The WASP Project and the SuperWASP Cameras

Pollacco, D.; Skillen, I.; Cameron, A. Collier; Christian, D. J.; Hellier, C.; Irwin, Jonathan; Lister, Tim; Street, R. A.; West, R. G.; Anderson, D. R.; Clarkson, W. I.; Deeg, H. J.; Enoch, B.; Evans, A.; Fitzsimmons, A.; Haswell, C. A.; Hodgkin, S. T.; Horne, K.; Kane, S. R.; Keenan, F. P.; Maxted, P. F. L.; Norton, A. J.; Osborne, J. P.; Parley, N.; Ryans, R.; Smalley, B.; Wheatley, P. J.; Wilson, David M.

doi:10.1086/508556

Cited by 1,111 publications

(687 citation statements)

References 21 publications

Supporting

Mentioning

680

Contrasting

Unclassified

Order By: Relevance

“…The sources that were successfully matched against the USNO-B1.0 catalogue are the ones available here, so transient sources are therefore unlikely to be seen in this data release. More details about the pipeline can be found in Pollacco et al (2006).…”

Section: The Wasp Observatoriesmentioning

confidence: 99%

The first WASP public data release

Butters¹,

West²,

Anderson

et al. 2010

A&A

Self Cite

279

164

View full text Add to dashboard Cite

The WASP (wide angle search for planets) project is an exoplanet transit survey that has been automatically taking wide field images since 2004. Two instruments, one in La Palma and the other in South Africa, continually monitor the night sky, building up light curves of millions of unique objects. These light curves are used to search for the characteristics of exoplanetary transits. This first public data release (DR1) of the WASP archive makes available all the light curve data and images from 2004 up to 2008 in both the Northern and Southern hemispheres. A web interface (www.wasp.le.ac.uk/public/) to the data allows easy access over the Internet. The data set contains 3 631 972 raw images and 17 970 937 light curves. In total the light curves have 119 930 299 362 data points available between them.

show abstract

Section: The Wasp Observatoriesmentioning

confidence: 99%

The first WASP public data release

Butters¹,

West²,

Anderson

et al. 2010

A&A

Self Cite

279

164

View full text Add to dashboard Cite

show abstract

“…The Wide Angle Search for Planets (WASP) project is designed to find transiting gas giants (Pollacco et al 2006). Observing the northern and southern hemispheres with sixteen 11-cm refractive telescopes, the WASP consortium has published more than 20 transiting planets in a large range of period, mass and radius, around stars with apparent magnitudes between 9 and 13.…”

Section: Introductionmentioning

confidence: 99%

Spin-orbit angle measurements for six southern transiting planets

Triaud

Cameron

Queloz

et al. 2010

A&A

Self Cite

433

440

View full text Add to dashboard Cite

Context. Several competing scenarios for planetary-system formation and evolution seek to explain how hot Jupiters came to be so close to their parent stars. Most planetary parameters evolve with time, making it hard to distinguish between models. The obliquity of an orbit with respect to the stellar rotation axis is thought to be more stable than other parameters such as eccentricity. Most planets, to date, appear aligned with the stellar rotation axis; the few misaligned planets so far detected are massive (>2 M J ). Aims. Our goal is to measure the degree of alignment between planetary orbits and stellar spin axes, to search for potential correlations with eccentricity or other planetary parameters and to measure long term radial velocity variability indicating the presence of other bodies in the system. Methods. For transiting planets, the Rossiter-McLaughlin effect allows the measurement of the sky-projected angle β between the stellar rotation axis and a planet's orbital axis. Using the HARPS spectrograph, we observed the Rossiter-McLaughlin effect for six transiting hot Jupiters found by the WASP consortium. We combine these with long term radial velocity measurements obtained with CORALIE. We used a combined analysis of photometry and radial velocities, fitting model parameters with the Markov Chain Monte Carlo method. After obtaining β we attempt to statistically determine the distribution of the real spin-orbit angle ψ. Results. We found that three of our targets have β above 90 • : WASP-2b: β = 153 • +11 −15 , WASP-15b: β = 139.6 • +5.2 −4.3 and WASP17b: β = 148.5 • +5.1 −4.2 ; the other three (WASP-4b, WASP-5b and WASP-18b) have angles compatible with 0 • . We find no dependence between the misaligned angle and planet mass nor with any other planetary parameter. All six orbits are close to circular, with only one firm detection of eccentricity e = 0.00848 +0.00085 −0.00095 in WASP-18b. No long-term radial acceleration was detected for any of the targets. Combining all previous 20 measurements of β and our six and transforming them into a distribution of ψ we find that between about 45 and 85% of hot Jupiters have ψ > 30 • . 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.

show abstract

“…In practice, many systems for which period changes indicative of circumbinary planets have been claimed, fall far short of this ideal. Therefore, here we search the archive of the SuperWASP (Wide Angle Search for Planets) project (Pollacco et al 2006) for evidence of period changes in those PCEBs from Zorotovic & Schreiber's Table 1 which have been observed by SuperWASP. The archive contains high-cadence photometric light curves for bright sources (V ∼ 8-15 mag) over almost the whole sky, stretching back to 2004 in many cases, and so should be capable of filling in gaps or extending the coverage of O−C diagrams for many of these systems.…”

Section: Introductionmentioning

confidence: 99%

Period and amplitude variations in post-common-envelope eclipsing binaries observed with SuperWASP

Lohr

Norton

Anderson

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

Period or amplitude variations in eclipsing binaries may reveal the presence of additional massive bodies in the system, such as circumbinary planets. Here, we have studied twelve previously-known eclipsing post-common-envelope binaries for evidence of such light curve variations, on the basis of multi-year observations in the SuperWASP archive. The results for HW Vir provided strong evidence for period changes consistent with those measured by previous studies, and help support a two-planet model for the system. ASAS J102322−3737.0 exhibited plausible evidence for a period increase not previously suggested; while NY Vir, QS Vir and NSVS 14256825 afforded less significant support for period change, providing some confirmation to earlier claims. In other cases, period change was not convincingly observed; for AA Dor and NSVS 07826147, previous findings of constant period were confirmed. This study allows us to present hundreds of new primary eclipse timings for these systems, and further demonstrates the value of wide-field high-cadence surveys like SuperWASP for the investigation of variable stars.

show abstract

The WASP Project and the SuperWASP Cameras

Cited by 1,111 publications

References 21 publications

The first WASP public data release

The first WASP public data release

Spin-orbit angle measurements for six southern transiting planets

Period and amplitude variations in post-common-envelope eclipsing binaries observed with SuperWASP

Contact Info

Product

Resources

About