Conclusions: Most hot Jupiters are misaligned, with a large variety of spin-orbit angles. We find observations and predictions using the Kozai mechanism match well. If these observational facts are confirmed in the future, we may then conclude that most hot Jupiters are formed from a dynamical and tidal origin without the necessity to use type I or II migration. At present, standard disc migration cannot explain the observations without invoking at least another additional process. Using observations with the high resolution échelle spectrograph HARPS mounted on the ESO 3.6 m (under proposals 072.C-0488, 082.C-0040 & 283.C-5017), and with the high resolution échelle spectrograph CORALIE on the 1.2 m Euler Swiss Telescope, both installed at the ESO La Silla Observatory in Chile.RV data is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/524/A25 [less ▲]Detailed reference viewed: 12 (2 ULg) WASP-22 b: A transiting "hot Jupiter" planet in a hierarchical triple systemMaxted, P. F. L.; Anderson, D. R.; Gillon, Michaël et alin Astronomical Journal (The) (2010), 140(6), 2007-2012We report the discovery of a transiting planet orbiting the star TYC 6446-326-1. The star, WASP-22, is a moderately bright (V=12.0) solar-type star (T_eff = 6000 +/- 100K, [Fe/H]= -0.05 \pm 0.08). The ... [more ▼]We report the discovery of a transiting planet orbiting the star TYC 6446-326-1. The star, WASP-22, is a moderately bright (V=12.0) solar-type star (T_eff = 6000 +/- 100K, [Fe/H]= -0.05 \pm 0.08). The lightcurve of the star obtained with the WASP-South instrument shows periodic transit-like features with a depth of about 1% and a duration of 0.14d. The presence of a transit-like feature in the lightcurve is confirmed using z-band photometry obtained with Faulkes Telescope South. High resolution spectroscopy obtained with the CORALIE and HARPS spectrographs confirm the presence of a planetary mass companion with an orbital period of 3.533d in a near-circular orbit. From a combined analysis of the spectroscopic and photometric data assuming that the star is a typical main-sequence star we estimate that the planet has a mass M_p = (0.56 +/- 0.02)M_Jup and a radius R_p = (1.12 +/- 0.04)R_Jup. In addition, there is a linear trend of 40m/s/y in the radial velocities measured over 16 months, from which we infer the presence of a third body with a long period orbit in this system. The companion may be a low mass M-dwarf or a second planet. [less ▲]Detailed reference viewed: 4 (1 ULg) WASP-26b: A 1-Jupiter-mass planet around an early-G-type starSmalley, B.; Anderson, D. R.; Collier Cameron, A. et alin Astronomy and Astrophysics (2010)We report the discovery of WASP-26b, a moderately over-sized Jupiter-mass exoplanet transiting its 11.3-magnitude early-G-type host star (1SWASP J001824.70-151602.3; TYC 5839-876-1) every 2.7566 days. A ... [more ▼]We report the discovery of WASP-26b, a moderately over-sized Jupiter-mass exoplanet transiting its 11.3-magnitude early-G-type host star (1SWASP J001824.70-151602.3; TYC 5839-876-1) every 2.7566 days. A simultaneous fit to transit photometry and radial-velocity measurements yields a planetary mass of 1.02 +/- 0.03 M_Jup and radius of 1.32 +/- 0.08 R_Jup. The host star, WASP-26, has a mass of 1.12 +/- 0.03 M_sun and a radius of 1.34 +/- 0.06 R_sun and is in a visual double with a fainter K-type star. The two stars are at least a common-proper motion pair with a common distance of around 250 +/- 15 pc and an age of 6 +/- 2 Gy. [less ▲]Detailed reference viewed: 6 (0 ULg) WASP-19b: The Shortest Period Transiting Exoplanet Yet DiscoveredHebb, L.; Collier-Cameron, A.; Triaud, A H M J et alin Astrophysical Journal (2010), 708We report on the discovery of a new extremely short period transiting extrasolar planet, WASP-19b. The planet has mass M [SUB]pl[/SUB] = 1.15 Â± 0.08 M[SUB]J[/SUB] , radius R [SUB]pl[/SUB] = 1.31 Â± 0.06 ... [more ▼]We report on the discovery of a new extremely short period transiting extrasolar planet, WASP-19b. The planet has mass M [SUB]pl[/SUB] = 1.15 Â± 0.08 M[SUB]J[/SUB] , radius R [SUB]pl[/SUB] = 1.31 Â± 0.06 R[SUB]J[/SUB] , and orbital period P = 0.7888399 Â± 0.0000008 days. Through spectroscopic analysis, we determine the host star to be a slightly super-solar metallicity ([M/H] = 0.1 Â± 0.1 dex) G-dwarf with T [SUB]eff[/SUB] = 5500 Â± 100 K. In addition, we detect periodic, sinusoidal flux variations in the light curve which are used to derive a rotation period for the star of P [SUB]rot[/SUB] = 10.5 Â± 0.2 days. The relatively short stellar rotation period suggests that either WASP-19 is somewhat young (~ 600 Myr old) or tidal interactions between the two bodies have caused the planet to spiral inward over its lifetime resulting in the spin-up of the star. Due to the detection of the rotation period, this system has the potential to place strong constraints on the stellar tidal quality factor, Q'[SUB] s [/SUB], if a more precise age is determined. [less ▲]Detailed reference viewed: 25 (1 ULg) WASP-16b: A New Jupiter-Like Planet Transiting a Southern Solar AnalogLister, T. A.; Anderson, D. R.; Gillon, Michaël et alin Astrophysical Journal (2009), 703We report the discovery from WASP-South of a new Jupiter-like extrasolar planet, WASP-16b, which transits its solar analog host star every 3.12 days. Analysis of the transit photometry and radial velocity ... [more ▼]We report the discovery from WASP-South of a new Jupiter-like extrasolar planet, WASP-16b, which transits its solar analog host star every 3.12 days. Analysis of the transit photometry and radial velocity spectroscopic data leads to a planet with R [SUB]p[/SUB] = 1.008 ± 0.071 R [SUB]Jup[/SUB] and M [SUB]p[/SUB] = 0.855 ± 0.059 M [SUB]Jup[/SUB], orbiting a host star with R [SUB]*[/SUB] = 0.946 ± 0.054 R [SUB]sun[/SUB] and M [SUB]*[/SUB] = 1.022 ± 0.101 M [SUB]sun[/SUB]. Comparison of the high resolution stellar spectrum with synthetic spectra and stellar evolution models indicates the host star is a near-solar metallicity ([Fe/H] =0.01 ± 0.10) solar analog (T [SUB]eff[/SUB] = 5700 ± 150 K and log g = 4.5 ± 0.2) of intermediate age (tau = 2.3[SUP]+5.8[/SUP] [SUB]--2.2[/SUB] Gyr). [less ▲]Detailed reference viewed: 39 (1 ULg) An orbital period of 0.94days for the hot-Jupiter planet WASP-18bHellier, Coel; Anderson, D. R.; Cameron, A Collier et alin Nature (2009), 460The hot Jupiters' that abound in lists of known extrasolar planets are thought to have formed far from their host stars, but migrate inwards through interactions with the proto-planetary disk from which ... [more ▼]The hot Jupiters' that abound in lists of known extrasolar planets are thought to have formed far from their host stars, but migrate inwards through interactions with the proto-planetary disk from which they were born, or by an alternative mechanism such as planet-planet scattering. The hot Jupiters closest to their parent stars, at orbital distances of only ~0.02 astronomical units, have strong tidal interactions, and systems such as OGLE-TR-56 have been suggested as tests of tidal dissipation theory. Here we report the discovery of planet WASP-18b with an orbital period of 0.94days and a mass of ten Jupiter masses (10M[SUB]Jup[/SUB]), resulting in a tidal interaction an order of magnitude stronger than that of planet OGLE-TR-56b. Under the assumption that the tidal-dissipation parameter Q of the host star is of the order of 10[SUP]6[/SUP], as measured for Solar System bodies and binary stars and as often applied to extrasolar planets, WASP-18b will be spiralling inwards on a timescale less than a thousandth that of the lifetime of its host star. Therefore either WASP-18 is in a rare, exceptionally short-lived state, or the tidal dissipation in this system (and possibly other hot-Jupiter systems) must be much weaker than in the Solar System. [less ▲]Detailed reference viewed: 27 (6 ULg) Discovery and characterization of WASP-6b, an inflated sub-Jupiter mass planet transiting a solar-type starGillon, Michaël ; Anderson, D. R.; Triaud, A H M J et alin Astronomy and Astrophysics (2009), 501We report the discovery of WASP-6b, an inflated sub-Jupiter mass planet transiting every 3.3610060[SUP]+ 0.0000022 [/SUP][SUB]- 0.0000035 [/SUB] days a mildly metal-poor solar-type star of magnitude V ... [more ▼]We report the discovery of WASP-6b, an inflated sub-Jupiter mass planet transiting every 3.3610060[SUP]+ 0.0000022 [/SUP][SUB]- 0.0000035 [/SUB] days a mildly metal-poor solar-type star of magnitude V = 11.9. A combined analysis of the WASP photometry, high-precision followup transit photometry and radial velocities yield a planetary mass M[SUB]p[/SUB] = 0.503[SUP]+0.019[/SUP][SUB]-0.038[/SUB] M[SUB]J[/SUB] and radius R[SUB]p[/SUB] = 1.224[SUP]+0.051[/SUP][SUB]-0.052[/SUB] R_J, resulting in a density rho[SUB]p[/SUB] = 0.27 ± 0.05 rho_J. The mass and radius for the host star are M_ast = 0.88[SUP]+0.05[/SUP][SUB]-0.08[/SUB] M_o and R_ast = 0.870[SUP]+0.025[/SUP][SUB]-0.036[/SUB] R_o. The non-zero orbital eccentricity e = 0.054^+0.018[SUB]-0.015[/SUB] that we measure suggests that the planet underwent a massive tidal heating 1 Gyr ago that could have contributed to its inflated radius. High-precision radial velocities obtained during a transit allow us to measure a sky-projected angle between the stellar spin and orbital axis beta = 11[SUP]+14[/SUP][SUB]-18[/SUB] deg. In addition to similar published measurements, this result favors a dominant migration mechanism based on tidal interactions with a protoplanetary disk. Based on data collected with the HARPS spectrograph at ESO La Silla Observatory in the programs 082.C-0040(E) and 082.C-0608. The photometric time-series and radial velocities (Tables 4, 5) used in this work are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/501/785 [less ▲]Detailed reference viewed: 20 (2 ULg) High-precision photometry by telescope defocusing - I. The transiting planetary system WASP-5Southworth, John; Hinse, T. C.; Jørgensen, U. G. et alin Monthly Notices of the Royal Astronomical Society (2009), 396We present high-precision photometry of two transit events of the extrasolar planetary system WASP-5, obtained with the Danish 1.54-m telescope at European Southern Obseratory La Silla. In order to ... [more ▼]We present high-precision photometry of two transit events of the extrasolar planetary system WASP-5, obtained with the Danish 1.54-m telescope at European Southern Obseratory La Silla. In order to minimize both random and flat-fielding errors, we defocused the telescope so its point spread function approximated an annulus of diameter 40 pixel (16 arcsec). Data reduction was undertaken using standard aperture photometry plus an algorithm for optimally combining the ensemble of comparison stars. The resulting light curves have point-to-point scatters of 0.50mmag for the first transit and 0.59mmag for the second. We construct detailed signal-to-noise ratio calculations for defocused photometry, and apply them to our observations. We model the light curves with the JKTEBOP code and combine the results with tabulated predictions from theoretical stellar evolutionary models to derive the physical properties of the WASP-5 system. We find that the planet has a mass of M[SUB]b[/SUB] = 1.637 +/- 0.075 +/- 0.033M[SUB]Jup[/SUB], a radius of R[SUB]b[/SUB] = 1.171 +/- 0.056 +/- 0.012R [SUB]Jup[/SUB], a large surface gravity of g[SUB]b[/SUB] = 29.6 +/- 2.8ms[SUP]-2[/SUP] and a density of rho[SUB]b[/SUB] = 1.02 +/- 0.14 +/- 0.01rho[SUB]Jup[/SUB] (statistical and systematic uncertainties). The planet's high equilibrium temperature of T[SUB]eq[/SUB] = 1732 +/- 80K makes it a good candidate for detecting secondary eclipses. Based on data collected by Microlensing Network for the Detection of Small Terrestrial Exoplanets (MiNDSTEp) with the Danish 1.54-m telescope at the ESO La Silla Observatory. E-mail: j.k.taylor@warwick.ac.uk â ¡ Royal Society University Research Fellow. [less ▲]Detailed reference viewed: 62 (16 ULg) The Low Density Transiting Exoplanet WASP-15bWest, R. G.; Anderson, D. R.; Gillon, Michaël et alin Astronomical Journal (The) (2009), 137We report the discovery of a low-density exoplanet transiting an 11th magnitude star in the Southern hemisphere. WASP-15b, which orbits its host star with a period P = 3.7520656 ± 0.0000028 d, has a mass ... [more ▼]We report the discovery of a low-density exoplanet transiting an 11th magnitude star in the Southern hemisphere. WASP-15b, which orbits its host star with a period P = 3.7520656 ± 0.0000028 d, has a mass M [SUB]p[/SUB] = 0.542 ± 0.050 M [SUB]J[/SUB] and radius R [SUB]p[/SUB] = 1.428 ± 0.077 R [SUB]J[/SUB], and is therefore one of the least dense transiting exoplanets so far discovered (rho[SUB]p[/SUB] = 0.247 ± 0.035 g cm[SUP]--3[/SUP]). An analysis of the spectrum of the host star shows it to be of spectral type around F5, with an effective temperature T [SUB]eff[/SUB] = 6300 ± 100 K and [Fe/H] = --0.17 ± 0.11. [less ▲]Detailed reference viewed: 18 (1 ULg) 1 2