- ID:
- ivo://CDS.VizieR/J/AJ/153/208
- Title:
- LCES HIRES/Keck radial velocity Exoplanet Survey
- Short Name:
- J/AJ/153/208
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We describe a 20 year survey carried out by the Lick-Carnegie Exoplanet Survey Team (LCES), using precision radial velocities from HIRES on the Keck I telescope to find and characterize extrasolar planetary systems orbiting nearby F, G, K, and M dwarf stars. We provide here 60949 precision radial velocities for 1624 stars contained in that survey. We tabulate a list of 357 significant periodic signals that are of constant period and phase, and not coincident in period and/or phase with stellar activity indices. These signals are thus strongly suggestive of barycentric reflex motion of the star induced by one or more candidate exoplanets in Keplerian motion about the host star. Of these signals, 225 have already been published as planet claims, 60 are classified as significant unpublished planet candidates that await photometric follow-up to rule out activity-related causes, and 54 are also unpublished, but are classified as "significant" signals that require confirmation by additional data before rising to classification as planet candidates. Of particular interest is our detection of a candidate planet with Msin(i)=3.8M_{Earth}_, and P=9.9 days orbiting Lalande 21185, the fourth-closest main-sequence star to the Sun. For each of our exoplanetary candidate signals, we provide the period and semi-amplitude of the Keplerian orbital fit, and a likelihood ratio estimate of its statistical significance. We also tabulate 18 Keplerian-like signals that we classify as likely arising from stellar activity.
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/562/A92
- Title:
- Li abundance in solar analogues
- Short Name:
- J/A+A/562/A92
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We want to study the effects of the formation of planets and planetary systems on the atmospheric Li abundance of planet host stars. In this work we present new determinations of lithium abundances for 326 main sequence stars with and without planets in the Teff range 5600-5900K. The 277 stars come from the HARPS sample, the remaining targets were observed with a variety of high-resolution spectrographs.
- ID:
- ivo://CDS.VizieR/J/MNRAS/403/1368
- Title:
- Li abundances & vsini for star-planet systems
- Short Name:
- J/MNRAS/403/1368
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We determine Li abundances and vsini values from new spectra of 53 stars with Doppler-detected planets not included in our previous papers in this series. We also examine two sets of stars without detected planets, which together serve as our comparison sample. Using the method of comparison of Li abundances and vsini values between two sets of stars we introduced in Gonzalez, we confirm that these two quantities are smaller among stars with planets (SWPs) compared to stars without detected planets near the solar temperature. The transition from low to high Li abundance among SWPs occurs near 5850K, a revision of about 50K from our previous determination. The transition from low to high vsini occurs near 6000K, but this temperature is not as well constrained.
- ID:
- ivo://CDS.VizieR/J/A+A/511/A3
- Title:
- Light curves of CoRoT-2 in z-band, 4.5um and 8um
- Short Name:
- J/A+A/511/A3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8um with the Spitzer Infrared Array Camera (IRAC). Our measured occultation depths are 0.510+/-0.042% at 4.5 and 0.41+/-0.11% at 8um. In addition to the CoRoT optical measurements, these planet/star flux ratios indicate a poor heat distribution on the night side of the planet and agree better with an atmosphere free of temperature inversion layer. Still, such an inversion is not definitely ruled out by the observations and a larger wavelength coverage is required to remove the current ambiguity. Our global analysis of CoRoT, Spitzer, and ground-based data confirms the high mass and large size of the planet with slightly revised values (M_p_=3.47+/-0.22M_J_, R_p_=1.466+/-0.044 R_J_). We find a small but significant offset in the timing of the occultation when compared to a purely circular orbital solution, leading to e*cos(omega)=-0.00291+/-0.00063 where e is the orbital eccentricity and omega is the argument of periastron. Constraining the age of the system to at most a few hundred Myr and assuming that the non-zero orbital eccentricity does not come from a third undetected body, we modeled the coupled orbital-tidal evolution of the system with various tidal Q values, core sizes, and initial orbital parameters. For Q_s'_=10^5^-10^6^, our modeling is able to explain the large radius of CoRoT-2b if Q_p'_<=10^5.5^ through a transient tidal circularization and corresponding planet tidal heating event. Under this model, the planet will reach its Roche limit within 20Myr at most.
- ID:
- ivo://CDS.VizieR/J/A+A/559/A32
- Title:
- Light curves of GJ3470b
- Short Name:
- J/A+A/559/A32
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- GJ3470b is a rare example of a "hot Uranus" transiting exoplanet orbiting a nearby M1.5 dwarf. It is crucial for atmospheric studies because it is one of the most inflated low-mass planets known, bridging the boundary between "super-Earths" and Neptunian planets. We present two new ground-based light curves of GJ3470b gathered by the LBC camera at the Large Binocular Telescope. Simultaneous photometry in the ultraviolet ({lambda}_c_=357.5nm) and optical infrared ({lambda}_c_=963.5nm) allowed us to detect a significant change in the effective radius of GJ3470b as a function of wavelength. This can be interpreted as a signature of scattering processes occurring in the planetary atmosphere, which should be cloud-free and with a low mean molecular weight. The unprecedented accuracy of our measurements demonstrates that the photometric detection of Earth-sized planets around M dwarfs is achievable using 8-10m size ground-based telescopes. We provide updated planetary parameters and a greatly improved orbital ephemeris for any forthcoming study of this planet.
- ID:
- ivo://CDS.VizieR/J/A+A/551/A11
- Title:
- Light curves of HAT-P-8
- Short Name:
- J/A+A/551/A11
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The extrasolar planet HAT-P-8 b was thought to be one of the more inflated transiting hot Jupiters. Aims. By using new and existing photometric data, we computed precise estimates of the physical properties of the system. Methods. We present photometric observations comprising eleven light curves covering six transit events, obtained using five medium-class telescopes and telescope-defocussing technique. One transit was simultaneously obtained through four optical filters, and two transits were followed contemporaneously from two observatories. We modelled these and seven published datasets using the jktebop code. The physical parameters of the system were obtained from these results and from published spectroscopic measurements. In addition, we investigated the theoretically-predicted variation of the apparent planetary radius as a function of wavelength, covering the range 330-960nm. Results. We find that HAT-P-8 b has a significantly lower radius (1.321R_Jup_) and mass (1.275M_Jup_) compared to previous estimates (1.50R_Jup_ and 1.52M_Jup_ respectively). We also detect a radius variation in the optical bands that, when compared with synthetic spectra of the planet, may indicate the presence of a strong optical absorber, perhaps TiO and VO gases, near the terminator of HAT-P-8 b. Conclusions. These new results imply that HAT-P-8 b is not significantly inflated, and that its position in the planetary mass-radius diagram is congruent with those of many other transiting extrasolar planets.
- ID:
- ivo://CDS.VizieR/J/A+A/532/A24
- Title:
- Light curves of HAT-P-13b
- Short Name:
- J/A+A/532/A24
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- TASTE (The Asiago Search for Transit timing variations of Exoplanets) project is collecting high-precision, short-cadence light curves for a selected sample of transiting exoplanets. It has been claimed that the hot jupiter HAT-P-13b suddenly deviated from a linear ephemeris by ~20min, implying that there is a perturber in the system. Using five new transits, we discuss the plausibility of this transit time variation (TTV), and show that a periodic signal should not be excluded. More follow-up observations are required to constrain the mass and the orbit of the hypothetical perturber.
- ID:
- ivo://CDS.VizieR/J/A+A/527/A85
- Title:
- Light curves of HAT-P-3b and HAT-P-14b
- Short Name:
- J/A+A/527/A85
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A promising method for detecting earth-sized exoplanets is the timing analysis of a known transit. The technique allows a search for variations in either the transit duration or the center induced by the perturbation of a third body, e.g. a second planet or an exomoon. By applying this method, the TASTE (The Asiago Search for Transit Timing variations of Exoplanets) project will collect high- precision, short-cadence light curves for a selected sample of transits by using imaging differential photometry at the Asiago 1.82m telescope. The first light curves show that our project can achieve a competitive timing accuracy, as well as a significant improvement of the orbital parameters. We derived refined ephemerides for HAT-P-3b and HAT-P-14b with a timing accuracy of 11 and 25s, respectively.
- ID:
- ivo://CDS.VizieR/J/ApJ/754/136
- Title:
- Light curves of HD 149026b in 3.6-16um
- Short Name:
- J/ApJ/754/136
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The dayside of HD 149026b is near the edge of detectability by the Spitzer Space Telescope. We report on 11 secondary-eclipse events at 3.6, 4.5, 3x5.8, 4x8.0, and 2x16{mu}m plus three primary-transit events at 8.0{mu}m. The eclipse depths from jointly fit models at each wavelength are 0.040%+/-0.003% at 3.6{mu}m, 0.034%+/-0.006% at 4.5{mu}m, 0.044%+/-0.010% at 5.8{mu}m, 0.052%+/-0.006% at 8.0{mu}m, and 0.085%+/-0.032% at 16{mu}m. Multiple observations at the longer wavelengths improved eclipse-depth signal-to-noise ratios by up to a factor of two and improved estimates of the planet-to-star radius ratio (R_p_/R_{sstarf}_=0.0518+/-0.0006). We also identify no significant deviations from a circular orbit and, using this model, report an improved period of 2.8758916+/-0.0000014 days. Chemical-equilibrium models find no indication of a temperature inversion in the dayside atmosphere of HD 149026b. Our best-fit model favors large amounts of CO and CO_2_, moderate heat redistribution (f=0.5), and a strongly enhanced metallicity. These analyses use BiLinearly-Interpolated Subpixel Sensitivity (BLISS) mapping, a new technique to model two position-dependent systematics (intrapixel variability and pixelation) by mapping the pixel surface at high resolution. BLISS mapping outperforms previous methods in both speed and goodness of fit. We also present an orthogonalization technique for linearly correlated parameters that accelerates the convergence of Markov chains that employ the Metropolis random walk sampler.
- ID:
- ivo://CDS.VizieR/J/ApJ/741/102
- Title:
- 21 light curves of OGLE-TR-56b
- Short Name:
- J/ApJ/741/102
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Although OGLE-TR-56b was the second transiting exoplanet discovered, only one light curve, observed in 2006, has been published besides the discovery data. We present 21 light curves of 19 different transits observed between 2003 July and 2009 July with the Magellan Telescopes and Gemini South. The combined analysis of the new light curves confirms a slightly inflated planetary radius relative to model predictions, with R_p_=1.378+/-0.090R_J_. However, the values found for the transit duration, semimajor axis, and inclination values differ significantly from the previous result, likely due to systematic errors. The new semimajor axis and inclination, a=0.01942+/-0.00015AU and i=73.72+/-0.18{deg}, are smaller than previously reported, while the total duration, T_14_=7931+/-38s, is 18 minutes longer. The transit midtimes have errors from 23s to several minutes, and no evidence is seen for transit midtime or duration variations. Similarly, no change is seen in the orbital period, implying a nominal stellar tidal decay factor of Q_*_=10^7^, with a 3{sigma} lower limit of 10^5.7^.