The Hyperactive L Dwarf 2mass J13153094–2649513: Continued Emission and a Brown Dwarf Companion

Burgasser, Adam J.; Sitarski, Breann N.; Gelino, Christopher R.; Logsdon, Sarah E.; Perrin, Marshall D.

doi:10.1088/0004-637x/739/1/49

Cited by 37 publications

(38 citation statements)

References 119 publications

(140 reference statements)

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“…However, close inspection reveals specific discrepancies near 1.3 and 1.6 μm, and a subtle "dip" feature at 1.62 μm. Such features have been previously noted in the combined-light spectra of very low mass spectral binary systems with late-type M or L dwarf primaries and T dwarf secondaries (e.g., Cruz et al 2004;Burgasser 2007b;Burgasser et al 2010Burgasser et al , 2011Burgasser et al , 2012Gelino & Burgasser 2010;Kirkpatrick et al 2012;Day-Jones et al 2013;Deacon et al 2014;Bardalez Gagliuffi et al 2014). To assess whether WISE J0720-0846 is such a system, we used the fitting method described in Burgasser et al (2010), comparing the spectrum of WISE J0720-0846 to 699 single star templates and 107,646 binary templates from the SPL.…”

Section: Identification As a Spectral Binarymentioning

confidence: 98%

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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Section: Identification As a Spectral Binarymentioning

confidence: 98%

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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“…Schmidt et al 2015). Nevertheless we included three objects with strong Hα emission in our program to help better diagnose these objects, including one object with a close T7.5 companion (2MASS J1315−2649AB; Burgasser et al 2011). Note that a fourth object known to have strong and variable Hα emission, 2MASS J1022+5825 ), was already included in our low-gravity sample (β in the optical but fld-g in the near-IR).…”

Section: Samplementioning

confidence: 99%

“…Based on a high-quality composite optical spectrum, assigned a spectral type of L5.5. Burgasser et al (2011) resolved 2MASS J1315−2649 into binary and determined component spectral types of L3.5±2.5 and T7±0.6 from H-band spectra. Using the composite near-IR spectrum of Burgasser et al (2011), we classify 2MASS J1315−2649AB as L6 fld-g on the Allers & Liu (2013a) system.…”

Section: Mass J08354256−0819237 (L5/-)mentioning

confidence: 99%

“…Burgasser et al (2011) resolved 2MASS J1315−2649 into binary and determined component spectral types of L3.5±2.5 and T7±0.6 from H-band spectra. Using the composite near-IR spectrum of Burgasser et al (2011), we classify 2MASS J1315−2649AB as L6 fld-g on the Allers & Liu (2013a) system. The composite near-IR spectrum shows subtle peculiarities, but these do not appear low-gravity in nature, and the H-cont index is consistent with field gravity.…”

Section: Mass J08354256−0819237 (L5/-)mentioning

confidence: 99%

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The Hawaii Infrared Parallax Program. Ii. Young Ultracool Field Dwarfs* †

Liu

Dupuy

Allers

2016

ApJ

242

320

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We present a large, uniform analysis of young (≈10-150 Myr) ultracool dwarfs, based on new high-precision infrared (IR) parallaxes for 68 objects. We find that low-gravity (vl-g) late-M and L dwarfs form a continuous sequence in IR color-magnitude diagrams, separate from the field population and from current theoretical models. These vl-g objects also appear distinct from young substellar (brown dwarf and exoplanet) companions, suggesting the two populations may have a different range of physical properties. In contrast, at the L/T transition, young, old, and spectrally peculiar objects all span a relatively narrow range in near-IR absolute magnitudes. At a given spectral type, the IR absolute magnitudes of young objects can be offset from ordinary field dwarfs, with the largest offsets occurring in the Y and J bands for late-M dwarfs (brighter than the field) and mid/late-L dwarfs (fainter than the field). Overall, low-gravity (vl-g) objects have the most uniform photometric behavior while intermediate-gravity (int-g) objects are more diverse, suggesting a third governing parameter beyond spectral type 1 This work is largely based on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, and the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii.2 Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. -2 -and gravity class. We examine the moving group membership for all young ultracool dwarfs with parallaxes, changing the status of 23 objects (including 8 previously identified planetary-mass candidates) and fortifying the status of another 28 objects. We use our resulting age-calibrated sample to establish empirical young isochrones and show a declining frequency of vl-g objects relative to int-g objects with increasing age. Notable individual objects in our sample include high-velocity ( 100 km s −1 ) int-g objects; very red late-L dwarfs with high surface gravities; candidate disk-bearing members of the MBM20 cloud and β Pic moving group; and very young distant interlopers. Finally, we provide a comprehensive summary of the absolute magnitudes and spectral classifications of young ultracool dwarfs, using a combined sample of 102 objects found in the field and as substellar companions to young stars.Subject headings: brown dwarfs -proper motions -parallaxes -solar neighborhood IntroductionObservational studies of brown dwarfs have been inspired by two complementary perspectives. One has been the desire to expand the parameter space of classical stellar astrophysics. Brown dwarfs are t...

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“…While this technique is more commonly associated with white-dwarf-M-dwarf pairs (e.g., Silvestri et al 2006), spectral binaries containing late-M or L dwarf primaries and T dwarf secondaries have also been recognized due to their unique and highly structured near-infrared spectra (Cruz et al 2004;Burgasser 2007b;Burgasser et al 2008aBurgasser et al , 2010Burgasser et al , 2011bStumpf et al 2008;Gelino & Burgasser 2010;Geißler et al 2011). Because blended light systems can be identified at any separation, M/L+T spectral binaries can probe the very closest separations that are inaccessible to direct imaging studies (a 50 mas).…”

Section: Introductionmentioning

confidence: 99%

Discovery of a Very Low Mass Triple With Late-M and T Dwarf Components: Lp 704-48/SDSS J0006–0852ab

Burgasser

Luk

Dhital

et al. 2012

ApJ

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We report the identification of the M9 dwarf SDSS J000649.16−085246.3 as a spectral binary and radial velocity (RV) variable with components straddling the hydrogen-burning mass limit. Low-resolution near-infrared spectroscopy reveals spectral features indicative of a T dwarf companion, and spectral template fitting yields component types of M8.5 ± 0.5 and T5 ± 1. High-resolution near-infrared spectroscopy with Keck/NIRSPEC reveals pronounced RV variations with a semi-amplitude of 8.2 ± 0.4 km s −1 . From these we determine an orbital period of 147.6 ± 1.5 days and eccentricity of 0.10 ± 0.07, making SDSS J0006−0852AB the third tightest very low mass binary known. This system is also found to have a common proper motion companion, the inactive M7 dwarf LP 704-48, at a projected separation of 820 ± 120 AU. The lack of Hα emission in both M dwarf components indicates that this system is relatively old, as confirmed by evolutionary model analysis of the tight binary. LP 704-48/SDSS J0006−0852AB is the lowest-mass confirmed triple identified to date, and one of only seven candidate and confirmed triples with total masses below 0.3 M currently known. We show that current star and brown dwarf formation models cannot produce triple systems like LP 704-48/SDSS J0006−0852AB, and we rule out Kozai-Lidov perturbations and tidal circularization as a viable mechanism to shrink the inner orbit. The similarities between this system and the recently uncovered low-mass eclipsing triples NLTT 41135AB/41136 and LHS 6343ABC suggest that substellar tertiaries may be common in wide M dwarf pairs.

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The Hyperactive L Dwarf 2mass J13153094–2649513: Continued Emission and a Brown Dwarf Companion

Cited by 37 publications

References 119 publications

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

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

The Hawaii Infrared Parallax Program. Ii. Young Ultracool Field Dwarfs* †

Discovery of a Very Low Mass Triple With Late-M and T Dwarf Components: Lp 704-48/SDSS J0006–0852ab

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