- ID:
- ivo://CDS.VizieR/J/AJ/157/43
- Title:
- WASP-161b, WASP-163b and WASP-170b
- Short Name:
- J/AJ/157/43
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the discovery by the WASP-South transit survey of three new transiting hot Jupiters, WASP-161 b, WASP-163 b and WASP-170 b. Follow-up radial velocities obtained with the Euler/CORALIE spectrograph and high-precision transit light curves obtained with the TRAPPIST-North, TRAPPIST-South, SPECULOOS-South, NITES, and Euler telescopes have enabled us to determine the masses and radii for these transiting exoplanets. WASP-161 b completes an orbit around its V=11.1 F6V-type host star in 5.406 days, and has a mass and radius of 2.5+/-0.2M_Jup_ and 1.14+/-0.06R_Jup_ respectively. WASP-163 b has an orbital period of 1.609-days, a mass of 1.9+/-0.2M_Jup_, and a radius of 1.2+/-0.1R_Jup_. Its host star is a V=12.5 G8-type dwarf. WASP-170 b is on a 2.344-days orbit around a G1V-type star of magnitude V=12.8. It has a mass of 1.7+/-0.2M_Jup_ and a radius of 1.14+/-0.09R_Jup_. Given their irradiations (~10^9^erg/s/cm^2^) and masses, the three new planets' sizes are in good agreement with classical structure models of irradiated giant planets.
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/610/A63
- Title:
- WASP-151b, WASP-153b, WASP-156b
- Short Name:
- J/A+A/610/A63
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of three transiting exoplanets by the SuperWASP survey and the SOPHIE spectrograph with mass and radius determined with a precision better than 15%. WASP-151b and WASP-153b are two hot Saturns with masses, radii, densities and equilibrium temperatures of 0.31^+0.04^_-0.03_M_J_, 1.13^+0.03^_-0.03_R_J_, 0.22^+0.03^_-0.02_rho_J_ and 1,290^+20^_-10_K, and 0.39^+0.02^_-0.02_M_J_, 1.55^+0.10^_-0.08_R_J_, 0.11^+0.02^_-0.02{rho}_J_ and 1,700^+40^ _-40_K, respectively. Their host stars are early G type stars (with magV ~ 13) and their orbital periods are 4.53 and 3.33 days, respectively. WASP-156b is a Super-Neptune orbiting a K type star (magV = 11.6). It has a mass of 0.128^+0.010^_-0.009_M_J_, a radius of 0.51^+0.02^_ -0.02 R_J_, a density of 1.0^+0.1^_-0.1_{rho}_J_, an equilibrium temperature of 970^+30^_-20_K and an orbital period of 3.83 days.
- ID:
- ivo://CDS.VizieR/J/A+A/563/A143
- Title:
- WASP-68b, WASP-73b, WASP-88b transits
- Short Name:
- J/A+A/563/A143
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery by the WASP transit survey of three new hot Jupiters, WASP-68 b, WASP-73 b and WASP-88 b. WASP-68 b has a mass of 0.95+/-0.03M_Jup_, a radius of 1.24_-0.06_^+0.10^R_Jup_, and orbits a V=10.7 G0-type star (1.24+/-0.03M_{sun}_, 1.69_-0.06_^+0.11^R_{sun}_, Teff=5911+/-60K) with a period of 5.084298+/-0.000015-days. Its size is typical of hot Jupiters with similar masses. WASP-73 b is significantly more massive (1.88_-0.06_^+0.07^M_Jup_) and slightly larger (1.16_-0.08_^+0.12^R_Jup_) than Jupiter. It orbits a V=10.5 F9-type star (1.34_-0.04_^+0.05^M_{sun}_, 2.07_-0.08_^+0.19^R_{sun}_, Teff=6036+/-120K) every 4.08722+/-0.00022-days. Despite its high irradiation (2.3*10^9^erg/s/cm^2^), WASP-73 b has a high mean density (1.20_-0.30_^+0.26^{rho}_Jup_) that suggests an enrichment of the planet in heavy elements. WASP-88 b is a 0.56+/-0.08M_Jup_ planet orbiting a V=11.4 F6-type star (1.45+/-0.05M_{sun}_, 2.08_-0.06_^+0.12^R_{sun}_, Teff=6431+/-130K) with a period of 4.954000+/-0.000019-days. With a radius of 1.70_-0.07_^+0.13^R_Jup_, it joins the handful of planets with super-inflated radii. The ranges of ages we determine through stellar evolution modeling are 4.5-7.0Gyr for WASP-68, 2.8-5.7Gyr for WASP-73 and 1.8-4.3Gyr for WASP-88. WASP-73 appears to be a significantly evolved star, close to or already in the subgiant phase. WASP-68 and WASP-88 are less evolved, although in an advanced stage of core H-burning.
- 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.
- 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.
- ID:
- ivo://CDS.VizieR/J/MNRAS/465/3693
- Title:
- 7 WASP-South transiting exoplanets
- Short Name:
- J/MNRAS/465/3693
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We describe seven exoplanets transiting stars of brightness V=10.1-12.4. WASP-130b is a 'warm Jupiter' having an orbital period of 11.6d around a metal-rich G6 star. Its mass and radius (1.23+/-0.04M_Jup_ and 0.89+/-0.03R_Jup_) support the trend that warm Jupiters have smaller radii than hot Jupiters. WASP-131b is a bloated Saturn-mass planet (0.27M_Jup_ and 1.22R_Jup_). Its large scaleheight and bright (V=10.1) host star make it a good target for atmospheric characterization. WASP-132b (0.41M_Jup_ and 0.87R_Jup_) is among the least irradiated and coolest of WASP planets, having a 7.1-d orbit around a K4 star. WASP-139b is a 'super-Neptune' akin to HATS-7b and HATS-8b, being the lowest mass planet yet found by WASP (0.12M_Jup_ and 0.80R_Jup_). The metal-rich K0 host star appears to be anomalously dense, akin to HAT-P-11. WASP-140b is a 2.4M_Jup_ planet in an eccentric (e=0.047+/-0.004) 2.2d orbit. The planet's radius is large (1.4R_Jup_), but uncertain owing to the grazing transit (b=0.93). The 10.4d rotation period of the K0 host star suggests a young age, and the time-scale for tidal circularization is likely to be the lowest of all known eccentric hot Jupiters. WASP-141b (2.7M_Jup_, 1.2R_Jup_ and P=3.3d) and WASP-142b (0.84M_Jup_, 1.53R_Jup_ and P=2.1d) are typical hot Jupiters orbiting metal-rich F stars. We show that the period distribution within the hot-Jupiter bulge does not depend on the metallicity of the host star.
2217. WASP 95-101 transits
- ID:
- ivo://CDS.VizieR/J/MNRAS/440/1982
- Title:
- WASP 95-101 transits
- Short Name:
- J/MNRAS/440/1982
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of the transiting exoplanets WASP-95b, WASP-96b, WASP-97b, WASP-98b, WASP-99b, WASP-100b and WASP-101b. All are hot Jupiters with orbital periods in the range 2.1-5.7d, masses of 0.5-2.8M_Jup_ and radii of 1.1-1.4R_Jup_. The orbits of all the planets are compatible with zero eccentricity. WASP-99b produces the shallowest transit yet found by WASP-South, at 0.4 per cent. The host stars are of spectral type F2-G8. Five have metallicities of [Fe/H] from -0.03 to +0.23, while WASP-98 has a metallicity of -0.60, exceptionally low for a star with a transiting exoplanet. Five of the host stars are brighter than V=10.8, which significantly extends the number of bright transiting systems available for follow-up studies. WASP-95 shows a possible rotational modulation at a period of 20.7d. We discuss the completeness of WASP survey techniques by comparing to the HATnet project.
2218. WASP-148 velocity curve
- ID:
- ivo://CDS.VizieR/J/A+A/640/A32
- Title:
- WASP-148 velocity curve
- Short Name:
- J/A+A/640/A32
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the discovery and characterization of WASP-148, a new extrasolar system that includes at least two giant planets. The host star is a slowly rotating inactive late-G dwarf with a V=12 magnitude. The planet WASP-148b is a hot Jupiter of 0.72R_Jup_ and 0.29MJup that transits its host with an orbital period of 8.80-days. We found the planetary candidate with the SuperWASP photometric survey, then characterized it with the SOPHIE spectrograph. Our radial velocity measurements subsequently revealed a second planet in the system, WASP-148c, with an orbital period of 34.5-days and a minimum mass of 0.40M_Jup_. No transits of this outer planet were detected. The orbits of both planets are eccentric and fall near the 4:1 mean-motion resonances. This configuration is stable on long timescales, but induces dynamical interactions so that the orbits differ slightly from purely Keplerian orbits. In particular, WASP-148b shows transit-timing variations of typically 15 minutes, making it the first interacting system with transit-timing variations that is detected on ground-based light curves. We establish that the mutual inclination of the orbital plane of the two planets cannot be higher than 35, and the true mass of WASP-148c is below 0.60M_Jup_. We present photometric and spectroscopic observations of this system that cover a time span of ten years. We also provide their Keplerian and Newtonian analyses; these analyses should be significantly improved through future TESS observations.
- ID:
- ivo://CDS.VizieR/J/PASJ/53/517
- Title:
- Water maser survey of late-type stars
- Short Name:
- J/PASJ/53/517
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper presents new results of a water maser survey of late-type stellar objects at 22.235GHz with the Kashima 34-m radio telescope. We have detected 179 out of 643 observed sources, including 32 new detections. The sources were selected in terms of the IRAS flux density and colors of late-type stars, involving optically observable Mira/semi-regular variables, IRC objects, OH/IR sources and proto-planetary nebulae. We found the highest H_2_O detection rate for the type of stars with a thin dust envelope (Mira/semi-regular variables) among other types of sources. This is attributed to the smaller distances to such stars in the sample. The velocity spread of the H_2_O maser profile has an increasing tendency with the IRAS color, though it becomes more difficult to access this color dependence beyond an edge of the transition of the (oxygen-rich) Asymptotic Giant Branch stars to protoplanetary nebulae in the two-color diagram.
- 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.
