Detection of the binarity of the star J1158+4239 |
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| Authors: | M Yu Khovrichev A M Kulikova E N Sokov V V Dyachenko D A Rastegaev A S Beskakotov Yu Yu Balega B S Safonov A V Dodin O V Vozyakova |
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| Institution: | 1.Pulkovo Astronomical Observatory,Russian Academy of Sciences,St. Petersburg,Russia;2.Special Astrophysical Observatory,Russian Academy of Sciences,Nizhnii Arkhyz, Karachai-Cherkessian Republic,Russia;3.Sternberg Astronomical Institute,Moscow State University,Moscow,Russia |
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| Abstract: | 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 Observatory (CO) 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 CO telescope have been carried out in 2015–2016. The weighted mean estimates of the pair parameters are ρ = 286.5 ± 1.2 mas and θ = 230.24? ± 0.16? at the epoch B2015.88248. The magnitude difference between the pair stars is Δm = 0.55 ± 0.03 (a filter with a central wavelength of 800 nm and a FWHM of 100 nm) and Δm = 0.9 ± 0.1 (an R filter). |
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