Trigonometric parallaxes of 71 large proper motion stars

Khovritchev, M. Yu.; Izmailov, I. S.; Khrutskaya, E. V.

doi:10.1093/mnras/stt1321

Cited by 13 publications

(7 citation statements)

References 29 publications

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“…Based on the parallaxes of π H = 16.81 ± 2.04 mas and π G = 14.4036±0.1174 mas, the mass sums of the components were obtained for the orbital solution by Tokovinin (2016) ( M H = 1.9M and M G = 3.03M ) and for the orbit presented here in Table 3. Using the parallax in Khovritchev et al (2013), the mass sums are M khov = 0.3M (Tokovinin 2016) and M khov = 0.58 ± 0.42M (this work). The mass sums using this parallax for both orbital solutions are implausibly low, therefore, this parallax was not used in a further study.…”

Section: Orbit Constructionmentioning

confidence: 88%

“…9 (Rastegaev et al 2007;Hartkopf et al 2012). The orbital period of the system was initially estimated as ∼ 10 years (Hartkopf et al 2012), the distance to the object was d = 54.3 ± 20.9 pc, and the trigonometric parallax π = 31.4 ± 7.1 mas (Khovritchev et al 2013). This distance value was obtained taking into account the Lutz-Kelker correction (Lutz & Kelker 1973); therefore, it differs from the preliminary estimates calculated as d = 1/π.…”

Section: Orbit Constructionmentioning

confidence: 92%

“…This distance value was obtained taking into account the Lutz-Kelker correction (Lutz & Kelker 1973); therefore, it differs from the preliminary estimates calculated as d = 1/π. Khovritchev et al (2013) 2016) constructed a preliminary orbit of the object and iteratively determined the masses of the components and dynamical parallax π dyn = 18.0 mas. The values obtained by Tokovinin (2016) analysis are shown in Tables 2 and 3.…”

Section: Orbit Constructionmentioning

confidence: 99%

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Speckle Interferometry of Nearby Multiple Stars: 2007-2019 Positional Measurements and Orbits of Eight Objects

Mitrofanova,

Dyachenko,

Beskakotov

et al. 2020

Preprint

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The orbits of 8 systems with low-mass components (HIP 14524, HIP 16025, HIP 28671, HIP 46199, HIP 47791, HIP 60444, HIP 61100 and HIP 73085) are presented. Speckle interferometric data were obtained at the 6 m Big Alt-azimuth Special Astrophysical Observatory of the Russian Academy of Sciences (BTA SAO RAS) from 2007 to 2019. New data, together with measures already in the literature, made it possible to improve upon previous orbital solutions in six cases and to construct orbits for the first time in the two remaining cases (HIP 14524 and HIP 60444). Mass sums are obtained using both Hipparcos and Gaia parallaxes, and a comparison with previously published values is made. Using the Worley & Heintz criteria, the classification of the orbits constructed is carried out.

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Section: Orbit Constructionmentioning

confidence: 88%

Section: Orbit Constructionmentioning

confidence: 92%

Section: Orbit Constructionmentioning

confidence: 99%

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Speckle Interferometry of Nearby Multiple Stars: 2007-2019 Positional Measurements and Orbits of Eight Objects

Mitrofanova,

Dyachenko,

Beskakotov

et al. 2020

Preprint

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“…Trigonometric parallaxes have been measured from the ground for the very nearest M dwarfs for decades (van Altena et al 1995;Gatewood et al 2003;Costa et al 2005;Henry et al 2006;Smart et al 2010;Khovritchev et al 2013;Dahn et al 2017;Henry et al 2018). However, robust results require significant time investment, so not all nearby stars have parallax measurements.…”

Section: Introductionmentioning

confidence: 99%

The Volume-Complete Sample of M Dwarfs with Masses 0.1 <= M/M_sol <= 0.3 within 15 Parsecs

Winters,

Charbonneau,

Henry

et al. 2020

Preprint

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M dwarfs with masses 0.1 ≤ M/M ≤ 0.3 are under increasing scrutiny because these fully convective stars pose interesting astrophysical questions regarding their magnetic activity and angular momentum history. They also afford the most accessible near-future opportunity to study the atmospheres of terrestrial planets. Because they are intrinsically low in luminosity, the identification of the nearest examples of these M dwarfs is essential for progress. We present the volume-complete, all-sky list of 512 M dwarfs with masses 0.1 ≤ M/M ≤ 0.3 and with trigonometric distances placing them within 15 pc (π trig ≥ 66.67 mas) from which we have created a sample of 413 M dwarfs for spectroscopic study. We present the mass function for these 512 M dwarfs, which increases with decreasing stellar mass in linear mass space, but is flat in logarithmic mass space. As part of this sample, we present new V J R KC I KC photometry for 17 targets, measured as a result of the RECONS group's long-term work at the CTIO/SMARTS 0.9m telescope. We also note the details of targets that are known to be members of multiple systems and find a preliminary multiplicity rate of 21 ± 2% for the primary M dwarfs in our sample, when considering known stellar and brown dwarf companions at all separations from their primaries. We further find that 43 ± 2% of all M dwarfs with masses 0.1 ≤ M/M ≤ 0.3 are found in multiple systems with primary stars of all masses within 15 pc.

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“…As a rule, solar-neighborhood stars are distinguished by large proper motions (µ> 0.1 arcsec•yr −1 ). Such stars are being actively investigated within the Pulkovo observational program (Khrutskaya et al (2011); Khovritchev et al (2013)). Some of the program stars have turned out to exhibit evidence for nonlinearity of their motion over the celestial sphere (astrometric binary candidates; see Khovritchev&Kulikova (2015)).…”

Section: Introductionmentioning

confidence: 99%

Detection of the binarity of the star J1158+4239

et al. 2016

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One of the goals of the Pulkovo program of research on stars with large proper motions is to reveal among the low-luminosity stars those that have evidence of binarity. Twelve astrometric binary candidates from the Pulkovo list have been included in the program of speckle observations with the BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS) and the 2.5-m telescope at the Caucasus Mountain Observatory (CMO) of the Sternberg Astronomical Institute of the Moscow State University to confirm their binarity and then to determine the parameters of the revealed stellar pairs. The binarity of the brightest of these stars, J1158+4239 (GJ 3697), has been confirmed. Four sessions of speckle observations with the BTA SAO RAS telescope and one session with the 2.5-m CMO telescope have been carried out in 2015-2016. The weighted mean estimates of the pair parameters are ρ=286.5±1.2 mas * e-mail: deimos@gao.spb.ru 1 and θ=230.24±0.16 • at the epoch B2015.88248. The magnitude difference between the pair stars is ∆m=0.55±0.03 (a filter with a central wavelength of 800 nm and a FWHM of 100 nm) and ∆m=0.9±0.1 (an R filter).

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Trigonometric parallaxes of 71 large proper motion stars

Cited by 13 publications

References 29 publications

Speckle Interferometry of Nearby Multiple Stars: 2007-2019 Positional Measurements and Orbits of Eight Objects

Speckle Interferometry of Nearby Multiple Stars: 2007-2019 Positional Measurements and Orbits of Eight Objects

The Volume-Complete Sample of M Dwarfs with Masses 0.1 <= M/M_sol <= 0.3 within 15 Parsecs

Detection of the binarity of the star J1158+4239

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