The object is a very hot gas giant; the estimated surface temperature is roughly 1200 K (930 °C or 1700 °F),[2] mostly due to gravitational contraction.[7] Its mass is well below the calculated limit for deuterium fusion in brown dwarfs, which is 13 Jupiter masses. The projected distance between 2M1207b and its primary is around 40 AU (similar to the mean distance between Pluto and the Sun).[8] Its infrared spectrum indicates the presence of water molecules in its atmosphere.[9][3] The object is not a likely candidate to support life, either on its surface or on any satellites.
Discovery and identification
Infrared image of 2M1207 (blueish) and 2M1207b (reddish). The two objects are separated by less than one arc second in Earth's sky. Image taken using the ESO's 8.2m Yepun VLT.
2M1207b is around 100 times fainter in the sky than its companion.[10] It was first spotted as a "faint reddish speck of light" in 2004 by the VLT. After the initial observation, there was some question as to whether the objects might be merely an optical double, but subsequent observations by the Hubble Space Telescope and the VLT have shown that the objects move together and are therefore presumably a binary system.[9]
An initial photometric estimate for the distance to 2M1207b was 70 parsecs.[4] In December 2005, American astronomer Eric Mamajek reported a more accurate distance (53±6 parsecs) to 2M1207b using the moving-cluster method.[11] Recent trigonometric parallax results have confirmed this moving-cluster distance, leading to a distance estimate of 52.75+1.04 −1.00 parsecs or 172 ± 3 light years.[4]
Properties
Estimates for the mass, size, and temperature of 2M1207b are still uncertain. Although spectroscopic evidence is consistent with a mass of 8 ± 2 Jupiter masses and a surface temperature of 1600 ± 100 kelvins, theoretical models for such an object predict a luminosity 10 times greater than observed. Because of this, lower estimates for the mass and temperature have been proposed. Alternatively, 2M1207b might be dimmed by a surrounding disk of dust and gas.[7] As an unlikely possibility, Mamajek and Michael Meyer have suggested that the planet is actually much smaller, but is radiating away heat generated by a recent collision.[12][13]
JWST observations of 2M1207B with NIRSpec did not detect any methane (CH4) and only weak carbon monoxide (CO) in the atmosphere of this object. The best-fit models show stronger methane and carbon monoxide bands than observed. A weaker methane band is a sign for nonequilibrium chemistry for young low-mass objects. The weakness of carbon monoxide could be attributed to other effects, such as temperature gradient or cloud thickness. The reasearchers used cloudless models that show some inconsistency with the temperature and absorption of methane and carbon monoxide, which might be resolved in the future with models that include clouds.[2]
The JWST observations were also able to detect emission of hydrogen (Paschen transitions) and the Helium I triplet at 1.083 μm. This is a sign of active accretion from a small circumstellar disk or circumplanetary disk.[2] For now this disk remains undetected, but it might be detected in future observations by JWST at longer wavelengths.[14]
Status as an exoplanet
Although the mass of 2M1207b is less than that required for deuterium fusion to occur, some 13 times the mass of Jupiter, and the image of 2M1207b has been widely hailed as the first direct image of an exoplanet, it may be questioned whether 2M1207b is actually a planet. Some definitions of the term planet require a planet to have formed in the same way as the planets in the Solar System did, by secondary accretion in a protoplanetary disk.[15] With such a definition, if 2M1207b formed by direct gravitational collapse of a gaseous nebula, it would be a sub-brown dwarf rather than a planet. A similar debate exists regarding the identity of GQ Lupi b, also first imaged in 2004.[16] On the other hand, the discovery of marginal cases like Cha 110913-773444—a free-floating, planetary-mass object—raises the question of whether distinction by formation is a reliable dividing line between stars/brown dwarfs and planets.[17] As of 2006, the International Astronomical Union Working Group on Extrasolar Planets described 2M1207b as a "possible planetary-mass companion to a brown dwarf."[18]
^A giant planet candidate near a young brown dwarf. Direct VLT/NACO observations using IR wavefront sensing, G. Chauvin, A.-M. Lagrange, C. Dumas, B. Zuckerman, D. Mouillet, I. Song, J.-L. Beuzit, P. Lowrance, Astronomy and Astrophysics, 425 (October 2004), pp. L29–L32. Bibcode:2004A&A...425L..29Cdoi:10.1051/0004-6361:200400056.
^ abThe Planetary Mass Companion 2MASS 1207-3932B: Temperature, Mass, and Evidence for an Edge-on Disk, Subhanjoy Mohanty, Ray Jayawardhana, Nuria Huelamo, and Eric Mamajek, Astrophysical Journal657, #2 (March 2007), pp. 1064–1091. Bibcode:2007ApJ...657.1064Mdoi:10.1086/510877.
^Estimated observed projected separation from observed angular separation and estimated distance.
^An Improbable Solution to the Underluminosity of 2M1207B: A Hot Protoplanet Collision Afterglow, Eric E. Mamajek and Michael R. Meyer, Astrophysical Journal668, #2 (October 2007), pp. L175–L178. Bibcode:2007ApJ...668L.175Mdoi:10.1086/522957.
