J/AJ/130/767 Radial velocity studies of close binary stars (Rucinski+, 2005)
Radial velocity studies of close binary stars. X.
Rucinski S.M., Pych W., Ogloza W., Debond H., Thomson J.R., Mochnacki S.W.,
Capobianco C.C., Conidis G., Rogoziecki P.
<Astron. J., 130, 767-775 (2005)>
=2005AJ....130..767R 2005AJ....130..767R
ADC_Keywords: Stars, variable ; Binaries, eclipsing ; Radial velocities
Keywords: binaries: close - binaries: eclipsing - stars: variables: other
Abstract:
Radial velocity measurements and sine-curve fits to orbital velocity
variations are presented for the ninth set of 10 close binary systems:
V395 And, HS Aqr, V449 Aur, FP Boo, SW Lac, KS Peg, IW Per, V592 Per,
TU UMi, and FO Vir. The first three are very close, possibly detached,
early-type binaries, and all three require further investigation.
Particularly interesting is V395 And, whose spectral type is as early
as B7/8 for a 0.685 day orbit binary. KS Peg and IW Per are
single-line binaries, with the former probably hosting a very low mass
star. We have detected a low-mass secondary in an important
semidetached system, FO Vir, at q=0.125±0.005. The contact binary
FP Boo is also a very small mass ratio system, q=0.106±0.005. The
other contact binaries in this group are V592 Per, TU UMi, and the
well-known SW Lac. V592 Per and TU UMi have bright tertiary
companions; for these binaries, and for V395 And, we used a novel
technique of arranging the broadening functions into a two-dimensional
image in phase. The case of TU UMi turned out to be intractable even
using this approach, and we have not been able to derive a firm radial
velocity orbit for this binary. Three systems of this group were
observed spectroscopically before: HS Aqr, SW Lac, and KS Peg.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stars.dat 76 10 Summary of stars observed
table1.dat 49 563 DDO radial velocity observations from erratum,
2007, AJ 134, 445
--------------------------------------------------------------------------------
See also:
J/A+A/387/850 : Radial velocities of eclipsing binaries (Imbert, 2002)
Byte-by-byte Description of file: stars.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 21 A21 --- Name Star name
23- 24 I2 h RAh Simbad Hour of Right Ascension (J2000.0)
26- 27 I2 min RAm Simbad Minute of Right Ascension (J2000.0)
29- 32 F4.1 s RAs Simbad Second of Right Ascension (J2000.0)
34 A1 --- DE- Simbad Sign of the Declination (J2000.0)
35- 36 I2 deg DEd Simbad Degree of Declination (J2000.0)
38- 39 I2 arcmin DEm Simbad Arcminute of Declination (J2000.0)
41- 42 I2 arcsec DEs Simbad Arcsecond of Declination (J2000.0)
46- 50 F5.2 mag Bmag Simbad B band magnitude
52- 56 F5.2 mag Vmag Simbad V band magnitude
58- 63 A6 --- SpType Simbad MK spectral type
65- 76 F12.10 d P ? GCVS period
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Source name (1)
10 A1 --- f_Name [n] Indicates no data, see text
12- 23 F12.4 d HJD ? Heliocentric Julian Date of the observation
25- 31 F7.2 km/s RV1 ? Stronger component radial velocity (2)
33- 36 F4.2 --- W1 ? Stronger component associated weight (3)
38- 44 F7.2 km/s RV2 ? Weaker component radial velocity
46- 49 F4.2 --- W2 ? Weaker component associated weight (3)
--------------------------------------------------------------------------------
Note (1): HS Aqr is more typical than the first, V395 And, for which radial
velocities were obtained from smoothed, averaged broadening functions
as described in the text. There are no radial velocity data for TU UMi.
Note (2): The radial velocities designated as V1 correspond to the
component which was stronger and easier to measure in the analysis of
the broadening functions; it was not always the component eclipsed
during the primary minimum at the epoch T0 (see Table 2). The
figures should help in identifying which star is which.
Note (3): Observations leading to entirely inseparable broadening- and
correlation-function peaks are given zero weight; these observations
may be eventually used in more extensive modeling of broadening
functions.
--------------------------------------------------------------------------------
History:
* 24-Apr-2006: From electronic version of the journal
* 26-Aug-2009: Corrected table from erratum (2007, AJ 134, 445)
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
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 24-Apr-2006