J/AJ/137/3646 Radial velocities of 10 close binaries (Pribulla+, 2009)
Radial velocity studies of close binary stars. XIV.
Pribulla T., Rucinski S.M., Debond H., De Ridder A., Karmo T.,
Thomson J.R., Croll B., Ogloza W., Pilecki B., Siwak M.
<Astron. J., 137, 3646-3654 (2009)>
=2009AJ....137.3646P 2009AJ....137.3646P
ADC_Keywords: Binaries, eclipsing ; Radial velocities
Keywords: binaries: close - binaries: eclipsing - binaries: spectroscopic -
stars: individual (TZ Boo, VW Boo, EL Boo, VZ CVn, GK Cep, RW Com,
V2610 Oph, V1387 Ori, AU Ser, FT UMa)
Abstract:
Radial velocity (RV) measurements and sine curve fits to the orbital
RV variations are presented for 10 close binary systems: TZ Boo, VW
Boo, EL Boo, VZ CVn, GK Cep, RW Com, V2610 Oph, V1387 Ori, AU Ser, and
FT UMa. Our spectroscopy revealed two quadruple systems, TZ Boo and
V2610 Oph, while three stars showing small photometric amplitudes, EL
Boo, V1387 Ori, and FT UMa, were found to be triple systems. GK Cep is
a close binary with a faint third component. While most of the studied
eclipsing systems are contact binaries, VZ CVn and GK Cep are detached
or semidetached double-lined binaries, and EL Boo, V1387 Ori, and FT
UMa are close binaries of uncertain binary type. The large fraction of
triple and quadruple systems found in this sample supports the
hypothesis of formation of close binaries in multiple stellar systems;
it also demonstrates that low photometric amplitude binaries are a
fertile ground for further discoveries of multiple systems.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 160 10 Spectroscopic orbital elements
table1.dat 55 672 DDO radial velocity observations
table2.dat 38 461 Radial velocity observations of third and
fourth components of multiple systems
(EL Boo, FT UMa, TZ Boo, V1387 Ori, V2610 Oph)
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Description:
J/AJ/130/767 : Radial velocities of 10 close binaries (Rucinski+, 2005)
J/AJ/132/769 : Radial velocities of 10 close binaries (Pribulla+, 2006)
J/AJ/133/1977 : Radial velocities of 10 close binaries (Pribulla+, 2007)
J/AJ/136/586 : Radial velocities of 10 close binaries (Rucinski+, 2008)
J/AJ/137/3655 : Radial velocities of 8 close binaries (Pribulla+, 2009)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Star name
11- 17 A7 --- Vtype Binary type (EB or EW)
19- 24 A6 --- SpType MK spectral type (1)
27- 36 A10 --- OName BD or HD other name
38- 40 A3 --- --- [HIP]
42- 47 I6 --- HIP ? HIP designation (Cat. I/311)
49- 54 F6.2 km/s V0 Center-of-mass velocity
56- 59 F4.2 km/s e_V0 rms uncertainty on V0
61- 66 F6.2 km/s K1 Velocity amplitude of the primary (2)
68- 71 F4.2 km/s e_K1 rms uncertainty on K1
73- 78 F6.2 km/s K2 Velocity amplitude of the secondary (2)
80- 83 F4.2 km/s e_K2 rms uncertainty on K2
85- 89 F5.2 --- e1 Standard unit-weight error of the solutions
for the primary, ε1 (2)
91- 95 F5.2 --- e2 Standard unit-weight error of the solutions
for the secondary, ε2 (2)
97-106 F10.4 d T0 Spectroscopically determined moment of upper
conjonction or more massive star, T0-2400000
108-109 I2 10-4d e_T0 rms uncertainty on T0
111-117 F7.4 d O-C (O-C) deviation corresponding to E (3)
119-126 F8.1 --- E Number of elapsed periods (cycle number)
128-137 F10.8 d Per Period
138-140 I3 10-7d e_Per ? rms uncertainty on Per
142-147 F6.4 --- q Mass ratio, M2/M1
149-151 I3 10-4 e_q rms uncertainty on q
153-157 F5.3 Msun f(M) (M1+M2)sin3i value
159-160 I2 10-3Msun e_f(M) rms uncertainty on f(M)
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Note (1): The spectral types relate to the combined spectral type of all
components in a system; they are given in parentheses if taken from
the literature, otherwise they are new.
Note (2): The convention of naming the binary components in the table is
that the more massive star is marked by the subscript "1," so that the
mass ratio is always defined to be q≤1.
Note (3): The corresponding (O-C) deviations have been calculated from the
available prediction on primary minimum, as given in the text, using
the assumed periods and the number of epochs given by E.
Ephemerides (HJD{min}-2400000 + period in days) used for the
computation of the (O-C) residuals:
* TZ Boo: 52500.1920 + 0.2971597 x E
* VW Boo: 52500.0062 + 0.3423157 x E
* EL Boo: 48500.1594 + 0.413772 x E
* VZ CVn: 52500.6560 + 0.84246123 x E
* GK Cep: 52500.325 + 0.936169 x E
* RW Com: 52500.1432 + 0.2373463 x E
* V2610 Oph: 52369.95 + 0.42651 x E
* V1387 Ori: 48500.6839 + 0.730166 x E
* AU Ser: 52500.3392 + 0.386497 x E
* FT UMa: 48500.3999 + 0.6547038 x E
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Object name
11- 22 F12.4 d HJD ? Heliocentric Julian Date (1)
24- 30 F7.2 km/s RV1 ?=0 Primary radial velocity (2)
32- 35 F4.2 --- w_RV1 ?=0 Weight of V1 (3)
37- 43 F7.2 km/s RV2 ?=0 Secondary radial velocity
45- 48 F4.2 --- w_RV2 ?=0 Weight of V2 (3)
50- 55 F6.4 --- Phase Orbital phase
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Note (1): For first program star, TZ Boo, where phase smoothed BFs
(broadening functions, see Rucinski 2002AJ....124.1746R 2002AJ....124.1746R) were used,
the heliocentric Julian dates are not given.
Note (2): Corresponding to the more massive component; it was always the
component eclipsed during the minimum at the epoch T0 (this does not
always correspond to the deeper minimum and photometric phase 0.0).
The phases correspond to spectroscopic T0 and periods given in Table
2, but not necessarily to the photometric ephemerides given below the
table).
Note (3): Observations leading to entirely inseparable broadening function
peaks are given zero weight; these observations may be eventually used
in more extensive modeling of the broadening functions. Zero weights
were assigned to observations of marginally visible peaks of the
secondary (sometimes even the primary) component.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Object name (1)
11- 22 F12.4 d HJD Heliocentric Julian Date
24- 30 F7.2 km/s RV3 Third component radial velocity
32- 38 F7.2 km/s RV4 ? Fourth component radial velocity
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Note (1): Observations of the quadruple system V2610 Oph leading to
entirely inseparable broadening function peaks of the components of
the second binary have been omitted from the table and are not used in
the computation of the orbit.
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References:
Lu & Rucinski, Paper I 1999AJ....118..515L 1999AJ....118..515L
Rucinski & Lu, Paper II 1999AJ....118.2451R 1999AJ....118.2451R
Rucinski et al., Paper III 2000AJ....120.1133R 2000AJ....120.1133R
Lu et al., Paper IV 2001AJ....122..402L 2001AJ....122..402L
Rucinski et al., Paper V 2001AJ....122.1974R 2001AJ....122.1974R
Rucinski et al., Paper VI 2002AJ....124.1738R 2002AJ....124.1738R
Rucinski, Paper VII 2002AJ....124.1746R 2002AJ....124.1746R
Rucinski et al., Paper VIII 2003AJ....125.3258R 2003AJ....125.3258R
Pych et al., Paper IX 2004AJ....127.1712P 2004AJ....127.1712P
Rucinski et al., Paper X 2005AJ....130..767R 2005AJ....130..767R, Cat. J/AJ/130/767
Pribulla et al., Paper XI 2006AJ....132..769P 2006AJ....132..769P, Cat. J/AJ/132/769
Pribulla et al., Paper XII 2007AJ....133.1977P 2007AJ....133.1977P, Cat. J/AJ/133/1977
Rucinski et al., Paper XIII 2008AJ....136..586R 2008AJ....136..586R, Cat. J/AJ/136/586
Pribulla et al., Paper XV 2009AJ....137.3655P 2009AJ....137.3655P, Cat. J/AJ/137/3655
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 27-Aug-2011