The WASP Project and the SuperWASP Cameras

By D. Pollacco, D. Christian, R. Street, A. Fitzsimmons, Rsi Ryans, I. Skillen, A. CollierCameron, T. Lister, K. Horne, Kané and 18 more. 2006

833 citations recorded by the source corpus.

The SuperWASP cameras are wide‐field imaging systems at the Observatorio del Roque de los Muchachos on the island of La Palma in the Canary Islands, and at the Sutherland Station of the South African Astronomical Observatory. Each instrument has a field of view of some 482 deg2 with an angular scale of 13 .″7 pixel−1, and is capable of delivering photometry with accuracy better than 1% for objects having V∼7.0–11.5. Lower quality data for objects brighter than V∼15.0 are stored in the project archive. The systems, while designed to monitor fields with high cadence, are capable of surveying the entire visible sky every 40 minutes. Depending on the observational strategy, the data rate can be up to 100 Gbytes per night. We have produced a robust, largely automatic reduction pipeline and advanced archive, which are used to serve the data products to the consortium members. The main science aim of these systems is to search for bright transiting exoplanet systems suitable for spectroscopic follow‐up observations. The first 6 month season of SuperWASP‐North observations produced light curves of ∼6.7 million objects with 12.9 billion data points.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

PASTIS: Bayesian extrasolar planet validation. I. General framework, models, and performance (2014, methodology): “The most successful method to find them has proven to be the wide-field surveys carried out from the ground (e.g. Bakos et al. 2004; Pollacco et al. 2006) and from space-based observatories like CoRoT (Auvergne et al. 2009) and Kepler (Koch et al. 2010).”
SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, background): “In this figure, we make the distinction between the secured and likely exoplanets and show the other EGPs21 detected and characterised by ground-based observatories like Super-WASP (Pollacco et al. 2006), HAT (Bakos et al. 2004), and from the CoRoT space telescope (Baglin et al. 2006).”
Observational Evidence for Tidal Interaction in Close Binary Systems (2007, background): “Furthermore, a new wave of observational effort to search for transiting planets by small, 10-cm class, telescopes is now at its full thrust (e.g., HATnet — Bakos et al. 2004; XO — McCullough et al. 2005; WASP — Pollacco et al. 2006; TrES — Alonso et al. 2007).”
TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26 (2021, background): “Many surveys were carried out to search for transiting exoplanets, including WASP (Pollacco et al. 2006), HAT (Bakos et al. 2004, 2013), KELT (Pepper et al. 2007, 2012), and others46 Other surveys have been conducted to search for stellar variability, such as ASAS (Pojmanski 1997), ASAS-SN (Shappee…”
Optimized transit detection algorithm to search for periodic transits of small planets (2019, methodology): “Analysis of variance (AoV, Schwarzenberg-Czerny & Beaulieu 2006) also uses a box-shaped transit model (which the authors refer to as top-hat), and has been demonstrated to have a lower detection efficiency than BLS in WASP data (Enoch et al. 2012).”
THE XO PLANETARY SURVEY PROJECT: ASTROPHYSICAL FALSE POSITIVES (2010, neutral): “The SuperWASP fields analyzed by Christian et al. (2006), Clarkson et al. (2007) and Kane et al. (2008) were 1507 deg2, 786 deg2 and 2162 deg2 with 41, 44 and 30 false positives, respectively.”
From thermal dissociation to condensation in the atmospheres of ultra hot Jupiters: WASP-121b in context (2018, background): “…actually a rare outcome of planet formation (Wright et al. 2012), yet fortunately many are known mainly due to the excellent sky coverage of groundbased transit surveys like WASP (Pollacco et al. 2006), HATNet and HATSouth (Bakos 2018), KELT (Pepper et al. 2007), and MASCARA (Snellen et al. 2013).”
A comprehensive study of the Kepler triples via eclipse timing (2015, background): “Some dozens of our sample EBs, however, were observed a few years before the beginning of the original Kepler mission in the photometric surveys of ASAS (Pigulski et al. 2009), HATNET (Hartman et al. 2004), TRESS (Devor et al. 2008) and SuperWASP (Pollacco et al. 2006).”
CHARACTERIZING K2 PLANET DISCOVERIES: A SUPER-EARTH TRANSITING THE BRIGHT K DWARF HIP 116454 (2014, methodology): “WASP HIP116454 was observed by the SuperWASP-N instrument on La Palma, Spain and the SuperWASP-S instrument at the South African Astronomical Observatory (Pollacco et al. 2006).”
THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES (2015, background): “Previous wide-field transit surveys, such as HAT (Bakos et al. 2004), TrES (Alonso et al. 2004), XO (McCullough et al. 2005), WASP (Pollacco et al. 2006), and KELT (Pepper et al. 2007), have been conducted with ground-based telescopes.”
Efficient identification of exoplanetary transit candidates from SuperWASP light curves (2007, methodology): “The SuperWASP instrument and data pipeline are described in full by Pollacco et al. (2006).”
Transits and Occultations (2010, background): “Many of today’s transiting planets are named after these surveys: for more details see Udalski et al. (2002), Alonso et al. (2004), McCullough et al. (2005), Bakos et al. (2007), and Pollacco et al. (2006).”
IMPROVED SPECTROSCOPIC PARAMETERS FOR TRANSITING PLANET HOSTS (2012, result): “Indirect evidence of these effects may perhaps be seen already in published results from the two surveys that have produced the majority of the transiting planet discoveries from the ground: the WASP project (Pollacco et al. 2006) and the HATNet project (Bakos et al. 2004).”
WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, methodology): “Most of the transiting exoplanets found by ground-based transit surveys (e.g. WASP, Pollacco et al. 2006; HATNet, Bakos et al. 2004) are Jovian-type planets with orbital periods of just a few days, these planets being the easiest to detect for such surveys.”