- ID:
- ivo://CDS.VizieR/J/AJ/129/1001
- Title:
- Radial velocities of HD 166181
- Short Name:
- J/AJ/129/1001
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have obtained extensive spectroscopic and velocity spectrometer observations of HD166181, a previously known single-lined spectroscopic binary. Our improved orbit for the G6 V primary has a period of 1.8098343days and is circular. Although the lines of additional components have not been detected, radial velocity measurements confirm that the system has additional velocity variations with a period of 2092days, or 5.73yr. This long-period orbit has an eccentricity of 0.76. An analysis of the Hipparcos observations produces a well-determined astrometric orbit for the long-period system that has an inclination of 78{deg}. Mass estimates of the components in this zero-age main-sequence multiple system indicate that the unseen secondary in the 5.73yr orbit may also be a binary. Thus, HD 166181 is at least a triple system and possibly quadruple.
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- ID:
- ivo://CDS.VizieR/J/A+A/470/1009
- Title:
- Radial velocities of HD 209625
- Short Name:
- J/A+A/470/1009
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The goal is to test the structure of hot metallic stars, and in particular the structure of a near-surface convection zone using asteroseismic measurements. Indeed, stellar models including a detailed treatment of the radiative diffusion predict the existence of a near-surface convection zone in order to correctly reproduce the anomalies in surface abundances that are observed in Am stars. The Am star HD 209625 was observed with the Harps spectrograph mounted on the 3.6-m telescope at the ESO La Silla Observatory (Chile) during 9 nights in August 2005. This observing run allowed to collect 1243 radial velocity measurements, with a standard deviation of 1.35m/s. The power spectrum associated with these RV measurements does not present any excess. Therefore, either the structure of the external layers of this star does not enable to excite solar-like oscillations, or the amplitudes of the oscillations remains below 20-30cm/s (depending of their frequency range).
- ID:
- ivo://CDS.VizieR/J/A+A/491/883
- Title:
- Radial velocities of HD 60532
- Short Name:
- J/A+A/491/883
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In the framework of the search for extrasolar planets and brown dwarfs around early-type stars, we present the results obtained for the F-type main-sequence star HD 60532 (F6V) with HARPS. Using 147 spectra obtained with HARPS at La Silla on a time baseline of two years, we studied the radial velocities of this star. HD 60532 radial velocities are periodically variable, and the variations have a Keplerian origin. This star is surrounded by a planetary system of two planets with minimum masses of 1 and 2.5M_{Jup}_ and orbital separations of 0.76 and 1.58AU, respectively. We also detect high-frequency, small- amplitude (10m/s peak-to-peak) pulsations. Dynamical studies of the system point toward a possible 3:1 mean-motion resonance that should be confirmed within the next decade.
- ID:
- ivo://CDS.VizieR/J/A+A/566/A35
- Title:
- Radial velocities of HD 41248
- Short Name:
- J/A+A/566/A35
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The search for planets orbiting metal-poor stars is of uttermost importance for our understanding of the planet formation models. However, no dedicated searches have been conducted so far for very low mass planets orbiting such objects. Only a few cases of low mass planets orbiting metal-poor stars are thus known. Amongst these, HD 41248 is a metal-poor, solar-type star on which a resonant pair of super-Earth like planets has been announced. This detection was based on 62 radial velocity measurements obtained with the HARPS spectrograph (public data). In the present paper we present a new planet search program that is using the HARPS spectrograph to search for Neptunes and Super-Earths orbiting a sample of metal-poor FGK dwarfs. We then present a detailed analysis of an additional 162 radial velocity measurements of HD 41248, obtained within this program, with the goal of confirming the existence of the proposed planetary system. We analyzed the precise radial velocities, obtained with the HARPS spectrograph, together with several stellar activity diagnostics and line profile indicators. A careful analysis shows no evidence for the planetary system previously announced. One of the signals, with a period of ~25 days, is shown to be related to the rotational period of the star, and is clearly seen in some of the activity proxies. The remaining signal (P~18 days) could not be convincingly retrieved in the new data set. We discuss possible causes for the complex (evolving) signals observed in the data of HD 41248, proposing that they may be explained by the appearance and disappearance of active regions on the surface of a star with strong differential rotation, or by a combination of the sparse data sampling and active region evolution.
- ID:
- ivo://CDS.VizieR/J/A+A/614/A133
- Title:
- Radial velocities of HD215152
- Short Name:
- J/A+A/614/A133
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of four super-earth planets around HD215152, with orbital periods of 5.76, 7.28, 10.86, and 25.2d, and minimum masses of 1.8, 1.7, 2.8, and 2.9M_Earth_ respectively. This discovery is based on 373 high quality radial velocity measurements taken by HARPS over thirteen years. Given the low masses of the planets, the S/N is not sufficient to constrain the planets eccentricities. However, a preliminary dynamical analysis suggests that eccentricities should be typically lower than about 0.03 for the system to remain stable. With two pairs of planets with a period ratio smaller than 1.5, with short orbital periods, small masses, and small eccentricities, HD215152 is similar to the very compact multi-planet systems found by Kepler, and very rare in RV surveys. This discovery proves that those systems are reachable with the RV technique, however they require a huge amount of observations to be characterized.
- ID:
- ivo://CDS.VizieR/J/A+A/406/373
- Title:
- Radial velocities of HD 192263
- Short Name:
- J/A+A/406/373
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table 1 contains the CORALIE radial-velocity measurements of HD 192263. CORALIE is a fiber-fed echelle spectrograph designed for high-precision radial-velocity measurements. It is mounted on the 1.2-m "Leonard Euler" Swiss Telescope at ESO-La Silla Observatory (Chile). Table 2 contains the results of our photometric campaign on this same star, obtained using the P7 photometer at the 1.2-m "Mercator" Belgium telescope at La Palma Observatory, spain.
- ID:
- ivo://CDS.VizieR/J/A+A/447/1159
- Title:
- Radial velocities of HD 142022
- Short Name:
- J/A+A/447/1159
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report precise Doppler measurements of HD 142022 obtained during the past six years with the CORALIE echelle spectrograph at La Silla Observatory together with a few additional observations made recently with the HARPS echelle spectrograph. Our radial velocities reveal evidence of a planetary companion with an orbital period P=1928^+53^_-39^d, an eccentricity e=0.53^+0.23^_-0.18_, and a velocity semiamplitude K=92^+102^_-29_m/s. The inferred companion minimum mass is M_2_sin{i}=5.1^+2.6^_-1.5_M_Jup_ and the semimajor axis a=3.03+/-0.05AU. Only one full orbital revolution has been monitored yet, and the periastron passage could not be observed since the star was too low on the horizon. The eccentricity and velocity semiamplitude remain therefore quite uncertain and the orbital solution is preliminary. HD 142022 is a chromospherically inactive K0 dwarf, metal rich relative to the Sun, and is the primary component of a wide binary. HD 142022b is thus a new "planet in binary" candidate, and its high eccentricity might be due to secular interactions with the distant stellar companion.
- ID:
- ivo://CDS.VizieR/J/A+A/528/A112
- Title:
- Radial velocities of HD 10180
- Short Name:
- J/A+A/528/A112
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Low-mass extrasolar planets are presently being discovered at an increased pace by radial velocity and transit surveys, which opens a new window on planetary systems. We are conducting a high-precision radial velocity survey with the HARPS spectrograph, which aims at characterizing the population of ice giants and super-Earths around nearby solar-type stars. This will lead to a better understanding of their formation and evolution, and will yield a global picture of planetary systems from gas giants down to telluric planets. Progress has been possible in this field thanks in particular to the sub-m/s radial velocity precision achieved by HARPS. We present here new high-quality measurements from this instrument. We report the discovery of a planetary system comprising at least five Neptune-like planets with minimum masses ranging from 12 to 25M_{earth}_, orbiting the solar-type star HD 10180 at separations between 0.06 and 1.4AU.
- ID:
- ivo://CDS.VizieR/J/A+A/496/521
- Title:
- Radial velocities of HD45364
- Short Name:
- J/A+A/496/521
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Precise radial-velocity measurements with the HARPS spectrograph reveal the presence of two planets orbiting the solar-type star HD 45364. The companion masses are Msini=0.187M_{Jup} and 0.658M_{Jup}, with semi-major axes of a=0.681AU and 0.897AU, and eccentricities of e=0.168 and 0.097, respectively. A dynamical analysis of the system further shows a 3:2 mean motion resonance between the two planets, which prevents close encounters and ensures the stability of the system over 5Gyr. This is the first time that such a resonant configuration has been observed for extra-solar planets, although there is an analogue in our Solar System formed by Neptune and Pluto. This singular planetary system may provide important constraints on planetary formation and migration scenarios.
- ID:
- ivo://CDS.VizieR/J/AJ/152/167
- Title:
- Radial velocities of HD 133131A and HD 133131B
- Short Name:
- J/AJ/152/167
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a new precision radial velocity (RV) data set that reveals multiple planets orbiting the stars in the ~360 au, G2+G2 "twin" binary HD133131AB. Our six years of high-resolution echelle observations from MIKE and five years from the Planet Finder Spectrograph (PFS) on the Magellan telescopes indicate the presence of two eccentric planets around HD133131A with minimum masses of 1.43+/-0.03 and 0.63+/-0.15M_J_ at 1.44+/-0.005 and 4.79+/-0.92au, respectively. Additional PFS observations of HD133131B spanning five years indicate the presence of one eccentric planet of minimum mass 2.50+/-0.05M_J_ at 6.40+/-0.59au, making it one of the longest-period planets detected with RV to date. These planets are the first to be reported primarily based on data taken with the PFS on Magellan, demonstrating the instrument's precision and the advantage of long-baseline RV observations. We perform a differential analysis between the Sun and each star, and between the stars themselves, to derive stellar parameters and measure a suite of 21 abundances across a wide range of condensation temperatures. The host stars are old (likely ~9.5Gyr) and metal-poor ([Fe/H]~-0.30), and we detect a ~0.03dex depletion in refractory elements in HD133131A versus B (with standard errors ~0.017). This detection and analysis adds to a small but growing sample of binary "twin" exoplanet host stars with precise abundances measured, and represents the most metal-poor and likely oldest in that sample. Overall, the planets around HD133131A and B fall in an unexpected regime in planet mass-host star metallicity space and will serve as an important benchmark for the study of long-period giant planets.
