J/AJ/132/769 Radial velocities of 10 close binaries (Pribulla+, 2006)
Radial velocity studies of close binary stars. XI.
Pribulla T., Rucinski S.M., Lu W., Mochnacki S.W., Conidis G., Blake R.M.,
Debond H., Thomson J.R., Pych W., Ogloza W., Siwak M.
<Astron. J., 132, 769-780 (2006)>
=2006AJ....132..769P 2006AJ....132..769P
ADC_Keywords: Binaries, eclipsing ; Radial velocities
Keywords: binaries: close - binaries: eclipsing - stars: variables: other
Abstract:
Radial-velocity measurements and sinecurve fits to orbital radial
velocity variations are presented for 10 close binary systems: DU Boo,
ET Boo, TX Cnc, V1073 Cyg, HL Dra, AK Her, VW LMi, V566 Oph, TV UMi,
and AG Vir. With this contribution, the David Dunlap Observatory
program has reached the point of 100 published radial velocity orbits.
The radial velocities have been determined using an improved fitting
technique that uses rotational profiles to approximate individual
peaks in broadening functions. Three systems, ET Boo, VW LMi, and
TV UMi, are found to be quadruple, while AG Vir appears to be a
spectroscopic triple. ET Boo, a member of a close visual binary with
Pvis=113yr, was previously known to be a multiple system, but we
show that the second component is actually a close, non-eclipsing
binary. The new observations have enabled us to determine the
spectroscopic orbits of the companion, non-eclipsing pairs in ET Boo
and VW LMi. A particularly interesting case is VW LMi, for which the
period of the mutual revolution of the two spectroscopic binaries is
only 355-days. While most of the studied eclipsing pairs are contact
binaries, ET Boo is composed of two double-lined detached binaries,
and HL Dra is a single-lined detached or semidetached system. Five
systems of this group have been observed spectroscopically before:
TX Cnc, V1073 Cyg, AK Her (as a single-lined binary), V566 Oph, and
AG Vir, but our new data are of much higher quality than in the
previous studies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 68 10 Stars positions (from Simbad) and orbital period
table1.dat 59 987 DDO radial velocity observations of
close binary systems
table3.dat 39 353 Radial velocity observations of the third and
fourth components of quadruple systems
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See also:
J/A+A/387/850 : Radial velocities of eclipsing binaries (Imbert, 2002)
J/AJ/130/767 : Radial velocity studies of close binary stars (Rucinski+, 2005)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Simbad name
11- 12 I2 h RAh Simbad Hour of Right Ascension (J2000.0)
14- 15 I2 min RAm Simbad Minute of Right Ascension (J2000.0)
17- 20 F4.1 s RAs Simbad Second of Right Ascension (J2000.0)
22 A1 --- DE- Simbad Sign of the Declination (J2000.0)
23- 24 I2 deg DEd Simbad Degree of Declination (J2000.0)
26- 27 I2 arcmin DEm Simbad Arcminute of Declination (J2000.0)
29- 30 I2 arcsec DEs Simbad Arcsecond of Declination (J2000.0)
33- 37 F5.2 mag Bmag Simbad B band magnitude
39- 43 F5.2 mag Vmag Simbad V band magnitude
45- 47 A3 --- SpType MK spectral type
51- 57 A7 --- Class Eclipsing class
59- 68 F10.8 d P Oribtal period
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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
24- 30 F7.2 km/s RV1 ? Radial velocity of stronger component (1)
32- 37 F6.4 --- W1 Stronger component weight (2)
39- 45 F7.2 km/s RV2 ? Radial velocity of weaker component
47- 52 F6.4 --- W2 ? Weaker component weight (2)
54- 59 F6.4 --- Phase Orbital phase
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Note (1): Correspond to the component which is more massive of the two,
even if it is not the one eclipsed at the primary minimum. This
explains why in the number of epochs elapsed to T0 given in Table 2
is not always an integer number.
Note (2): Observations leading to entirely inseparable broadening function
peaks are given zero weight; these observations may be eventually used
in more extensive modelling of broadening functions.
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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 Object name (1)
11- 23 F13.5 d HJD Heliocentric Julian Date
25- 30 F6.2 km/s RV3 Third component radial velocity
32- 37 F6.2 km/s RV4 Fourth component radial velocity
39 A1 --- Flag [b] Indicates RVs determined from blended
profiles
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Note (1): Observations of quadruple systems ET Boo, VW LMi and TV UMi
leading to entirely inseparable broadening function peaks of
components of the second binary are omitted from the table.
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History:
From electronic version of the journal
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
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 08-Feb-2008