View source for 2M1207

{{Short description|Brown dwarf in the constellation Centaurus}}
{{Starbox begin
| name = 2M1207
}}
{{Starbox image
| image = [[Image:2M1207b - First image of an exoplanet.jpg|250px]]
| caption = [[European Southern Observatory]] infrared image of 2M1207 (bluish) and companion planet [[2M1207b]] (reddish), taken in 2004.
}}
{{Starbox observe
| epoch = [[J2000.0]] ([[International Celestial Reference System|ICRS]])
| constell = [[Centaurus]]<ref>{{cite constellation|2M1207}}</ref>
| ra = {{RA|12|07|33.47}}<ref name=dr3/>
| dec = {{DEC|−39|32|54.0}}<ref name=dr3/>
| appmag_v = 20.15<ref name=dc08>{{cite journal | doi=10.1051/0004-6361:20078886 | title=An accurate distance to 2M1207Ab | date=2008 | last1=Ducourant | first1=C. | last2=Teixeira | first2=R. | last3=Chauvin | first3=G. | last4=Daigne | first4=G. | last5=Le Campion | first5=J.-F. | last6=Song | first6=I. | last7=Zuckerman | first7=B. | journal=Astronomy & Astrophysics | volume=477 | issue=1 | pages=L1–L4 | arxiv=0711.0842 | bibcode=2008A&A...477L...1D }}</ref>
}}
{{Starbox character
| type = [[brown dwarf]]<ref name=sb />
| v-r = +2.1<ref name=dc08 />
| r-i = +2.1<ref name=dc08 />
| class = M8IVe<ref name=sb />
}}
{{Starbox astrometry
| prop_mo_ra = {{val|-64.040|0.087}}<ref name=dr3/>
| prop_mo_dec = {{val|-23.678|0.072}}<ref name=dr3/>
| parallax = 15.4624
| p_error = 0.1163
| parallax_footnote = <ref name=dr3>{{Cite Gaia DR3|3459372646830687104}}</ref>
}}
{{Starbox detail
| mass = ~0.025<ref name=mamajek />
| temperature = 2550 ± 150<ref name=mohanty>{{cite journal | doi=10.1086/510877 | title=The Planetary Mass Companion 2MASS 1207−3932B: Temperature, Mass, and Evidence for an Edge-on Disk | date=2007 | last1=Mohanty | first1=Subhanjoy | last2=Jayawardhana | first2=Ray | last3=Huelamo | first3=Nuria | last4=Mamajek | first4=Eric | journal=The Astrophysical Journal | volume=657 | issue=2 | pages=1064–1091 | arxiv=astro-ph/0610550 | bibcode=2007ApJ...657.1064M }}</ref>
| age = 5-10 Million<ref name=mohanty />
| radius = ~0.25<ref name=mohanty />
| luminosity = ~0.002<ref name=mohanty />
}}
{{Starbox catalog
| names = 2MASSW J1207334−393254, 2MASS J12073346−3932539, TWA 27<ref name=sb>{{cite simbad|title=TWA 27|access-date=June 15, 2008}}</ref>
}}
{{Starbox reference
| Simbad = NAME+2M1207A
}}
{{Starbox end}}
'''2M1207''', '''2M1207A''' or '''2MASS J12073346−3932539''' is a [[brown dwarf]] located in the [[constellation]] [[Centaurus]]; a companion object, [[2M1207b]], may be the first [[exoplanet|extrasolar]] [[planetary-mass object|planetary-mass companion]] to be directly imaged, and is the first discovered orbiting a brown dwarf.<ref name=mohanty /><ref>{{cite journal
  | last = Chauvin
  | first = G.
  |author2=Lagrange, A.-M.|author3=Dumas, C.|author4=Zuckerman, B.|author5=Mouillet, D.|author6=Song, I.|author7=Beuzit, J.-L.|author8=Lowrance, P.
  | title = A Giant Planet Candidate near a Young Brown Dwarf
  | journal = Astron. Astrophys.
  | volume = 425
  | issue = 2
  | pages = L29–L32
  | year = 2004
  | arxiv = astro-ph/0409323
  | doi = 10.1051/0004-6361:200400056|bibcode = 2004A&A...425L..29C | s2cid = 15948759
 }}</ref>

2M1207 was discovered during the course of the [[2MASS]] [[infrared]] sky survey: hence the "2M" in its name, followed by its celestial coordinates.  With a fairly early (for a brown dwarf) [[stellar classification|spectral type]] of M8,<ref name=sb /> it is very young, and probably a member of the [[TW Hydrae]] association.  Its estimated mass is around 25 [[Jupiter]] masses.<ref name=mamajek /> The companion, 2M1207b, is estimated to have a mass of 5–6 Jupiter masses.<ref name="Luhman et al 2023">{{Cite journal |last1=Luhman |first1=K. L. |last2=Tremblin |first2=P. |last3=Birkmann |first3=S. M. |last4=Manjavacas |first4=E. |last5=Valenti |first5=J. |last6=Alves de Oliveira |first6=C. |last7=Beck |first7=T. L. |last8=Giardino |first8=G. |last9=Lützgendorf |first9=N. |last10=Rauscher |first10=B. J. |last11=Sirianni |first11=M. |date=2023-06-01 |title=JWST/NIRSpec Observations of the Planetary Mass Companion TWA 27B |journal=The Astrophysical Journal |volume=949 |issue=2 |pages=L36 |doi=10.3847/2041-8213/acd635 |issn=0004-637X|doi-access=free |arxiv=2305.18603 |bibcode=2023ApJ...949L..36L }}</ref>  Still glowing red hot, it will shrink to a size slightly smaller than Jupiter as it cools over the next few billion years.

An initial photometric estimate for the distance to 2M1207 was 70 parsecs.<ref name=mamajek />  In December 2005, American astronomer {{Interlanguage link multi|Eric Mamajek|fr}} reported a more accurate distance (53 ± 6 parsecs) to 2M1207 using the [[moving cluster method]].<ref>{{cite journal | bibcode=2005ApJ...634.1385M | author=Mamajek| title= A Moving Cluster Distance to the Exoplanet 2M1207b in the TW Hydrae Association | journal= The Astrophysical Journal| volume=634 | issue=2 | year=2005 | pages=1385–1394| doi= 10.1086/468181 |arxiv = astro-ph/0507416 | s2cid=17162407}}</ref> The new distance gives a fainter [[luminosity]] for 2M1207.  Recent trigonometric [[parallax]] results have confirmed this moving cluster distance, leading to a distance estimate of 53 ± 1 [[parsec]] or 172 ± 3 [[light years]].<ref name="mamajek">[http://www.cfa.harvard.edu/~emamajek/memo_2m1207.html "The Distance to the 2M1207 System"] {{webarchive|url=https://web.archive.org/web/20080124115127/http://www.cfa.harvard.edu/~emamajek/memo_2m1207.html |date=2008-01-24 }}, Eric Mamajek, November 8, 2007.  Accessed on line June 15, 2008.</ref>
==Planetary system==
Like classical [[T Tauri stars]], many brown dwarfs are surrounded by [[protoplanetary disk|disks of gas and dust]] which accrete onto the brown dwarf.<ref>[http://origins.jpl.nasa.gov/library/extrasolar/121302-a.html More Sun-like stars may have planetary systems than currently thought] {{webarchive|url=https://web.archive.org/web/20080917173420/http://origins.jpl.nasa.gov/library/extrasolar/121302-a.html |date=2008-09-17 }}, library, Origins program, [[NASA]].  Accessed on line June 16, 2008.</ref><ref name=uv>{{cite journal | doi=10.1086/462414 | title=First Ultraviolet Spectrum of a Brown Dwarf: Evidence for H <sub>2</sub> Fluorescence and Accretion | date=2005 | last1=Gizis | first1=John E. | last2=Shipman | first2=Harry L. | last3=Harvin | first3=James A. | journal=The Astrophysical Journal | volume=630 | issue=1 | pages=L89–L91 | arxiv=astro-ph/0507429 | bibcode=2005ApJ...630L..89G }}</ref>  2M1207 was first suspected to have such a disk because of its broad H<sub>α</sub> line.  This was later confirmed by [[ultraviolet]] [[spectroscopy]].<ref name=uv />  The existence of a dust disk has also been confirmed by [[infrared]] observations<ref>{{cite journal | doi=10.1086/502647 | title=''Spitzer'' Observations of Two TW Hydrae Association Brown Dwarfs | date=2006 | last1=Riaz | first1=Basmah | last2=Gizis | first2=John E. | last3=Hmiel | first3=Abraham | journal=The Astrophysical Journal | volume=639 | issue=2 | pages=L79–L82 | arxiv=astro-ph/0606666 | bibcode=2006ApJ...639L..79R }}</ref> and with [[Atacama Large Millimeter Array|ALMA]].<ref name="Ricci et al. 2017">{{Cite journal |last1=Ricci |first1=L. |last2=Cazzoletti |first2=P. |last3=Czekala |first3=I. |last4=Andrews |first4=S. M. |last5=Wilner |first5=D. |last6=Szűcs |first6=L. |last7=Lodato |first7=G. |last8=Testi |first8=L. |last9=Pascucci |first9=I. |last10=Mohanty |first10=S. |last11=Apai |first11=D. |last12=Carpenter |first12=J. M. |last13=Bowler |first13=B. P. |date=2017-07-01 |title=ALMA Observations of the Young Substellar Binary System 2M1207 |journal=The Astronomical Journal |volume=154 |issue=1 |pages=24 |doi=10.3847/1538-3881/aa78a0 |issn=0004-6256|doi-access=free |arxiv=1706.03708 |bibcode=2017AJ....154...24R |hdl=10150/624920 |hdl-access=free }}</ref>  In general, [[accretion disk|accretion from disks]] are known to produce fast-moving [[jet (astronomy)|jets]], perpendicular to the disk, of ejected material.<ref>Accretion-ejection models of astrophysical jets, R. E. Pudritz, in ''Accretion Disks, Jets and High-energy Phenomena in Astrophysics'', Vassily Beskin, Gilles Henri, Francois Menard, Guy Pelletier, and [[Jean Dalibard]], eds., NATO Advanced Study Institute, Les Houches, session LXXVIII, EDP Sciences/Springer, 2003.  {{ISBN|3-540-20171-8}}.</ref>  This has also been observed for 2M1207; an April 2007 paper in the ''[[Astrophysical Journal]]'' reports that this brown dwarf is spouting jets of material from its poles.<ref name="Whelan et al 2007">{{cite journal | doi= 10.1086/516734 | author=Whelan| title= Discovery of a Bipolar Outflow from 2MASSW J1207334-393254, a 24 MJup Brown Dwarf| journal= The Astrophysical Journal| volume=659 | date=April 10, 2007 | issue= 1 | pages=L45 – L48 | bibcode = 2007ApJ...659L..45W | last2= Ray | first2= T. P. | last3= Randich | first3= S. | last4= Bacciotti | first4= F. | last5= Jayawardhana | first5= R. | last6= Testi | first6= L. | last7= Natta | first7= A. | last8= Mohanty | first8= S. |arxiv = astro-ph/0703112 | s2cid=14575014|display-authors=etal}}</ref>  The jets, which extend around 10<sup>9</sup> kilometers into space, were discovered using the [[Very Large Telescope]] (VLT) at the [[European Southern Observatory]].  Material in the jets streams into space at a few kilometers per second.<ref name=sp>[http://www.space.com/scienceastronomy/070528_mm_bdwarf_jets.html Small Stars Create Big Fuss], Ker Than, May 28, 2007, space.com.  Accessed on line June 15, 2008.</ref> While previous observations with the [[Spitzer Space Telescope|Spitzer]] spectrograph already detected [[acetylene]] (C<sub>2</sub>H<sub>2</sub>) [[Emission spectrum|emission]] in the disk of 2M1207, new observations with [[Mid-Infrared Instrument|MIRI]] revealed emission of a wide variety of [[chemicals]] in the disk, showing a [[carbon]]-rich chemistry. In this study 2M1207 and [[ISO-ChaI 147]] showed the largest number of [[organic molecules]], including the only detection of [[ethylene]] (C<sub>2</sub>H<sub>4</sub>) in this sample. The detected chemicals include 9 [[hydrocarbons]], with [[diacetylene]] (C<sub>4</sub>H<sub>2</sub>) and [[benzene]] (C<sub>6</sub>H<sub>6</sub>) being two prominent emission lines in the spectrum of 2M1207. Other emissions by chemicals in the disk are [[hydrogen]] gas (H<sub>2</sub>), [[hydrogen cyanide]] (HCN) and [[carbon dioxide]] (CO<sub>2</sub>).<ref name="Arabhavi2025">{{cite journal|arxiv=2506.02748 |last1=Arabhavi |first1=A. M. |last2=Kamp |first2=I. |last3=Henning |first3=Th. |last4=van Dishoeck |first4=E. F. |last5=Jang |first5=H. |last6=Waters |first6=L. B. F. M. |last7=Christiaens |first7=V. |last8=Gasman |first8=D. |last9=Pascucci |first9=I. |last10=Perotti |first10=G. |last11=Grant |first11=S. L. |last12=Güdel |first12=M. |last13=Lagage |first13=P. -O. |last14=Barrado |first14=D. |last15=Caratti o Garatti |first15=A. |last16=Lahuis |first16=F. |last17=Kaeufer |first17=T. |last18=Kanwar |first18=J. |last19=Morales-Calderón |first19=M. |last20=Schwarz |first20=K. |last21=Sellek |first21=A. D. |last22=Tabone |first22=B. |last23=Temmink |first23=M. |last24=Vlasblom |first24=M. |last25=Patapis |first25=P. |title=MINDS: The very low-mass star and brown dwarf sample. Detections and trends in the inner disk gas |journal=Astronomy & Astrophysics |date=2025 |volume=699 |pages=A194 |doi=10.1051/0004-6361/202554109 |bibcode=2025A&A...699A.194A }}</ref>

2M1207b shows weak accretion from a disk, inferred from emission lines of [[hydrogen]] and [[helium]] in medium-resolution [[NIRSpec]] data. Surprisingly 2M1207b does not show absorption due to [[methane]], which was predicted to be present for this object. It was suggested that very young objects have a L/T-transition starts at a later spectral type.<ref>{{Cite journal |last1=Elena |first1=Manjavacas |last2=Tremblin |first2=Pascal |last3=Birkmann |first3=Stephan |last4=Valenti |first4=Jeff |last5=Alves de Oliveira |first5=Catarina |last6=Beck |first6=Tracy L. |last7=Giardino |first7=G. |last8=Luetzgendorf |first8=N. |last9=Rauscher |first9=B. J. |last10=Sirianni |first10=M. |date=February 2024 |title=Medium Resolution 0.97-5.3 micron spectra of Very Young Benchmark Brown Dwarfs with NIRSpec onboard the James Webb Space Telescope |url=https://ui.adsabs.harvard.edu/abs/2024arXiv240204230M/abstract |journal=AJ |arxiv=2402.04230}}</ref>

{{OrbitboxPlanet begin
| name = 2M1207A
| table_ref =<ref name="Luhman et al 2023"/><ref name="Ricci et al. 2017"/><ref>{{Cite journal |last1=Blunt |first1=Sarah |last2=Nielsen |first2=Eric L. |last3=De Rosa |first3=Robert J. |last4=Konopacky |first4=Quinn M. |last5=Ryan |first5=Dominic |last6=Wang |first6=Jason J. |last7=Pueyo |first7=Laurent |last8=Rameau |first8=Julien |last9=Marois |first9=Christian |last10=Marchis |first10=Franck |last11=Macintosh |first11=Bruce |last12=Graham |first12=James R. |last13=Duchêne |first13=Gaspard |last14=Schneider |first14=Adam C. |date=2017-05-01 |title=Orbits for the Impatient: A Bayesian Rejection-sampling Method for Quickly Fitting the Orbits of Long-period Exoplanets |journal=The Astronomical Journal |volume=153 |issue=5 |pages=229 |doi=10.3847/1538-3881/aa6930 |issn=0004-6256|doi-access=free |arxiv=1703.10653 |bibcode=2017AJ....153..229B }}</ref>
| period_unit = year
}}
{{OrbitboxPlanet disk
| disk = circumstellar disk
| apoapsis = {{val|9.4|1.5}}
| inclination = {{val|35|20|15}}
}}
{{OrbitboxPlanet
| exoplanet = [[2M1207b|b]]
| radius = 1.399&nbsp;{{±|0.008|0.010}}<ref name=Zhang2025/>
| mass = {{val|5.5|0.5}}<ref name="Luhman et al 2023"/>
| semimajor = ≥ 49.8 ± 1.1{{efn|From Gaia distance of 64.7 ± 0.5 parsec and observed angular separation of 769 ± 10 milliarseconds (angular separation from Mohanty 2007, above). Real semimajor axis might be higher due to viewing angle and eccentricity of the orbit.}}
| period = {{val|633|–|20046}}
| eccentricity = {{val|0.02|–|0.98}}
| inclination = {{val|13|–|150}}
}}
{{Orbitbox end}}

== See also ==
* [[Lists of exoplanets]]
* [[Methods of detecting exoplanets#Direct imaging|Direct imaging of extrasolar planets]]

==Notes==
{{efnlist}}
==References==
{{reflist|refs=

<ref name=Zhang2025>{{cite journal |title=Elemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b |url=https://ui.adsabs.harvard.edu/abs/2025AJ....170...64Z/abstract |date=August 2025 |access-date=27 October 2025 | author1=Zhang, Zhoujian |author2=Mollière, Paul |author3=Fortney, Jonathan J. |author4=Marley, Mark S. |journal= The Astronomical Journal|volume=170 |issue=2  |page=64 |doi=10.3847/1538-3881/addfcb |doi-access=free |arxiv=2502.18559 |bibcode=2025AJ....170...64Z }}</ref>

}}

==External links==
* [http://space.com/scienceastronomy/aas_exoplanet_050110.html Space.com - Astronomers Confident: Planet Beyond Solar System Has Been Photographed]
* [http://www.space.com/scienceastronomy/planet_photo_040910.html Space.com article on the discovery]
* {{cite encyclopedia|url=http://exoplanet.eu/star.php?st=2M1207 |title=Notes for star 2M1207 |author=Jean Schneider |year=2011 |access-date=3 October 2011 |url-status=dead |archive-url=https://web.archive.org/web/20111006004013/http://exoplanet.eu/star.php?st=2M1207 |encyclopedia=[[Extrasolar Planets Encyclopaedia]] |archive-date=6 October 2011 }}
* [https://web.archive.org/web/20041013153848/http://www.sc.eso.org/~gchauvin/Gg222.pdf "A Giant Planet Candidate Near a Young Brown Dwarf" (PDF)] from the [[European Southern Observatory]].
* {{cite journal |arxiv=astro-ph/0507416|bibcode=2005ApJ...634.1385M |title=A Moving Cluster Distance to the Exoplanet 2M1207b in the TW Hydrae Association |last1=Mamajek |first1=Eric E. |journal=The Astrophysical Journal |date=2005 |volume=634 |issue=2 |page=1385 |doi=10.1086/468181 }}

{{Sky|12|07|33.47|-|39|32|54.0|172}}

{{Stars of Centaurus}}

{{DEFAULTSORT:2M1207}}
[[Category:2M1207| ]]
[[Category:M-type brown dwarfs]]
[[Category:Centaurus]]
[[Category:TW Hydrae association]]
[[Category:Planetary systems with one confirmed planet]]
[[Category:2MASS objects|J12073346-3932539]]
[[Category:Free-floating substellar objects]]