- ID:
- ivo://CDS.VizieR/J/A+A/506/303
- Title:
- CoRoT-7 radial velocities
- Short Name:
- J/A+A/506/303
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on an intensive observational campaign carried out with HARPS at the 3.6m telescope at La Silla on the star CoRoT-7. Additional simultaneous photometric measurements carried out with the Euler Swiss telescope have demonstrated that the observed radial velocity variations are dominated by rotational modulation from cool spots on the stellar surface. Several approaches were used to extract the radial velocity signal of the planet(s) from the stellar activity signal.
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- ID:
- ivo://CDS.VizieR/J/A+A/603/A43
- Title:
- CoRoT-9 radial velocity curve
- Short Name:
- J/A+A/603/A43
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- CoRoT-9b is one of the rare long-period (P=95.3days) transiting giant planets with a measured mass known to date. We present a new analysis of the CoRoT-9 system based on five years of radial-velocity (RV) monitoring with HARPS and three new space-based transits observed with CoRoT and Spitzer. Combining our new data with already published measurements we redetermine the CoRoT-9 system parameters and find good agreement with the published values. We uncover a higher significance for the small but non-zero eccentricity of CoRoT-9b (e=0.133^+0.042^_-0.037_) and find no evidence for additional planets in the system. We use simulations of planet-planet scattering to show that the eccentricity of CoRoT-9b may have been generated by an instability in which a ~50M_{earth}_ planet was ejected from the system. This scattering would not have produced a spin-orbit misalignment, so we predict that the CoRoT-9b orbit should lie within a few degrees of the initial plane of the protoplanetary disk. As a consequence, any significant stellar obliquity would indicate that the disk was primordially tilted.
- ID:
- ivo://CDS.VizieR/J/AJ/146/113
- Title:
- Differential griz photometry of HATS-3
- Short Name:
- J/AJ/146/113
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery by the HATSouth survey of HATS-3b, a transiting extrasolar planet orbiting a V=12.4 F dwarf star. HATS-3b has a period of P=3.5479days, mass of M_p_=1.07M_J_, and radius of R_p_=1.38R _J_. Given the radius of the planet, the brightness of the host star, and the stellar rotational velocity (vsini=9.0km/s), this system will make an interesting target for future observations to measure the Rossiter-McLaughlin effect and determine its spin-orbit alignment. We detail the low-/medium-resolution reconnaissance spectroscopy that we are now using to deal with large numbers of transiting planet candidates produced by the HATSouth survey. We show that this important step in discovering planets produces logg and T_eff_ parameters at a precision suitable for efficient candidate vetting, as well as efficiently identifying stellar mass eclipsing binaries with radial velocity semi-amplitudes as low as 1km/s.
- ID:
- ivo://CDS.VizieR/J/AJ/147/144
- Title:
- Differential griz photometry of HATS-5
- Short Name:
- J/AJ/147/144
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of HATS-5b, a transiting hot Saturn orbiting a G-type star, by the HATSouth survey. HATS-5b has a mass of M_p_{approx}0.24M_J_, radius of R_p_{approx}0.91R_J_, and transits its host star with a period of P{approx}4.7634days. The radius of HATS-5b is consistent with both theoretical and empirical models. The host star has a V-band magnitude of 12.6, mass of 0.94M_{sun}_, and radius of 0.87R_{sun}_. The relatively high scale height of HATS-5b and the bright, photometrically quiet host star make this planet a favorable target for future transmission spectroscopy follow-up observations. We reexamine the correlations in radius, equilibrium temperature, and metallicity of the close-in gas giants and find hot Jupiter-mass planets to exhibit the strongest dependence between radius and equilibrium temperature. We find no significant dependence in radius and metallicity for the close-in gas giant population.
- ID:
- ivo://CDS.VizieR/J/A+A/501/785
- Title:
- Discovery and characterization of WASP-6b
- Short Name:
- J/A+A/501/785
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of WASP-6b, an inflated sub-Jupiter mass planet transiting every 3.3610060^+0.0000022^_-0.0000035_days a mildly metal-poor solar-type star of magnitude V=11.9. A combined analysis of the WASP photometry, high-precision followup transit photometry and radial velocities yield a planetary mass M_p_=0.503^+0.019^_-0.038_ and radius R_p_=1.224^+0.051^_0.052_, resulting in a density {rho}_p_=0.27{+/-}0.05{rho}_J_. The mass and radius for the host star are M_*_=0.88^+0.05^-0.08_M_{sun}_ and R_*_=0.870^0.025^_-0.036_R_{sun}_. The non-zero orbital eccentricity e=0.054^+0.018^_-0.015_ that we measure suggests that the planet underwent a massive tidal heating ~1Gyr ago that could have contributed to its inflated radius. High-precision radial velocities obtained during a transit allow us to measure a sky-projected angle between the stellar spin and orbital axis {beta}=11^+14^_-18_{deg}. In addition to similar published measurements, this result favors a dominant migration mechanism based on tidal interactions with a protoplanetary disk.
- ID:
- ivo://CDS.VizieR/J/A+A/410/1051
- Title:
- ELODIE survey for northern extra-solar planets. II.
- Short Name:
- J/A+A/410/1051
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Here are the 69 radial-velocity measurements of GJ 777A (HD 190360) used for deriving the orbital solution of this star. These velocities were obtained using the ELODIE echelle spectrograph mounted on the 1.93-m Telescope at Observatoire de Haute-Provence (France) and the AFOE spectrograph mounted on the 1.5-m Telescope at the Fred Lawrence Whipple Observatory (USA).
- ID:
- ivo://CDS.VizieR/J/A+A/414/351
- Title:
- ELODIE survey for northern extrasolar planets III
- Short Name:
- J/A+A/414/351
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present here the radial-velocity measurements for 9 solar-type stars: Ups And (HD 9826), HD 74156, 55 Cnc (HD 75732), 47 UMa (HD 95128), 70 Vir (HD 117176), 14 Her (HD 145675), HD 187123, HD 209458 and 51 Peg (HD 217014). These velocities were obtained using the ELODIE echelle spectrograph mounted on the 1.93-m telescope at the Observatoire de Haute-Provence (France) and the CORALIE echelle spectrograph mounted on the 1.2-m Euler Swiss telescope at the ESO-La Silla Observatory (Chile).
- ID:
- ivo://CDS.VizieR/J/A+A/546/A5
- Title:
- eps CrB radial velocity curve
- Short Name:
- J/A+A/546/A5
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Our aim is to search for and study the origin of the low-amplitude and long-periodic radial velocity (RV) variations in K giants. We present high-resolution RV measurements of K2 giant epsilon CrB from February 2005 to January 2012 using the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at the Bohyunsan Optical Astronomy Observatory (BOAO). We find that the RV measurements for epsilon CrB exhibit a periodic variation of 417.9+/-0.5days with a semi-amplitude of 129.4+/-2.0m/s. There is no correlation between RV measurements and chromospheric activity in the Ca II H region, the Hipparcos photometry, or bisector velocity span. Keplerian motion is the most likely explanation, with the RV variations arising from an orbital motion. Assuming a possible stellar mass of 1.7+/-0.1M_{sun}_ for epsilon CrB, we obtain a minimum mass for the planetary companion of 6.7+/-0.3M_Jup_ with an orbital semi-major axis of 1.3AU and eccentricity of 0.11. We also discuss the implications of our observations for stellar metallicity versus planet occurrence rate and stellar mass versus planetary mass relations.
- ID:
- ivo://CDS.VizieR/J/A+A/613/A41
- Title:
- 5 exoplanet light and RV curves
- Short Name:
- J/A+A/613/A41
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The measurement of the orbital obliquity of hot Jupiters, with different physical characteristics, can provide clues to the mechanisms of migration and orbital evolution of this particular class of giant exoplanets. We aim to derive the degree of alignment between planetary orbit and stellar spin angular momentum vectors and look for possible links with other orbital and fundamental physical parameters of the star-planet system. Here we focus on the characterisation of five transiting planetary systems (HAT-P-3, HAT-P-12, HAT-P-22, WASP-39 and WASP-60) and the determination of their sky-projected planet orbital obliquity through the measurement of the Rossiter-McLaughlin effect. We used HARPS-N high-precision radial velocity measurements, gathered during transit events, to measure the Rossiter-McLaughlin effect in the target systems and determine the sky-projected angle between the planetary orbital plane and the stellar equator. The characterisation of stellar atmospheric parameters was performed exploiting the HARPS-N spectra, using line equivalent width ratios, and spectral synthesis methods. Photometric parameters of the five transiting exoplanets were re-analysed through 17 new light curves, obtained with an array of medium-class telescopes, and other light curves from the literature. Survey-time-series photometric data were analysed for determining the rotation periods of the five stars and their spin inclination. From the analysis of the Rossiter-McLaughlin effect we derived a sky-projected obliquity of {lambda}=21.2+/-8.7{deg}, {lambda=-54^+41^_-13_{deg}, {lambda=-2.1+/-3.0{deg}, lambda=0+/-11{deg} and lambda=-129+/-17{deg} for HAT-P-3 b, HAT-P-12 b, HAT-P-22 b, WASP-39 b and WASP-60 b, respectively. The latter value indicates that WASP-60 b is moving on a retrograde orbit. These values represent the first measurements of {lambda} for the five exoplanetary systems under study. The stellar activity of HAT-P-22 indicates a rotation period of 28.7+/-0.4-days, which allowed us to estimate the true misalignment angle of HAT-P-22 b, {psi}=24+/-18{deg}. The revision of the physical parameters of the five exoplanetary systems returned values fully compatible with those existing in the literature, with the exception of the WASP-60 system, for which, based on higher quality spectroscopic and photometric data, we found a more massive and younger star, and a larger and hotter planet.
- ID:
- ivo://CDS.VizieR/J/A+A/559/A36
- Title:
- Exoplanets WASP-65b and WASP-75b
- Short Name:
- J/A+A/559/A36
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present two newly discovered hot Jupiters from the WASP transit survey. WASP-65b (M_pl_=1.55+/-0.16M_J_; R_pl_=1.11+/-0.06R_J_), and WASP-75b (M_pl_=1.07+/-0.05M_J_; R_pl_=1.27+/-0.05R_J_). They orbit their host star every 2.311, and 2.484 days, respectively. WASP-65b is one of the densest known exoplanets in the mass range 0.1 and 2.0M_J_, and is one of only a handful of planets with masses of around 1.5M_J_. The radius of WASP-75b is slightly inflated (~<10%) as compared to theoretical planet models with no core. We present the Radial Velocity measurements, the WASP light curves, and the high-precision light curves for the transiting planetary systems WASP-65, and WASP-75.