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.
<Mon. Not. R. Astron. Soc. 422, 14-24 (2012); 464, 4966-4976 (2017)>
=2012MNRAS.422...14H 2012MNRAS.422...14H
+2017MNRAS.464.4966H 2017MNRAS.464.4966H
=2016yCat.3278....0H 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:
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FileName Lrecl Records Explanations
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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)
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Note on table2v1.dat, table2v2.dat: in Vizier, the individual measurements in
table 2 may be accessed from the column "Nmes" in table 1.
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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
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Bytes Format Units Label Explanations
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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(χ2) 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
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Note (1): P(χ2) is the probability of obtaining a χ2 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)
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Byte-by-byte Description of file: table2v[12].dat
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Bytes Format Units Label Explanations
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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)
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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
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Byte-by-byte Description of file: taborbit.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: noteorb.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tabwb.dat
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Bytes Format Units Label Explanations
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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)
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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
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Acknowledgements:
Jean-Louis Halbwachs, jean-louis.halbwachs(at)astro.unistra.fr
(End) Jean-Louis Halbwachs, Patricia Vannier [CDS] 13-Oct-2016