III/278 Double stars with wide separations in the AGK3 (Halbwachs+, 2016) ================================================================================ Double stars with wide separations in the AGK3. I. The components which are themselves spectroscopic binaries. II. The wide binaries and the multiple systems. Halbwachs J.L., Mayor M., Udry S. =2012MNRAS.422...14H +2017MNRAS.464.4966H =2016yCat.3278....0H ================================================================================ ADC_Keywords: Stars, double and multiple ; Binaries, spectroscopic ; Radial velocities Keywords: binaries: spectroscopic - brown dwarfs - stars: low-mass - binaries: general - stars: formation - stars: solar-type Description: A large list of common proper motion stars selected from the third Astronomischen Gesellschaft Katalog (AGK3) was monitored with the CORAVEL (for COrrelation RAdial VELocities) spectrovelocimeter, in order to prepare a sample of physical binaries with very wide separations. In paper I,66 stars received special attention, since their radial velocities (RV) seemed to be variable. These stars were monitored over several years in order to derive the elements of their spectroscopic orbits. In addition, 10 of them received accurate RV measurements from the SOPHIE spectrograph of the T193 telescope at the Observatory of Haute-Provence. For deriving the orbital elements of double-lined spectroscopic binaries (SB2s), a new method was applied, which assumed that the RV of blended measurements are linear combinations of the RV of the components. 13 SB2 orbits were thus calculated. The orbital elements were eventually obtained for 52 spectroscopic binaries (SBs), two of them making a triple system. 40 SBs received their first orbit and the orbital elements were improved for 10 others. In addition, 11 SBs were discovered with very long periods for which the orbital parameters were not found. It appeared that HD 153252 has a close companion, which is a candidate brown dwarf with a minimum mass of 50 Jupiter masses. In paper II, 80 wide binaries (WBs) were detected, and 39 optical pairs were identified. Adding CPM stars with separations close enough to be almost certain they are physical, a "bias-controlled" sample of 116 wide binaries was obtained, and used to derive the distribution of separations from 100 to 30,000 au. The distribution obtained doesn't match the log-constant distribution, but is in agreement with the log-normal distribution. The spectroscopic binaries detected among the WB components were used to derive statistical informations about the multiple systems. The close binaries in WBs seem to be similar to those detected in other field stars. As for the WBs, they seem to obey the log-normal distribution of periods. The number of quadruple systems is in agreement with the "no correlation" hypothesis; this indicates that an environment conducive to the formation of WBs doesn't favor the formation of subsystems with periods shorter than 10 years. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1v1.dat 91 66 Summary of CPM stars observed (Paper I) table1v2.dat 91 200 Summary of CPM stars observed (Paper II) table2v1.dat 48 2275 *Radial Velocities observed (Paper I) table2v2.dat 48 1473 *Radial Velocities observed (Paper II) taborbit.dat 272 52 Orbital elements of SBs (Paper I) noteorb.dat 80 127 Individual notes to the table of orbital elements of SBs (Paper I) tabwb.dat 93 149 The wide binaries (Paper II, table 3, followed by table 6) orbit/* . 100 Figures (eps) of velocity of SBs with phase (Paper I) drift/* . 34 Figures (eps) of velocity drifts (Paper I) -------------------------------------------------------------------------------- Note on table2v1.dat, table2v2.dat: in Vizier, the individual measurements in table 2 may be accessed from the column "Nmes" in table 1. -------------------------------------------------------------------------------- See also: I/121 : Common proper motions stars in AGK3 (Halbwachs, 1986) I/2 : AGK2/3 (Lacroute, Valbousquet, 1974) I/130 : LDS Catalogue: Doubles with Common Proper Motion (Luyten 1940-87) B/sb9 : 9th Catalogue of Spectroscopic Binary Orbits (Pourbaix+ 20141) I/61 : AGK3 Catalogue (Dieckvoss, Heckmann 1975) J/A+A/521/A4 : CPMDS catalogue (Gavras+, 2010) J/MNRAS/355/585 : New Northern common proper-motion pairs (Greaves, 2004) J/other/JDSO/6.30 : New Wide Common Proper Motion Binaries (Benavides+, 2010) Byte-by-byte Description of file: table1v[12].dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 I1 --- tno [1/2] Table of CPM catalog (3) 3- 5 I3 --- CPM Designation of CPM pair (3) 6 A1 --- m_CPM [AB] Component designation (3) 8- 15 A8 --- AG AGK3 designation of component 17- 27 A11 --- OName Other name (HIP/HD/BD/AG) 29- 33 F5.2 mag B-V B-V color index assumed to derive the radial velocities 35- 37 I3 --- Nmes Number of measurements (linked to table2 in VizieR) 40- 46 F7.3 km/s Mean heliocentric radial velocity of the star 49- 53 F5.3 km/s e_ Uncertainty in 55- 59 F5.3 --- Pchi2 [0/0.999]?=- P({chi}^2^) of constant velocity (1) 61- 64 A4 --- Var Final variability status of the star (2) 65 A1 --- n_Var [+] HRV measurements from other sources (4) 67- 68 I2 h RAh ? Right ascension (J2000) of component 70- 71 I2 min RAm ? Right ascension (J2000) of component 73- 78 F6.3 s RAs ? Right ascension (J2000) of component 80 A1 --- DE- ? Declination sign (J2000) of component 81- 82 I2 deg DEd ? Declination (J2000) of component 84- 85 I2 arcmin DEm ? Declination (J2000) of component 87- 91 F5.2 arcsec DEs ? Declination (J2000) of component -------------------------------------------------------------------------------- Note (1): P({chi}^2^) is the probability of obtaining a {chi}^2^ larger than the one actually obtained, assuming the RV is constant in reality (computed from primary component). Note (2): the following statuses are used: CST? = star that could have a constant RV VAR = radial velocity seems to be variable SB1 = at least part of the velocity curve of the primary is visible SB2 = at least part of the velocity curves of both components is visible SB1O = orbital elements of SB1 were derived SB2O = orbital elements of SB2 were derived CST = radial velocity seems to be constant Note (3): the designation of a CPM star follows Halbwachs (1986, Cat. I/121): a table number (1 = physical binaries with a probability>=98.7%, 2 = physical binaries with a probability>=60%) and a sequential number in this table. Note (4): A "+" follows the variability status for SB1O or SB2O when RV measurements from an external source were taken into account to derive the orbital elements. These additional measurements were found in the SB9 online catalogue (Cat. B/sb9) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2v[12].dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 I1 --- tno [1/2] Table of CPM catalog (Cat. I/121) 3- 5 I3 --- CPM Designation of CPM pair (Cat. I/121) 6 A1 --- m_CPM [AB] Component designation 8- 15 A8 --- AG AGK3 designation of component 18- 27 F10.4 d JD-2400000 Observation epoch (BJD-2400000) 29- 36 F8.3 km/s RV Radial velocity measured 38- 42 F5.3 km/s e_RV Uncertainty of RV 44 I1 --- c [0/2]? Component measured: blank for SB1; 1=primary, 2=secondary, 0=blend for SB2 46 A1 --- f [RF] flag on RV: R=Rejected, F=Fixed velocity 48 A1 --- T [CEST] Telescope used (1) -------------------------------------------------------------------------------- Note (1): Telescope coded as follows; C = 1m/CORAVEL at Haute-Provence Observatory; E = Euler/CORALIE telescope at La Silla, Chile S = 193cm/SOPHIE telescope at Haute-Provence Observatory T = 1m telescope of the Simeis Observatory in Crimea -------------------------------------------------------------------------------- Byte-by-byte Description of file: taborbit.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 I1 --- tno [1/2] Table of CPM catalog (Cat. I/121) 3- 5 I3 --- CPM Designation of CPM pair (Cat. of component "A" I/121) 6 A1 --- m_CPM [AB] Component designation 8- 15 A8 --- AG AGK3 designation of component 17- 29 A13 --- OName Other name (HD/BD/HIP) 31- 43 F13.7 d P Orbital period 45- 55 F11.7 d e_P ? Uncertainty of P 57- 67 F11.5 d T0 Periastron epoch (BJD-2400000) 69- 77 F9.5 d e_T0 Uncertainty of T0 79- 84 F6.4 --- Ecc Eccentricity 86- 91 F6.4 --- e_Ecc ? Uncertainty of Ecc 93- 98 F6.2 deg w ? Periastron longitude 100-104 F5.2 deg e_w ? Uncertainty of w 106-112 F7.3 km/s K1 Semi-amplitude of RV of the primary component 114-119 F6.3 km/s e_K1 Uncertainty of K1 121-127 F7.3 km/s K2 ? Semi-amplitude of the secondary component 129-134 F6.3 km/s e_K2 ? Uncertainty of K2 136-143 F8.3 km/s V0 ? RV of the barycentre 145-149 F5.3 km/s e_V0 ? Uncertainty of V0 151-155 F5.3 km/s O-C ? Standard deviation of the residuals 157-159 I3 --- N1 Number of new measurements of the primary RV 161-163 I3 --- n1 ? Number of RV measurements of the primary from other sources 165-167 I3 --- N2 ? Number of new measurements of the secondary RV 169-170 I2 --- n2 ? Number of RV measurements of the secondary from other sources 172-174 I3 --- N0 ? Number of RV measurements of the blend 176-180 F5.3 --- C0 ? Relative contribution of the primary to the velocity of the blend 182-186 F5.3 --- e_C0 ? Uncertainty of C0 188-196 F9.4 Gm a1sini Semi-major axis of the primary orbit *sini 198-205 F8.4 Gm e_a1sini Uncertainty of a1sini 207-215 F9.4 Gm a2sini ? Semi-major axis of the secondary orbit *sini 217-224 F8.4 Gm e_a2sini ? Uncertainty of a2sini 226-233 F8.6 Msun fM ? Mass function of SB1 systems 235-242 F8.6 Msun e_fM ? Uncertainty of fM 244-249 F6.4 Msun M1sin3i ? Primary mass * sin^3 i 251-256 F6.4 Msun e_M1sin3i ? Uncertainty of M1sin3i 258-263 F6.4 Msun M2sin3i ? Secondary mass * sin^3 i 265-270 F6.4 Msun e_M2sin3i ? Uncertainty of M2sin3i 272 A1 --- R [r] r when more information about the orbit in the noteorb.dat file -------------------------------------------------------------------------------- Byte-by-byte Description of file: noteorb.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 I1 --- tno [1/2] Table of CPM catalog 2 A1 --- --- [:] 3- 5 I3 --- CPM Designation of CPM pair 6 A1 --- m_CPM [AB] Component designation 8- 80 A73 --- Note Text of the note -------------------------------------------------------------------------------- Byte-by-byte Description of file: tabwb.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 I1 --- tno [1/2] Table of CPM catalog (Cat. I/121) 3- 5 I3 --- CPM Designation of CPM pair (Cat. I/121) 7- 14 A8 --- AGA AGK3 designation of component "A" 16- 20 F5.2 mag VA Visual magnitude of component "A" 22- 26 F5.2 mag B-VA B-V colour index of component "A" 28- 36 A9 --- TSPA Spectral type of component "A" 38- 45 A8 --- AGB AGK3 designation of component "B" 47- 51 F5.2 mag VB Visual magnitude of component "B" 53- 57 F5.2 mag B-VB B-V colour index of component "B" 59- 66 A8 --- TSPB Spectral type of component "B" 68- 73 F6.2 mas varpi ? Trigonometric parallax of the system 75- 79 F5.2 mas e_varpi ? Uncertainty of varpi 81- 85 I5 pc D Distance in parsec 87- 91 I5 AU s projected separation 93 I1 --- f [0/4]? Flag (1) -------------------------------------------------------------------------------- Note (1): the flag is coded as follows; a flag larger than 0 leads to the rejection of the wide binary from the bias-controlled sample of main-sequence WBs. Therefore, the flag indicates only the first reason justifying the rejection as follows: 0 = System of the supplementary sample (Table 6 of Paper 2, at the end of the file). These systems are classified as physical binaries, but they were not observed with CORAVEL. 1 = System belonging to an open cluster 2 = Primary component earlier than F5 or far from main sequence 3 = Components both fainter than mpg=9.1 mag in cat I/2 4 = The system contains the faintest component of a triple system -------------------------------------------------------------------------------- Acknowledgements: Jean-Louis Halbwachs, jean-louis.halbwachs(at)astro.unistra.fr ================================================================================ (End) Jean-Louis Halbwachs, Patricia Vannier [CDS] 13-Oct-2016