20 Orbits of binaries based on soar speckle observations

MNRAS 509, 4229–4245 (2022) https://doi.org/10.1093/mnras/stab2633 Advance Access publication 2021 September 16 20 Orbits of binaries based on soar speckle obser v ations Jorge G ´ omez, 1 , 2 Jos ´ e A. Docobo, 1 , 2 , 3 ‹Pedro P. Campo, 1 , 2 ‹Manuel Andrade, 1 , 2 , 4 Rene A. Mendez. 5 ‹and Edgardo Costa 5 1 Observatorio Astron ´ omico Ram ´ on Mar ´ ıa Aller, Universidade de Santiago de Compostela (USC), Avenida das Ciencias s/n, Campus Vida, Santiago de Compostela, E-15782 Galiza, Spain 2 Instituto de Matem ´ aticas and Departamento de Matem ´ atica Aplicada, Facultade de Matem ´ aticas, USC, R ´ ua Lope G ´ omez de Marzoa, s/n, Campus Vida, Santiago de Compostela, E-15782 Galiza, Spain 3 Real Academia de Ciencias de Zaragoza, Facultad de Ciencias, C/ Pedro Cerbuna 12, E-50009 Zaragoza, Spain 4 Escola Polit ´ ecnica Superior de Enxe ˜ nar ´ ıa, USC, Benigno Ledo s/n, Campus Terra, Lugo, E-27002 Galiza, Spain 5 Universidad de Chile, Casilla 36-D, Santiago, Chile Accepted 2021 September 9. Received 2021 August 30; in original form 2021 June 3 A B S T R A C T Ne w observ ational data obtained during the 2018, 2019, and 2020 speckle runs with the 4.1-m Southern Astrophysical Research (SOAR) telescope located at Cerro Pach ´ on (Chile) allowed us to recalculate the orbits of the visual binaries: WDS 00277-1625 (YR 1 Aa,Ab), WDS 00462-2214 (RST4155), WDS 03124-4425 (JC 8), WDS 07427-3510 (HDS 1091), WDS 10093 + 2020 (A2145), WDS 10116 + 1321 (HU 874 AB), WDS 10217-0946 (BU 25), WDS 11585-2350 (RST 3767 AB), WDS 13117-2633 (FIN 305), WDS 13305 + 0729 (A 1789), and WDS 16458-0046 (A1141). In addition, we present the first orbits calculated for the following binaries: WDS 07303-5657 (FIN 105), WDS 09110-1929 (I 824), WDS 12111-5302 (HU 1604), WDS 14592-4206 (HDS 2116 Aa,Ab), WDS 15157-2736 (BU 350), WDS 15493 + 0503 (A 1126), WDS 16402-2800 (VOU 44 AB), and WDS 18126 + 1224 (HDS 2570). All of them are placed below Dec. + 21 ◦and the majority are main-sequence stars. Except in cases with giant components or close triple systems, the ANAPAR method was used in order to obtain precise dynamical parallaxes and individual masses. These parallaxes were compared with those obtained by Gaia and/or Hipparcos satellites. In the case of FIN 305, we present two different orbital solutions. Also, using the dynamical parallaxes given by these orbits, we have been able to calculate the luminosity of these systems. Said luminosities allow us to indicate an approximate age for the components of these systems, situating them within the Hertzsprung-Russell (HR) diagram. In addition, a commentary for each binary about the physical and dynamical properties of the studied binaries has been included. Key words: techniques: high angular resolution – astrometry – binaries: visual – stars: fundamental parameters. 1 INTRODUCTION Speckle interferometry was disco v ered and first applied 50 yr ago (Labeyrie 1970 ), and it continues to yield astrometric and photometric data that are especially important for the study of binary and multiple star systems. The determination of close visual orbits combined with the parallaxes measured by Gaia (Gaia Collaboration 2016 , 2018 ) allows us to calculate the total mass of the system and estimate approximate values for the masses of each component based on the difference of magnitude between the components and their spectral decomposition. Moreo v er, using the ANAPAR method (Andrade 2019 ), we cannot only obtain very precise values of the dynamical parallaxes but also the individual masses, except in cases when there is a giant component in a system. In this article, we have used measurements of the Southern Astrophysical Research (SOAR) 2018 (Tokovinin et al. 2019 ), 2019, and 2020 speckle runs in order  E-mail: [email protected] (JAD); [email protected] (PPC); [email protected] (RAM) to calculate new orbits for 11 systems that need to be impro v ed. The orbits as well as their corresponding physical parameters of another eight systems: FIN 105, I 824, HU 1604, HDS 2116 Aa,Ab, BU 350, A 1126, VOU 44 AB, and HDS 2570 were calculated for the first time. Except in the cases with giant components, the Gaia and the Hipparcos parallaxes have been compared with the dynamical parallaxes. The HRCam, a fast imager that works either as a standalone instrument or with SOAR Adaptive Module (SAM; Tokovinin et al. 2016 ) was used in all of those observational speckle runs. The device is installed at the 4.1-m SOAR telescope located at Cerro Pach ´ on (Chile) and allows for interferometry combined with adaptive optics yielding resolutions in the 0.012–3.37 arcsec range. In a typical observing run, the calibration measurements are characterized by rms errors of 0 ◦1–0 ◦2 in orientation and 0.002–0.004 in scale. SOAR speckle runs were specifically designed to collect a large quantity of rele v ant data from well kno wn, less kno wn, and even from those systems with undetected subcomponents (Tokovinin 2018a ). The SOAR speckle campaigns (Tokovinin et al. 2015 , 2018 , 2019 ; Tokovinin 2016 ) increase the number of measurements and © 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License ( http://cr eativecommons.or g/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 4230 J. Gomez et al. the quality of the samples of the orbits of southern systems year by year. As a matter of fact, these data were used in several orbital calculations (e.g. Tokovinin 2017 , 2018b ; Mendez et al. 2017 ; Mason et al. 2018 ) and consequently, in the precise determination of stellar masses and dynamical parallaxes. Together with the precise data provided by SOAR, the whole set of previous measurements, those available in the USNO Catalogue of Interferometric Measurements of Binary Stars (Hartkopf, McAlister & Mason 2001b ) and also those included in the historical data base of micrometric measurements, (Worley & Douglass 1997 ), have been used. The weights of the visual observations follow the scheme shown in Docobo & Ling ( 2003 ), whereas for the interferometric measurements we have assigned them according to the aperture of the telescope: weight 5 for apertures smaller than 1, 10 for 1-2, 15 for 2-4, 20 for 4-6 m., and 30 for larger apertures. To impro v e or calculate from the beginning all of those orbits, the well-known analytic method of Docobo ( 1985 , 2012 ) was used. The method is based on a mapping from the interval (0,2 π) into the set of Keplerian orbits whose corresponding apparent orbits pass through three base points ( θi , ρi ; t i ) (i = 1, 2, 3). In contrast to the Thiele– Innes–van den Bos method, knowledge of the areal constant is not necessary. In a recent paper by Docobo, Tamazian & Campo ( 2018 ), the different selection criteria for the orbit were explained: the solution with minimal rms of the O–C residuals from all of the weighted observations, matching dynamical and trigonometric ( Gaia or Hipparcos ) parallaxes, and/or the agreement between the calculated masses and those that correspond to the spectral types, etc. The rms error of the residuals is calculated using the following expression: rms =   n i= 1 w i ( O i −C i ) 2  n i= 1 w i , (1) where n is the number of observations, O i and C i are the observed and the calculated v alues, respecti vely, and w i represents the weight assigned for the corresponding i observation. For each of the orbits generated by this method, the software yields not only the rms (with weights) both for the position angle ( θ) and for the angular separation ( ρ) but also the dynamical parallaxes with the individual masses and the total mass calculated from the Hipparcos or Gaia parallaxes. We also obtain for each orbit the residuals for θ and ρcorresponding to the measurements with large weights. With all of these quality controls, the interval of most probable orbits is delimited and the standard errors of each orbital element are deduced. Dynamical parallaxes and individual masses have been accurately computed using the ANAPAR method, a colour-dependent model comprising an exact analytical theory along with a non-linear mass– luminosity relationship that allows us to take into account the spectral types of the main-sequence components. In addition, their uncertainties have been calculated from uncertainties in the orbital elements and in the apparent magnitudes by means of Monte Carlo simulations. We have compared these dynamical parallaxes with the values provided by Hipparcos and Gaia DR2. In some cases, the Gaia EDR3 provided new values for the parallaxes, and we commented them in the text. This investigation represents the continuation of the collaboration between the research groups of the Universidad de Chile and the Ramon Maria Aller Astronomical Observatory at the Universidade de Santiago de Compostela for the investigation of binary and multiple stellar systems in the context of the IAU G1 Commission (Gomez et al. 2016 ; Docobo et al. 2019 ). A detailed description of the procedure for processing data is described in Tokovinin et al. ( 2018 ). In Section 2, we present the results and discussion with individual comments for each binary. Tables 1 –5 summarize the information related to the obtained orbital elements, the ephemerides, the weighted rms quality controls, the masses, and the dynamical parallaxes yielded by previous and new orbits. Figs 1 –19 show the apparent orbits along with the available observations. The new orbit is indicated with a solid line and the previous orbit is shown with a broken line. The Fig. 1 caption contains details associated with the plots. In Section 3, we calculate the absolute magnitudes and luminosities (Table 6 ) in order to determine the locations of the systems in the HR diagram as plotted relative to the isochrones generated with MESA Isochrones and Stellar Tracks, MIST (Paxton et al. 2011 , 2013 , 2015 ; Choi et al. 2016 ; Dotter 2016 ). Absolute luminosities for the A 1126, A 2145, and HDS 2570 systems were not included because the y hav e at least one giant component, and for BU 25 because of the existence of a spectroscopic subcomponent for the primary star. The ef fecti ve temperature was selected from de Jager & Nieuwenhuijzen ( 1987 ) according to the spectral type of each component. We used the metallicity data from Ammons et al. ( 2006 ), Gontcharov ( 2012 ), Gaspar, Rieke & Ballering ( 2016 ), and Netopil ( 2017 ) to calculate the isochrones when available. Otherwise, we used the metallicity of the Sun. Table 7 shows the data utilized. Figs 20 –35 each present one HR diagram per system in which different MIST-generated isochrones are displayed with the position of the system components. Conclusions are discussed in Section 4. The orbits of the binaries FIN 105, HDS 1091, I 824, HU 874 AB, BU 25, HU 1604, FIN 305, A 1789, HDS 2116 Aa,Ab, A 1126, VOU 44 AB, and HDS 2570 were announced in the IAUDS No 201 (Docobo et al. 2020 ), and those of the binaries YR 1 Aa,Ab, RST 4155, JC 8, A 2145, RST 3767 AB, BU 350, and A 1141 are published for the first time in this work. 2 RESULTS AND DISCUSSION In Tables 1 and 2 , each system is identified in the first column by its Washington Double Star Catalogue (WDS) number (Mason et al. ) and by the disco v erer code, which is the name of the binary. In Table 1 , we list each binary and the corresponding orbital elements with their standard errors (Columns 2–8): period, P , in years; periastron passage, T , in years; eccentricity, e ; the semimajor axis, a , in arcseconds; inclination, i ; angle of the node, , and the argument of the periastron, ω, in degrees. We include the correction for precession used to refer the position angles to the standard equinox of J2000.0 (column 9). The epoch of the last observation used for the orbit calculation is in the same column. Table 2 lists ephemerides for the next 5 yr with θvalues in degrees and those of ρin arcseconds. Table 3 contains the magnitudes, the spectral types, the parallaxes, and the calculated masses. In Column 1, the WDS number and the Hipparcos identifier (ESA 1997 ) appear. The name of the binary is in column 2. Columns 3 and 4 list the apparent magnitudes for each component that are preferably taken from the WDS catalogue (Mason et al. 2001 ). If they do not appear in said catalogue, they are obtained using the SIMBAD total magnitude (Wenger et al. 2000 ) as well as the magnitude difference given by SOAR speckle observations. The same occurs with the spectral types in Columns 5, 6, and 7. We used the WDS data whenever available. Otherwise, the individual spectral type were obtained from the composite spectrum taking into account the calculated magnitude difference for the system. Columns 8 and 9 show the Gaia (Gaia Collaboration 2016 , 2018 ) or the Hipparcos (H) parallaxes (Perryman et al. 1997 ; van Leeuwen 2007 ) as well MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 20 orbits of binaries 4231 Table 1. Orbital elements. WDS P(yr) T(B1950.0) e a(arcsec) i( ◦) ( ◦) ω( ◦) Prec. ( ◦) name σ σ σ σ σ σ σ last obs 00277-1625 6.5343 2020.890 0.7845 0.0674 13.17 110.27 56.98 0.0007 YR 1 Aa,Ab ±0.0210 ±0.050 ±0.0110 ±0.0012 ±5.0 ±30.0 ±30.0 2020.8342 00462-2214 49.13 2003.96 0.261 0.162 143.8 3.1 322.5 0.0012 RST 4155 ±0.8 ±0.25 ±0.002 ±0.004 ±2.0 ±4.0 ±5.0 2020.9270 03124-4425 45.35 2022.65 0.872 0.407 156.1 167.8 176.1 0.0058 JC 8 ±0.35 ±0.20 ±0.015 ±0.002 ±10.0 ±25.0 ±30.0 2020.8344 07303-5657 170.0 2046.15 0.578 0.244 153.5 52.1 107.1 0.0095 FIN 105 ±40.0 ±10.05 ±0.17 ±0.015 ±3.0 ±35.0 ±30.0 2018.2355 07427-3510 275.0 2017.4 0.690 0.332 115.2 93.3 200.2 0.0062 HDS 1091 ±50. ±0.4 ±0.03 ±0.026 ±0.5 ±1.0 ±2.0 2018.8438 09110-1929 940. 2029.37 0.869 0.492 130.3 116.5 18.0 0.0040 I 824 ±140.0 ±13.23 ±0.231 ±0.050 ±19.7 ±28.5 ±40.0 2018.2358 10093 + 2020 74.71 1991.86 0.829 0.139 160.6 127.1 91.4 0.0028 A 2145 ±1.2 ±0.20 ±0.010 ±0.002 ±0.8 ±20.0 ±20.0 2019.3833 10116 + 1321 17.96 2022.828 0.930 0.117 78.5 106.2 355.2 0.0026 HU 874 AB ±0.35 ±0.30 ±0.005 ±0.001 ±0.5 ±2.5 ±15.0 2019.3816 10217-0946 1340. 1960.53 0.297 2.546 133.9 168.2 20.3 0.0024 BU 25 ±60.0 ±2.50 ±0.025 ±0.100 ±1.0 ±1.0 ±2.0 2018.1811 11585-2350 740.0 1950.53 0.661 0.914 44.5 137.6 14.3 0.0000 RST 3767 AB ±50.0 ±1.50 ±0.015 ±0.035 ±2.0 ±4.0 ±2.0 2018.2536 12111-5302 205.0 2049.09 0.431 0.341 55.6 89.2 32.7 -0.0005 HU 1604 ±20.0 ±14.95 ±0.080 ±0.003 ±2.5 ±3.0 ±10.0 2018.1621 13117-2633 20.07 2021.801 0.989 0.226 114.4 8.4 91.7 −0.0019 FIN 305 a ±0.50 ±0.80 ±0.008 ±0.002 ±1.0 ±1.0 ±3.0 2019.0494 13117-2633 40.70 2006.5 0.045 0.219 98.6 93.3 304.5 -0.0019 FIN 305 b ±0.80 ±1.10 ±0.025 ±0.002 ±1.0 ±1.0 ±8.5 2019.0494 13305 + 0729 143.44 1962.714 0.420 0.191 137.8 67.9 105.4 -0.0022 A 1789 ±1.2 ±5.0 ±0.024 ±0.002 ±0.5 ±10.0 ±5.0 2018.2361 14592-4206 58.52 2011.10 0.304 0.287 90.9 156.1 215.1 -0.0053 HDS 2116 Aa,Ab ±1.50 ±0.30 ±0.009 ±0.008 ±0.5 ±0.5 ±2.0 2019.3798 15157-2736 695.0 2020.82 0.851 0.972 138.0 178.7 188.8 -0.0048 BU 350 ±90.0 ±1.50 ±0.020 ±0.035 ±1.0 ±1.0 ±3.5 2018.1814 15493 + 0503 289.0 1999.09 0.647 0.197 63.5 34.4 357.9 -0.0047 A 1126 ±14.0 ±0.3 ±0.015 ±0.005 ±0.5 ±1.0 ±2.0 2019.5387 16402-2800 104.67 2067.037 0.204 0.192 41.0 13.4 154.0 -0.0060 VOU 44 AB ±5.0 ±19.0 ±0.050 ±0.015 ±5.0 ±8.0 ±25.0 2019.3773 16458-0046 62.39 2042.46 0.067 0.216 103.4 15.7 46.4 -0.0053 A 1141 ±0.50 ±2.50 ±0.003 ±0.002 ±0.5 ±0.5 ±11.5 2018.1832 18126 + 1224 87.33 2010.28 0.457 0.161 73.3 131.3 153.6 -0.0057 HDS 2570 ±0.95 ±0.40 ±0.037 ±0.008 ±1.0 ±1.0 ±1.0 2019.5363 Note. a Short orbital solution for FIN 305. b Long orbital solution for FIN 305 . as the total mass deduced using the new orbital parameters. The dynamical parallaxes determined using ANAPAR, appear in Column 10 and the derived individual masses in Columns 11 and 12. All mass values are listed with the associated standard errors. The mass errors were calculated using the propagation of uncertainties. Absolute magnitudes used for calculation were taken from Gray ( 2005 ). Both parallax es are e xpressed in milliarcseconds (mas) and the masses in solar masses (M ). Tables 4 and 5 show the different quality controls used to compare each orbit. First, we calculated the rms error of the differences between the observed and the calculated values of the θand ρcoordinates using the data weighting scheme mentioned. We emphasize that the highest weights were assigned to interferometric observations. In Table 5 , Column 1 contains the WDS and the Hipparcos designations. Column 2 shows the disco v erer code (name of the binary). Column 3 presents the author and the year of the previous orbit and Column 4, the Gaia or Hipparcos parallax value. Columns 5 and 6 show the previous and new values for the dynamical parallaxes, respectively. 2.1 WDS 00277-1625 (YR 1 Aa,Ab) This system has a very short period. Orbits for this system were calculated in 2017 (Cv etko vi ´ c, P avlo vi ´ c & Boe v a 2017 ) and 2019 (Tokovinin 2019 ). Both show large rms uncertainties in θ, even though all of the available observations of this system are high MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 4232 J. Gomez et al. Table 2. Ephemerides. 2021.0 2022.0 2023.0 2024.0 2025.0 WDS Name θ ρ θ ρ θ ρ θ ρ θ ρ ( ◦) (arcsec) ( ◦) (arcsec) ( ◦) (arcsec) ( ◦) (arcsec) ( ◦) (arcsec) 00277-1625 YR 1 Aa,Ab 233.4 0.019 316.6 0.080 333.3 0.108 344.8 0.118 356.0 0.112 00462-2214 RST 4155 240.2 0.164 234.7 0.169 229.7 0.175 224.9 0.180 220.4 0.184 03124-4425 JC 8 118.9 0.183 84.8 0.093 287.9 0.067 231.0 0.156 215.1 0.235 07303-5657 FIN 105 65.7 0.233 64.0 0.228 62.2 0.223 60.3 0.218 58.3 0.212 07427-3510 HDS 1091 243.1 0.076 234.6 0.069 224.4 0.064 212.7 0.060 199.9 0.058 09110-1929 I 824 156.8 0.074 151.3 0.073 145.7 0.072 139.9 0.071 133.9 0.070 10093 + 2020 A2145 223.2 0.232 222.3 0.234 221.4 0.235 220.5 0.237 219.7 0.238 10116 + 1321 HU 874 AB 289.6 0.112 292.4 0.062 250.0 0.008 278.9 0.075 281.1 0.119 10217-0946 BU 25 127.9 1.535 127.4 1.532 126.9 1.529 126.5 1.525 126.0 1.522 11585-2350 RST 3767 AB 275.7 0.590 276.3 0.597 276.9 0.605 277.5 0.612 278.1 0.619 12111-5302 HU 1604 37.0 0.195 36.7 0.196 42.4 0.197 45.1 0.198 47.7 0.200 13117-2633 FIN 305 a 65.7 0.064 141.9 0.029 119.5 0.076 112.6 0.105 108.5 0.127 13117-2633 FIN 305 b 62.3 0.0630 36.22 0.0401 345.77 0.0356 311.18 0.0545 296.76 0.0811 13305 + 0729 A 1789 158.5 0.196 156.9 0.197 155.3 0.197 153.7 0.198 152.2 0.199 14592-4206 HDS 2116 Aa,Ab 157.1 0.176 156.9 0.205 156.8 0.231 156.6 0.255 156.5 0.276 15157-2736 BU 350 350.5 0.144 341.1 0.142 331.5 0.140 321.8 0.140 312.1 0.141 15493 + 0503 A 1126 143.0 0.061 147.2 0.064 151.0 0.068 154.4 0.071 157.5 0.074 16402-2800 VOU 44 AB 4.8 0.227 6.7 0.227 8.5 0.227 10.3 0.227 12.1 0.226 16458-0046 A1141 79.6 0.058 63.6 0.068 52.5 0.082 44.7 0.098 39.0 0.113 18126 + 1224 HDS 2570 348.6 0.060 357.1 0.054 7.3 0.050 19.2 0.047 32.1 0.046 Note . a Short orbital solution for FIN 305. b long orbital solution for FIN 305. precision speckle observations (ten observations carried out by E. P. Horch from 1977-2014 and four by A. Tokovinin between 2017 and 2020). Using the new measurement of 2020.8342 obtained with the HRCam@SOAR, we have achieved a solution that yields a rms of 0 ◦084 in θand 0  0128 in ρ, whereas the previous orbit was 18 ◦719 and 0  0168 (see Table 4 ). Moreo v er, the dynamical parallax (14.33 ±0.31 mas) fits the value given by Gaia 14.22 ±0.15 mas (Gaia Collaboration 2018 ). The inferred masses of the components (M A = 1.362 ±0.033 M and M B = 1.073 ±0.024 M ) do not differ much from those that correspond to the F4V + G1V spectral decomposition if we use the table of values of Gray ( 2005 ). These spectral types are the result of using the spectral decomposition method proposed by Edwards ( 1976 ), taking into account the spectral type of the system (F5/6V) and the difference of magnitude among the components given by SOAR (  m V ∼1.21). The low inclination ( ∼13 ◦, see Fig. 1 ) may represent a handicap regarding obtaining a spectroscopic orbit. 2.2 WDS 00462-2214 (RST4155) The orbit presented here represents an impro v ement of the previous one that was calculated by Heintz ( 1984 ). In recent decades, seven more speckle observations were obtained along with that by Hipparcos in 1991 (Perryman et al. 1997 ). The previous orbit had rms θ = 8 ◦519 and rms ρ= 0  0287 while the new orbit decreases them to rms θ= 3 ◦105 and rms ρ= 0  0145. The new dynamical parallax of 9.53 ±0.30 mas is close to that by Gaia , 9.21 ±0.33 mas (Gaia Collaboration 2018 ). Using the dynamical parallax, the total mass of the system is M T = 2.033 M with M A = 1.043 ±0.026 M and M B = 0.990 ±0.024 M . These values are in accord with those expected for a system on the basis of the combined spectrum F9V + G1V assigned by using the previously cited algorithm. In Fig. 2 , the previous orbit (Heintz 1984 ) and that contributed in this paper are shown. 2.3 WDS 03124-4425 (JC 8) In 1935, Finsen ( 1935 ) calculated an orbital solution for this system for the first time that was followed by those presented by Wierzbi ´ nski ( 1958 ), Eggen ( 1965 ), Starikova ( 1977a ), Heintz ( 1979 ), and S ¨ oderhjelm ( 1999 ). Our solution reduces the rms uncertainty in θof the orbit of S ¨ oderhjelm ( 1999 ), from 4 ◦733 to 1 ◦930. In addition, the dynamical parallax associated with the new orbit, 23.58 ±0.24 mas, approximates the v alue gi ven by Hipparcos , 23.53 ±0.62 mas. The spectral decomposition of the system given in Simbad is A8V + F3V, while the masses that we obtain for each component are M A = 1.365 ±0.031 M and M B = 1.134 ±0.024 M which correspond with the ranges of F5V-F8V for the main and F8V-G0V for the secondary according to the values given by Gray ( 2005 ). This may be due to an incorrect spectral classification of the star. The A8V + F3V decomposition adopted in Simbad comes from (Malaroda 1973 ), but there are other listed measurements, some of them assigning a combined spectrum of F6III (de Vaucouleurs 1957 ; Buscombe & Morris 1958 ; Edwards 1976 ), F2 (Cannon & Pickering 1918-1924 ), and F5V (Houk 1978 ). This last value appears to be more plausible, considering the calculated mass yielded by our orbit, the absolute magnitudes obtained from MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 20 orbits of binaries 4233 Table 3. Magnitudes, spectral types, parallaxes, and masses. The  Sat column contains Gaia or Hipparcos values of parallax es, giv en in miliarcseconds. The H superscript means that the parallax value comes from Hipparcos , no superscript indicates Gaia . M Sat AB shows the total mass (in units of M ) derived from these parallaxes with the same superscripts. WDS Name m A m B Sp AB Sp A Sp B  Sat M Sat AB  dyn M dyn A M dyn B Hipparcos σσσσσ 00277-1625 YR 1 Aa,Ab 7.51 8.72 F5/6V F4V G1V 14.22 2.49 14.33 1.36 1.07 ±0.15 ±0.16 ±0.31 ±0.03 ±0.02 00462-2214 RST 4155 9.76 10.03 G0V F9V G1V 9.21 2.26 9.53 1.04 0.99 ±0.33 ±0.30 ±0.30 ±0.03 ±0.02 03124-4425 JC 8 6.42 7.36 A8V + F3V A8V F3V 23.53 H 2.52 H 23.58 1.37 1.13 ±0.62 ±0.21 ±0.24 ±0.03 ±0.02 07303-5657 FIN 105 9.55 9.62 F6V F6V F6V 5.7 1.35 1.33 ±1.5 ±0.13 ±0.13 07427-3510 HDS 1091 10.04 10.59 G1V G0V G4V 4.86 4.22 6.0 1.20 1.08 37578 ±0.30 ±1.99 ±1.1 ±0.10 ±0.09 09110-1929 I 824 9.30 9.40 F0 F0V F0V 3.33 3.64 3.34 1.83 1.79 ±0.20 ±1.69 ±0.60 ±0.16 ±0.15 10093 + 2020 A2145 7.30 7.50 G8III + A2m G8III A2V 3.63 10.06 ––– 49747 ±0.56 ±4.69 ––– 10116 + 1321 HU 874 AB 6.90 7.87 F6V F4V G0V 15.48 H 1.34 H 11.75 1.68 1.38 49929 ±0.72 ±0.20 ±0.23 ±0.04 ±0.03 10217-0946 BU 25 8.41 8.96 G5 G3V G7V 16.25 2.14 ––– 50747 ±0.10 ±0.32 ––– 11585-2350 RST 3767 AB 10.85 11.08 K0 K0V K1V 9.06 1.88 9.37 0.86 0.83 ±0.67 ±0.53 ±0.66 ±0.03 ±0.03 12111-5302 HU 1604 10.19 10.54 G0 F9V G1V 7.86 1.94 7.75 1.05 0.98 59395 ±0.80 ±0.71 ±0.62 ±0.04 ±0.04 13117-2633 FIN 305 a 7.20 7.43 A5V A5V A6V 7.08 80.72 23.17 1.18 1.13 64375 ±0.72 ±25.04 ±0.56 ±0.04 ±0.04 13117-2633 FIN 305 b 7.20 7.43 A5V A5V A6V 7.08 17.87 12.89 1.52 1.44 64375 ±0.72 ±5.52 ±0.27 ±0.06 ±0.05 13305 + 0729 A 1789 9.14 9.39 A5 A5V A6V 4.83 H 3.01 H 4.79 1.58 1.50 65897 ±0.85 ±1.59 ±0.07 ±0.04 ±0.04 14592-4206 HDS 2116 Aa,Ab 3.34 4.71 B2V B2V B3V 7.46 16.63 8.14 8.38 4.41 73334 ±0.70 ±4.96 ±0.33 ±0.27 ±0.36 15157-2736 BU 350 7.06 8.58 F2 F0IV F6V 8.19 H 3.46 H 8.26 1.98 1.39 74675 ±0.88 ±1.48 ±0.71 ±0.11 ±0.01 15493 + 0503 A 1126 9.40 9.40 K0 K0III K0III 2.62 5.09 ––– 77489 ±0.06 0.72 ––– 16402-2800 VOU 44 AB 9.19 10.61 F0/2V A9V F8V 6.00 2.99 6.44 1.38 1.04 ±0.43 ±0.99 ±0.64 ±0.09 ±0.06 16458-0046 A1141 9.10 9.20 F8 F7V F8V 8.47 4.26 10.49 1.14 1.12 82062 ±0.48 ±0.90 ±0.14 ±0.03 ±0.02 18126 + 1224 HDS 2570 8.04 8.88 F0 F0III A6V 4.71 5.237 ––– 89235 ±0.16 ±1.481 ––– Note. a Short orbital solution for FIN 305. b Long orbital solution for FIN 305. the Hipparcos parallax (3.28 for the primary and 4.21 for the secondary), and even the colour index, using the values listed in Simbad for the combined B and V magnitudes of the system, B −V = 0.44. 2.4 WDS 07303-5657 (FIN 105) The first visual observation of this system occurred in mid-1929 (Finsen 1932 ). Between 1941 and 1983, a total of seven visual observations were reported from 136 ◦to 106 ◦. The Hipparcos reductions resolve the system but do not provide any value for the parallax nor do the measurements of the Gaia satellite. The last available observation used for the calculation of the orbit ( t = 2018.2355, θ= 70 ◦03, ρ= 0  2465) was performed at SOAR. This was the first high precision observation obtained for this system, as we can see in Fig. 4 . Due to the similar magnitudes of the components, the composite spectrum, F6V (Houk & Cowley 1975 ), can be separated into two MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 4234 J. Gomez et al. Table 4. RMS quality controls. New orbit Previous orbit RMS RMS WDS Name θ ρ θ ρ 00277-1625 YR 1 Aa,Ab 0.843 0.0128 18.719 0.0168 00462-2214 RST 4155 3.105 0.0145 8.519 0.0287 03124-4425 JC 8 1.930 0.0427 4.733 0.0421 07303-5657 FIN 105 5.363 0.0262 – – 07427-3510 HDS 1091 0.414 0.0023 0.433 0.0020 09110-1929 I 824 2.219 0.0369 – – 10093 + 2020 A2145 4.775 0.0156 8.873 0.0202 10116 + 1321 HU 874 AB 2.871 0.0211 8.240 0.0474 10217-0946 BU 25 0.986 0.0690 1.278 0.0664 11585-2350 RST 3767 AB 4.780 0.0478 6.254 0.0600 12111-5302 HU 1604 3.965 0.0397 – – 13117-2633 FIN 305 a 5.763 0.0168 6.339 0.0134 13117-2633 FIN 305 b 5.768 0.0270 6.339 0.0134 13305 + 0729 A 1789 5.991 0.0687 9.694 0.0593 14592-4206 HDS 2116 Aa,Ab 0.887 0.0445 – – 15157-2736 BU 350 2.437 0.0576 – – 15493 + 0503 A 1126 6.967 0.0167 – – 16402-2800 VOU 44 AB 1.054 0.0048 – – 16458-0046 A1141 5.439 0.0193 7.376 0.0218 18126 + 1224 HDS 2570 0.981 0.0025 – – Note. a Short orbital solution for FIN 305. b Long orbital solution for FIN 305. F6V stars. For our calculations, we determined that the combined m V = 8.87 (Høg et al. 2000 ) value corresponds to m V = 9.55 for the primary and m V = 9.62 to the secondary. The dynamical parallax obtained from the new orbit (5.7 ±1.5 mas) yields values of masses, M A = 1.35 ±0.13 M and M B = 1.33 ±0.13 M , that agree with those assigned to F6V spectral types in Gray ( 2005 ). The rms uncertainty in position angle and separation, rms( θ, ρ) = (5 ◦363, 0  0262), are relatively small considering the limited amount of measurements available for the determination of the orbital elements. The orbit should be considered to be preliminary until it is possible to obtain measurements when the separations between the components will be smaller in the near future. 2.5 WDS 07427-3510 (HDS 1091) In this report, we of fer an alternati ve orbit with a considerably greater period, P = 275 yr, as compared to that presented by Tokovinin et al. ( 2019 ), P = 120.6 yr, as we can see in Fig. 5 . The new orbital elements are quite different from the orbital elements of the previous solution but both yield rms uncertainties that are similar in θ, 0 ◦414 versus 0 ◦433, as well as in ρ, 0  0023 versus 0  0020. The dynamical parallaxes of both orbits are also similar, 5.89 mas for Tokovinin et al. ( 2019 ) versus 6.0 ±1.1 mas, and in agreement with the vales provided by Gaia (4.86 ±0.30 mas in the DR2 and 5.95 ±0.31 mas in the EDR3). Future observations will permit more accurate determinations of the orbital elements. 2.6 WDS 09110-1929 (I 824) The system I824 presents a variability of the delta Scuti type (Smalley et al. 2011 ), with a parallax that is estimated by Gaia to be 3.33 ±0.20. The first visual observations were obtained by R. T. A. Innes in the early 1900s (Aitken & Doolittle 1932 ). In total, there are ten micrometric observations including the last that was conducted by Heintz in 1985. The SOAR observation ( t = 2018.2358, θ= 170 ◦63, ρ= 0  0788) is the second speckle observation that was carried out approximately 30 yr after that by McAllister in 1989. The weight of these two measurements allows us determine the first orbit for this system with a period of 940 yr and a periastron passage estimated for the end of this decade (see Table 1 ). The dynamical parallax (3.34 ±0.60 mas) coincides with that given by Gaia DR2 (3.33 ±0.20 mas), and it is close tothe value of the EDR3 (3.48 ±0.29 mas). The obtained masses (M A = 1.83 ±0.16 M  and M B = 1.79 ±0.15 M ) are slightly superior to that expected for type F0V stars. The rms uncertainty in position angle and separation, 2 ◦219 and 0  0369, are relatively small but we cannot consider it to be very rele v ant because of the small arc co v ered by the available observations. The good fit between the orbit and both the micrometric and speckle observations can be appreciated in Fig. 6 . The imminent periastron passage should be taken advantage of in order to obtain new speckle registers that are fundamental for the tracking of this binary. 2.7 WDS 10093 + 2020 (A 2145) The first orbit for this system was calculated by Baize ( 1957 ) and later orbits were determined by Starikova ( 1977b ), Finsen ( 1977 ), Tokovinin ( 1987 ), Olevic & Cv etko vic ( 2004 ), and Mason & Hartkopf ( 2011 ). The first orbits gradually increased the value of the period from 60.0 yr (Baize 1957 ) to 71.1 yr Tokovinin ( 1987 ). Olevic & Cv etko vic ( 2004 ) calculated an orbit based on visual observations that was much slower with P = 119.25 ±3.62 yr. The solution of Mason & Hartkopf ( 2011 ) and that presented in MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 20 orbits of binaries 4235 Table 5. Gaia & Hipparcos versus dynamical parallaxes.  Sat represents Gaia or Hipparcos values of parallaxes. The H superscript means Hipparcos parallax. No superscript means Gaia parallax. Previous orbit Previous orbit New orbit WDS Name Author  Sat  dyn  dyn Hipparcos (yr) σ σ 00277-1625 YR 1 Aa,Ab Tokovinin 14.22 16.30 14.33 (2019) ±0.15 –±0.31 00462-2214 RST 4155 Heintz 9.21 12.18 9.53 (1984) ±0.33 –±0.30 03124-4425 JC 8 Soderhjelm 23.53 H 23.90 23.58 (1999) ±0.62 –±0.24 07303-5657 FIN 105 5.70 ±1.50 07427-3510 HDS 1091 Tokovinin et al. 4.86 5.89 6.00 37578 (2019) ±0.30 –±1.10 09110-1929 I 824 3.33 –3.34 ±0.20 –±0.60 10093 + 2020 A2145 Mason & Hartkopf 3.63 – – 49747 (2011) ±0.56 – – 10116 + 1321 HU 874 AB Mason & Hartkopf 15.48 H 14.64 11.75 15.48 49929 (2011) ±0.72 ±1.01 ±0.23 10217-0946 BU 25 Tokovinin & Latham 16.25 – – 50747 (2020) ±0.10 – – 11585-2350 RST 3767 AB Josties & Mason 9.06 63.71 9.37 (2019) ±0.67 –±0.66 12111-5302 HU 1604 7.86 –7.75 59395 ±0.80 –±0.62 13117-2633 FIN 305 a Tokovinin 7.08 9.72 23.17 64375 (2018) ±0.72 ±0.45 ±0.56 13117-2633 FIN 305 b Tokovinin 7.08 9.72 12.89 64375 (2018) ±0.72 ±0.45 ±0.27 13305 + 0729 A 1789 Heintz 4.83 H 4.36 4.79 65897 (1998) ±0.85 –±0.07 14592-4206 HDS 2116 Aa,Ab 7.46 –8.14 73334 ±0.70 –±0.33 15157-2736 BU 350 8.19 H –8.26 74675 ±0.88 –±0.71 15493 + 0503 A 1126 2.62 – – 77489 ±0.06 – – 16402-2800 VOU 44 AB 6.00 –6.44 ±0.43 –±0.64 16458-0046 A1141 Heintz 8.47 8.51 10.49 82062 (1982) ±0.48 –±0.14 18126 + 1224 HDS 2570 4.71 – – 89235 ±0.16 – – Note. a Short and long orbital solution for FIN 305. b Long orbital solution for FIN 305. this report are based on the most recent high precision observations obtained using speckle interferometry, because of the programs of Calern, SAO, WIYN, and SOAR, and suggest an orbital period that is closer to that given by Tokovinin ( 1987 ). The five new observations at SOAR during the past decade allow the refinement of the orbit of Mason & Hartkopf ( 2011 ). Using the new calculation, the period changes from 80.59 to 74.71 yr As a giant component exists within the system (G8III + A2V), the calculation of the dynamical parallax is not reliable and it has not been included in Tables 3 and 5 . The new orbit impro v es the rms yielding a decrease in rms θfrom 8 ◦873 to 4 ◦775 and, in rms ρ, from 0  0202 to 0  0156. The previous and the new orbits are shown in Fig. 7 . 2.8 WDS 10116 + 1321 (HU 874 AB) The system HU 874 AB (34 Leo) has a parallax of 15.48 ±0.72 mas as given by Hipparcos . The first visual observation took place in 1905 (W. J. Hussey) and the first speckle observation in 1980 (H. MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 4236 J. Gomez et al. Figure 1. For all the Figures and following the Sixth Catalogue of Orbits of Visual Binary Stars (ORB6) standards, the micrometric observations are plotted as the green crosses ( + ), Hipparcos as a red H (H), the interferometric observations are identified by the blue circles, which are filled ( •) in the case of speckle interferometry and other high angular resolution techniques, and open ( ◦) for eyepiece interferometry measurements, and the latest ones obtained by SOAR are designated with the magenta crosses ( + ). All of these symbols are united by their respective colour line to the new orbit, joining the real observation with its expected position according to the time of observation. The previous apparent orbit is represented by a black-dashed line and our new apparent orbit by a solid line. The line of nodes is traced by a solid straight line upon which the position of the primary star can be seen as a large cross. In the right corner, we indicate the orientation of the axes, and the direction of orbital motion. The new orbit of YR 1 Aa,Ab (the shorter period orbit) is compared to the previous one. Figure 2. RST 4155 orbit fits better the speckle observations. Figure 3. JC 8 previous and new apparent orbits. A. McAllister). Of the total of 73 measurements, the last four were obtained using the HRCam@SOAR. The first orbit for this system was calculated by Baize ( 1984 ) and was impro v ed because of speckle observations by Hartkopf, Mason & McAlister ( 1996 ). Measurements obtained since then allow us to determine a new orbit Figure 4. FIN 105 first orbit. Figure 5. The apparent orbit of HDS 1091 orbit compared with the previous one. Figure 6. I 824 first orbit. with a period of 17.962 yr and a periastron passage estimated for 2022.828. The dynamical parallax, 11.75 ±0.23 mas, is lower than that provided by Hipparcos (15.48 ±0.42 mas). We should consider that the total mass of the system calculated with the Hipparcos parallax, M T = 1.338 M , seems to be too MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 20 orbits of binaries 4237 Figure 7. A 2145 previous and new apparent orbits. Figure 8. New HU 874 orbit compared with previous one. small for this system. Meanwhile, the total mass obtained with the new dynamical parallax, M T = 3.063 M , breaks down to M A = 1.682 ±0.042 M and M B = 1.381 ±0.032 M , both superior to those expected for the type F4V + G0V stars. These spectral types result from applying the previously mentioned spectral decomposition method to the spectral type of the system (F6V) and the difference of magnitude provided by SOAR ( ∼1.5). The rms uncertainty in position angle and separation (2 ◦871 and 0  0211, respectively) are smaller than those obtained from the previous orbit calculated by Hartkopf et al. ( 1996 ) that shows rms θ = 8 ◦240 and rms ρ= 0  0474 (see Fig. 8 ). The eccentricity of the new orbit (0.93) and also the fact that the periastron passage takes place next year are notable features. For that reason, this binary should be a preferred object of observation. 2.9 WDS 10217-0946 (BU 25) The binary BU 25 has a very long period orbit with an Hipparcos parallax of 16.68 ±1.18 mas and a Gaia parallax of 16.25 ±0.10 mas for the DR2, and 15.01 ±0.08 for the EDR3. The first visual observation was carried out by G. M. Searle in 1867 and the first speckle observation was obtained with the Washington Speckle Interferometer in 1991 (Douglass, Hindsley & Worley 1997 ). In total, we have 93 available observations of which the last four were conducted using the HRCam@SOAR (see Fig. 9 ). Figure 9. BU 25 previous and new apparent orbits. Due to its slow orbital mo v ement, the first orbit was not calculated until the last decade (Zirm & Rica 2012 ). In 2019, Izmailov (Izmailov 2019 ) obtained another solution, and recently, after the calculation of our orbit, an article considering the system as a triple star has been published (Tokovinin & Latham 2020 ). In this last contribution, the authors present the A component as a SB1, with a orbital period of 8.39 yr and a mass ratio, q = 0.25. Moreo v er, the postulated masses of the components are: Aa = 1.07 M , Ab = 0.27 M , and B = 0.96 M , which imply, as noted by Tokovinin and Latham, a small but detectable wobble motion in the system. The existence of this spectroscopic subcomponent prevents us from calculating the dynamical parallax of the system, because the ANAPAR algorithm is not calibrated for triple stars. The corresponding spectral types will be, probably, G3 and M4-5 for the components of the inner binary, and G7 for the B component. Nevertheless, the outer orbit is not currently well defined and the three orbits of Zirm & Rica (circular), Tokovinin & Latham (with small inclination and moderate eccentricity), and that presented herein (with the longest period) remain among the possibilities; they not only yield similar rms uncertainties in theta and rho, but also, when using the Gaia parallax, similar inferred total masses. 2.10 WDS 11585-2350 (RST 3767 AB) The new orbit presented here has a long period, i.e. P = 740 yr, and supersedes the orbit ( P = 122.03 yr) proposed by Josties & Mason ( 2019 ). In addition to improving the rms uncertainty in θand in ρ, we point out that the dynamical parallax of the new orbit, 9.37 ±0.66 mas, permits the calculation of a total mass of 1.692 M , with M A = 0.864 ±0.031 M and M B = 0.828 ±0.030 M , which approximates that expected for a system that we have resolved as K0V + K1V. The previous orbit does not yield a total mass that is compatible with the component spectral types. Although this system does not have a trigonometric parallax assigned in SIMBAD, the Gaia EDR3 lists two objects located at less than 1 arcsec of the coordinates of the system provided by Simbad, with parallaxes of 9.06 ±0.67 and 8.72 ±0.71 mas, which are within 1 σof the calculated dynamical parallax. Their proper motions and the G magnitude also appear to be consistent with the values expected for this binary therefore they are likely to be the components of this system. As can be seen in Fig. 10 , the new orbit fits better with the new high precision speckle measurements obtained by SOAR: ( t , θ, ρ) MNRAS 509, 4229–4245 (2022) Downloaded from https://academic.oup.com/mnras/article/509/3/4229/6371110 by Irene Ruiz user on 01 July 2022 4244 J. Gomez et al. Figure 33. BU 350 HR diagram. Figure 34. VOU 44 HR diagram. Figure 35. A 1141 HR diagram. measurements collected between 2018 and 2020, we were able to calculate for the first time the orbits of 8 systems and to impro v e the orbits of 11 more. In one case, FIN 305, we presented two solutions that fit with the observational data available. We also calculated precise dynamical parallaxes for 15 of the systems using the new methodology ANAPAR. Those dynamical parallaxes allowed us to determine the masses and the absolute luminosities for the components of those 15 systems. We used this information together with public data regarding metallicities and ef fecti ve temperatures to plot their position in the HR diagram against the most suitable isochrones produced by MIST. All of those plots show similar ages for the components and are coherent with a coevolution and common origin context. In the case of HDS 2116 Aa,Ab, the plot shows discrepancies between the luminosities calculated and the ef fecti ve temperatures expected according to the spectra assigned to each component. Those discrepancies suggest that the dynamical parallaxes must be improved. The large list of speckle measurements performed by A. Tokovinin, and the quality of them, using the HRCam attached to the 4.1 m. SOAR telescope, confirms the suitability of this instrumentation + telescope in order to continue in the future with this class of observations in benefit of the knowledge of austral close binaries. ACKNOWLEDGEMENTS The authors thank Andrei Tokovinin for his collaboration with speckle runs carried out at SOAR in 2018, 2019, and 2020. We must also express our deep gratitude to the operator and engineer teams of SOAR that were involved with the observation campaigns. We are very grateful for the continuous support of the Chilean Telescope Allocation Committee: http:// www.das.uchile.cl/ das cnt ac.html under programs CN2018A-1, CN2019A-2, CN2019B-13, and CN2020A-19 and 2020B-10. This paper was supported by the ‘Xunta de Galicia’ (Spain), under the ED431B 2020/38 grant. RAM and EC acknowledge support from ANID/FONDECYT grant 1190038. This work used the SIMBAD service operated by the Centre des Donn ´ ees Stellaires (Strasbourg, France, Wenger et al. 2000 ); bibliographic references from the Astrophysics Data System maintained by SAO/NASA; the Site Informatique des ´ etoiles Doubles de Nice (SIDONIe, Le Contel, Valtier & Bonneau 2001 ) compiled principally by Dr. Paul Couteau; the historical data base of micrometric measurements provided by the WDS (Mason et al. 2001 ) the Catalogue of Interferometric Measurements of Binary Stars (WDS INT4, Hartkopf et al. 2001b ) and the Sixth Catalogue of Orbits of Visual Binary Stars (WDS ORB6, Hartkopf, Mason & Worley 2001a ), all of them maintained at USNO. This work has used data from the European Space Agency (ESA) mission Gaia ( ht tps://www.cosmos.esa.int /gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https: // www.cosmos.esa.int/web/gaia/ dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Minist ´ erio da Ci ˆ encia, Tecnologia, e Inova c ¸˜ ao (MCTI) da Rep ´ ublica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). DATA AVAILABILITY The new measurements used for the calculation will be published in an upcoming article and can be accessed through the Arxiv repository (Tokovinin et al. 2021 ). The rest of the measurements and the stellar data were obtained from the catalogs and data bases mentioned in the acknowledgements. 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