J/MNRAS/549/G838 Known mult. stellar systems within 10pc (Gonzalez-Payo+, 2026) ================================================================================ Characterisation of all known multiple stellar systems within 10 pc. Gonzalez-Payo J., Caballero J.A., Cifuentes C., Cortes-Contreras M., Rica F. =2026MNRAS.549ag838G (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Stars, double and multiple ; Stars, nearby ; Optical Keywords: catalogues - astrometry - binaries: spectroscopic - binaries: visual - solar neighbourhood Abstract: The study of stellar multiplicity offers important constraints on the structure of the Galaxy as well as stellar and planet formation and evolution. Focusing on the most immediate solar neighbourhood benefits from obtaining both complete and accurate data for reliable statistics. Our goal is to describe the solar neighbourhood within 10pc in terms of multiplicity by evaluating the angular and physical separations, masses, and orbital periods of the systems from the most complete volume-limited sample. We carried out a comprehensive data compilation from the Washington Double Star catalogue and the literature of all known multiple systems at any separation range, and completed this information with a common proper motion and parallax search with Gaia DR3 data. We also used public astrometric and radial-velocity data to compute orbital solutions of seven pairs. From a sample of 424 stars and brown dwarfs within 10pc we identified 215 of them in 92 systems in double (68), triple (19), quadruple (3), and quintuple (2) configurations. All except eight pairs have been resolved. Their orbital periods range over ten orders of magnitude from about one day to millions of years. We measured precise mass and companion star fractions at different mass intervals. The multiplicity fraction smoothly decreases from 41^+11^_-10_ per cent for stars with M>=0.50M_{sun}_ to 9.3^+7.4^_-4.3_ per cent for stars and brown dwarfs with M<=0.10M_{sun}_ Description: In this study, we analysed the multiplicity of all stars and brown dwarfs at a maximum heliocentric distance of 10pc, originally compiled by C. Reyle et al. (2022, in Brun A.S., Bouvier J., Petit P., eds, The 21st Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (CS21). Toulouse, France, p. 218 10.5281/zenodo.7669746). Table C1 displays the default name in the Simbad data base, Gliese-Jahreiss identifier when available, J2000 equatorial coordinates, and proper motions of 424 stars and brown dwarfs at less than 10pc. Tables C2 and C3 summarise our analysis and data compilation. In particular, Table C2 lists the individual components in all multiple systems at 10pc (e.g. two entries for a double system -A, B-, three entries for a triple system -A, B, C-, etc.), while Table C3 lists the pairs (e.g. one entry for a double system -AB-, two entries for a triple system -A-B and A-C-, etc.). The first column, the WDS identifier, is common to both tables. Of the 92 multiple systems at 10pc, only five do not have a WDS identifier, namely Wolf 227, QY Aur, L 768-119, G 203-47, and 2M1750-00 (2MASS J17502484-0016151). We write their names in parentheses in Tables C2 and C3. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablec1.dat 89 424 Stars and brown dwarfs at d < 10pc tablec2.dat 203 215 Individual components in all multiple systems at d < 10 pc tablec3.dat 292 123 Pairs in all multiple systems at d < 10pc fig/* . 92 Diagram sketch of the systems -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablec1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 29 A29 --- Name Name of the star as registered in Simbad 31- 38 A8 --- GJ Gliese-Jahreiss identifier when available (G1) 40- 41 I2 h RAh Right ascension (J2000) 43- 44 I2 min RAm Right ascension (J2000) 46- 50 F5.2 s RAs Right ascension (J2000) 52 A1 --- DE- Declination sign (J2000) 53- 54 I2 deg DEd Declination (J2000) 56- 57 I2 arcmin DEm Declination (J2000) 59- 62 F4.1 arcsec DEs Declination (J2000) 65- 73 F9.3 mas/yr pmRA Proper motion in right ascension direction 75- 83 F9.3 mas/yr pmDE Proper motion in declination direction 85- 89 F5.2 pc d Heliocentric distance -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablec2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 A11 --- WDS Washington Double Star Id (1) 13- 40 A28 --- Name Name of the star as registered in Simbad 42- 65 A24 --- AName Only for stars with bright, variable, historical, or widely accepted denominations 67- 72 A6 --- GJ Gliese-Jahreiss identifier when available (G1) 74- 77 A4 --- Comp Component letter used by WDS or MCS (2) 79- 80 I2 h RAh ? Right ascension (J2000) 82- 83 I2 min RAm ? Right ascension (J2000) 85- 89 F5.2 s RAs ? Right ascension (J2000) 91 A1 --- DE- Declination sign (J2000) 92- 93 I2 deg DEd ? Declination (J2000) 95- 96 I2 arcmin DEm ? Declination (J2000) 98-102 F5.2 arcsec DEs ? Declination (J2000) 104-108 F5.2 pc d ? Heliocentric distance 111-116 A6 --- SpType Spectral type (Colons indicate estimated spectral type) 118 A1 --- l_Gmag Limit flag on Gmag 119-124 F6.3 mag Gmag ? Gaia G magnitude 125 A1 --- n_Gmag [:] Colons stand for G-band magnitudes estimated from previously-published magnitude differences in other optical and near-infrared bands 126 A1 --- l_Mass Limit flag on Mass 127-132 F6.4 Msun Mass Mass 134-139 F6.4 Msun e_Mass Standard error of the mass 141-159 A19 --- r_Mass Bibliographic reference of the mass 161-175 A15 --- Planets Reported planets candidates (3) 177 A1 --- l_rbem Limit flag on rbem (|U*_g_|) 178-186 F9.1 10+33J rbem ? Reduced binding energy modulus (|U*_g_| in 10^33^J, usually measured between the widest component and the rest of the components in the system 188-203 A16 --- System Diagram sketch of the system image name (4) -------------------------------------------------------------------------------- Note (1): In parentheses is shown the primary star when the system has not a WDS Id Note (2): In square brackets, component not identified by any of these catalogues. Note (3): The letters that designate the planets are placed in square brackets when their existence has not yet been confirmed. Note (4): Colours in system diagrams indicate spectral types (dark blue: A, light blue: B, yellow: G, orange: K, red: M, black: L, T, and Y, white: WD). Concentric circles indicate unresolved binaries. Stripped circles indicate exoplanet host stars. Symbol sizes are approximate proportional to stellar masses, but are not to scale to the physical separations. When separation is about 1 arcsec or less, the black connection line is not drawn. -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablec3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 A11 --- WDS Washington Double Star Id. When the WDS identifier is missing, the common system name is shown in parentheses 13- 19 A7 --- Disc WDS discoverer cod 21- 24 A4 --- PrimComp Letter of 'primary' component used by WDS or MCS (in square brackets, component not identified by any of these catalogues) 26- 29 A4 --- SecComp Letter of 'secondary' component used by WDS or MCS (in square brackets, component not identified by any of these catalogues) 31- 37 A7 --- Det Detection method of the system (1) 39- 43 F5.1 deg theta ? Position angle (measured from North to East, empty when rho < 1 arcsec) 45- 55 F11.5 arcsec rho ? Angular separation from primary to companion 57- 63 F7.5 arcsec e_rho ? Standard error of the angular separation 65- 74 F10.3 au Sep ? Projected physical separation 76- 94 A19 --- r_theta Bibliographic reference for theta and rho 96-115 F20.15 arcsec alpha ? Angular semi-major axis of the orbit 116-126 F11.6 arcsec e_alpha ? Lower error of the angular semi-major axis of the orbit 128-137 F10.6 arcsec E_alpha ? Upper error of the spatial semi-major axis of the orbit 139-148 F10.5 au a ? Spatial semi-major axis of the orbit 149-158 F10.5 au e_a ? Lower error of the spatial semi-major axis of the orbit 161-169 F9.5 au E_a ? Upper error of the spatial semi-major axis of the orbit 171-175 A5 --- Ori Original measurement (2) 177-190 F14.9 --- Per Orbital period 192-205 F14.8 --- e_Per Lower error of the orbital period 207-219 F13.8 --- E_Per Upper error of the orbital period 221-222 A2 --- x_Per Orbital period units (d: days, a: years, ka: thousand years, Ma: million years) 224 A1 --- n_Grade < when improved with respect to ORB6 225-227 F3.1 --- Grade ? Orbital grade from the Sixth Catalog of Orbits of Visual Binary Stars (ORB6) of the WDS which estimates the quality of period measurement (blank when not provided) 229-292 A64 --- r_alpha Bibliographic reference for alpha, a, or P -------------------------------------------------------------------------------- Note (1): Detection method of the system as follows: Gaia = Gaia DR3 DI = Direct seeing-limited imaging "not in Gaia DR3" HRI = High-resolution imaging "Hubble, adaptive optics, speckle, interferometry, etc." SB1 = Single-lined spectroscopic binarity SB2 = Double-lined spectroscopic binarity Note (2): Original measurement as follows: a = means that the value of alpha has been derived from a alpha = means that the value of a has been derived from alpha both = means that a and alpha are original none = means that none of the data are original -------------------------------------------------------------------------------- Global notes: Note (G1): For homogeneity and readability, we write 'GJ' (1979A&AS...38..423G, 1991adc..rept.....G) even for stars in the catalogue of nearby stars of 1969VeARI..22....1G, which originally had a 'Gl' identifier. We refrain from tabulating stars with 'GJ' identifier >= 9000, as they were not part of any Gliese or Gliese-Jahreiss catalogues. -------------------------------------------------------------------------------- Acknowledgements: Javier Gonzalez-Payo, fcojgonz(at)ucm.es License: CC-BY-4.0 History: 21-May-2026 : on-line version 03-Aug-2026 : Position of L 143-23 corrected ================================================================================ (End) Patricia Vannier [CDS] 04-May-2026