New proper-motion stars, (second list)

Ross, Frank E.

doi:10.1086/104699

Cited by 11 publications

(7 citation statements)

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“…Ross 128 entered the literature as the 128th entry in the Ross (1926) Including brown dwarfs, it is the 13 th closest (sub-)stellar system to the Sun. Ross 128 is moving towards us and will actually become our closest neighbour in just 71,000 years from now (D ca = 1.9 pc; García-Sánchez et al 2001).…”

Section: Starmentioning

confidence: 99%

A temperate exo-Earth around a quiet M dwarf at 3.4 parsec

Bonfils

Astudillo-Defru

Díaz

et al. 2018

A&A

122

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The combination of high-contrast imaging and high-dispersion spectroscopy, which has successfully been use to detect the atmosphere of a giant planet, is one of the most promising potential probes of the atmosphere of Earth-size worlds. The forthcoming generation of extremely large telescopes (ELTs) may obtain sufficient contrast with this technique to detect O2 in the atmosphere of those worlds that orbit low-mass M dwarfs. This is strong motivation to carry out a census of planets around cool stars for which habitable zones can be resolved by ELTs, i.e. for M dwarfs within ∼5 parsecs. Our HARPS survey has been a major contributor to that sample of nearby planets. Here we report on our radial velocity observations of Ross 128 (Proxima Virginis, GJ447, HIP 57548), an M4 dwarf just 3.4 parsec away from our Sun. This source hosts an exo-Earth with a projected mass m sin i = 1.35M⊕ and an orbital period of 9.9 days. Ross 128 b receives ∼1.38 times as much flux as Earth from the Sun and its equilibrium ranges in temperature between 269 K for an Earth-like albedo and 213 K for a Venus-like albedo. Recent studies place it close to the inner edge of the conventional habitable zone. An 80-day long light curve from K2 campaign C01 demonstrates that Ross 128 b does not transit. Together with the All Sky Automated Survey (ASAS) photometry and spectroscopic activity indices, the K2 photometry shows that Ross 128 rotates slowly and has weak magnetic activity. In a habitability context, this makes survival of its atmosphere against erosion more likely. Ross 128 b is the second closest known exo-Earth, after Proxima Centauri b (1.3 parsec), and the closest temperate planet known around a quiet star. The 15 mas planet-star angular separation at maximum elongation will be resolved by ELTs (> 3λ/D) in the optical bands of O2.

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Section: Starmentioning

confidence: 99%

A temperate exo-Earth around a quiet M dwarf at 3.4 parsec

Bonfils

Astudillo-Defru

Díaz

et al. 2018

A&A

122

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“…We now know that they constitute an important part of the objects in our Galaxy, while even the brightest of them (AX Mic) is invisible to the naked eye. Astronomers such as Max Wolf and Frank E. Ross catalogued stars with a large proper motion to try discovering faint, but nearby stars (Wolf 1917;Ross 1926). Willem J. Luyten produced many catalogues (e.g.…”

Section: Introductionmentioning

confidence: 99%

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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“…Stars in the solar neighborhood have been identified primarily through their large proper motions (e.g., Barnard 1916;Wolf 1919;Ross 1926;van Biesbroeck 1944;Giclas et al 1971;Luyten 1979;Lépine & Shara 2005). Most brown dwarfs, on the other hand, have been found through their distinctive colors (e.g., Burgasser et al 2004;Cruz et al 2007;Burningham et al 2010;Albert et al 2011;Kirkpatrick et al 2011) because wide-field infrared (IR) surveys initially offered limited data on proper motions.…”

Section: Introductionmentioning

confidence: 99%

DISCOVERY OF A BINARY BROWN DWARF AT 2 pc FROM THE SUN

Luhman

2013

ApJ

191

162

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I am using multi-epoch astrometry from the Wide-field Infrared Survey Explorer (WISE) to search for new members of the solar neighborhood via their high proper motions. Through this work, I have identified WISE J104915.57-531906.1 as a high proper motion object and have found additional detections in images from the Digitized Sky Survey, the Two Micron All-Sky Survey, and the Deep Near-Infrared Survey of the Southern Sky. I have measured a parallax of 0.496±0.037 ′′ (2.0±0.15 pc) from the astrometry in these surveys, making WISE J104915.57-531906.1 the third closest system to the Sun. During spectroscopic observations with GMOS at Gemini Observatory, an i-band acquisition image resolved it as a 1. ′′ 5 (3 AU) binary. A spectrum was collected for the primary, which I classify as L8±1. The secondary is probably near the L/T transition as well given that it is only modestly fainter than the primary (∆i = 0.45 mag).

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New proper-motion stars, (second list)

Cited by 11 publications

References 0 publications

A temperate exo-Earth around a quiet M dwarf at 3.4 parsec

A temperate exo-Earth around a quiet M dwarf at 3.4 parsec

The 10 parsec sample in the Gaia era

DISCOVERY OF A BINARY BROWN DWARF AT 2 pc FROM THE SUN

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