J/MNRAS/496/1355 Accurate SB2 radial velocities (Halbwachs+, 2020)
Masses of the components of SB2 binaries observed with Gaia. V.
Accurate SB2 orbits for 10 binaries and masses of the components of 5 binaries.
Halbwachs J.-L., Kiefer F., Lebreton Y., Boffin H.M.J., Arenou F.,
Le Bouquin J.-B., Famaey B., Pourbaix D., Guillout P., Salomon J.-B.,
Mazeh T.
<Mon. Not. R. Astron. Soc. 496, 1355-1368 (2020)>
=2020MNRAS.496.1355H 2020MNRAS.496.1355H (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Radial velocities
Keywords: binaries: spectroscopic - stars: fundamental parameters -
stars: individual: HIP 104987
Abstract:
Double-lined spectroscopic binaries (SB2s) are one of the main sources
of stellar masses, as additional observations are only needed to give
the inclinations of the orbital planes in order to obtain the
individual masses of the components. For this reason, we are observing
a selection of SB2s using the SOPHIE spectrograph at the
Haute-Provence observatory in order to precisely determine their
orbital elements. Our objective is to finally obtain masses with an
accuracy of the order of one percent by combining our radial velocity
(RV) measurements and the astrometric measurements that will come from
the Gaia satellite. We present here the RVs and the re-determined
orbits of 10 SB2s. In order to verify the masses we will derive from
Gaia, we obtained interferometric measurements of the ESO VLTI for one
of these SB2s. Adding the interferometric or speckle measurements
already published by us or by others for 4 other stars, we finally
obtain the masses of the components of 5 binary stars, with masses
ranging from 0.51 to 2.2 solar masses, including main-sequence dwarfs
and some more evolved stars whose location in the HR diagram has been
estimated.
Description:
The observations were performed at the T193 telescope of the
Haute-Provence Observatory, with the SOPHIE spectrograph. SOPHIE is
dedicated to the search of extrasolar planets, and, thanks to its high
resolution (R∼75000), it enables accurate stellar RVs to be measured
for SB2 components.
The RVs of the components are derived using the TwO-Dimensional
CORrelation algorithm todcor (Zucker & Mazeh 1994ApJ...420..806Z 1994ApJ...420..806Z;
Zucker et al. 2004, Cat. J/A+A/426/695).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 38 10 10 SB2 analysed in this paper
table3.dat 78 146 New radial velocities from SOPHIE and obtained
with TODCOR
table4.dat 36 10 Correction terms of the uncertainties for the 10
SB2 analysed in this paper (Table 4, col. 1,7-10)
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
J/A+A/498/627 : Radial velocities of SB with M giant (Famaey+, 2009)
J/MNRAS/458/3272 : Paper III: Radial velocities of 10 SB2 (Kiefer+, 2016)
J/MNRAS/474/731 : Paper IV: Radial velocities of 14 SB2 (Kiefer+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1 A1 --- Note [P1] Note (1)
3- 8 I6 --- HIP HIP number
10- 15 I6 --- HD ? HD number
17- 20 F4.2 mag Vmag V magnitude
22- 25 I4 d Per Period (2)
27- 28 I2 --- Nsp Number of spectra collected with SOPHIE
30- 34 F5.2 --- Tspan Total span of observation epochs,
counted in number of periods
(rounded to 2 digits)
36- 38 I3 --- SNR Median signal-to-noise ratio of each sample
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Note (1): Note as follows:
P = Previously published SB2
1 = SB2 identified in paper I, Halbwachs et al., 2014MNRAS.445.2371H 2014MNRAS.445.2371H,
previously published as SB1
Note (2): The period values are taken from our solution.
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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- 3 A3 --- --- [HIP]
5- 10 I6 --- HIP HIP number
12- 21 F10.4 d BJD Barycentric Julian date (BJD-2400000)
23- 30 F8.4 km/s RV1 Primary radial velocity
31 A1 --- n_RV1 [*] Note on RV1 (1)
33- 38 F6.4 km/s e_RV1 rms uncertainty on RV1, derived from TODCOR
(to be corrected with the terms in table 4)
39 A1 --- neRV1 [*] Note on e_RV1 (1)
41- 49 F9.4 km/s RV2 Secondary radial velocity
50 A1 --- n_RV2 [*] Note on RV2 (1)
52- 57 F6.4 km/s e_RV2 rms uncertainty on RV2, derived from TODCOR
(to be corrected with the terms in table 4)
58 A1 --- neRV2 [*] Note on e_RV2 (1)
60- 67 F8.4 km/s O1-C1 Observed minus computed for RV1
68 A1 --- n_O1-C1 [*] Note on O1-C1 (1)
70- 77 F8.4 km/s O2-C2 Observed minus computed for RV2
78 A1 --- n_O2-C2 [*] Note on O2-C2 (1)
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Note (1): * indicates outlier, not taken into account in the analysis
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [HIP]
5- 10 I6 --- HIP HIP number
12- 17 F6.4 km/s eps1 Noise to be quadratically added to e_RV1
19- 23 F5.3 --- phi1 Correction coefficient; the final
uncertainty of RV1 is:
phi1*sqrt(e_RV12 +eps12)
25- 30 F6.4 km/s eps2 Noise to be quadratically added to e_RV2
32- 36 F5.3 --- phi2 Correction coefficient; the final
uncertainty of RV2 is:
phi2*sqrt(e_RV22 +eps22)
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History:
Jean-Louis Halbwachs, jean-louis.halbwachs(at)astro.unistra.fr
References:
Halbwachs et al., Paper I 2014MNRAS.445.2371H 2014MNRAS.445.2371H
Halbwachs et al., Paper II 2016MNRAS.455.3303H 2016MNRAS.455.3303H
Kiefer et al., Paper III 2016MNRAS.458.3272K 2016MNRAS.458.3272K, Cat. J/MNRAS/458/3272
Kiefer et al., Paper IV 2018MNRAS.474..731K 2018MNRAS.474..731K, Cat. J/MNRAS/474/731
(End) Jean-Louis Halbwachs [Strasbourg Obs.], Patricia Vannier [CDS] 05-Jul-2020