Giant Planet Companion to 2MASSW J1207334-393254

By G. Chauvin, Anne-Marie Lagrange, C. Dumas, B. Zuckerman, David Mouillet, Inseok Song, J. Beuzit, P. Lowrance. 2005

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We report new VLT/NACO imaging observations of the young, nearby brown dwarf 2MASSW J1207334-393254 and its suggested planetary mass companion (2M1207 b). Three epochs of VLT/NACO measurements obtained over nearly one year show that the planetary mass companion candidate shares the same proper motion and, with a high confidence level, is not a stationary background object. This result confirms the status of 2M1207 b as of planetary mass (5 times the mass of Jupiter) and the first image of a planetary mass companion in a different system than our own. This discovery offers new perspectives for our understanding of chemical and physical properties of planetary mass objects as well as their mechanisms of formation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d03fd10a14644081a1a5c0a85a32a6f4f5097ddc

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A probable giant planet imaged in the beta Pictoris disk. VLT/NaCo deep L'-band imaging (2008, background): “Its closeness and location inside theβ Pic disk suggest a formation process by core accretion or disk instabilities rather an binary like formation mechanisms proposed for the companions to 2M1207 and AB Pic (Chauvin et al. 2005a, b).”
THE NIRSPEC ULTRACOOL DWARF RADIAL VELOCITY SURVEY (2010, background): “…found orbiting a young brown dwarf in a Doppler survey conducted by Joergens & Müller (2007), a giant planetary companion to 2M1207−39 found by Chauvin et al. (2005) in a direct imaging survey, and a possible super-Earth orbiting the UCD MOA-2007-BLG-192 detected via microlensing (Bennett…”
Photometric characterization of exoplanets using angular and spectral differential imaging (2010, methodology): “Over the last decade, a handful of objects close to the planetary mass regime have been imaged with existing instruments, such as 2M 1207 b (Chauvin et al. 2005), DH Tau B (Itoh et al. 2005), GQ Lup b (Neuhäuser et al. 2005), AB Pic b (Chauvin et al. 2005), CHXR 73 B (Luhman et al. 2006), and more…”
The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation (2008, result): “One of the unbound low-mass binaries comprises a BD and a PM; it is therefore quite similar to 2MASS 1207-3932 (Chauvin et al. 2004, 2005).”
Hubble Space Telescope NICMOS Observations of T Dwarfs: Brown Dwarf Multiplicity and New Probes of the L/T Transition (2006, background): “However, two wider brown dwarf binaries systems have been recently identified in young cluster/associations: 2MASS J110119267732383 (Luhman 2004), a 240 AU binary in the ∼2 Myr Chameleon I association; and 2MASS J1207334-393254 (Chauvin et al. 2004, 2005), a 40 AU, very low mass (Mtot ∼ 0.03 M⊙) bro”
Adaptive Optics for Astronomy (2012, background): “In terms of their low luminosities, the favoured explanation – which was successfully applied to the first exoplanet directly imaged, 2MASS 1207 b (Chauvin et al. 2005) – is that very thick high latitude cloud bands absorb and scatter light when the planet is viewed pole-on (Skemer et al. 2011a).”
A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192 (2008, background): “Two brown dwarfs have previously been reported to have companions that could be of planetary mass (Chauvin et al. 2005; Joergens Müller 2007), but their mass ratios are q ∼ 0.2, which suggests that they did not form like the planetary systems around more massive stars.”
Discovery of Two T Dwarf Companions with the Spitzer Space Telescope (2006, background): “…G196-3 B (Rebolo et al. 1998), TWA 5 B (Lowrance et al. 1999; Neuhäuser et al. 2000b), HR 7329 B (Lowrance et al. 2000; Guenther et al. 2001), AB Pic B (Chauvin et al. 2005b), HD 49197 B (Metchev & Hillenbrand 2004), 2M 1207-3932 B (Chauvin et al. 2004, 2005a), and HD 203030 B (Metchev &…”
On the Luminosity of Young Jupiters (2006, background): “The companion to 2MASS1207 (Chauvin et al. 2005; Song et al. 2006) has an estimated luminosity of log(L/L⊙) ≈ −4.30 at an age of 8±3Myr.”
Synthetic Spectra and Colors of Young Giant Planet Atmospheres: Effects of Initial Conditions and Atmospheric Metallicity (2008, background): “Since there is some evidence from both observations (Chauvin et al. 2005) and theory (Boss 2001; Kroupa & Bouvier 2003; Ida & Lin 2004) that the “planetary” and “stellar” formation modes may overlap at several Jupiter masses, it will be important to be able to decipher a formation mechanism based…”
THE PALOMAR/KECK ADAPTIVE OPTICS SURVEY OF YOUNG SOLAR ANALOGS: EVIDENCE FOR A UNIVERSAL COMPANION MASS FUNCTION (2008, background): “…six known L/Ttransition companions (GJ 584C, Kirkpatrick et al. 2001; GJ 337CD, Wilson et al. 2001; Burgasser et al. 2005; 2MASS J1207334–393254B, Chauvin et al. 2005a; HD 203030B, Metchev & Hillenbrand 2006; HN PegB, Luhman et al. 2007a) are likely younger than the 2.9 Gyr model-dependent mean…”
High-Contrast Imaging from Space: Speckle Nulling in a Low-Aberration Regime (2005, unknown): “Chauvin et al. (2004, 2005) have reported the infrared imaging of an EGP orbiting the nearby young brown dwarf 2M1207 (2MASSWJ1207334 393254)withNACO (association of NAOS [Nasmyth Adaptive Optics System] and CONICA [High Resolution Near Infrared Camera]) at VLT (Very Large Telescope), whereas…”
THE VECTOR VORTEX CORONAGRAPH: LABORATORY RESULTS AND FIRST LIGHT AT PALOMAR OBSERVATORY (2009, background): “After the first resolved observation of a bound planetary mass object was obtained by Chauvin et al. (2005), several exoplanets have recently been imaged.”
Imaging Extrasolar Giant Planets (2016, background): “Two other substellar companions were discovered in this survey: GSC 08047-00232 B (Chauvin et al. 2005c), also independently found by Neuhäuser et al. (2003), and AB Pic B (Chauvin et al. 2005b), which resides near the deuterium-burning limit.”
THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, methodology): “…(e.g., Taurus and Upper Sco; Lafrenière et al. 2008; Todorov et al. 2010; Kraus & Ireland 2012), (2) members of nearby young moving groups (ages of 10–300 Myr, e.g., Lagrange et al. 2010; Chauvin et al. 2005a; Marois et al. 2008), and (3) unassociated nearby young stars (e.g., Kalas et al. 2008).”
The Interior Structure, Composition, and Evolution of Giant Planets (2009, background): “At long last, these searches are now bearing fruit (Chauvin et al. 2005; Marois et al. 2008; Kalas et al. 2008).”
Combining high-dispersion spectroscopy with high contrast imaging : Probing rocky planets around our nearest neighbors (2015, unknown): “This technique is now well established for young, massive self-luminous planets at significant orbital distances from their host star (e.g. Chauvin et al. 2005, Lagrange et al. 2009, Marois et al. 2008, Kalas et al. 2008).”
YOUNG L DWARFS IDENTIFIED IN THE FIELD: A PRELIMINARY LOW-GRAVITY, OPTICAL SPECTRAL SEQUENCE FROM L0 TO L5 (2008, background): “If indeed this object is quite young and very low-mass, it would be the lowest-mass L dwarf identified in the field and an analog to 2M 1207−39B, the very cool L dwarf companion found in TWA (Chauvin et al. 2005).”
CLOUDS AND CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HR8799b (2011, background): “Direct imaging of exoplanets is now becoming a regular occurrence with the recent discoveries of 2M1207b (Chauvin et al. 2005), Fomalhaut b (Kalas et al. 2008), Beta Pic b (Lagrange et al. 2009), 1RXS J1609 b (Lafrenière et al. 2008), and the quadruple-planetary system HR8799 b, c, d, and e…”