Investigation of the motions of fast stars based on observations with the Pulkovo normal astrograph

Khrutskaya, E. V.; Berezhnoi, A. A.; Khovrichev, M. Yu.

doi:10.1134/s1063773711060053

Cited by 6 publications

(6 citation statements)

References 10 publications

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“…Its proper motion components in the LSPM catalog are -330 and 61 mas·yr −1 in RA and Dec, respectively. Its quasi-instantaneous proper motion in Khrutskaya et al (2011) turned out to be -303.3±8.8 and 114.1±9.0 mas·yr −1 , which provided F = 4.44. Figure 1 shows the motion of the photocenter for J1158+4239.…”

Section: Motion Of the Photocenter Of J1158+4239mentioning

confidence: 99%

“…The difference between the quasi-instantaneous and quasi-mean proper motions turned out to be significant for 70 stars. The data on this were published in Khrutskaya et al (2011) and are accessible in electronic form in the Pulkovo astrometric database system 1 . The described method of solving the problem has a number of problems.…”

Section: Implementing the Methods Based On Sky Survey Data And Pulkovomentioning

confidence: 99%

“…This idea was applied by Wielen et al (1999) to bright stars from the FK6 catalog. When implementing the Pulkovo program of research on stars with large proper motions, this technique was adapted to reveal astrometric binaries among the low-luminosity stars in the solar neighborhood (Khrutskaya et al (2011);Khovritchev&Kulikova (2015)). …”

Section: Revealing the Nonlinearity Of The Binary Photocenter Motion mentioning

confidence: 99%

“…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)).…”

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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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Section: Motion Of the Photocenter Of J1158+4239mentioning

confidence: 99%

Section: Implementing the Methods Based On Sky Survey Data And Pulkovomentioning

confidence: 99%

Section: Revealing the Nonlinearity Of The Binary Photocenter Motion mentioning

confidence: 99%

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Detection of the binarity of the star J1158+4239

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“…The quasi-mean proper motions were taken from the LSPM catalog. As a result, 70 ∆µ binaries were revealed (Khrutskaya et al (2011)).…”

Section: Introductionmentioning

confidence: 98%

Δμ binaries among stars with large proper motions

Khovritchev¹,

Kulikova²

2015

Astron. Lett.

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Based on observations performed with the Pulkovo normal astrograph in 2008-2015 and data from sky surveys (DSS, 2MASS, SDSS DR12, WISE), we have investigated the motions of 1308 stars with proper motions larger than 300 mas/yr down to magnitude 17. The main idea of our search for binary stars based on this material is reduced to comparing the quasi-mean (POSS2-POSS1; an epoch difference of ≈50 yr) and quasi-instantaneous (2MASS, SDSS, WISE, Pulkovo; an epoch difference of ≈10 yr) proper motions. If the difference is statistically significant compared to the proper motion errors, then the object may be considered as a ∆µ-binary candidate. One hundred and twenty one stars from among those included in the observational program satisfy this requirement. Additional confirmations of binarity for a number of stars have been obtained by comparing the calculated proper motions with the data from several programs of stellar trigonometric parallax determinations and by analyzing the asymmetry of stellar images on sky-survey CCD frames. Analysis of the highly accurate SDSS photometric data for four stars (J0656+3827, J0838+3940, J1229+5332, J2330+4639) allows us to reach a conclusion about the probability that these ∆µ binaries are white dwarf + M dwarf pairs.

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