Editing 2M1207 (section)

==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>First Ultraviolet Spectrum of a Brown Dwarf: Evidence for H<sub>2</sub> Fluorescence and Accretion, John E. Gizis, Harry L. Shipman, and James A. Harvin, ''Astrophysical Journal'' '''630''', #1 (September 2005), pp. L89–L91. {{bibcode|2005ApJ...630L..89G}} {{doi|10.1086/462414}}.</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>Spitzer Observations of Two TW Hydrae Association Brown Dwarfs, Basmah Riaz, John E. Gizis, and Abraham Hmiel, ''Astrophysical Journal'' '''639''', #2 (March 2006), pp. L79–L82. {{bibcode|2006ApJ...639L..79R}} {{doi|10.1086/502647}}.</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>

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]]
| mass = 5–6
| semimajor = ≥49.8 ± 1.1<ref>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.</ref>
| period = 633-20046
| eccentricity = 0.02-0.98
| inclination = 13-150
}}
{{Orbitbox end}}