A catalogue of RR Lyrae stars from the Northern Sky Variability Survey

Wils, P.; Lloyd, C.; Bernhard, Klaus

doi:10.1111/j.1365-2966.2006.10236.x

Cited by 50 publications

(61 citation statements)

References 19 publications

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“…Compared to incidences 5.1% (SF07) and 4.3% (Wils et al 2006), our percentage is significantly higher and roughly approximates the percentage based on precise measurements -48% ) based on Kepler data, or 47% (Jurcsik at al. 2009a), who utilized precise ground-base observations.…”

Section: Statistics Of the Blazhko Variables In The Samplementioning

confidence: 89%

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Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys

Skarka

2014

A&A

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Aims. Period study of 321 fundamental mode RR Lyrae type stars (RRab), which had appropriate data in ASAS and SuperWASP surveys, was performed to complement and extend the list of known Blazhko stars in galactic field with bright stars up to 12.5 mag in maximum light.Methods. An individual approach was applied to each studied star. Permanent visual supervision was maintained to each procedure in data analysis (data cleaning, frequency spectra examination) to avoid missing any possible sign of the Blazhko effect. Period analysis was performed using Period04 software. Results. We found 100 stars to be definitely modulated. In 25 cases, previously unknown modulation was revealed and 8 new candidates for Blazhko stars were identified. Their modulation needs to be confirmed. In 18 previously found Blazhko stars, no modulation was detectable. Multiple modulation was revealed for eight stars that were previously proposed to show simple modulation. In total, there were twelve stars with some peculiarity in their modulation in the sample. This brings the incidence rate of multiple/irregularlymodulated stars to 12%. The ratio of the modulation periods of five of the double-modulated stars was within the ratios of small integers. One of stars studied, IK Hya, showed a very interesting frequency spectrum, which we interpret as changing Blazhko period between 71.81 and 75.57 days and an additional 1403-day-long cycle analogous to a four-year cycle of the prototype RR Lyr. The limits of the shorter period produce a beating period that is approximately twice as big as a 1403-day period. The newly revealed Blazhko star RZ CVn seems to undergo changes in the amplitude of the modulation, as well as in the basic pulsation and Blazhko periods. We found that the incidence rate of the Blazhko RR Lyraes is at least 31%, more likely even higher. It was also found that the majority of the Blazhko variables show triplet structures in their frequency spectra and that in 89% of these cases, the peak with larger amplitude is on the right-hand side of the main pulsation component.

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Section: Statistics Of the Blazhko Variables In The Samplementioning

confidence: 89%

“…Among others, Kinemuchi et al (2006) and Wils et al (2006) utilized data from Northern sky variability survey (NSVS, Woźniak et al 2004), e.g. Kovács (2005), Szczygieł et al (2009) studied RR Lyraes based on ASAS data, and Drake et al (2013) dealt with RR Lyraes measured in Catalina sky survey 1 .…”

Section: Introductionmentioning

confidence: 99%

Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys

Skarka

2014

A&A

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“…Good examples in the field of classification, are the series of papers on MACHO, OGLE and ASAS data (for RR Lyrae stars, for example, see Alcock et al (2003), Soszynski et al (2003) and Wils et al (2006), for MACHO, OGLE and the NSVS respectively), where catalogues of distinct variability classes are compiled according to several selection criteria (rules) and, in some occasions, with human intervention. Basically, the problem of supervised classification of variable objects can be described as that of defining general boundaries (hard or fuzzy) in the hyperspace of the features that describe the classes, based on a set of examples of each class.…”

Section: Automatic Variability Classificationmentioning

confidence: 99%

VSOP: the variable star one-shot project

Dall¹,

Foellmi²,

Pritchard

et al. 2007

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Context. About 500 new variable stars enter the General Catalogue of Variable Stars (GCVS) every year. Most of them however lack spectroscopic observations, which remains critical for a correct assignement of the variability type and for the understanding of the object. Aims. The Variable Star One-shot Project (VSOP) is aimed at (1) providing the variability type and spectral type of all unstudied variable stars, (2) process, publish, and make the data available as automatically as possible, and (3) generate serendipitous discoveries. This first paper describes the project itself, the acquisition of the data, the dataflow, the spectroscopic analysis and the on-line availability of the fully calibrated and reduced data. We also present the results on the 221 stars observed during the first semester of the project. Methods. We used the high-resolution echelle spectrographs HARPS and FEROS in the ESO La Silla Observatory (Chile) to survey known variable stars. Once reduced by the dedicated pipelines, the radial velocities are determined from cross correlation with synthetic template spectra, and the spectral types are determined by an automatic minimum distance matching to synthetic spectra, with traditional manual spectral typing cross-checks. The variability types are determined by manually evaluating the available light curves and the spectroscopy. In the future, a new automatic classifier, currently being developed by members of the VSOP team, based on these spectroscopic data and on the photometric classifier developed for the COROT and Gaia space missions, will be used. Results. We confirm or revise spectral types of 221 variable stars from the GCVS. We identify 26 previously unknown multiple systems, among them several visual binaries with spectroscopic binary individual components. We present new individual results for the multiple systems V349 Vel and BC Gru, for the composite spectrum star V4385 Sgr, for the T Tauri star V1045 Sco, and for DM Boo which we re-classify as a BY Draconis variable. The complete data release can be accessed via the VSOP web site.

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“…This is partially due to the moderate number of known stars: at the moment of this writing we know 30 more or less bright RRd stars (V < 14 mag) in the Galactic field discovered by the NSVS and ASAS all-sky variability surveys (Wils et al 2006;Szczygiel & Fabrycky 2007;Pilecki & Szczygiel 2007;Khruslov 2007). Only two stars (GSC 4868-0831 and V372 Ser) are known with V < 11.5 mag.…”

Section: Introductionmentioning

confidence: 99%