Two very nearby (<i>d</i> ~  5 pc) ultracool brown dwarfs detected by their large proper motions from WISE, 2MASS, and SDSS data

Scholz, R.‐D.; Bihain, G.; Schnurr, O.; Storm, J.

doi:10.1051/0004-6361/201117297

Cited by 55 publications

(41 citation statements)

References 30 publications

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“…Kinematic searches, on the other hand, avoid such a bias by using proper motion alone as a judge of distance. By identifying objects with large proper motions, unusual brown dwarfs overlooked by previous surveys can be identified (e.g., Metchev et al 2008;Deacon et al 2009;Sheppard & Cushing 2009;Artigau et al 2010;Kirkpatrick et al 2010;Deacon et al 2011;Gizis et al 2011;Liu et al 2011;Scholz et al 2011Scholz et al , 2012Scholz 2014).…”

Section: Introductionmentioning

confidence: 99%

A Proper Motion Survey Using the First Sky Pass of Neowise-Reactivation Data

Schneider

Greco

Cushing

et al. 2016

ApJ

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The Wide-field Infrared Survey Explorer (WISE) was reactivated in 2013 December (NEOWISE) to search for potentially hazardous near-Earth objects. We have conducted a survey using the first sky pass of NEOWISE data and the AllWISE catalog to identify nearby stars and brown dwarfs with large proper motions ( total m  250 mas yr −1 ). A total of 20,548 high proper motion objects were identified, 1006 of which are new discoveries. This survey has uncovered a significantly larger sample of fainter objects (W 2 13  mag) than the previous WISE motion surveys of Luhman and Kirkpatrick et al. Many of these objects are predicted to be new L and T dwarfs based on near-and mid-infrared colors. Using estimated spectral types along with distance estimates, we have identified several objects that likely belong to the nearby solar neighborhood (d < 25 pc). We have followed up 19 of these new discoveries with near-infrared or optical spectroscopy, focusing on potentially nearby objects, objects with the latest predicted spectral types, and potential late-type subdwarfs. This subset includes six M dwarfs, five of which are likely subdwarfs, as well as eight L dwarfs and five T dwarfs, many of which have blue near-infrared colors. As an additional supplement, we provide 2MASS and AllWISE positions and photometry for every object found in our search, as well as 2MASS/AllWISE calculated proper motions.

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Section: Introductionmentioning

confidence: 99%

A Proper Motion Survey Using the First Sky Pass of Neowise-Reactivation Data

Schneider

Greco

Cushing

et al. 2016

ApJ

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“…Yet, despite their apparent brightness and high proper motion, up to ∼20% of our nearest < ( 20 pc) VLM neighbors remain "missing," particularly toward the Galactic plane Lépine 2005;Henry et al 2006), as exemplified by the very recent discovery of the third (Luhman 16AB;Luhman 2013) and fourth (WISE J085510.83-071442.5; Kirkpatrick et al 2014;Luhman 2014) closest systems to the Sun, comprised of L, T, and Y dwarfs. Several very low-temperature T and Y dwarfs (Artigau et al 2010;Lucas et al 2010;Cushing et al 2011;Kirkpatrick et al 2011;Scholz et al 2011;Bihain et al 2013) and even M dwarfs (e.g., Teegarden et al 2003;Hambly et al 2004;Deacon et al 2005a;Scholz et al 2005;Henry et al 2006;Scholz 2014) have also been uncovered within 5 pc of the Sun in the past decade.…”

Section: Introductionmentioning

confidence: 99%

WISE J072003.20-084651.2: AN OLD AND ACTIVE M9.5 + T5 SPECTRAL BINARY 6 pc FROM THE SUN

Burgasser

Gillon

Melis

et al. 2015

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We report observations of the recently discovered, nearby late-M dwarf WISE J072003.20-084651.2. New astrometric measurements obtained with the TRAPPIST telescope improve the distance measurement to 6.0 ± 1.0 pc and confirm the low tangential velocity (3.5 ± 0.6 km s −1 ) reported by Scholz. Low-resolution optical spectroscopy indicates a spectral type of M9.5 and prominent Hα emission (á ñ a L L log H 10 bol = −4.68 ± 0.06), but no evidence of subsolar metallicity or Li I absorption. Near-infrared spectroscopy reveals subtle peculiarities that can be explained by the presence of a T5 binary companion, and high-resolution laser guide star adaptive optics imaging reveals a faint (ΔH = 4.1) candidate source  0. 14 (0.8 AU) from the primary. With high-resolution optical and near-infrared spectroscopy, we measure a stable radial velocity of +83.8 ± 0.3 km s −1 , indicative of old disk kinematics and consistent with the angular separation of the possible companion. We measure a projected rotational velocity of v sin i = 8.0 ± 0.5 km s −1 and find evidence of low-level variabilty (∼1.5%) in a 13 day TRAPPIST light curve, but cannot robustly constrain the rotational period. We also observe episodic changes in brightness (1%-2%) and occasional flare bursts (4%-8%) with a 0.8% duty cycle, and order-of-magnitude variations in Hα line strength. Combined, these observations reveal WISE J0720-0846 to be an old, very low-mass binary whose components straddle the hydrogen burning minimum mass, and whose primary is a relatively rapid rotator and magnetically active. It is one of only two known binaries among late M dwarfs within 10 pc of the Sun, both of which harbor a mid T-type brown dwarf companion. We show that while this specific configuration is rare (≲1.6% probability), roughly 25% of binary companions to late-type M dwarfs in the local population are likely low-temperature T or Y brown dwarfs.

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“…BDs are thought to be more numerous than low mass stars, and recently five new BDs have been discovered at ∼10 pc (Burgasser et al 2011) and two at ∼5 pc (Scholz et al 2011) with WISE increasing the number of targets for observation of planetary transit.…”

Section: Introductionmentioning

confidence: 99%

Tidal evolution of planets around brown dwarfs

Bolmont

Raymond

Leconte

2011

A&A

114

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Context. The tidal evolution of planets orbiting brown dwarfs (BDs) presents an interesting case study because BDs' terrestrial planet forming region is located extremely close-in. In fact, the habitable zones of BDs range from roughly 0.001 to 0.03 AU and for the lowest-mass BDs are located interior to the Roche limit. Aims. In contrast with stars, BDs spin up as they age. Thus, the corotation distance moves inward. This has important implications for the tidal evolution of planets around BDs. Methods. We used a standard equilibrium tidal model to compute the orbital evolution of a large ensemble of planet-BD systems. We tested the effect of numerous parameters such as the initial semi-major axis and eccentricity, the rotation period of the BD, the masses of both the BD and planet, and the tidal dissipation factors. Results. We find that all planets that form at or beyond the corotation distance and with initial eccentricities smaller than ∼0.1 are repelled from the BD. Some planets initially interior to corotation can survive if their inward tidal evolution is slower than the BD's spin evolution, but most initially close-in planets fall onto the BD. Conclusions. We find that the most important parameter for the tidal evolution is the initial orbital distance with respect to the corotation distance. Some planets can survive in the habitable zone for Gyr timescales, although in many cases the habitable zone moves inward past the planet's orbit in just tens to hundreds of Myr. Surviving planets can have orbital periods of less than 10 days (as small as 10 h), so they could be observable by transit.

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Two very nearby (d ~ 5 pc) ultracool brown dwarfs detected by their large proper motions from WISE, 2MASS, and SDSS data

Cited by 55 publications

References 30 publications

A Proper Motion Survey Using the First Sky Pass of Neowise-Reactivation Data

A Proper Motion Survey Using the First Sky Pass of Neowise-Reactivation Data

WISE J072003.20-084651.2: AN OLD AND ACTIVE M9.5 + T5 SPECTRAL BINARY 6 pc FROM THE SUN

Tidal evolution of planets around brown dwarfs

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