Results from the Wide Angle Search for Planets Prototype (WASP0) - II. Stellar variability in the Pegasus field

Kane, Stephen R.; Lister, Tim; Cameron, A. Collier; Horne, K.; James, D. J.; Pollacco, D.; Street, R. A.; Tsapras, Y.

doi:10.1111/j.1365-2966.2005.09286.x

Cited by 11 publications

(6 citation statements)

References 26 publications

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“…The figure shows that periodic variable stars are found roughly equally distributed over stellar luminosity. The obtained precision is comparable to what has been obtained by other small wide-angle telescopes ( Hartman et al 2004;Kane et al 2004Kane et al , 2005aKane et al , 2005b.…”

Section: Photometrysupporting

confidence: 73%

Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

et al. 2007

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The COROT space mission will monitor several target fields for up to 150 days to perform asteroseismology and to search for extrasolar planets by photometric transits. Variable stars in the target fields are important objects for additional scientific studies but can also disturb the search for planetary transits. A variability characterization of the target fields prior to COROT observations is therefore important for two reasons: to find interesting variable stars to monitor further and to make an analysis of the impact of the variable stars on detecting extrasolar planet transits with COROT. The Berlin Exoplanet Search Telescope ( BEST ) is a small wide-angle telescope dedicated to highprecision photometry. It has observed a 9 deg 2 field of view centered at ( ; ) ¼ (19 h 00 m 00:0 s ; þ00 01 0 55:2 00 ) (J2000.0) over 98 nights to search for variable stars in the surroundings of the first long-run target field ( LRc1) of the COROT space mission. In this data set we identified 92 periodic variable stars, 86 of which are new discoveries and 6 of which are known from the General Catalogue of Variable Stars (GCVS). For five of the GCVS stars, variability could not be confirmed. Forty-three of the 92 detected periodic variable stars are identified as eclipsing binaries. We have evaluated the completeness of our survey for eclipsing binaries by comparing it to the expected fraction of eclipsing binaries based on Hipparcos observations. From this evaluation we show that the BEST data set presented here has a completeness of 20%Y30% for periods longer than 1 day and is complete relative to Hipparcos for short-period binaries.

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Section: Photometrysupporting

confidence: 73%

Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

et al. 2007

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“…Unlike the radial velocity surveys, these dedicated programs were able to observe all night, every night. By using wide-field cameras, those transit surveys (such as the Wide-Angle Search for Planets, WASP; e.g., Kane et al 2004Kane et al , 2005aKane et al , 2005bChristian et al 2006;Butters et al 2010; HAT-Net and HAT-South; e.g., Bakos et al 2004Bakos et al , 2007Bakos et al , 2013Hartman et al 2011;Zhou et al 2014; and the multi-purpose CoRoT space observatory; e.g., Baglin et al 2006;Alonso et al 2008;Barge et al 2008;Deleuil et al 2008;Léger et al 2009) were able to monitor the brightness of thousands of stars at once, continually-playing a numbers game to ensure large numbers of detections. The ultimate expression of that philosophy came with the launch of Kepler, in 2009.…”

Section: Current and Future Exoplanet Surveysmentioning

confidence: 99%

Solar System Physics for Exoplanet Research

Horner

Kane

Marshall

et al. 2020

PASP

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Over the past three decades, we have witnessed one of the great revolutions in our understanding of the cosmos—the dawn of the Exoplanet Era. Where once we knew of just one planetary system (the solar system), we now know of thousands, with new systems being announced on a weekly basis. Of the thousands of planetary systems we have found to date, however, there is only one that we can study up-close and personal—the solar system. In this review, we describe our current understanding of the solar system for the exoplanetary science community—with a focus on the processes thought to have shaped the system we see today. In section one, we introduce the solar system as a single well studied example of the many planetary systems now observed. In section two, we describe the solar system's small body populations as we know them today—from the two hundred and five known planetary satellites to the various populations of small bodies that serve as a reminder of the system's formation and early evolution. In section three, we consider our current knowledge of the solar system's planets, as physical bodies. In section four we discuss the research that has been carried out into the solar system's formation and evolution, with a focus on the information gleaned as a result of detailed studies of the system's small body populations. In section five, we discuss our current knowledge of planetary systems beyond our own—both in terms of the planets they host, and in terms of the debris that we observe orbiting their host stars. As we learn ever more about the diversity and ubiquity of other planetary systems, our solar system will remain the key touchstone that facilitates our understanding and modeling of those newly found systems, and we finish section five with a discussion of the future surveys that will further expand that knowledge.

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“…Fast transients may have previously been detected in single images, but simply discarded as unconfirmed or spurious events. However, there have been a number of planetary transit and variable star studies, which offer the required high cadence (e.g.,; Kane et al 2005;Kraus et al 2007;Lister et al 2007). These experiments typically target dense Galactic fields and thus a large stellar population.…”

Section: Rates Of Fast Transients In Nearby Galaxiesmentioning

confidence: 99%

A Survey for Fast Transients in the Fornax Cluster of Galaxies

Rau

Ofek

Kulkarni

et al. 2008

ApJ

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The luminosity gap between novae (M_R < -10) and supernovae (M_R > -14) is well known since the pioneering research of Zwicky and Hubble. Nearby galaxy clusters and concentrations offer an excellent opportunity to search for explosions brighter than classical novae and fainter than supernovae. Here, we present the results of a B-band survey of 23 member galaxies of the Fornax cluster, performed at the Las Campanas 2.5-m Irene duPont telescope. Observations with a cadence of 32 minutes discovered no genuine fast transient to a limiting absolute magnitude of M_B=-9.3 mag. We provide a detailed assessment of the transient detection efficiency and the resulting upper limits on the event rate as function of peak magnitude. Further, we discuss the discoveries of five previously unknown foreground variables which we identified as two flare stars, two W Uma type eclipsing binaries and a candidate delta Scuti/SX Phe star.Comment: final version, 13 pages, 15 figures, emulateapj.st

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Results from the Wide Angle Search for Planets Prototype (WASP0) - II. Stellar variability in the Pegasus field

Cited by 11 publications

References 26 publications

Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

Solar System Physics for Exoplanet Research

A Survey for Fast Transients in the Fornax Cluster of Galaxies

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