The Gemini Nici Planet-Finding Campaign: Discovery of a Substellar L Dwarf Companion to the Nearby Young M Dwarf Cd–35 2722

Wahhaj, Z.; Liu, Mengmeng; Biller, Beth; Clarke, Fraser; Nielsen, Eric L.; Close, Laird M.; Hayward, T. L.; Mamajek, Eric E.; Cushing, Michael C.; Dupuy, Trent J.; Tecza, Matthias; Thatte, Niranjan; Chun, Mark; Ftaclas, C.; Hartung, Markus; Reid, I. Neill; Shkolnik, Evgenya L.; Alencar, S. H. P.; Artymowicz, Pawel; Boss, Alan P.; Pino, E. M. de Gouveia Dal; Gregorio-Hetem, J.; Ida, Shigeru; Kuchner, Marc J.; Lin, D. N. C.; Toomey, Douglas W.

doi:10.1088/0004-637x/729/2/139

Cited by 135 publications

(107 citation statements)

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“…The third sample is made of spectra of members of 1−150 Myr old young moving groups and clusters (Lodieu et al 2008;Rice et al 2010;Bonnefoy et al 2014;Gagné et al 2014). The fourth sample is composed of spectra of young MLT companions (Patience et al 2010;Lafrenière et al 2010;Wahhaj et al 2011;Bonnefoy et al 2010Bonnefoy et al , 2014). …”

Section: Appendix A: Details On the Orbital Fitmentioning

confidence: 99%

Physical and orbital properties ofβPictoris b

Bonnefoy

Marleau

Galicher

et al. 2014

A&A

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The intermediate-mass star β Pictoris is known to be surrounded by a structured edge-on debris disk within which a gas giant planet was discovered orbiting at 8−10 AU. The physical properties of β Pic b were previously inferred from broad-and narrow-band 0.9−4.8 µm photometry. We used commissioning data of the Gemini Planet Imager (GPI) to obtain new astrometry and a lowresolution (R ∼ 35−39) J-band (1.12−1.35 µm) spectrum of the planet. We find that the planet has passed the quadrature. We constrain its semi-major axis to ≤10 AU (90% prob.) with a peak at 8.9 +0.4 −0.6 AU. The joint fit of the planet astrometry and the most recent radial velocity measurements of the star yields a planet dynamical mass lower than 20 M Jup (≥96% prob.). The extracted spectrum of β Pic b is similar to those of young L1 +1 −1.5 dwarfs. We used the spectral type estimate to revise the planet luminosity to log(L/L ) = −3.90±0.07. The 0.9−4.8 µm photometry and spectrum are reproduced for T eff = 1650 ± 150 K and a log g ≤ 4.7 dex by 12 grids of PHOENIX-based and LESIA atmospheric models. For the most recent system age estimate (21 ± 4 Myr), the bolometric luminosity and the constraints on the dynamical mass of β Pic b are only reproduced by warm-and hot-start tracks with initial entropies S i > 10.5 k B /baryon. These initial conditions may result from an inefficient accretion shock and/or a planetesimal density at formation higher than in the classical core-accretion model. Considering a younger age for the system or a conservative formation time for β Pic b does not change these conclusions.

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Section: Appendix A: Details On the Orbital Fitmentioning

confidence: 99%

Physical and orbital properties ofβPictoris b

Bonnefoy

Marleau

Galicher

et al. 2014

A&A

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“…Near infrared signatures of low gravity are visible in the Pleiades at 125 Myr (Bihain et al 2010) and in other L dwarf benchmarks with ages in the range 50 − 200 Myr, e.g. G 196-3B (Rebolo et al 1998;Allers et al 2007), CD-35 2722B (Wahhaj et al 2011) and 1RXS J2351+3127 B (Bowler et al 2012). By contrast, the somewhat older L4+L4 pair HD 130948 BC, aged 790 +220 −150 Myr, was described by Allers et al (2010) as the youngest L dwarf benchmark showing no signs of low surface gravity.…”

Section: Discussion and Summarymentioning

confidence: 98%

Discovery of a brown dwarf companion to the A3V star β Circini

Smith

Lucas

Peña

et al. 2015

Mon. Not. R. Astron. Soc.

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We report the discovery of an L dwarf companion to the A3V star β Circini. VVV J151721.49-585131.5, or β Cir B, was identified in a proper motion and parallax catalogue of the Vista Variables in the Vía Láctea survey as having near infrared luminosity and colour indicative of an early L dwarf, and a proper motion and parallax consistent with that of β Cir. The projected separation of ∼3.6 ′ corresponds to 6656 au, which is unusually wide. The most recent published estimate of the age of the primary combined with our own estimate based on newer isochrones yields an age of 370 − 500 Myr. The system therefore serves as a useful benchmark at an age greater than that of the Pleiades brown dwarfs and most other young L dwarf benchmarks. We have obtained a medium resolution echelle spectrum of the companion which indicates a spectral type of L1.0±0.5 and lacks the typical signatures of low surface gravity seen in younger brown dwarfs. This suggests that signs of low surface gravity disappear from the spectra of early L dwarfs by an age of ∼ 370 − 500 Myr, as expected from theoretical isochrones. The mass of β Cir B is estimated from the BHAC15 isochrones as 0.056 ± 0.007 M ⊙ .

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“…Their absolute photometry was synthesised from their spectra Mace et al 2013;Allers & Liu 2013;Gizis et al 2015) and the corresponding parallaxes (Kirkpatrick et al 2011;Faherty et al 2012;Zapatero Osorio et al 2014;Liu et al 2016). We added the photometry of companions using the spectra and distances reported in Wahhaj et al (2011a) …”

Section: Astrometry and Photometrymentioning

confidence: 99%

Orbiting a binary

Bonavita

D’Orazi

Mesa

et al. 2017

A&A

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Aims. In this paper we present the results of the SPHERE observation of the HD 284149 system, aimed at a more detailed characterisation of both the primary and its brown dwarf companion. Methods. We observed HD 284149 in the near-infrared with SPHERE, using the imaging mode (IRDIS+IFS) and the long-slit spectroscopy mode (IRDIS-LSS). The data were reduced using the dedicated SPHERE pipeline, and algorithms such as PCA and TLOCI were applied to reduce the speckle pattern. Results. The IFS images revealed a previously unknown low-mass (∼ 0.16 M ) stellar companion (HD 294149 B) at ∼ 0.1 , compatible with previously observed radial velocity differences, as well as proper motion differences between Gaia and Tycho-2 measurements. The known brown dwarf companion (HD 284149 b) is clearly visible in the IRDIS images. This allowed us to refine both its photometry and astrometry. The analysis of the medium resolution IRDIS long slit spectra also allowed a refinement of temperature and spectral type estimates. A full reassessment of the age and distance of the system was also performed, leading to more precise values of both mass and semi-major axis. Conclusions. As a result of this study, HD 284149 ABb therefore becomes the latest addition to the (short) list of brown dwarfs on wide circumbinary orbits, providing new evidence to support recent claims that object in such configuration occur with a similar frequency to wide companions to single stars.

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The Gemini Nici Planet-Finding Campaign: Discovery of a Substellar L Dwarf Companion to the Nearby Young M Dwarf Cd–35 2722

Cited by 135 publications

References 92 publications

Physical and orbital properties ofβPictoris b

Physical and orbital properties ofβPictoris b

Discovery of a brown dwarf companion to the A3V star β Circini

Orbiting a binary

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