Gas giants transiting bright nearby stars are key objects for our understanding of planetary system formation and evolution mechanisms. This paper presents a new transiting exoplanet discovered by the WASP-South transit survey, WASP-193b. WASP-193b orbits its Vmag = 12.0 F9 main-sequence host star every 6.25d. Our analyses found that WASP-193b has a mass of Mp = 0.146 ± 0.033 M_Jup, a radius of R_p = 1.58 ± 0.14R_Jup, translating into an extremely low density of rho_p = 0.049 ± 0.015g/cm3. The planet was confirmed photometrically by the 0.6-m TRAPPIST-South and 1.0-m SPECULOOS-South telescopes and spectroscopically by the ESO-3.6-m/HARPS and Euler-1.2-m/CORALIE spectrographs. The combination of its large transit depth (dF≈1.4%), its super-low density, its high-equilibrium temperature (T_eq = 1275 ± 40K), and the infrared brightness of its host star (magnitude Kmag=10.7) makes WASP-193b an exquisite target for a detailed atmospheric characterization by transmission spectroscopy.

We report the discovery of WASP-190b, an exoplanet on a 5.37 day orbit around a mildly evolved F6 IV-V star with V  =  11.7, T eff  =  6400  ±  100 K, M *  =  1.35  ±  0.05 M e , and R *  =  1.6  ±  0.1 R e . The planet has a radius of R P  =  1.15  ±  0.09 R Jup and a mass of M P  =  1.0  ±  0.1 M Jup , making it a mildly in fl ated hot Jupiter. It is the fi rst hot Jupiter con fi rmed via Doppler tomography with an orbital period of > 5 days. The orbit is also marginally misaligned with respect to the stellar rotation, with λ  =  21 °  ±  6 ° measured using Doppler tomography.

We report the discovery of a 7.3 MJ exoplanet WASP-14b, one of the most massive transiting exoplanets observed to date. The planet orbits the tenth-magnitude F5V star USNO-B1 11118-0262485 with a period of 2.243752 days and orbital eccentricity e = 0.09. A simultaneous fit of the transit light curve and radial velocity measurements yields a planetary mass of 7.3±0.5 MJ and a radius of 1.28±0.08 RJ. This leads to a mean density of about 4.6 g cm making it densest transiting exoplanets yet found at an orbital period less than 3 days. We estimate this system to be at a distance of 160± 20 pc. Spectral analysis of the host star reveals a temperature of 6475± 100 K, log g = 4.07 cm s and v sin i = 4.9± 1.0 km s, and also a high lithium abundance, log N(Li) = 2.84±0.05. The stellar density, effective temperature and rotation rate suggest an age for the system of about 0.5–1.0 Gyr.

We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated pla net of mass 0.636 +0.025 −0.024 MJ and radius 1.653 +0.090 −0.083 RJ. It orbits a F9 star, evolving o ff the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit ( e = 0.067+0.033 −0.025) for WASP-54b. We investigated further the veracity of our d etection of the eccentric orbit for WASP-54b, and we find that it could be real . However, given the brightness of WASP-54 V =10.42 magnitudes, we encourage observations of a secondary eclipse to draw robus t conclusions on both the orbital eccentricity and the therm al structure of the planet. WASP-56b and WASP-57b have masses of 0.571 +0.034 −0.035 MJ and 0.672 +0.049 −0.046 MJ , respectively; and radii of 1 .092 +0.035 −0.033 RJ for WASP-56b and 0 .916+0.017 −0.014 RJ for WASP-57b. They orbit main sequence stars of spectral typ e G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy ele m nts; possibly as high as∼50 M⊕ in the case of WASP-57b. However, the composition of the deep interior of exoplanets remain still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and co nstrain giant planets’ physical properties.

Lithium abundances determined by spectral synthesis from both the 6708 Å resonance line and the 6104 Å subordinate line are reported for 11 Pleiades late-G and early-K stars observed at the William Herschel Telescope. Firm detections of the weak subordinate line are found for four objects, marginal detections for four, and upper limits for the remaining three stars. Some of these spectra were previously analysed by Russell (1996), where he reported that abundances derived from the 6104 Å line were systematically higher than those obtained from the 6708 Å line by 0.2–0.7 dex. He also reported a reduced spread in the 6104 Å line abundances compared with those determined from the 6708 Å feature. Using spectral synthesis we have re-analysed Russell’s data, along with our own. Our results do not entirely support Russell’s conclusions. We report a ∼0.7 dex scatter in the abundances from 6708 Å and a scatter at least as large from the 6104 Å line. We find that this is partly explained by our inclusion of a nearby Fe  line and careful modelling of damping wings in the strong metal lines close to the 6104 Å feature; neglect of these leads to overestimates of the Li abundance which are most severe in those objects with the weakest 6104 Å lines, thus reducing the abundance scatter. We find a reasonable correlation between the 6104 Å and 6708 Å Li abundances, although four stars have 6104 Å-determined abundances which are significantly larger than the 6708 Å-determined values by up to 0.5 dex, suggesting problems with the homogeneous, 1-dimensional atmospheres being used. We show that these discrepancies can be explained, although probably not uniquely, by the presence of star spots with plausible coverage fractions. The addition of spots does not significantly reduce the apparent scatter in Li abundances, leaving open the possibility that at least some of the spread is caused by real star-to-star differences in pre-main sequence Li depletion.

We report the discovery of two hot-Jupiter planets, each orbiting one of the stars of a wide binary system. WASP-94A (2MASS 20550794-3408079) is an F8 type star hosting a transiting planet with a radius of 1.72 +/- 0.06 R_Jup, a mass of 0.452 +/- 0.034 M_Jup, and an orbital period of 3.95 days. The Rossiter-McLaughlin effect is clearly detected, and the measured projected spin-orbit angle indicates that the planet occupies a retrograde orbit. WASP-94B (2MASS 20550915-3408078) is an F9 stellar companion at an angular separation of 15" (projected separation 2700 au), hosting a gas giant with a minimum mass of 0.618 +/- 0.028 M_Jup with a period of 2.008 days, detected by Doppler measurements. The orbital planes of the two planets are inclined relative to each other, indicating that at least one of them is inclined relative to the plane of the stellar binary. These hot Jupiters in a binary system bring new insights into the formation of close-in giant planets and the role of stellar multiplicity.

We report the discovery of the transiting exoplanets WASP-69b, WASP-70Ab and WASP84b, each of which orbits a bright star (V∼ 10). WASP-69b is a bloated Saturn-mass planet (0.26 MJup, 1.06 RJup) in a 3.868-d period around an active mid-K dwarf. We estimate a stellar age of 1 Gyr from both gyrochronological and age-activity relations, though an alternative gyrochronological relation suggests an age of 3 Gyr. ROSAT detected X-rays at a distance of 60±27 ′′ from WASP-69. If the star is the source then the planet could be undergoing massloss at a rate of ∼10 12 g s −1 . This is 1‐2 orders of magnitude higher than the evaporation rate estimated for HD 209458b and HD 189733b, both of which have exhibited anomalouslylarge Lyman-α absorption during transit. WASP-70Ab is a sub-Jupiter-mass planet (0.59 MJup, 1.16 RJup) in a 3.713-d orbit around the primary of a spatially-resolv ed G4+K3 binary, with a separation of 3. ′′ 3 (>800 AU). We exploit the binary nature of the system to construct a Hertzsprung-Russell diagram, from which we estimate its age to be 9‐10 Gyr. WASP-84b is a sub-Jupiter-mass planet (0.69 MJup, 0.94 RJup) in an 8.523-d orbit around an active earlyK dwarf. Of the transiting planets discovered from the ground to date, WASP-84b has the third-longest period. From a combination of gyrochronological and age-activity relations we estimate the age of WASP-84 to be∼1 Gyr. For both the active stars WASP-69 and WASP-84 we find a modulation of the radial velocities with a period similar to the photometrically-de termined stellar rotation period. We fit the residuals with a low-order harmonic series and subtra ct the best fit from the RVs prior to deriving the system parameters. In each case the solution is essentially unchanged, with much less than a 1-σ change to the planetary mass. We found this method of pre-whitening using a harmonic fit to result in a greater reduction in the res idual RV scatter than the oft-used method of pre-whitening with a fit to the RV residuals and the b isector spans.