 = 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. | image2 = APEX Turns its Eye to Dark Clouds in Taurus (pan).ogv | width2 = 300 | alt2 = | caption2 = 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. It is only 140 pc (430 ly) away from Earth, making it possibly the nearest large star formation region. It hosts a stellar nursery containing hundreds of newly formed stars.<ref name="LuhmanAllen2010">{{cite journal |last1=Luhman |first1=K. L. |last2=Allen |first2=P. R. |last3=Espaillat |first3=C. |author3-link=Catherine Espaillat |last4=Hartmann |first4=L. |last5=Calvet |first5=N. |author5-link=Nuria Calvet |year=2010 |title=The Disk Population of the Taurus Star-Forming Region |journal=The Astrophysical Journal Supplement Series |volume=186 |issue=1 |pages=111–174 |arxiv=0911.5457 |bibcode=2010ApJS..186..111L |doi=10.1088/0067-0049/186/1/111 |issn=0067-0049 |s2cid=119189843}}</ref> 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.

It has been important in star formation studies at all wavelengths of Electromagnetic spectrum.<ref>{{cite journal |author=Guedel, M. |author2=Briggs, K. R. |author3=Arzner, K. |display-authors=etal |year=2007 |title=The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST) |journal=Astronomy and Astrophysics |volume=468 |issue=2 |pages=353–377 |arxiv=astro-ph/0609160 |bibcode=2007A&A...468..353G |doi=10.1051/0004-6361:20065724 |s2cid=8846597}}</ref> 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.

== Composition == The Taurus molecular clouds are notable because they contain many complex molecules, some of which are organic, and so far there have been over 100 different molecules including 75 main isotopic species, 20 carbon-13 substituted species, and seven deuterium-substituted species.<ref>{{Cite web |date=2025-10-27 |title=Astronomical data collection of Taurus Molecular Cloud-1 reveals over 100 different molecules |url=https://news.mit.edu/2025/astronomical-data-collection-reveals-over-100-different-molecules-1027 |access-date=2026-01-10 |website=MIT News {{!}} Massachusetts Institute of Technology |language=en}}</ref> The number of molecular species discovered make it the most prolific source of interstellar molecular discoveries. There is a stark contrast of the populations of molecules between TMC-1 and protoplanetary disks around protostars. TMC-1 has many unsaturated hydrocarbons while the disk of protostars have oxygen-rich organics found in sublimated ices.<ref>{{Cite journal |last1=Xue |first1=Ci |last2=Byrne |first2=Alex N. |last3=Morgan |first3=Larry |last4=Wenzel |first4=Gabi |last5=Changala |first5=P. Bryan |last6=Fried |first6=Zachary T. P. |last7=Loomis |first7=Ryan A. |last8=Remijan |first8=Anthony |last9=Bergin |first9=Edwin A. |last10=Cooke |first10=Ilsa R. |last11=Frayer |first11=David |last12=Burkhardt |first12=Andrew M. |last13=Charnley |first13=Steven B. |last14=Cordiner |first14=Martin A. |last15=Lipnicky |first15=Andrew |date=2025-10-23 |title=The Molecular Inventory of TMC-1 with GOTHAM Observations |journal=The Astrophysical Journal Supplement Series |volume=281 |issue=1 |pages=9 |doi=10.3847/1538-4365/ae04e5 |doi-access=free |arxiv=2509.06256 |bibcode=2025ApJS..281....9X |issn=0067-0049}}</ref>

Molecular that have been discovered in the Taurus molecular cloud includes Cyanopolyynes (HC<sub>''n''</sub>N for ''n''&nbsp;=&nbsp;3,5,7,9)<ref>{{cite journal | last1=Freeman | first1=A. | last2=Millar | first2=T. J. | title=Formation of complex molecules in TMC-1 | journal=Nature | volume=301 | issue=5899 | year=1983 | issn=0028-0836 | doi=10.1038/301402a0 | pages=402–404| bibcode=1983Natur.301..402F | s2cid=26107828 }}</ref>, cumulene carbenes ({{chem2|H2C_{''n''} }} for ''n''&nbsp;=&nbsp;3–6),<ref name="Cabezas 2021">{{cite journal |last1=Cabezas |first1=C. |last2=Tercero |first2=B. |last3=Agúndez |first3=M. |display-authors=etal |year=2021 |title=Cumulene carbenes in TMC-1: Astronomical discovery of ''l''-H<sub>2</sub>C<sub>5</sub> |journal=Astronomy & Astrophysics |volume=650 |page=L9 |arxiv=2106.00635 |bibcode=2021A&A...650L...9C |doi=10.1051/0004-6361/202141274 |issn=0004-6361 |pmc=7611420 |pmid=34334798}}</ref> ''N''-Chlorosuccinimide (NCS), Thioketenes (H<sub>2</sub>CCCS),<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Cabezas |first2=C. |last3=Agúndez |first3=M. |last4=Tercero |first4=B. |last5=Pardo |first5=J. R. |last6=Marcelino |first6=N. |last7=Gallego |first7=J. D. |last8=Tercero |first8=F. |last9=López-Pérez |first9=J. A. |last10=Vicente |first10=P. de |date=2021-04-01 |title=TMC-1, the starless core sulfur factory: Discovery of NCS, HCCS, H2CCS, H2CCCS, and C4S and detection of C5S |url=https://www.aanda.org/articles/aa/abs/2021/04/aa40642-21/aa40642-21.html |journal=Astronomy & Astrophysics |language=en |volume=648 |pages=L3 |doi=10.1051/0004-6361/202140642 |pmid=33850333 |pmc=7610586 |issn=0004-6361}}</ref> Thioacetaldehyde (CH<sub>3</sub>CHS),<ref name="thioacetaldehyde">{{cite journal |display-authors=1 |last1=Agúndez |first1=M. |last2=Molpeceres |first2=G. |last3=Cabezas |first3=C. |last4=Marcelino |first4=N. |last5=Tercero |first5=B. |last6=Fuentetaja |first6=R. |last7=de Vicente |first7=P. |last8=Cernicharo |first8=J. |title=Detection of thioacetaldehyde (CH 3 CHS) in TMC-1: Sulfur-oxygen differentiation along the hydrogenation sequence |journal=Astronomy & Astrophysics |date=January 2025 |volume=693 |pages=L20 |doi=10.1051/0004-6361/202453459 |arxiv=2501.05125 |url=https://www.aanda.org/articles/aa/full_html/2025/01/aa53459-24/aa53459-24.html}}</ref> Tricarbon monosulfide (HC<sub>3</sub>S<sup>+</sup>),<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Cabezas |first2=C. |last3=Endo |first3=Y. |last4=Marcelino |first4=N. |last5=Agúndez |first5=M. |last6=Tercero |first6=B. |last7=Gallego |first7=J. D. |last8=Vicente |first8=P. de |date=2021-02-01 |title=Space and laboratory discovery of HC3S+ |url=https://www.aanda.org/articles/aa/abs/2021/02/aa40013-20/aa40013-20.html |journal=Astronomy & Astrophysics |language=en |volume=646 |pages=L3 |doi=10.1051/0004-6361/202040013 |pmid=33824540 |pmc=7610522 |issn=0004-6361}}</ref> Vinylacetylene (CH<sub>2</sub>CHCCH), allenyl acetylene,<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Cabezas |first2=C. |last3=Agúndez |first3=M. |last4=Tercero |first4=B. |last5=Marcelino |first5=N. |last6=Pardo |first6=J. R. |last7=Tercero |first7=F. |last8=Gallego |first8=J. D. |last9=López-Pérez |first9=J. A. |last10=deVicente |first10=P. |date=2021-03-01 |title=Discovery of allenyl acetylene, H2CCCHCCH, in TMC-1 - A study of the isomers of C5H4 |url=https://www.aanda.org/articles/aa/abs/2021/03/aa40482-21/aa40482-21.html |journal=Astronomy & Astrophysics |language=en |volume=647 |pages=L3 |doi=10.1051/0004-6361/202140482 |pmid=33850332 |pmc=7610584 |issn=0004-6361}}</ref> Propionitrile (CH<sub>3</sub>CH<sub>2</sub>CN)<ref name=":1">{{Cite journal |last1=Cernicharo |first1=J. |last2=Agúndez |first2=M. |last3=Cabezas |first3=C. |last4=Marcelino |first4=N. |last5=Tercero |first5=B. |last6=Pardo |first6=J. R. |last7=Gallego |first7=J. D. |last8=Tercero |first8=F. |last9=López-Pérez |first9=J. A. |last10=Vicente |first10=P. de |date=2021-03-01 |title=Discovery of CH2CHCCH and detection of HCCN, HC4N, CH3CH2CN, and, tentatively, CH3CH2CCH in TMC-1 |url=https://www.aanda.org/articles/aa/abs/2021/03/aa40434-21/aa40434-21.html |journal=Astronomy & Astrophysics |language=en |volume=647 |pages=L2 |doi=10.1051/0004-6361/202140434 |pmid=33833468 |pmc=7610549 |issn=0004-6361}}</ref> ethynyl cyclopropenylidene (1,2),<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Agúndez |first2=M. |last3=Kaiser |first3=R. I. |last4=Cabezas |first4=C. |last5=Tercero |first5=B. |last6=Marcelino |first6=N. |last7=Pardo |first7=J. R. |last8=Vicente |first8=P. de |date=2021-11-01 |title=Discovery of two isomers of ethynyl cyclopentadiene in TMC-1: Abundances of CCH and CN derivatives of hydrocarbon cycles |url=https://www.aanda.org/articles/aa/abs/2021/11/aa42226-21/aa42226-21.html |journal=Astronomy & Astrophysics |language=en |volume=655 |pages=L1 |doi=10.1051/0004-6361/202142226 |arxiv=2110.09105 |bibcode=2021A&A...655L...1C |issn=0004-6361}}</ref> cyclopentadiene and indene.<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Agúndez |first2=M. |last3=Cabezas |first3=C. |last4=Tercero |first4=B. |last5=Marcelino |first5=N. |last6=Pardo |first6=J. R. |last7=Vicente |first7=P. de |date=2021-05-01 |title=Pure hydrocarbon cycles in TMC-1: Discovery of ethynyl cyclopropenylidene, cyclopentadiene, and indene |url=https://www.aanda.org/articles/aa/abs/2021/05/aa41156-21/aa41156-21.html |journal=Astronomy & Astrophysics |language=en |volume=649 |pages=L15 |doi=10.1051/0004-6361/202141156 |pmid=34257463 |pmc=7611194 |arxiv=2104.13991 |bibcode=2021A&A...649L..15C |issn=0004-6361}}</ref> The QUIJOTE survey have discovered several molecules such as cyanoacenaphthylene (3, 4),<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Tercero |first2=B. |last3=Marcelino |first3=N. |last4=López-Pérez |first4=J. A. |last5=Gallego |first5=J. D. |last6=Tercero |first6=F. |last7=Esplugues |first7=G. |last8=Cabezas |first8=C. |last9=Agúndez |first9=M. |last10=Limeres |first10=C. |last11=Steber |first11=A. L. |last12=Pérez |first12=D. |last13=Pérez |first13=C. |last14=Lesarri |first14=A. |last15=Vicente |first15=P. de |date=2026-01-01 |title=Discovery of two new isomers of cyanoacenaphthylene (C12H7CN) in the Taurus molecular cloud 1 with the QUIJOTE line survey |url=https://www.aanda.org/articles/aa/abs/2026/01/aa57893-25/aa57893-25.html |journal=Astronomy & Astrophysics |language=en |volume=705 |pages=L7 |doi=10.1051/0004-6361/202557893 |issn=0004-6361|doi-access=free }}</ref> ortho-benzyne (''o''-C<sub>6</sub>H<sub>4</sub>)<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Agúndez |first2=M. |last3=Kaiser |first3=R. I. |last4=Cabezas |first4=C. |last5=Tercero |first5=B. |last6=Marcelino |first6=N. |last7=Pardo |first7=J. R. |last8=Vicente |first8=P. de |date=2021-08-01 |title=Discovery of benzyne, o-C6H4, in TMC-1 with the QUIJOTE line survey |url=https://www.aanda.org/articles/aa/abs/2021/08/aa41660-21/aa41660-21.html |journal=Astronomy & Astrophysics |language=en |volume=652 |pages=L9 |doi=10.1051/0004-6361/202141660 |issn=0004-6361|arxiv=2108.02308 }}</ref> and fulvenallene.<ref>{{Cite journal |last1=Cernicharo |first1=J. |last2=Fuentetaja |first2=R. |last3=Agúndez |first3=M. |last4=Kaiser |first4=R. I. |last5=Cabezas |first5=C. |last6=Marcelino |first6=N. |last7=Tercero |first7=B. |last8=Pardo |first8=J. R. |last9=Vicente |first9=P. de |date=2022-07-01 |title=Discovery of fulvenallene in TMC-1 with the QUIJOTE line survey |url=https://www.aanda.org/articles/aa/abs/2022/07/aa44399-22/aa44399-22.html |journal=Astronomy & Astrophysics |language=en |volume=663 |pages=L9 |doi=10.1051/0004-6361/202244399 |arxiv=2207.09369 |bibcode=2022A&A...663L...9C |issn=0004-6361}}</ref> In 2007 the polyatomic anion octatetraynyl radical was detected in TMC-1, making it the second type of anion to be found in the interstellar medium and the largest such molecule detected to date.<ref>{{cite journal| journal=The Astrophysical Journal| volume=664 | issue=1 | pages=L47–L50 | date= July 20, 2007| title=Detection of C<sub>8</sub>H<sup>−</sup> and Comparison with C<sub>8</sub>H toward IRC +10 216| first1=Anthony J.| last1= Remijan|author2=J. M. Hollis |author3=F. J. Lovas |author4=M. A. Cordiner |author5=T. J. Millar |author6=A. J. Markwick-Kemper |author7=P. R. Jewell |doi=10.1086/520704 |bibcode=2007ApJ...664L..47R|doi-access=free }}</ref><ref>{{cite journal | journal= The Astrophysical Journal | issue=1 | volume=664 | pages=L43–L46 | date=July 20, 2007 | title=Detection of the Carbon Chain Negative Ion C<sub>8</sub>H<sup>−</sup> in TMC-1| first=S.| last= Brünken|author2=H. Gupta |author3=C. A. Gottlieb |author4=M. C. McCarthy |author5=P. Thaddeus |doi=10.1086/520703 |bibcode=2007ApJ...664L..43B| s2cid=120912943 }}</ref> 1-Butyne (CH<sub>3</sub>CH<sub>2</sub>CCH) was tentatively discovered.<ref name=":1" />

== Content == The stars in the Taurus molecular cloud are newly formed having an age of only 1–2 million years.<ref>{{Cite journal |last1=Kenyon |first1=Scott J. |last2=Hartmann |first2=Lee |date=November 1995 |title=Pre-Main-Sequence Evolution in the Taurus–Auriga Molecular Cloud |journal=Astrophysical Journal Supplement Series |language=en |volume=101 |pages=117 |bibcode=1995ApJS..101..117K |doi=10.1086/192235 |issn=0067-0049}}</ref> 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.<ref name=":0">{{Cite journal |last1=Gagné |first1=Jonathan |last2=Mamajek |first2=Eric E. |last3=Malo |first3=Lison |last4=Riedel |first4=Adric |last5=Rodriguez |first5=David |last6=Lafrenière |first6=David |last7=Faherty |first7=Jacqueline K. |author7-link=Jackie Faherty |last8=Roy-Loubier |first8=Olivier |last9=Pueyo |first9=Laurent |last10=Robin |first10=Annie C. |last11=Doyon |first11=René |date=March 2018 |title=BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc |journal=Astrophysical Journal |language=en |volume=856 |issue=1 |pages=23 |arxiv=1801.09051 |bibcode=2018ApJ...856...23G |doi=10.3847/1538-4357/aaae09 |issn=0004-637X |doi-access=free}}</ref> HH 30 is a protoplanetary disk seen edge-on located in TMC-1.<ref>{{Citation |last1=Tazaki |first1=Ryo |title=JWST Imaging of Edge-on Protoplanetary Disks. IV. Mid-infrared Dust Scattering in the HH 30 disk |date=2025-01-10 |arxiv=2412.07523 |last2=Ménard |first2=François |last3=Duchêne |first3=Gaspard |last4=Villenave |first4=Marion |last5=Ribas |first5=Álvaro |last6=Stapelfeldt |first6=Karl R. |last7=Perrin |first7=Marshall D. |last8=Pinte |first8=Christophe |last9=Wolff |first9=Schuyler G. |journal=The Astrophysical Journal |volume=980 |issue=1 |page=49 |doi=10.3847/1538-4357/ad9c6f |doi-access=free |bibcode=2025ApJ...980...49T }}</ref> Based on distance estimates of HP Tau G2, the right side of the cloud is a farther edge of the nebula.<ref>{{Cite journal |last=Torres |first=Rosa M. |last2=Loinard |first2=Laurent |last3=Mioduszewski |first3=Amy J. |last4=Rodríguez |first4=Luis F. |date=2009-05-19 |title=VLBA DETERMINATION OF THE DISTANCE TO NEARBY STAR-FORMING REGIONS. III. HP TAU/G2 AND THE THREE-DIMENSIONAL STRUCTURE OF TAURUS |url=https://iopscience.iop.org/article/10.1088/0004-637X/698/1/242 |journal=The Astrophysical Journal |volume=698 |issue=1 |pages=242–249 |doi=10.1088/0004-637X/698/1/242 |issn=0004-637X |via=IOP Science|arxiv=0903.5338 }}</ref>

Below is a list of members<ref name=":0" /><ref>{{Cite journal|last1=Kwon|first1=Woojin|last2=Looney|first2=Leslie W.|last3=Mundy|first3=Lee G.|title=Resolving the Circumstellar Disk of Hl Tauri at Millimeter Wavelengths|date=October 2011|journal=The Astrophysical Journal|language=en|volume=741|issue=1|pages=3|doi=10.1088/0004-637X/741/1/3|arxiv=1107.5275|bibcode=2011ApJ...741....3K|s2cid=118525138|issn=0004-637X}}</ref> of the Taurus–Auriga association with a circumstellar disk or exoplanet:

*HL Tauri – directly imaged disk with impressive details *SU Aurigae – circumstellar disk *AB Aurigae – circumstellar disk and hints of an exoplanet *CI Tauri – directly imaged circumstellar disk, one confirmed exoplanet and hints of additional exoplanets *V830 Tauri – circumstellar disk and one exoplanet V830 Tauri b *LkCa 15 – directly imaged circumstellar disk and one possible directly imaged exoplanet LkCa 15 b *GG Tauri – circumstellar disk *UX Tauri – circumstellar disk *2MASS J04202144+2813491 – directly imaged disk, jets and disk wind *DH Tauri – exoplanet DH Tauri b *DG Tauri B – circumstellar disk associated with jets *2M0437b – directly imaged exoplanet *V1298 Tauri – four confirmed transiting exoplanets<ref>{{Cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=V1298%20Tau&type=PLANET_HOST|title=V1298 Tau|website=exoplanetarchive.ipac.caltech.edu|access-date=2020-02-21}}</ref><ref>{{Cite journal|last1=David|first1=Trevor J.|last2=Petigura|first2=Erik A.|last3=Luger|first3=Rodrigo|last4=Foreman-Mackey|first4=Daniel|last5=Livingston|first5=John H.|last6=Mamajek|first6=Eric E.|last7=Hillenbrand|first7=Lynne A.|date=November 2019|title=Four Newborn Planets Transiting the Young Solar Analog V1298 Tau|journal=Astrophysical Journal Letters|language=en|volume=885|issue=1|pages=L12|doi=10.3847/2041-8213/ab4c99|arxiv=1910.04563|bibcode=2019ApJ...885L..12D|s2cid=204008446|issn=0004-637X |doi-access=free }}</ref><!-- This star might belong to "Group 29" in Oh et al. 2017, but this association is not confirmed --> * 2MASS J04442713+2512164 brown dwarf with a resolved disk and a planet candidate

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[[File:Regioni_celesti_scelte_-_Osc_A.png|thumb|350px|Main dark nebulae of the Solar apex half of the galactic plane, with the Taurus molecular cloud at the left edge.]]

== See also ==

* Taurus-Auriga association * Orion molecular cloud complex * Rho Ophiuchi cloud complex * Perseus molecular cloud * Cygnus X *List of nearby stellar associations and moving groups

==References== {{reflist}}

== External links == * [https://scixplorer.org/search?p=1&q=abs%3A%22taurus+molecular+cloud%22&sort=score+desc&sort=date+desc&d=astrophysics Taurus Molecular Cloud] at Science Explorer by ADS

{{Sky|04|41|00|+|25|52|00|430}}

Category:Dark nebulae Category:Gould Belt Category:Molecular clouds Category:Taurus (constellation) Category:Articles containing video clips Category:Star-forming regions