Speckle interferometry of nearby multiple stars. V. 2002–2006 positional measurements

Балега, И. И.; Balega, Yu. Yu.; Гасанова, Л. Т.; Dyachenko, V. V.; Максимов, А. Ф.; Малоголовец, Е. В.; Растегаев, Д. А.; Shkhagosheva, Z. U.

doi:10.1134/s1990341313010057

Cited by 46 publications

(35 citation statements)

References 16 publications

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“…We also note that orbital parameters from the CORAVEL RV data are briefly discussed in Halbwachs et al (2003) and an independent estimate of the orbit from the Hipparcos intermediate data is presented in Goldin & Makarov (2007). Balega et al (2013) also present speckle interferometry measurements of NO UMa from the 6 m BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO-RAS). Their observations span ∼4 years from 2002 to 2006 and were obtained using filters with λ c =545, 750, or 800 nm.…”

Section: Known Fundamental and Orbitalmentioning

confidence: 99%

“…Due to the good coverage of both our astrometric and spectroscopic data over different phases of the orbit, we found that choices of initial guess comparable to previous estimates have no significant effect on the results of the fits. The measured t, x, and y inputs to the orbit analysis include those from our three LBTI/LMIRcam images, the Keck/NIRC2 image, and the six speckle interferometry measurements from Balega et al (2013). 17 The measured astrometry is provided in Table 3.…”

Section: Orbit Analysismentioning

confidence: 99%

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THE LEECH EXOPLANET IMAGING SURVEY: ORBIT AND COMPONENT MASSES OF THE INTERMEDIATE-AGE, LATE-TYPE BINARY NO UMa* †

Schlieder

Skemer

Maire

et al. 2016

ApJ

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We present high-resolution Large Binocular Telescope LBTI/LMIRcam images of the spectroscopic and astrometric binary NO UMa obtained as part of the LBT Interferometer Exozodi Exoplanet Common Hunt exoplanet imaging survey. Our H-, K s -, and L′-band observations resolve the system at angular separations <0 09. The components exhibit significant orbital motion over a span of ∼7 months. We combine our imaging data with archival images, published speckle interferometry measurements, and existing spectroscopic velocity data to solve the full orbital solution and estimate component masses. The masses of the K2.0±0.5 primary and K6.5±0.5 secondary are 0.83±0.02 M e and 0.64±0.02 M e , respectively. We also derive a system distance of d=25.87±0.02 pc and revise the Galactic kinematics of NO UMa. Our revised Galactic kinematics confirm NO UMa as a nuclear member of the ∼500 Myr old Ursa Major moving group, and it is thus a mass and age benchmark. We compare the masses of the NO UMa binary components to those predicted by five sets of stellar evolution models at the age of the Ursa Major group. We find excellent agreement between our measured masses and model predictions with little systematic scatter between the models. NO UMa joins the short list of nearby, bright, late-type binaries having known ages and fully characterized orbits.

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Section: Known Fundamental and Orbitalmentioning

confidence: 99%

Section: Orbit Analysismentioning

confidence: 99%

THE LEECH EXOPLANET IMAGING SURVEY: ORBIT AND COMPONENT MASSES OF THE INTERMEDIATE-AGE, LATE-TYPE BINARY NO UMa* †

Schlieder

Skemer

Maire

et al. 2016

ApJ

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“…New measurements, because they will be performed after the system passed through the periastron, could contribute to a more accurate determination of the orbital elements. In Balega et al (2007Balega et al ( , 2013 we find that the position angles from 2003.9275 and 2004.8237 have 180…”

Section: Individual Systemsmentioning

confidence: 99%

“…Seven measurements are given in INT4 and they are used for the calculation of the first orbit (Table 1). Recently in Balega et al (2013) we found one more measurement for the epoch 2003.9275. It has small residuals, (O − C) θ = 1.…”

Section: Individual Systemsmentioning

confidence: 99%

ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

Cvetković

Pavlović

Ninković

2014

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In this paper, we analyze new orbital elements and the quantities that follow from them for eight binaries: WDS 00101+3825 = HDS 23Da,Db, WDS 00321−1218 = HDS 71, WDS 04287+2613 = HDS 576, WDS 04389−1207 = HDS 599, WDS 16206+4535 = HDS 2309, WDS 17155+1052 = HDS 2440, WDS 22161−0705 = HDS 3158, and WDS 23167+3441 = HDS 3315. For seven of them, the orbital elements are calculated for the first time. Binaries, denoted as HDS, were discovered during the Hipparcos mission, and their first observational epoch is 1991.25, the same as the mean epoch of the Hipparcos catalog. We found all other measurements of these binaries in databases. They were obtained in the last 15 yr using the speckle interferometric technique. All studied pairs are close, and all measured separations are less than 0. 4. The resulting orbital periods fall within 26 and 80 yr. In addition to the orbital elements, we also give (O − C) residuals in θ and ρ, masses, dynamical parallaxes, absolute magnitudes, spectral types, and ephemerides for the next 5 yr.

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“…First we have collected observational data of HD 87646 from the literature (Horch et al 2008, Hartkopf & Mason 2009, Horch et al 2010, Balega et al 2013) and combined them with our AO data to constrain the binary orbit of HD 87646. Our best fitting binary orbital solution (solid line) and the observational data (black dots) are shown in Fig.…”

Section: Dynamical Stability Of Hd 87646mentioning

confidence: 99%

Very Low-Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Vi. A Giant Planet and a Brown Dwarf Candidate in a Close Binary System Hd 87646

Wolszczan

et al. 2016

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We report the detections of a giant planet (MARVELS-7b) and a brown dwarf candidate (MARVELS-7c) around the primary star in the close binary system, HD 87646. It is the first close binary system with more than one substellar circum-primary companion discovered to the best of our knowledge. The detection of this giant planet was accomplished using the first multi-object Doppler instrument (KeckET) at the Sloan Digital Sky Survey (SDSS) telescope. Subsequent radial velocity observations using ET at Kitt Peak National Observatory, HRS at HET, the "Classic" spectrograph at the Automatic Spectroscopic Telescope at Fairborn Observatory, and MARVELS from SDSS-III confirmed this giant planet discovery and revealed the existence of a long-period brown dwarf in this binary. HD 87646 is a close binary with a separation of ∼ 22 AU between the two stars, estimated using the Hipparcos catalogue and our newly acquired AO image from PALAO on the 200-inch Hale Telescope at Palomar. The primary star in the binary, HD 87646A, has T eff = 5770± 80K, log g =4.1±0.1 and [Fe/H] = −0.17 ± 0.08. The derived minimum masses of the two substellar companions of HD 87646A are 12.4±0.7 M Jup and 57.0±3.7 M Jup . The periods are 13.481±0.001 days and 674±4 days and the measured eccentricities are 0.05±0.02 and 0.50±0.02 respectively. Our dynamical simulations show the system is stable if the binary orbit has a large semi-major axis and a low eccentricity, which can be verified with future astrometry observations.

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Speckle interferometry of nearby multiple stars. V. 2002–2006 positional measurements

Cited by 46 publications

References 16 publications

THE LEECH EXOPLANET IMAGING SURVEY: ORBIT AND COMPONENT MASSES OF THE INTERMEDIATE-AGE, LATE-TYPE BINARY NO UMa* †

THE LEECH EXOPLANET IMAGING SURVEY: ORBIT AND COMPONENT MASSES OF THE INTERMEDIATE-AGE, LATE-TYPE BINARY NO UMa* †

ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

Very Low-Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Vi. A Giant Planet and a Brown Dwarf Candidate in a Close Binary System Hd 87646

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