- ID:
- ivo://CDS.VizieR/J/A+A/454/301
- Title:
- Radial velocities of 6 binaries
- Short Name:
- J/A+A/454/301
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Radial velocity measurements of the two components of three new discovered SB2 systems, HD183957, BD+15 4538, and BD+33 4462, have been obtained from optical spectra acquired with both ELODIE and AURELIE spectrographs at the Observatoire de Haute-Provence (OHP) and FRESCO spectrograph at the Osservatorio Astrofisico di Catania (OAC) by means of the cross-correlation technique (Tables 2-4). Radial velocities of three new discovered SB1 systems, HD 237215, HD 57267, and BD+38 2140, obtained with the same instruments are reported in Tables 5-7.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/ApJ/700/1349
- Title:
- Radial velocities of Capella
- Short Name:
- J/ApJ/700/1349
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report extensive radial velocity measurements of the two giant components of the detached, 104 day period binary system of Capella. Our highly accurate three-dimensional orbital solution based on all existing spectroscopic and astrometric observations including our own yields much improved masses for the primary and secondary of 2.466+/-0.018M_{sun}_ and 2.443+/-0.013M_{sun}_, with relative errors of only 0.7% and 0.5%, respectively. The mass ratio is considerably closer to unity than previously believed, which has an impact on assessing the evolutionary state of the system. Improved values are presented also for the radii (11.87+/-0.56R_{sun}_ and 8.75+/-0.32R_{sun}_), effective temperatures (4920+/-70K and 5680+/-70K), and luminosities (79.5+/-4.8L_{sun}_ and 72.1+/-3.6L_{sun}_). The distance is determined to be 13.042+/-0.028pc, based on the accurate orbital parallax. The projected rotational velocities and individual rotation periods are also known. Capella is unique among evolved stars in that, in addition to all of the above, the chemical composition is known as well.
- ID:
- ivo://CDS.VizieR/J/A+AS/116/497
- Title:
- Radial velocities of 4 Cepheids
- Short Name:
- J/A+AS/116/497
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Continued radial velocity observations over several years, have allowed to discover four spectroscopic binary systems among our sample of twenty five galactic Cepheids. Each system is composed by the Cepheid and an invisible probably hot dwarf star. A spectroscopic orbit has been determined for each system. The orbital periods for RX Cam, MW Cyg, Z Lac and U Vul are 1113, 439, 383 and 2510 days, respectively. For the pulsation motion, radial velocity versus phase diagram have been fitted by an analytic relation, formally similar to a Kepler motion. The stellar radius variation of each cepheid has been derived by integration of this relation over the whole pulsating period.
- ID:
- ivo://CDS.VizieR/J/A+A/638/A131
- Title:
- Radial velocities of 643 DA white dwarfs
- Short Name:
- J/A+A/638/A131
- Date:
- 14 Jan 2022 08:18:09
- Publisher:
- CDS
- Description:
- Close double degenerate binaries are one of the favoured progenitor channels for type Ia supernovae, but it is unclear how many suitable systems there are in the Galaxy. We report results of a large radial velocity survey for double degenerate (DD) binaries using the UVES spectrograph at the ESO VLT (ESO SNIa Progenitor surveY - SPY). Exposures taken at different epochs are checked for radial velocity shifts indicating close binary systems.We observed 689 targets classified as DA (displaying hydrogen-rich atmospheres), of which 46 turned out to possess a cool companion. We measured radial velocities (RV) of the remaining 643 DA white dwarfs.We managed to secure observations at two or more epochs for 625 targets, supplemented by eleven objects meeting our selection criteria from literature. The data reduction and analysis methods applied to the survey data are described in detail. The sample contains 39 double degenerate binaries, only four of which were previously known. 20 are double-lined systems, in which features from both components are visible, the other 19 are single-lined binaries. We provide absolute RVs transformed to the heliocentric system suitable for kinematic studies. Our sample is large enough to sub-divide by mass: 16 out of 44 low mass targets (<=0.45M_{sun}_) are detected as DDs, while just 23 of the remaining 567 with multiple spectra and mass >0.45M_{sun}_ are double. Although the detected fraction amongst the low mass objects (36.4+/-7.3%) is significantly higher than for the higher-mass, carbon/oxygen-core dominated part of the sample (3.9+/-0.8%), it is lower than the detection efficiency based upon companion star masses of 0.05M_{sun}_ or higher and a 100% binary fraction. This suggests either companion stars of mass below 0.05M_{sun}_ or some of the low mass white dwarfs are single.
- ID:
- ivo://CDS.VizieR/J/MNRAS/454/2344
- Title:
- Radial velocities of {delta} Sagittae
- Short Name:
- J/MNRAS/454/2344
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Radial-velocity observations spanning more than a century are used to produce a reliable orbit of the {delta} Sagittae system. We find an orbital period of 3703.7+/-1.5 d and a semi-amplitude of 7.73+/-0.05 km/s. In addition, we find quasi-periodic variations with time-scales in the range of 550-750 d and a typical amplitude of 1 km/s. The phase and amplitude are both irregular, sometimes changing very abruptly. We consider pulsation, rotational modulation and convection as possible causes of the variations, finally favouring convection.
- ID:
- ivo://CDS.VizieR/J/ApJ/766/119
- Title:
- Radial velocities of {delta} Sco
- Short Name:
- J/ApJ/766/119
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We describe the results of the world-wide observing campaign of the highly eccentric Be binary system {delta} Scorpii 2011 periastron passage which involved professional and amateur astronomers. Our spectroscopic observations provided a precise measurement of the system orbital period at 10.8092+/-0.0005yr. Fitting of the HeII 4686{AA} line radial velocity curve determined the periastron passage time on 2011 July 3, UT 9:20 with a 0.9-day uncertainty. Both these results are in a very good agreement with recent findings from interferometry. We also derived new evolutionary masses of the binary components (13 and 8.2M_{sun}_) and a new distance of 136pc from the Sun, consistent with the HIPPARCOS parallax. The radial velocity and profile variations observed in the H{alpha} line near the 2011 periastron reflected the interaction of the secondary component and the circumstellar disk around the primary component. Using these data, we estimated a disk radius of 150R_{sun}_. Our analysis of the radial velocity variations measured during the periastron passage time in 2000 and 2011 along with those measured during the 20th century, the high eccentricity of the system, and the presence of a bow shock-like structure around it suggest that {delta} Sco might be a runaway triple system. The third component should be external to the known binary and move on an elliptical orbit that is tilted by at least 40{deg} with respect to the binary orbital plane for such a system to be stable and responsible for the observed long-term radial velocity variations.
- ID:
- ivo://CDS.VizieR/J/MNRAS/356/545
- Title:
- Radial velocities of DG Leo
- Short Name:
- J/MNRAS/356/545
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- DG Leo is a spectroscopic triple system composed of three stars of late-A spectral type, one of which was suggested to be a delta Scuti star. Seven nights of observations at high spectral and high time-resolution at the Observatoire de Haute-Provence with the ELODIE spectrograph were used to obtain the component spectra by applying a Fourier transform spectral disentangling technique. Comparing these with synthetic spectra, the stellar fundamental parameters (effective temperature, surface gravity, projected rotation velocity and chemical composition) are derived. The inner binary consists of two Am components, at least one of which is not yet rotating synchronously at the orbital period though the orbit is a circular one. The distant third component is confirmed to be a delta Scuti star with normal chemical composition.
- ID:
- ivo://CDS.VizieR/J/A+A/461/1077
- Title:
- Radial velocities of DW Car
- Short Name:
- J/A+A/461/1077
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have studied the high-mass short-period detached eclipsing binary DW Carinae using high-resolution echelle spectroscopy and photoelectric Stroemgren uvby light curves. We derived masses and radii accurate to 1% as well as the effective temperatures and reddening of the system. The high rotational velocities of the component stars meant that blending was a major problem when deriving radial velocities from the spectroscopy. Only helium lines provided good results, and a critique of different methods of measurement showed that spectral disentangling and fitting double Gaussians showed that these were the best able to provide reliable results in this case. The final spectroscopic orbit was calculated using spectral disentangling but we also provided radial velocities by fitting double Gaussians to the He-I 4472-A spectral line in each spectrum as this gives a good idea as to the quality of the data whilst providing a result very close to that adopted to calculate the masses. The light curves of DW Car are published as part of an accompanying paper (Clausen et al., 2006, Cat. <J/A+A/461/1065>).
- ID:
- ivo://CDS.VizieR/J/A+A/402/745
- Title:
- Radial velocities of ER Vul
- Short Name:
- J/A+A/402/745
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- ER Vul is an eclipsing binary consisting of two solar type stars in a very close orbit with a period of 0.7d. Accordingly, the two stars rotate very fast, leading to a blending of many spectral features at all phases. Therefore, measuring the radial velocity curve without systematic errors is not trivial. Here, we use a two-dimensional cross-correlation method applied to 137 high quality spectra, collected over 3 years, in order to obtain the radial velocity curve and determine the orbital and some physical parameters of the system from it. Primarily, we improve the binary period to 0.69809458d+/-0.00000014d, and find that the two amplitudes are slightly smaller than those measured by others, while the mass ratio is still similar. While at least the primary almost fills its Roche lobe, the system is still detached, i.e. not yet a fully fledged W UMa-system. The behaviour of the CaII IRT line at 8662{AA} confirms that the secondary is the more active component, and that the chromospheric emission is not symmetrically distributed over the surfaces of either star.
- ID:
- ivo://CDS.VizieR/J/AJ/145/111
- Title:
- Radial velocities of five spectroscopic binaries
- Short Name:
- J/AJ/145/111
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have determined spectroscopic orbits for five single-lined spectroscopic binaries, HD100167, HD135991, HD140667, HD158222, HD217924. Their periods range from 60.6 to 2403days and the eccentricities from 0.20 to 0.84. Our spectral classes for the stars confirm that they are of solar type, F9-G5, and all are dwarfs. Their [Fe/H] abundances, determined spectroscopically, are close to the solar value and on average are 0.12 greater than abundances from a photometric calibration. Four of the five stars are rotating faster than their predicted pseudosynchronous rotational velocities.
