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J/MNRAS/474/731     Accurate SB2 radial velocities           (Kiefer+, 2018)

Masses of the components of SB2 binaries observed with Gaia. IV. Accurate SB2 orbits for 14 binaries and masses of three binaries. Kiefer F., Halbwachs J.-L., Lebreton Y., Soubiran C., Arenou F., Pourbaix D., Famaey B., Guillout P., Ibata R., Mazeh T. <Mon. Not. R. Astron. Soc. 474, 731 (2018)> =2018MNRAS.474..731K (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Radial velocities Keywords: binaries: spectroscopic - stars: fundamental parameters - stars: individual: HIP 61100, HIP 95995, HIP 101382 Abstract: The orbital motion of non-contact double-lined spectroscopic binaries (SB2s), with periods of a few tens of days to several years, holds unique, accurate information on individual stellar masses, which only long-term monitoring can unlock. The combination of radial velocity measurements from high-resolution spectrographs and astrometric measurements from high-precision interferometers allows the derivation of SB2 component masses down to the percent precision. Since 2010, we have observed a large sample of SB2s with the SOPHIE spectrograph at the Observatoire de Haute-Provence, aiming at the derivation of orbital elements with sufficient accuracy to obtain masses of components with relative errors as low as 1 per cent when the astrometric measurements of the Gaia satellite are taken into account. In this paper, we present the results from 6 yr of observations of 14 SB2 systems with periods ranging from 33 to 4185 days. Using the TODMOR algorithm, we computed radial velocities from the spectra and then derived the orbital elements of these binary systems. The minimum masses of the 28 stellar components are then obtained with an average sample accuracy of 1.0±0.2 per cent. Combining the radial velocities with existing interferometric measurements, we derived the masses of the primary and secondary components of HIP 61100, HIP 95995 and HIP 101382 with relative errors for components (A,B) of, respectively, (2.0, 1.7) per cent, (3.7, 3.7) per cent and (0.2, 0.1) per cent. Using the CESAM2K stellar evolution code, we constrained the initial He abundance, age and metallicity for HIP 61100 and HIP 95995. 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; Zucker et al. 2004, Cat. J/A+A/426/695). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 49 14 14 SB2 analysed in this paper table3.dat 77 204 New radial velocities from SOPHIE and obtained with TODCOR table4.dat 36 14 Correction terms of the uncertainties for the 14 SB2 analysed in this paper (Table 4, col. 1, 7-10)
See also: I/337 : Gaia DR1 (Gaia Collaboration, 2016) J/MNRAS/458/3272 : Paper III: Radial velocities of 10 SB2 (Kiefer+, 2016) J/A+A/498/627 : Radial velocities of SB with M giant (Famaey+, 2009) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
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 40- 49 A10 --- Name HIP or HD designation
Note (1): Note as follows: P = Previously published SB2 1 = SB2 identified in paper I, Halbwachs et al., 2014MNRAS.445.2371H, previously published as SB1 Note (2): The period values are taken from the SB9 catalogue (Pourbaix et al., 2004, Cat. B/sb9).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Name HIP or HD designation 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- 76 F7.4 km/s O2-C2 Observed minus computed for RV2 77 A1 --- n_O2-C2 [*] Note on O2-C2 (1)
Note (1): * indicates outlier, not taken into account in the analysis.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Name HIP or HD designation 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)
Acknowledgements: Jean-Louis Halbwachs, jean-louis.halbwachs(at) References: Halbwachs et al., Paper I 2014MNRAS.445.2371H Halbwachs et al., Paper II 2016MNRAS.455.3303H Kiefer et al., Paper III 2016MNRAS.458.3272K, J/MNRAS/458/3272
(End) Patricia Vannier [CDS] 21-Dec-2017
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