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8141. WASP-74 griz_s_ light curves
ID:
ivo://CDS.VizieR/J/A+A/642/A50
Title:
WASP-74 griz_s_ light curves
Short Name:
J/A+A/642/A50
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present new transit observations of the hot Jupiter WASP-74 b (Teq~1860K) using the high-resolution spectrograph HARPS-N and the multi-colour simultaneous imager MuSCAT2. We refined the orbital properties of the planet and its host star and measured its obliquity for the first time. The measured sky-projected angle between the stellar spin-axis and the orbital axis of the planet is compatible with an orbit that is well-aligned with the equator of the host star ({lambda}=0.77+/-0.99{deg}). We are not able to detect any absorption feature of H{alpha} or any other atomic spectral features in the high-resolution transmission spectra of this source owing to low S/N at the line cores. Despite previous claims regarding the presence of strong optical absorbers such as TiO and VO gases in the atmosphere of WASP-74 b, new ground-based photometry combined with a reanalysis of previously reported observations from the literature show a slope in the low-resolution transmission spectrum that is steeper than expected from Rayleigh scattering alone.
8142. WASP-148 Ground-based Photometric Observations
ID:
ivo://CDS.VizieR/J/AcA/70/203
Title:
WASP-148 Ground-based Photometric Observations
Short Name:
J/AcA/70/203
Date:
21 Oct 2021
Publisher:
CDS
Description:
The WASP-148 planetary system has a rare architecture with a transiting Saturn-mass planet on a tight orbit which is accompanied by a slightly more massive planet on a nearby outer orbit. Using new space-born photometry and ground-based follow-up transit observations and data available in literature, we performed modeling that accounts for gravitational interactions between both planets. Thanks to the new transit timing data for planet b, uncertainties of orbital periods and eccentricities for both planets were reduced relative to previously published values by a factor of 3-4. Variation in transit timing has an amplitude of about 20 min and can be easily followed-up with a 1-m class telescopes from the ground. An approximated transit ephemeris, which accounts for gravitational interactions with an accuracy up to 5 min, is provided. No signature of transits was found for planet c down to the Neptune-size regime. No other transiting companions were found down to a size of about 2.4 Earth radii for interior orbits. We notice, however, that the regime of terrestrial-size planets still remains unexplored in that system.
8143. WASP-80 photometric and radial velocity data
ID:
ivo://CDS.VizieR/J/A+A/551/A80
Title:
WASP-80 photometric and radial velocity data
Short Name:
J/A+A/551/A80
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of a planet transiting the star WASP-80 (1SWASP J201240.26-020838.2; 2MASS J20124017-0208391; TYC 5165-481-1; BPM 80815; V=11.9, K=8.4). Our analysis shows this is a 0.55+/-0.04M_jup_, 0.95+/-0.03R_jup_ gas giant on a circular 3.07 day orbit around a star with a spectral type between K7V and M0V. This system produces one of the largest transit depths so far reported, making it a worthwhile target for transmission spectroscopy. We find a large discrepancy between the vsini* inferred from stellar line broadening and the observed amplitude of the Rossiter-McLaughlin effect. This can be understood either by an orbital plane nearly perpendicular to the stellar spin or by an additional, unaccounted for source of broadening.
8144. WASP-23 photometric and radial velocity data
ID:
ivo://CDS.VizieR/J/A+A/531/A24
Title:
WASP-23 photometric and radial velocity data
Short Name:
J/A+A/531/A24
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of a new transiting planet in the southern hemisphere. It was found by the WASP-south transit survey and confirmed photometrically and spectroscopically by the 1.2m Swiss Euler telescope, LCOGT 2m Faulkes South Telescope, the 60cm TRAPPIST telescope, and the ESO 3.6m telescope. The orbital period of the planet is 2.94 days. We find that it is a gas giant with a mass of 0.88+/-0.10M_J_ and an estimated radius of 0.96+/-0.05R_J_. We obtained spectra during transit with the HARPS spectrograph and detect the Rossiter-McLaughlin effect despite its small amplitude.
8145. WASP-18 Photometric timeseries and timing data
ID:
ivo://CDS.VizieR/J/AcA/70/1
Title:
WASP-18 Photometric timeseries and timing data
Short Name:
J/AcA/70/1
Date:
21 Oct 2021
Publisher:
CDS
Description:
From its discovery, the WASP-18 system with its massive transiting planet on a tight orbit was identified as a unique laboratory for studies on tidal planet-star interactions. In an analysis of Doppler data, which include five new measurements obtained with the HIRES/Keck-I instrument between 2012 and 2018, we show that the radial velocity signal of the photosphere following the planetary tidal potential can be distilled for the host star. Its amplitude is in agreement with both theoretical predictions of the equilibrium tide approximation and an ellipsoidal modulation observed in an orbital phase curve. Assuming a circular orbit, we refine system parameters using photometric time series from TESS. With a new ground-based photometric observation, we extend the span of transit timing observations to 28 years in order to probe the rate of the orbital period shortening. Since we found no departure from a constant-period model, we conclude that the modified tidal quality parameter of the host star must be greater than 3.9e6 with 95% confidence. This result is in line with conclusions drawn from studies of the population of hot Jupiters, predicting that the efficiency of tidal dissipation is 1 or 2 orders of magnitude weaker. As the WASP-18 system is one of the prime candidates for detection of orbital decay, further timing observations are expected to push the boundaries of our knowledge on stellar interiors.
8146. WASP-12 transit light curves
ID:
ivo://CDS.VizieR/J/A+A/588/L6
Title:
WASP-12 transit light curves
Short Name:
J/A+A/588/L6
Date:
21 Oct 2021
Publisher:
CDS
Description:
Most hot Jupiters are expected to spiral in toward their host stars because the angular momentum of the orbital motion is transferred to the stellar spin. Their orbits can also precess as a result of planet-star interactions. Calculations show that both effects might be detected for the very-hot exoplanet WASP-12 b using the method of precise transit-timing over a time span of about 10yr. We acquired new precise light curves for 29 transits of WASP-12 b, spanning four observing seasons from November 2012 to February 2016. New mid-transit times, together with those from the literature, were used to refine the transit ephemeris and analyze the timing residuals. We find that the transit times of WASP-12 b do not follow a linear ephemeris with a 5-{sigma} confidence level. They may be approximated with a quadratic ephemeris that gives a change rate in the orbital period of (-2.56+/-0.40)x10^-2^s/yr. The tidal quality parameter of the host star was found to be equal to 2.5x10^5^, which is similar to theoretical predictions for Sun-like stars. We also considered a model in which the observed timing residuals are interpreted as a result of the apsidal precession. We find, however, that this model is statistically less probable than the orbital decay.
8147. WASP-22, WASP-41, WASP-42, WASP-55
ID:
ivo://CDS.VizieR/J/MNRAS/457/4205
Title:
WASP-22, WASP-41, WASP-42, WASP-55
Short Name:
J/MNRAS/457/4205
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present 13 high-precision and four additional light curves of four bright southern-hemisphere transiting planetary systems: WASP-22, WASP-41, WASP-42 and WASP-55. In the cases of WASP-42 and WASP-55, these are the first follow-up observations since their discovery papers. We present refined measurements of the physical properties and orbital ephemerides of all four systems. No indications of transit timing variations were seen. All four planets have radii inflated above those expected from theoretical models of gas-giant planets; WASP-55 b is the most discrepant with a mass of 0.63M_Jup_ and a radius of 1.34R_Jup_. WASP-41 shows brightness anomalies during transit due to the planet occulting spots on the stellar surface. Two anomalies observed 3.1d apart are very likely due to the same spot. We measure its change in position and determine a rotation period for the host star of 18.6+/-1.5d, in good agreement with a published measurement from spot-induced brightness modulation, and a sky-projected orbital obliquity of {lambda}=6+/-11{deg}. We conclude with a compilation of obliquity measurements from spot-tracking analyses and a discussion of this technique in the study of the orbital configurations of hot Jupiters.
8148. WD+dMs from the SUPERBLINK proper motion survey
ID:
ivo://CDS.VizieR/J/AJ/154/118
Title:
WD+dMs from the SUPERBLINK proper motion survey
Short Name:
J/AJ/154/118
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present an activity and kinematic analysis of high proper motion white dwarf-M dwarf binaries (WD+dMs) found in the SUPERBLINK survey, 178 of which are new identifications. To identify WD+dMs, we developed a UV-optical-IR color criterion and conducted a spectroscopic survey to confirm each candidate binary. For the newly identified systems, we fit the two components using model white dwarf spectra and M dwarf template spectra to determine physical parameters. We use H{alpha} chromospheric emission to examine the magnetic activity of the M dwarf in each system, and investigate how its activity is affected by the presence of a white dwarf companion. We find that the fraction of WD+dM binaries with active M dwarfs is significantly higher than their single M dwarf counterparts at early and mid-spectral types. We corroborate previous studies that find high activity fractions at both close and intermediate separations. At more distant separations, the binary fraction appears to approach the activity fraction for single M dwarfs. Using derived radial velocities and the proper motions, we calculate 3D space velocities for the WD+dMs in SUPERBLINK. For the entire SUPERBLINK WD+dMs, we find a large vertical velocity dispersion, indicating a dynamically hotter population compared to high proper motion samples of single M dwarfs. We compare the kinematics for systems with active M dwarfs and those with inactive M dwarfs, and find signatures of asymmetric drift in the inactive sample, indicating that they are drawn from an older population.
8149. WD luminosity functions from the PS1 3pi Survey
ID:
ivo://CDS.VizieR/J/MNRAS/482/715
Title:
WD luminosity functions from the PS1 3pi Survey
Short Name:
J/MNRAS/482/715
Date:
21 Oct 2021
Publisher:
CDS
Description:
A large sample of white dwarfs is selected by both proper motion and colours from the Pan-STARRS 1 3{pi} Steradian Survey Processing Version 2 to construct the white dwarf luminosity functions of the discs and halo in the solar neighbourhood. Four-parameter astrometric solutions were recomputed from the epoch data. The generalized maximum volume method is then used to calculate the density of the populations. After removal of crowded areas near the Galactic plane and centre, the final sky area used by this work is 7.833sr, which is 83 per cent of the 3{pi} sky and 62 per cent of the whole sky. By dividing the sky using Voronoi tessellation, photometric and astrometric uncertainties are recomputed at each step of the integration to improve the accuracy of the maximum volume. Interstellar reddening is considered throughout the work. We find a disc-to-halo white dwarf ratio of about 100.
8150. WeCAPP Survey. M31 variables
ID:
ivo://CDS.VizieR/J/A+A/445/423
Title:
WeCAPP Survey. M31 variables
Short Name:
J/A+A/445/423
Date:
21 Oct 2021
Publisher:
CDS
Description:
The observations in the WeCAPP microlensing survey towards the Andromeda galaxy (M31) for a period of three years (2000-2003) resulted in a database with unprecedented time coverage for an extragalactic variable star study. We have monitored a 16.1' x 16.6' field centered on the nucleus of M31 in two optical bands (R and I) using the 0.8-m telescope at Wendelstein, Germany and the 1.2-m telescope at Calar Alto, Spain. Using the difference imaging method we detected 23781 variable sources for which we calculated the periods and variation amplitudes. We classified the variables according to their position in the R-band period-amplitude plane. Three groups can be distinguished; while the first two groups can be mainly associated with Cepheid-like variables (population I Cepheids in group I; type II Cepheids and RV Tauri stars in group II), the third one consists of Long Period Variables (LPVs). We detected 37 RV Tauri stars and 11 RV Tauri candidates, which makes this catalogue one of the largest collections of this class of stars to date. The classification scheme is supported by Fourier decomposition of the light curves. The catalogue of variable stars contains the positions, the periods in R and I, the significance of the assigned periods, and the variation amplitudes in the R and I bands.