- ID:
- ivo://CDS.VizieR/J/A+A/527/A63
- Title:
- Radial velocities of 7 new HARPS planetary systems
- Short Name:
- J/A+A/527/A63
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We are conducting a planet search survey with HARPS since seven years. The volume-limited stellar sample includes all F2 to M0 main-sequence stars within 57.5pc, where extrasolar planetary signatures are systematically searched for with the radial-velocity technics. In this paper, we report the discovery of new substellar companions of seven main-sequence stars and one giant star, detected through multiple Doppler measurements with the instrument HARPS installed on the ESO 3.6m telescope, La Silla, Chile.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/563/A22
- Title:
- Radial velocities of 3 new hot Jupiters
- Short Name:
- J/A+A/563/A22
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present high-precision radial-velocity measurements of three solar-type stars: HD 13908, HD 159243, and HIP 91258. The observations were made with the SOPHIE spectrograph at the 1.93m telescope of the Observatoire de Haute-Provence (France). They show that these three bright stars host exoplanetary systems composed of at least two companions.
- ID:
- ivo://CDS.VizieR/J/AJ/101/625
- Title:
- Radial velocities of NGP wide binaries
- Short Name:
- J/AJ/101/625
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present precise radial velocities from a survey of 247 stars centered on Selected Area 57 at the North Galactic Pole, complete for late-type stars with V magnitude brighter than 12.0. The radial velocities have a typical precision of 0.2-0.3km/s. New spectral types and distances estimates are presented for 120 of the stars in the sample. We have considered all pairs of stars with angular separations between 1 and 600arcsec, and find 11 candidate pairs with velocity differences less than 1.5km/s. We estimate that 4 or 5 of the 11 candidate pairs are actually bound binaries, but none with separations larger than 0.1pc. The constraints imposed by these results on the actual distribution of wide binaries in the Galaxy should now be reanalyzed. The unusual precision of our velocities led to the discovery of a new cluster associated with the multiple system ADS 8811 ABC.
- ID:
- ivo://CDS.VizieR/J/ApJS/162/207
- Title:
- Radial velocities of solar-type stars
- Short Name:
- J/ApJS/162/207
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We studied for duplicity the 167 F7-G8 IV or V primaries within 25pc of the Sun according to their Hipparcos parallaxes and between declinations of -30{deg} and +75{deg}.
- ID:
- ivo://CDS.VizieR/J/A+A/545/A139
- Title:
- Radial Velocities of stars observed in M67
- Short Name:
- J/A+A/545/A139
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Precise stellar radial velocities are used to search for massive (Jupiter masses or higher) exoplanets around the stars of the open cluster M67. We observed a total of 88 main-sequence stars, subgiants, and giants all highly probable members of M67, using four telescopes and instrument combinations: the HARPS spectrograph at the ESO 3.6m, the SOPHIE spectrograph at OHP, the CORALIE spectrograph at the Euler Swiss telescope and the HRS spectrograph at Hobby Eberly Telescope. We investigate whether exoplanets are present by obtaining radial velocities with precisions as good as 10m/s.
- ID:
- ivo://CDS.VizieR/J/A+A/588/A145
- Title:
- Radial velocities of 8 stars with giant planets
- Short Name:
- J/A+A/588/A145
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new radial velocity measurements of eight stars that were secured with the spectrograph SOPHIE at the 193cm telescope of the Haute-Provence Observatory. The measurements allow detecting and characterizing new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes of between 6.7 and 9.6; the planets have minimum masses M_p_sini of between 0.4 to 3.8M_Jup_ and orbitalperiods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD 143105, HIP 109600, HD 35759, HIP 109384, HD 220842, and HD 12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP 65407, allows the discovery of two giant planets that orbit just outside the 12:5 resonance in weak mutual interaction. The last star, HD 141399, was already known to host a four-planet system; our additional data and analyses allow new constraints to be set on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planet systems. HD 143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted even though this is not a transiting system. The giant planets HIP 109600b, HIP 109384b, and HD 141399c are located in the habitable zone of their host star.
- ID:
- ivo://CDS.VizieR/J/AJ/153/142
- Title:
- Radial velocities of systems hosting sub-Saturns
- Short Name:
- J/AJ/153/142
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results from a Keck/HIRES radial velocity campaign to study four sub-Saturn-sized planets, K2-27b, K2-32b, K2-39b, and K2-108b, with the goal of understanding their masses, orbits, and heavy-element enrichment. The planets have similar sizes (R_P_=4.5-5.5R_{Earth}_), but have dissimilar masses (M_P_=16-60M_{Earth}_), implying a diversity in their core and envelope masses. K2-32b is the least massive (M_P_=16.5+/-2.7M_{Earth}_) and orbits in close proximity to two sub-Neptunes near a 3:2:1 period commensurability. K2-27b and K2-39b are significantly more massive at M_P_=30.9+/-4.6M_{Earth}_ and M_P_=39.8+/-4.4M_{Earth}_, respectively, and show no signs of additional planets. K2-108b is the most massive at M_P_=59.4+/-4.4M_{Earth}_, implying a large reservoir of heavy elements of about {simeq}50M__. Sub-Saturns as a population have a large diversity in planet mass at a given size. They exhibit remarkably little correlation between mass and size; sub-Saturns range from {simeq}6-60M_{Earth}_, regardless of size. We find a strong correlation between planet mass and host star metallicity, suggesting that metal-rich disks form more massive planet cores. The most massive sub-Saturns tend to lack detected companions and have moderately eccentric orbits, perhaps as a result of a previous epoch of dynamical instability. Finally, we observe only a weak correlation between the planet envelope fraction and present-day equilibrium temperature, suggesting that photo-evaporation does not play a dominant role in determining the amount of gas sub-Saturns accrete from their protoplanetary disks.
- ID:
- ivo://CDS.VizieR/J/AJ/160/251
- Title:
- Radial velocities & orbital data, 5 triple stars
- Short Name:
- J/AJ/160/251
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Joint analysis of radial velocities and position measurements of five hierarchical stellar systems is undertaken to determine elements of their inner and outer orbits and, whenever possible, their mutual inclinations. The inner and outer periods are 12.9 and 345yr for HD12376 (ADS1613), 1.14 and ~1500yr for HD19971 (ADS2390), 8.3 and 475yr for HD89795 (ADS7338), 1.11 and 40yr for HD152027, 0.69 and 7.4yr for HD190412. The latter system with its coplanar and quasi-circular orbits belongs to the family of compact planetary-like hierarchies, while the orbits in HD12376 have a mutual inclination of 131{deg}.
- ID:
- ivo://CDS.VizieR/J/MNRAS/467/1414
- Title:
- Radial velocity changes for 439 white dwarfs
- Short Name:
- J/MNRAS/467/1414
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- From a sample of spectra of 439 white dwarfs (WDs) from the ESO-VLT Supernova-Ia Progenitor Survey (SPY), we measure the maximal changes in radial velocity ({Delta}RVmax) between epochs (generally two epochs, separated by up to 470d), and model the observed {Delta}RVmax statistics via Monte Carlo simulations, to constrain the population characteristics of double WDs (DWDs). The DWD fraction among WDs is f_bin_=0.10+/-0.02 (1{sigma}, random) +0.02 (systematic), in the separation range <~4au within which the data are sensitive to binarity. Assuming the distribution of binary separation, a, is a power law, dN/da{prop.to}a^alpha^, at the end of the last common-envelope phase and the start of solely gravitational-wave-driven binary evolution, the constraint by the data is alpha=-1.3+/-0.2(1{sigma}) +/-0.2 (systematic). If these parameters extend to small separations, the implied Galactic WD merger rate per unit stellar mass is R_merge_=(1-80)x10^-13^yr^-1^M_[sun}_^-1^ (2{sigma}), with a likelihood-weighted mean of R_merge_=(7+/-2)x10^-13^yr^-1^M_{sun}_^-1^ (1{sigma}). The Milky Way's specific Type Ia supernova (SN Ia) rate is likely R_Ia_~=1.1x10^-13^yr^-1^M_{sun}_^-1^ and therefore, in terms of rates, a possibly small fraction of all merging DWDs (e.g. those with massive-enough primary WDs) could suffice to produce most or all SNe Ia.
- ID:
- ivo://CDS.VizieR/J/AJ/148/118
- Title:
- Radial velocity curves of LMC ellipsoidal variables
- Short Name:
- J/AJ/148/118
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Ellipsoidal red giant binaries are close binary systems where an unseen, relatively close companion distorts the red giant, leading to light variations as the red giant moves around its orbit. These binaries are likely to be the immediate evolutionary precursors of close binary planetary nebula and post-asymptotic giant branch and post-red giant branch stars. Due to the MACHO and OGLE photometric monitoring projects, the light variability nature of these ellipsoidal variables has been well studied. However, due to the lack of radial velocity curves, the nature of their masses, separations, and other orbital details has so far remained largely unknown. In order to improve this situation, we have carried out spectral monitoring observations of a large sample of 80 ellipsoidal variables in the Large Magellanic Cloud and we have derived radial velocity curves. At least 12 radial velocity points with good quality were obtained for most of the ellipsoidal variables. The radial velocity data are provided with this paper. Combining the photometric and radial velocity data, we present some statistical results related to the binary properties of these ellipsoidal variables.