The WASP Project and SuperWASP Camera

The WASP project and infrastructure supporting the SuperWASP Facility are described. As the instrument, reduction pipeline and archive system are now fully operative we expect the system to have a major impact in the discovery of bright exo-planet candidates as well in more general variable star projects.

WASP-3b: a strongly irradiated transiting gas-giant planet

We report the discovery of WASP-3b, the third transiting exoplanet to be discovered by the WASP and SOPHIE collaboration. WASP-3b transits its host star USNO-B1.01256-0285133 every 1.846834 +/- 0.000002 d. Our high-precision radial velocity measurements present a variation with amplitude characteristic of a planetary-mass companion and in phase with the light curve. Adaptive optics imaging shows no evidence for nearby stellar companions, and line-bisector analysis excludes faint, unresolved binarity and stellar activity as the cause of the radial velocity variations. We make a preliminary spectroscopic analysis of the host star and find it to have Teff = 6400 +/- 100K and log g = 4.25 +/- 0.05 which suggests it is most likely an unevolved main-sequence star of spectral type F7-8V. Our simultaneous modelling of the transit photometry and reflex motion of the host leads us to derive a mass of 1.76+0.08-0.14 MJ and radius 1.31+0.07-0.14 RJ for WASP-3b. The proximity and relative temperature of the host star suggests that WASP-3b is one of the hottest exoplanets known, and thus has the potential to place stringent constraints on exoplanet atmospheric models.

WASP-4b: A 12th magnitude transiting hot Jupiter in the southern hemisphere

We report the discovery of WASP-4b, a large transiting gas-giant planet with an orbital period of 1.34 days. This is the first planet to be discovered by the SuperWASP-South observatory and CORALIE collaboration and the first planet orbiting a star brighter than 16th magnitude to be discovered in the southern hemisphere. A simultaneous fit to high-quality light curves and precision radial velocity measurements leads to a planetary mass of 1.22(-0.08)(+0.09) M-Jup and a planetary radius of 1.42(-0.04)(+0.07) R-Jup. The host star is USNO-B1.0 0479-0948995, a G7 V star of visual magnitude 12.5. As a result of the short orbital period, the predicted surface temperature of the planet is 1761 K, making it an ideal candidate for detections of the secondary eclipse at infrared wavelengths.

Updated parameters for the transiting exoplanet WASP-3b using RISE, a new fast camera for the Liverpool Telescope

Some of the first results are reported from RISE - a new fast camera mounted on the Liverpool Telescope primarily designed to obtain high time-resolution light curves of transiting extrasolar planets for the purpose of transit timing. A full and partial transit of WASP-3 are presented, and a Markov-Chain Monte Carlo analysis is used to update the parameters from the discovery paper. This results in a planetary radius of 1.29(-0.12)(+0.05) R-J and therefore a density of 0.82(-0.09)(+0.14) rho(J), consistent with previous results. The inclination is 85.06(-0.15)(+0.16) deg, in agreement (but with a significant improvement in the precision) with the previously determined value. Central transit times are found to be consistent with the ephemeris given in the discovery paper; however, a new ephemeris calculated using the longer baseline results in T-c(0) = 2 454 605.55915 +/- 0.00023 HJD and P = 1.846835 +/- 0.000002 days.

The 0.5M(J) transiting exoplanet WASP-13b

We report the discovery of WASP-13b, a low-mass M-p = 0.46(-0.05)(+0.06) M-J transiting exoplanet with an orbital period of 4.35298 +/- 0.00004 days. The transit has a depth of 9 mmag, and although our follow-up photometry does not allow us to constrain the impact parameter well (0 <b <0.46), with radius in the range R-p similar to 1.06-1.21 R-J the location of WASP-13b in the mass-radius plane is nevertheless consistent with H/He-dominated, irradiated, low core mass and core-free theoretical models. The G1V host star is similar to the Sun in mass (M-* = 1.03(-0.09)(+0.11) M-circle dot) and metallicity ([M/H] = 0.0 +/- 0.2), but is possibly older (8.5(-4.9)(+5.5) Gyr).

WASP-14b: 7.3 M-J transiting planet in an eccentric orbit

We report the discovery of a 7.3 M-J exoplanet WASP-14b, one of the most massive transiting exoplanets observed to date. The planet orbits the 10th-magnitude F5V star USNO-B1 11118-0262485 with a period of 2.243 752 d 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 M-J and a radius of 1.28 +/- 0.08 R-J. This leads to a mean density of about 4.6 g cm(-3) making it the densest transiting exoplanets yet found at an orbital period less than 3 d. 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(-2) and v sin i = 4.9 +/- 1.0 km s(-1), 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.

WASP-10b: a 3M(J), gas-giant planet transiting a late-type K star

We report the discovery of WASP-10b, a new transiting extrasolar planet (ESP) discovered by the Wide Angle Search for Planets ( WASP) Consortium and confirmed using Nordic Optical Telescope FIbre-fed Echelle Spectrograph and SOPHIE radial velocity data. A 3.09-d period, 29 mmag transit depth and 2.36 h duration are derived for WASP-10b using WASP and high-precision photometric observations. Simultaneous fitting to the photometric and radial velocity data using a Markov Chain Monte Carlo procedure leads to a planet radius of 1.28R(J), a mass of 2.96M(J) and eccentricity of approximate to 0.06. WASP-10b is one of the more massive transiting ESPs, and we compare its characteristics to the current sample of transiting ESP, where there is currently little information for masses greater than approximate to 2M(J) and non-zero eccentricities. WASP-10's host star, GSC 2752-00114 (USNO-B1.0 1214-0586164) is among the fainter stars in the WASP sample, with V = 12.7 and a spectral type of K5. This result shows promise for future late-type dwarf star surveys.

An orbital period of 0.94days for the hot-Jupiter planet WASP-18b

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 (10MJup), 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 106, 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.

The Low Density Transiting Exoplanet WASP-15b

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 p = 0.542 ± 0.050 M J and radius R p = 1.428 ± 0.077 R J, and is therefore one of the least dense transiting exoplanets so far discovered (?p = 0.247 ± 0.035 g cm-3). An analysis of the spectrum of the host star shows it to be of spectral type around F5, with an effective temperature T eff = 6300 ± 100 K and [Fe/H] = -0.17 ± 0.11.

Wasp-7: A Bright Transiting-Exoplanet System in the Southern Hemisphere

We report that a Jupiter-mass planet, WASP-7b, transits the V = 9.5 star HD 197286 every 4.95 d. This is the brightest discovery from the WASP-South transit survey so far and is currently the brightest transiting-exoplanet system in the southern hemisphere. WASP-7b is among the densest of the known Jupiter-mass planets, suggesting that it has a massive core. The planet mass is 0.96+0.12 -0.18 M Jup, the radius is 0.915+0.046 -0.040 R Jup, and the density is 1.26+0.25 -0.21 ?Jup (1.67+0.33 -0.28 g cm-3).

The structure of helokinestatin-5 and its biosynthetic precursor from Gila monster (Heloderma suspectum) venom: Evidence for helokinestatin antagonism of bradykinin-induced relaxation of rat tail artery smooth muscle

Here we report the primary structure of a novel peptide, named helokinestatin-5 (VPPPLQMPLIPR), from the venom of the Gila monster (Heloderma suspectum). Helokinestatin-5 differs in structure from helokinestatin-3 by deletion of a single prolyl residue in the N-terminally located polyproline region. Two different biosynthetic precursors were consistently cloned from a venom-derived cDNA library. The first encoded helokinestatins 1–4 and a single copy of C-type natriuretic peptide, as previously described, whereas the second was virtually identical, lacking only a single prolyl codon as found in the mature attenuated helokinestatin-5 peptide. Helokinestatins 1–3 and 5 were synthesized by solid-phase fmoc chemistry and each synthetic replicate was found to antagonize the relaxation effect induced by bradykinin on rat tail artery smooth muscle. Helokinestatins thus represent a novel family of vasoactive peptides from the venom of helodermatid lizards

Molecular cloning of the helokinestatin/CNP precursor from a venom-derived cDNA library of the Mexican beaded lizard, Heloderma horridum, and identification of a novel encoded bradykinin-antagonist peptide, helokinestatin-6

Helokinestatins 1–5 represent a novel family of bradykinin antagonist peptides originally isolated from the venom of the Gila Monster, Heloderma suspectum. We found that they were encoded in tandem along with a single copy of C-type natriuretic peptide (CNP), by two different but almost identical biosynthetic precursors that were cloned from a venom-derived cDNA library. Here we have applied the same strategy to the venom of a related species, the Mexican beaded lizard, Heloderma horridum. Lyophilised venom was used as a surrogate tissue to generate a cDNA library that was interrogated with primers from the previous study and for reverse phase HPLC fractionation. The structure of a single helokinestatin precursor was obtained following sequencing of 20 different clones. The open-reading frame contained 196 amino acid residues, somewhat greater than the 177–178 residues of the corresponding helokinestatin precursors in H. suspectum. The reason for this difference in size was the insertion of an additional domain of 18 amino acid residues encoding an additional copy of helokinestatin-3. Helokinestatin-6 (GPPFNPPPFVDYEPR) was a novel peptide from this precursor identified in venom HPLC fractions. A synthetic replicate of this peptide antagonised the relaxation effect of bradykinin on rat arterial smooth muscle. The novel peptide family, the helokinestatins, have been shown to be present in the venom of H. horridum and to be encoded by a single precursor of different structure to those from H. suspectum. Studies such as this reveal the naturally-selected structures of bioactive peptides that have been optimised for purpose and provide the scientist with a natural analogue library for pharmacological investigation.

Molecular cloning and deduced organization of the pHpG/CNP precursor from the venom of the African forest viper, Atheris squamigera

The discovery that the hypotensive sequela of envenomation by the South American viper, Bothrops jararaca, was mediated by peptides, represented a milestone in drug discovery research that led to the introduction of ACE inhibitors. These bradykinin-potentiating peptides (BPPs) have been found in the venoms of many species of viper and molecular cloning of biosynthetic precursors has revealed that each encodes several different BPPs in tandem with a single copy of a C-type natriuretic peptide (CNP) located at the C-terminus. Venoms of the African forest vipers (Atheris) have been poorly studied possibly because they do not represent a major danger to humans. However, initial studies have indicated that they contain some of the “classical” protein toxins of viper venoms and a novel class of peptide, the polyglycine/polyhistidine (pGpH) peptides. These peptides occur in several molecular forms with different numbers of repetitive glycine and histidine repeats. We have cloned the biosynthetic precursor of A. squamigera pGpH peptides from a venom-derived cDNA library and have confirmed that a single copy of CNP is located at the C-terminus and additionally that, like BPPs in other vipers, pGpH peptides are encoded in tandem within this single precursor. Solid phase peptide synthesis of pGpH peptides has proven to be extremely difficult but is progressing and acquisition of synthetic replicates of each peptide is a necessary prerequisite for systematic pharmacological characterisation as establishment of a biological function for these peptides remains elusive. pGpH peptides may prove to play a role as fundamental as that of the BPPs.