WISEA J064750.85-154616.4: a new nearby L/T transition dwarf

Scholz, R.‐D.; Bihain, G.; Storm, J.

doi:10.1051/0004-6361/201424070

Cited by 11 publications

(15 citation statements)

References 46 publications

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“…Other new nearby (D ≤ 10 pc), low-mass mass objects discovered in the solar neighborhood include those reported by Artigau et al (2010); Lucas et al (2010); Scholz et al (2011Scholz et al ( , 2014; Luhman (2013Luhman ( , 2014, among others. Nearby examples of low-mass stellar and substellar objects are important targets for understanding stellar interiors near the hydrogen-burning limit (Dieterich et al 2014), the diversity of stellar and substellar atmospheres and testing atmospheric models (e.g., Leggett et al 2010), initial mass function (e.g., Kirkpatrick et al 2011), activity trends (e.g., Berger et al 2010), the multiplicity and formation of low-mass objects (e.g., Faherty et al 2010;Dieterich et al 2012), and providing bright low-mass targets for planet surveys (e.g., Blake et al 2010).…”

Section: Introductionmentioning

confidence: 81%

“…Typically, the missed objects are cool, making the Wide-field Infrared Survey Explorer (WISE; Wright et al 2010) satellite an excellent tool for discovering them. Indeed, Scholz (2014) used color and proper motion criteria based on WISE and 2MASS (Two Micron All Sky Survey; Skrutskie et al 2006) photom-Fig. 1.…”

Section: Amongmentioning

confidence: 99%

“…The star is cataloged in USNO B1.0 (Monet et al 2013) with proper motion µ α cos δ=−36±13, µ δ =−102±27 mas yr −1 . Scholz (2014) astrometrically re-calibrated the archival images from the previous surveys that had detected WISE J0720, and measured a trigonometric parallax of ̟ = 142±38 mas (d=7.0±1.9 pc), and a revised proper motion of µ α cos δ=−41±2, µ δ =−116±2 mas yr −1 . The colors of the object were used to estimate a spectral type of M9±1.…”

Section: Amongmentioning

confidence: 99%

“…Recently, Scholz (2014) reported the discovery of a new nearby M-type star, WISE J072003.20−084651.2 (hereafter, WISE J0720), demonstrating yet again that our knowledge of the late-type stellar content of the Solar neighbourhood is incomplete. Other new nearby (D≤10pc), low-mass mass objects discovered in the solar neighborhood include those reported by Artigau et al (2010), Lucas et al (2010), Scholz (2011), Luhman (2013), Luhman (2014), Scholz et al (2014)…”

Section: Introductionmentioning

confidence: 99%

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Properties of the solar neighbor WISE J072003.20−084651.2

Ivanov

Vaïsänen

Kniazev

et al. 2015

A&A

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Context. The severe crowding towards the Galactic plane suggests that the census of nearby stars in that direction may be incomplete. Recently, Scholz reported a new M9 object at an estimated distance d 7 pc (WISE J072003.20−084651.2; hereafter WISE J0720) at Galactic latitude b = 2.3• . Aims. Our goals are to determine the physical characteristics of WISE J0720, its kinematic properties, and to address the question of whether it is a binary object, as was suggested in the discovery paper. Methods. Optical and infrared spectroscopy from the Southern African Large Telescope and Magellan, respectively, and spectral energy distribution fitting were used to determine the spectral type of WISE J0720. The measured radial velocity, proper motion, and parallax yielded its Galactic velocities. We also investigated if WISE J0720 may show X-ray activity based on archival data. Results. Our spectra are consistent with spectral type L0 ± 1. We find no evidence for binarity, apart from a minor 2σ level difference in the radial velocities taken at two different epochs. The spatial velocity of WISE J0720 does not connect it to any known moving group; instead, it places the object with high probability in the old thin disk or in the thick disk. The spectral energy distribution fit hints at excess in the 12 μm and 22 μm WISE bands which may be due to a redder companion, but the same excess is visible in other late-type objects, and it more likely implies a shortcoming of the models (e.g., problems with the effective wavelengths of the filters for these extremely cool objects, etc.) rather than a disk or redder companion. The optical spectrum shows some Hα emission, indicative of stellar activity. Archival X-ray observations yield no detection. Conclusions. WISE J0720 is a new member of the solar neighborhood, the third nearest L dwarf. Our data do not support the hypothesis of its binary nature.

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Section: Introductionmentioning

confidence: 81%

Section: Amongmentioning

confidence: 99%

Section: Amongmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Properties of the solar neighbor WISE J072003.20−084651.2

Ivanov

Vaïsänen

Kniazev

et al. 2015

A&A

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“…We also use data from the XHIP (X) catalog (Anderson & Francis 2012) and the XHIP catalog adapted by (Dybczyński & Berski 2015) (D). We also include WISE J072003.20-084651.2 (W0720) with data from (Scholz, Bihain & Storm 2014;Mamajek et al 2015) (M). In summary, the catalogs of G, R, P and X are from BJ15, and catalog D and M are from their corresponding references.…”

Section: Datamentioning

confidence: 99%

Finding the imprints of stellar encounters in long-period comets

Feng

Bailer‐Jones

2015

Mon. Not. R. Astron. Soc.

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The solar system's Oort cloud can be perturbed by the Galactic tide and by individual passing stars. These perturbations can inject Oort cloud objects into the inner parts of the solar system, where they may be observed as the long-period comets (periods longer than 200 years). Using dynamical simulations of the Oort cloud under the perturbing effects of the tide and 61 known stellar encounters, we investigate the link between long-period comets and encounters. We find that past encounters were responsible for injecting at least 5% of the currently known long-period comets. This is a lower limit due to the incompleteness of known encounters. Although the Galactic tide seems to play the dominant role in producing the observed long-period comets, the non-uniform longitude distribution of the cometary perihelia suggests the existence of strong -but as yet unidentified -stellar encounters or other impulses. The strongest individual future and past encounters are probably HIP 89825 (Gliese 710) and HIP 14473, which contribute at most 8% and 6% to the total flux of long-period comets, respectively. Our results show that the strength of an encounter can be approximated well by a simple proxy, which will be convenient for quickly identifying significant encounters in large data sets. Our analysis also indicates a smaller population of the Oort cloud than is usually assumed, which would bring the mass of the solar nebula into line with planet formation theories.

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The 10 parsec sample in the Gaia era

Reylé

Jardine²,

Fouqué

et al. 2021

A&A

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Context. The nearest stars provide a fundamental constraint for our understanding of stellar physics and the Galaxy. The nearby sample serves as an anchor where all objects can be seen and understood with precise data. This work is triggered by the most recent data release of the astrometric space mission Gaia and uses its unprecedented high precision parallax measurements to review the census of objects within 10 pc. Aims. The first aim of this work was to compile all stars and brown dwarfs within 10 pc observable by Gaia and compare it with the Gaia Catalogue of Nearby Stars as a quality assurance test. We complement the list to get a full 10 pc census, including bright stars, brown dwarfs, and exoplanets. Methods. We started our compilation from a query on all objects with a parallax larger than 100 mas using the Set of Identifications, Measurements, and Bibliography for Astronomical Data database (SIMBAD). We completed the census by adding companions, brown dwarfs with recent parallax measurements not in SIMBAD yet, and vetted exoplanets. The compilation combines astrometry and photometry from the recent Gaia Early Data Release 3 with literature magnitudes, spectral types, and line-of-sight velocities. Results. We give a description of the astrophysical content of the 10 pc sample. We find a multiplicity frequency of around 28%. Among the stars and brown dwarfs, we estimate that around 61% are M stars and more than half of the M stars are within the range from M3.0 V to M5.0 V. We give an overview of the brown dwarfs and exoplanets that should be detected in the next Gaia data releases along with future developments. Conclusions. We provide a catalogue of 541 stars, brown dwarfs, and exoplanets in 339 systems, within 10 pc from the Sun. This list is as volume-complete as possible from current knowledge and it provides benchmark stars that can be used, for instance, to define calibration samples and to test the quality of the forthcoming Gaia releases. It also has a strong outreach potential.

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WISEA J064750.85-154616.4: a new nearby L/T transition dwarf

Cited by 11 publications

References 46 publications

Properties of the solar neighbor WISE J072003.20−084651.2

Properties of the solar neighbor WISE J072003.20−084651.2

Finding the imprints of stellar encounters in long-period comets

The 10 parsec sample in the Gaia era

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