Orbits of 14 binaries based on 2018 SOAR speckle observations

Docobo, J. A.; Gómez, Jorge; Campo, P. P.; Andrade, Manuel Correia de; Horch, Elliott; Costa, E.; Mendez, Rene A.

doi:10.1093/mnras/sty2704

Cited by 13 publications

(6 citation statements)

References 69 publications

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“…Three of them were the brown dwarfs WISE J053516.80-750024.9, WISE J035934.06-540154.6, and WISE J154214.00+223005.2, with published parallaxes of 250± 79 mas, 145 ± 39 mas (Marsh et al 2013), and 96 ± 41 mas (Tinney et al 2014), respectively, which now have higher-precision parallax measurements from Kirkpatrick et al (2021) that move them outside the 10 pc limit. The other two objects were also low-mass stars: LP 388-55, an M7.5 V + L0 binary that had its parallax re-estimated from 110.7±5.8 mas (Dittmann et al 2014) to 64.3 ± 0.7 mas in Gaia EDR3 and the binary G 19-15 had a dynamical parallax measured of 74.0 ± 0.99 mas from Docobo et al (2019).…”

Section: Catalogue Compilationmentioning

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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Section: Catalogue Compilationmentioning

confidence: 99%

The 10 parsec sample in the Gaia era

Reylé

Jardine²,

Fouqué

et al. 2021

A&A

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“…Of these (which include suspected binaries from Hipparcos and tight spectroscopic binariessee previous paragraph) we have been able to confirm, resolve, and measure 1,183 systems -many several times-(see e.g. Tokovinin et al (2015), Gomez et al (2016), Mendez et al (2017), Docobo et al (2019) and Tokovinin et al (2020)). Other notable results from our observations include the discovery of almost sixty inner or outer subsystems in previously known binaries, as well as two quadruple systems (Tokovinin et al 2015(Tokovinin et al , 2016.…”

Section: Introductionmentioning

confidence: 77%

Orbits and masses of binaries from Speckle Interferometry at SOAR

Mendez,

Claveria,

Costa

2021

Preprint

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We present results from Speckle inteferometric observations of fifteen visual binaries and one doubleline spectroscopic binary, carried out with the HRCam Speckle camera of the SOAR 4.1 m telescope. These systems were observed as a part of an on-going survey to characterize the binary population in the solar vicinity, out to a distance of 250 parsec.We obtained orbital elements and mass sums for our sample of visual binaries. The orbits were computed using a Markov Chain Monte Carlo algorithm that delivers maximum likelihood estimates of the parameters, as well as posterior probability density functions that allow us to evaluate their uncertainty. Their periods cover a range from 5 yr to more than 500 yr; and their spectral types go from early A to mid M -implying total system masses from slightly more than 4 M down to 0.2 M . They are located at distances between approximately 12 and 200 pc, mostly at low Galactic latitude.For the double-line spectroscopic binary YSC8 we present the first combined astrometric /radial velocity orbit resulting from a self-consistent fit, leading to individual component masses of 0.897 ± 0.027 M and 0.857 ± 0.026 M ; and an orbital parallax of 26.61 ± 0.29 mas, which compares very well with the Gaia DR2 trigonometric parallax (26.55 ± 0.27 mas).In combination with published photometry and trigonometric parallaxes, we place our objects on an H-R diagram and discuss their evolutionary status. We also present a thorough analysis of the precision and consistency of the photometry available for them.

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“…Gaia vs Hipparcos: the Accuracy of Parallax Measurements Mashhoor A. Al-Wardat The mass sums estimated by our method are 3.16 M ⊙ using the Hipparcos-2 parallax measurements, far below the main sequence using the Gaia DR2 parallaxes (unacceptable solution), and 3.17 M ⊙ using the Gaia DR3 measurements. We also calculated the dynamical mass sum using the orbital period 𝑃 = 79.08 years and semi-major axis 𝑎 = 0.223 arcsec from Docobo et al [14] and the formula:…”

Section: Pos(muto2022)010mentioning

confidence: 99%

Gaia vs Hipparcos: the Accuracy of Parallax Measurements

Al-Wardat¹,

Hussein²,

Abu-Alrob³

2022

Proceedings of the Multifaceted Universe: Theory and Observations - 2022 — PoS(MUTO2022)

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We present a solution for the problem of the discrepancy in the measured trigonometric parallaxes for the stellar binary system HIP 84092. To solve the discrepancy, we used the orbital parameters and our method for analyzing binary and multiple stellar systems (BMSSs)s, described by Al-Wardat in 2002. We used all the available parallax measurements from Gaia DR3, DR2 and Hipparcos-2 in estimating the fundamental parameters of the individual components of the system. Such measurements are usually affected by the orbital motion of the components and the shift of the system photocenter. The masses estimated using the Al-Wardat method along with the modified orbital elements lead to a new dynamical parallax for the system 𝜋 𝐷𝑦𝑛 = 8.24 ± 0.15 mas, which lies in between the measurements of Hipparcos-2 (8.29±0.97 mas) and Gaia DR3 (8.4806±0.4863 mas), while the parallax from Gaia DR2 (20.0561 ± 1.1615 mas) is far from being accurate. This can be explained by the fact that the Gaia telescope has a higher resolution than that of Hipparcos. Based on the fundamental parameters of the binary system components and their positions on the evolutionary tracks, we conclude that the system consists of A7.5 and F1 solar-metalicity mainsequence stars with an age of 0.708 Gyr. Fragmentation is proposed as the most likely scenario for the formation and evolution of the system.

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Orbits of 14 binaries based on 2018 SOAR speckle observations

Cited by 13 publications

References 69 publications

The 10 parsec sample in the Gaia era

The 10 parsec sample in the Gaia era

Orbits and masses of binaries from Speckle Interferometry at SOAR

Gaia vs Hipparcos: the Accuracy of Parallax Measurements

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