Properties of the Nearby Brown Dwarf Wisep J180026.60+013453.1

Gizis, John E.; Burgasser, Adam J.; Vrba, F. J.

doi:10.1088/0004-6256/150/6/179

Cited by 11 publications

(14 citation statements)

References 38 publications

(42 reference statements)

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“…This is consistent with Stauffer & Hartmann (1986a) who measured v sin i=15 km s −1 , and similar to v sin i=12.7 derived by Houdebine (2010). However, Gizis (1998) estimated v sin i=30±5 km s −1 and this resulted in a different interpretation of how Wolf 1130B evolved. For comparison, we also determined v sin i for Gl 494 (Ross 458) from the IGRINS spectrum shown in Figure 4.…”

Section: • Tidal Locking -supporting

confidence: 90%

“…We used the Systemic Console 2 software package (Meschiari et al 2009;Meschiari & Laughlin 2010) to find the orbital solution and its uncertainties with the constant assumption that Wolf 1130A has a mass of 0.3 M (this assumption is motivated in Section 4.1). The best fit we find to the 27 radial velocities in Gizis (1998) is most similar to solution C in Table 3 of that paper. The most notable aspect of the fit to the visible-light radial velocities is the non-zero eccentricity, which is surprising given the systems old age and short orbital period.…”

Section: Orbital Solutionsupporting

confidence: 78%

“…The prominent emission features observed in each optical spectrum are highlighted in Figure 3. Gizis (1998) finds no correlation of the Hα emission with orbital phase.…”

Section: Optical Spectroscopymentioning

confidence: 92%

“…Gizis (1998) derived 27 radial velocities for Wolf 1130A by cross-correlating 0.3Å resolution visiblelight spectra (4700 to 9600Å). Most of the observations from Gizis (1998) were obtained on two adjacent nights in 1996 August and have typical uncertainties of ±2 km s −1 . The combination of those observations with 40 IGRINS epochs produces a baseline of almost 20 years.…”

Section: Radial Velocity Determinationmentioning

confidence: 99%

“…Wolf 1130 (Gl 781, LHS 482, HIP 98906) is a nearby (16.7±0.2 pc, Gaia Collaboration et al 2016a,b) M subdwarf (Wolf 1130A) and white dwarf (Wolf 1130B) binary with a 0.4967 day orbital period (Gizis 1998). It is also classified as a flare star with the designation V1513 Cyg.…”

Section: Introductionmentioning

confidence: 99%

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Wolf 1130: A Nearby Triple System Containing a Cool, Ultramassive White Dwarf

Mace

Mann

Skiff

et al. 2018

ApJ

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Following the discovery of the T8 subdwarf WISE J200520.38+542433.9 (Wolf 1130C), with common proper motion to a binary (Wolf 1130AB) consisting of an M subdwarf and a white dwarf, we set out to learn more about the old binary in the system. We find that the A and B components of Wolf 1130 are tidally locked, which is revealed by the coherence of more than a year of V band photometry phase folded to the derived orbital period of 0.4967 days. Forty new high-resolution, near-infrared spectra obtained with the Immersion Grating Infrared Spectrometer (IGRINS) provide radial velocities and a projected rotational velocity (v sin i) of 14.7 ± 0.7 km s −1 for the M subdwarf. In tandem with a Gaia parallax-derived radius and verified tidal-locking, we calculate an inclination of i=29±2 degrees. From the single-lined orbital solution and the inclination we derive an absolute mass for the unseen primary (1.24 +0.19 −0.15 M ). Its non-detection between 0.2 and 2.5µm implies that it is an old (>3.7 Gyr) and cool (T eff <7000K) ONe white dwarf. This is the first ultramassive white dwarf within 25 pc. The evolution of Wolf 1130AB into a cataclysmic variable is inevitable, making it a potential Type Ia supernova progenitor. The formation of a triple system with a primary mass >100 times the tertiary mass and the survival of the system through the common-envelope phase, where ∼80% of the system mass was lost, is remarkable. Our analysis of Wolf 1130 allows us to infer its formation and evolutionary history, which has unique implications for understanding low-mass star and brown dwarf formation around intermediate mass stars.

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Section: • Tidal Locking -supporting

confidence: 90%

Section: Orbital Solutionsupporting

confidence: 78%

“…The prominent emission features observed in each optical spectrum are highlighted in Figure 3. Gizis (1998) finds no correlation of the Hα emission with orbital phase.…”

Section: Optical Spectroscopymentioning

confidence: 92%

Section: Radial Velocity Determinationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Wolf 1130: A Nearby Triple System Containing a Cool, Ultramassive White Dwarf

Mace

Mann

Skiff

et al. 2018

ApJ

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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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A New Sample of Cool Subdwarfs From Sdss: Properties and Kinematics

Savcheva

West

Bochanski

2014

ApJ

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We present a new sample of M subdwarfs compiled from the 7th data release of the Sloan Digital Sky Survey. With 3517 new subdwarfs, this new sample significantly increases the number of spectroscopically confirmed low-mass subdwarfs. This catalog also includes 905 extreme and 534 ultra sudwarfs. We present the entire catalog including observed and derived quantities, and template spectra created from co-added subdwarf spectra. We show color-color and reduced proper motion diagrams of the three metallicity classes, which are shown to separate from the disk dwarf population. The extreme and ultra subdwarfs are seen at larger values of reduced proper motion as expected for more dynamically heated populations. We determine 3D kinematics for all of the stars with proper motions. The color-magnitude diagrams show a clear separation of the three metallicity classes with the ultra and extreme subdwarfs being significantly closer to the main sequence than the ordinary subdwarfs. All subdwarfs lie below (fainter) and to the left (bluer) of the main sequence. Based on the average (U, V, W ) velocities and their dispersions, the extreme and ultra subdwarfs likely belong to the Galactic halo, while the ordinary subdwarfs are likely part of the old Galactic (or thick) disk. An extensive activity analysis of subdwarfs is performed using Hα emission and 208 active subdwarfs are found. We show that while the activity fraction of subdwarfs rises with spectral class and levels off at the latest spectral classes, consistent with the behavior of M dwarfs, the extreme and ultra subdwarfs are basically flat. -3 -1. Introduction M subdwarfs are low-mass (0.08M < M < 0.8M ), low-luminosity (L < 0.05L ) stars that are the metal-poor ([Fe/H] -0.5) counterparts of cool, late-type dwarfs. Although M subdwarfs are not as abundant (0.25% of the Galactic stellar population; Reid & Hawley 2005) as typical disk M dwarfs (M dwarfs make up 70% of the Galactic stellar population; Bochanski et al. 2010), they have similar properties, such as low temperatures and lifetimes greater than the Hubble time (Laughlin et al. 1997), making them excellent tracers ofGalactic chemical and dynamical evolution. Thus, exploring populations of different metallicities helps probe the composition and evolution of the different components of the Galaxy, and the Galactic merger history. Since some subdwarfs lie close to the hydrogen burning limit, they can be used to probe the lower end of the stellar mass function, extending it into the hydrogen-burning limit. In addition, the cool, dim atmospheres of these stars and their surroundings provide conditions for studying molecule and dust formation in low metallicity environments as well as radiative transfer in cool, metal-poor atmospheres, which cannot be tackled using metal-rich M dwarfs.M subdwarfs exhibit large metallicity-induced changes in their spectra relative to M dwarfs. The main difference between M dwarfs and subdwarfs is the strength of the TiO bands, which are much weaker in subdwarfs due to their low metall...

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Properties of the Nearby Brown Dwarf Wisep J180026.60+013453.1

Cited by 11 publications

References 38 publications

Wolf 1130: A Nearby Triple System Containing a Cool, Ultramassive White Dwarf

Wolf 1130: A Nearby Triple System Containing a Cool, Ultramassive White Dwarf

The 10 parsec sample in the Gaia era

A New Sample of Cool Subdwarfs From Sdss: Properties and Kinematics

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