<i>HST</i>NICMOS Imaging of the Planetary‐mass Companion to the Young Brown Dwarf 2MASSW J1207334−393254

Song, Inseok; Schneider, Glenn; Zuckerman, B.; Farihi, Jay; Becklin, E. E.; Bessell, M. S.; Lowrance, P.; Macintosh, Bruce

doi:10.1086/507831

Cited by 72 publications

(63 citation statements)

References 25 publications

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“…By contrast, the frequency of hot Jupiters around M-stars is lower than that for higher mass stars (e.g., Johnson et al 2010). The detection of brown dwarfs with directly-imaged planetary mass companions (Chauvin et al 2004;Song et al 2006) indicate that at least some substellar objects are associated with planet formation early in their history. The overall exoplanet population frequency remains unclear around brown dwarfs.…”

Section: Introductionmentioning

confidence: 90%

The Taurus Boundary of Stellar/Substellar (TBOSS) Survey

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Patience

Ward-Duong

et al. 2014

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With the PACS instrument on Herschel, 134 low mass members of the Taurus star-forming region spanning the M4-L0 spectral type range and covering the transition from low mass stars to brown dwarfs were observed. Combining the new Herschel results with other Herschel programs, a total of 150 of the 154 M4-L0 Taurus members have observations, and we have added an additional 3 targets from Spitzer to form the 153-object TBOSS (Taurus Boundary of Stellar/Substellar) sample, a 99% complete study. Among the 150 targets, 70 µm flux densities were measured for 7 of the 7 Class I objects, 48 of the 67 Class II objects, and 3 of the 76 Class III objects. For the detected Class II objects, the median 70 µm flux density level declines with spectral type; however, the distribution of excess relative to central object flux density does not change across the stellar/substellar boundary in the M4-L0 range. Connecting the 70 µm TBOSS values with the results from K0-M3 Class II members results in the first comprehensive census of far-IR emission across the full mass spectrum of the stellar and substellar population of a star-forming region, and the median flux density declines with spectral type in a trend analogous to the flux density decline expected for the central objects. Spectral energy distributions (SEDs) were constructed for all TBOSS targets covering the optical to far-IR range and extending to the submm/mm for a subset of sources with longer wavelength data. Based on an initial exploration of the impact of different physical parameters on the Herschel flux densities, geometrical factors such as inclination and structural parameters such as scale height and flaring have the largest influence on the flux densities in the PACS bands. From the 24 µm to 70 µm spectral index of the SEDs, 5 new candidate transition disks were identified. Considering the previously known and new candidate transition disks, the spectral indices over longer wavelengths (≥70 µm) are not distinct from those of the full Class II population, suggesting that the outer regions of the transition disks are similar to Class II disks. The steep 24 µm to 70 µm slope for a subset of 8 TBOSS targets may be an indication of truncated disks in these systems, however additional measurements are required to establish the outer radii of these disks conclusively. From existing high angular resolution companion search observations, two examples of mixed pair systems that include secondaries with disks were measured in the Herschel data. Finally, comparing the TBOSS results with a Herschel study of Ophiuchus brown dwarfs reveals a lower fraction of disks around the Taurus substellar population with flux densities comparable to the Ophiuchus disks.

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Section: Introductionmentioning

confidence: 90%

The Taurus Boundary of Stellar/Substellar (TBOSS) Survey

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Patience

Ward-Duong

et al. 2014

A&A

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“…More recently, Mamajek (2005) has discussed the membership of TWA22 AB to TWA based on its kinematics properties and estimates a probability of 2% for TWA22 to be a member of TWA from an implemented convergence point technique (de Bruijne 1999). However, Song et al (2006) mentioned that the strong Li line of TWA22 AB is observed only for young active M dwarfs in the direction of TWA with the exception of a very few M-type members of the β Pictoris moving group (BPMG). Finally, Mentuch et al (2008) obtained a new visible high-resolution spectrum of TWA22 AB.…”

Section: Age and Membership Of Twa22 Abmentioning

confidence: 99%

The young, tight, and low-mass binary TWA22AB: a new calibrator for evolutionary models?

Bonnefoy¹,

Chauvin²,

Dumas³

et al. 2009

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Context. Tight binaries discovered in young, nearby associations are ideal targets for providing dynamical mass measurements to test the physics of evolutionary models at young ages and very low masses. Aims. We report the binarity of TWA22 for the first time. We aim at monitoring the orbit of this young and tight system to determine its total dynamical mass using an accurate distance determination. We also intend to characterize the physical properties (luminosity, effective temperature, and surface gravity) of each component based on near-infrared photometric and spectroscopic observations. Methods. We used the adaptive-optics assisted imager NACO to resolve the components, to monitor the complete orbit and to obtain the relative near-infrared photometry of TWA22 AB. The adaptive-optics assisted integral field spectrometer SINFONI was also used to obtain medium-resolution (R λ = 1500−2000) spectra in JHK bands. Comparison with empirical and synthetic librairies were necessary for deriving the spectral type, the effective temperature, and the surface gravity for each component of the system. Results. Based on an accurate trigonometric distance (17.5±0.2 pc) determination, we infer a total dynamical mass of 220±21 M Jup for the system. From the complete set of spectra, we find an effective temperature T eff = 2900 +200 −200 K for TWA22 A and T eff = 2900 +200 −100 K for TWA22 B and surface gravities between 4.0 and 5.5 dex. From our photometry and an M6 ± 1 spectral type for both components, we find luminosities of log(L/L ) = −2.11 ± 0.13 dex and log(L/L ) = −2.30 ± 0.16 dex for TWA22 A and B, respectively. By comparing these parameters with evolutionary models, we question the age and the multiplicity of this system. We also discuss a possible underestimation of the mass predicted by evolutionary models for young stars close to the substellar boundary.

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“…By converting the K s absolute magnitude into luminosity using a bolometric correction appropriate for mid and late-L dwarfs (Golimowski et al 2004), based on his nearer distance estimate, he derived a mass of 3-4 M Jup from both DUSTY and COND evolutionary models (Baraffe et al 2003). With HST/NICMOS multi-band (0.9 to 1.6 µm) photometry and a distance estimate of 59±7 pc, Song et al (2006) derived a mass of 5 ±3 M Jup for 2M1207 b, due to its brighter flux than expected from model predictions at shorter wavelengths (for a given mass and age) and to the scatter in the emergent flux predicted by the DUSTY and COND03 evolutionary models at wavelengths less than 2.2 µm (and shown in Fig. 3).…”

Section: Discussionmentioning

confidence: 99%

“…The space motion determination for the TWA was based on the four members with known Hipparcos distance: TWA1, TWA4, TWA9, and TWA11. Song et al (2006) suggests that significant uncertainties in the Hipparcos distance to TWA9 might affect the cluster distance estimation. They proposed a new distance estimate of 59 ± 7 pc based on an improved proper motion determination for 2M1207A scaled with the proper motion and the Hipparcos distance to HR 4796 A (TWA11).…”

Section: Introductionmentioning

confidence: 99%

An accurate distance to 2M1207Ab

Ducourant¹,

Teixeira

Chauvin³

et al. 2007

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Context. In April 2004, the first image was obtained of a planetary mass companion (now known as 2M1207 b) in orbit around a self-luminous object different from our own Sun (the young brown dwarf 2MASSW J1207334-393254, hereafter 2M1207 A). That 2M1207 b probably formed via fragmentation and gravitational collapse offered proof that such a mechanism can form bodies in the planetary mass regime. However, the predicted mass, luminosity, and radius of 2M1207 b depend on its age, distance, and other observables, such as effective temperature. Aims. To refine our knowledge of the physical properties of 2M1207 b and its nature, we accurately determined the distance to the 2M1207 A and b system by measuring of its trigonometric parallax at the milliarcsec level. Methods. With the ESO NTT/SUSI2 telescope, we began a campaign of photometric and astrometric observations in 2006 to measure the trigonometric parallax of 2M1207 A.Results. An accurate distance (52.4 ± 1.1 pc) to 2M1207A was measured. From distance and proper motions we derived spatial velocities that are fully compatible with TWA membership. Conclusions. With this new distance estimate, we discuss three scenarios regarding the nature of 2M1207 b: (1) a cool (1150 ± 150 K) companion of mass 4 ± 1 M Jup , (2) a warmer (1600 ± 100 K) and heavier (8 ± 2 M Jup ) companion occulted by an edge-on circumsecondary disk, or (3) a hot protoplanet collision afterglow.

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HSTNICMOS Imaging of the Planetary‐mass Companion to the Young Brown Dwarf 2MASSW J1207334−393254

Cited by 72 publications

References 25 publications

The Taurus Boundary of Stellar/Substellar (TBOSS) Survey

The Taurus Boundary of Stellar/Substellar (TBOSS) Survey

The young, tight, and low-mass binary TWA22AB: a new calibrator for evolutionary models?

An accurate distance to 2M1207Ab

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