J/AJ/133/1977 Radial velocities of 10 close binaries (Pribulla+, 2007)
Radial velocity studies of close binary stars. XII.
Pribulla T., Rucinski S.M., Conidis G., Debond H., Thomson J.R., Gazeas K.,
Ogloza W.
<Astron. J., 133, 1977-1987 (2007)>
=2007AJ....133.1977P 2007AJ....133.1977P
ADC_Keywords: Binaries, eclipsing ; Radial velocities
Keywords: binaries: close - binaries: eclipsing - stars: variables: other
Abstract:
Radial velocity measurements and sine-curve fits to the orbital radial
velocity variations are presented for 10 close binary systems: OO Aql,
CC Com, V345 Gem, XY Leo, AM Leo, V1010 Oph, V2612 Oph, XX Sex, W UMa,
and XY UMa. Most of these binaries have been observed spectroscopically
before, but our data are of higher quality and consistency than in the
previous studies. While most of the studied eclipsing pairs are
contact binaries, V1010 Oph is probably a detached or semidetached
double-lined binary, and XY UMa is a detached, chromospherically
active system whose broadening functions clearly show well-defined and
localized dark spots on the primary component. A particularly
interesting case is XY Leo, which is a member of visually unresolved
quadruple system composed of a contact binary and a detached,
noneclipsing, active binary with an 0.805 day orbital period. V345 Gem
and AM Leo are known members of visual binaries. We found faint visual
companions at about 2"-3" from XX Sex and XY UMa.
Description:
The radial velocity (RV) observations reported in this paper were
collected between 2005 April and 2006 April.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 76 10 Star positions (from Simbad)
table1.dat 55 667 DDO radial velocity observations
table3.dat 30 157 Radial velocity observations of visual companion
to V345 Gem and third component in XY Leo
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See also:
J/AJ/130/767 : Radial velocity studies of close binary stars (Rucinski+, 2005)
J/AJ/132/769 : Radial velocities of 10 close binaries (Pribulla+, 2006)
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- 44 F6.3 mag Vmag Simbad V band magnitude
46- 52 A7 --- SpType Simbad MK spectral type
53- 64 F12.4 d T0 Spectroscopically determined moments of
primary or secondary minima, T0 (1)
67- 76 F10.8 d Per Period (1)
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Note (1): From table2 of the paper.
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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 Star name
11- 22 F12.4 d HJD Heliocentric Julian Date
24- 30 F7.2 km/s RV1 ?=0.00 More massive component radial velocity (1)
32- 35 F4.2 --- w_RV1 Primary radial velocity weight (2)
37- 43 F7.2 km/s RV2 ?=0.00 Least massive component radial velocity
45- 48 F4.2 --- w_RV2 Secondary radial velocity weight (2)
50- 55 F6.4 --- Phase Orbital phase (3)
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Note (1): This is always the component eclipsed during the minimum at the
epoch T0 (this not always corresponds to the deeper minimum and
photometric phase 0.0).
Note (2): Observations leading to entirely inseparable broadening function
peaks are given zero weight; these observations may be eventually used
in more extensive modeling of broadening functions.
Note (3): The phases correspond to T0 and periods given in stars.dat file.
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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- 8 A8 --- Name Star name
11- 23 F13.5 d HJD Heliocentric Julian Date
25- 30 F6.2 km/s RV3 Radial velocity (1)
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Note (1): The radial velocities of V345 Gem until HJD 2453785 were derived
from spectra where the single, dominant component was centered on the
spectrograph slit. After HJD 2453788 the spectrograph slit was
centered on the fainter eclipsing binary and the radial velocities
were determined by Gaussian profile fitting to the BFs with the light
contamination L3/(L1+L2)>0.10.
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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
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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
Rucinski et al., Paper XII 2008AJ....136..586R 2008AJ....136..586R
Pribulla et al., Paper XIV 2009AJ....137.3646P 2009AJ....137.3646P
Pribulla et al., Paper XV 2009AJ....137.3655P 2009AJ....137.3655P
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 21-Mar-2009