A comprehensive study of the SX Phoenicis star  BL Camelopardalis

Fauvaud, S.; Rodríguez, E.; Zhou, A. Y.; Sareyan, J. P.; Ribas, I.; Reed, M. D.; Klingenberg, G.; Farrell, Jeremiah; Michelet, J.; Robinson, Sarah E.; Santacana, G.; Rives, J.-J.

doi:10.1051/0004-6361:20053841

Cited by 20 publications

(35 citation statements)

References 34 publications

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“…d 003 and period about 150 days was detected in the (O-C) diagram, produced by the light-time effect in a binary or multiple system (Fauvaud et al 2007). This effect leads to a slight shift of the main frequency, f 0 , depending on the chosen data set.…”

Section: Frequency Analysismentioning

confidence: 98%

“…The observations considered as additional (i.e. acquired using "smaller" telescopes or "without any filter") will be used to determine additional times of light maxima, in order to further improve the (O-C) analysis (Fauvaud et al 2007). In the present work we describe the results concerning the star's pulsational content.…”

Section: Obsmentioning

confidence: 99%

“…The most remarkable one is that of the high-amplitude δ Sct star V974 Oph (∆V = 0. m 4, Rodríguez et al 2000) where Poretti (2003) finds five independent frequencies, with several likely nonradial modes, resembling the much more complex power spectra of the lowamplitude δ Sct variables. In a few other cases of high-amplitude pulsators, previously assumed as pure monoperiodic (DY Peg) or biperiodic (AI Vel, SX Phe or RV Ari) (Garrido & Rodríguez 1996;Walraven et al 1992;Pócs et al 2002), one or more additional radial and/or nonradial excited modes have been detected with very small amplitudes. Hence, these objects can be considered as very interesting targets for asteroseismological studies.…”

Section: Introductionmentioning

confidence: 96%

“…This is a field high-amplitude SX Phe variable (∆V = 0. m 33, Rodríguez et al 2000) with very low metal content ([M/H] = −2. 4, McNamara 1997) where multiperiodicity has been detected in its light curves by different authors (see Fauvaud et al 2006, for a review, hereafter F06). Besides the main periodicity, at least six additional independent modes seem to be excited in this star, the majority probably nonradial.…”

Section: Introductionmentioning

confidence: 99%

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The field high-amplitude SX Phoenicis variable BL Camelopardalis: results from a multisite photometric campaign

Rodríguez‐López¹,

Fauvaud²,

Farrell³

et al. 2007

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Context. BL Cam is an extreme metal-deficient field high-amplitude SX Phe-type variable where a very complex frequency spectrum is detected, with a number of independent nonradial modes excited, unusual among the high-amplitude pulsators in the Lower Classical Instability Strip.Aims. An extensive and detailed study has been carried out to investigate the pulsational content and properties of this object. Methods. The analysis is based on 283 h of CCD observations obtained in the Johnson V filter, during a long multisite photometric campaign carried out along the Northern autumn-winter of [2005][2006]. Additionally, multicolour BI photometry was also collected to study the phase shifts and amplitude ratios, between light curves obtained in different filters, for modal discrimination of the main excited modes. Results. The detailed frequency analysis revealed a very rich and dense pulsational content consisting of 25 significant peaks, 22 of them corresponding to independent modes: one is the already known main periodicity f 0 = 25.5765 cd −1 (∆V = 153 mmag) and the other 21 are excited modes showing very small amplitudes. Some additional periodicities are probably still remaining in the residuals. This represents the most complex spectrum ever detected in a high-amplitude pulsator of this type. The majority of the secondary modes suspected from earlier works are confirmed here and, additionally, a large number of new peaks are detected. The amplitude of the main periodicity f 0 seems to be stable during decades, but the majority of the secondary modes show strong amplitude changes from one epoch to another. The suspected fundamental radial nature of the main periodicity of BL Cam is confirmed, while the secondary peak f 1 = 25.2523 cd −1 is identified as a nonradial mixed mode g 4 with = 1. The radial double-mode nature, claimed by some authors for the main two frequencies of BL Cam, is not confirmed. Nevertheless, the frequency f 6 = 32.6464 cd −1 could correspond to the first radial overtone.

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Section: Frequency Analysismentioning

confidence: 98%

Section: Obsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

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The field high-amplitude SX Phoenicis variable BL Camelopardalis: results from a multisite photometric campaign

Rodríguez‐López¹,

Fauvaud²,

Farrell³

et al. 2007

A&A

Self Cite

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“…Ribeiro et al 2007) and the extreme metal-deficient, high-amplitude SX Phe variable BL Cam (e.g. Fauvaud et al 2010).…”

Section: Boao 18 M Telescopementioning

confidence: 99%

The VVV Templates Project Towards an automated classification of VVV light-curves

Angeloni

Ramos

Catelan

et al. 2014

A&A

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Context. The Vista Variables in the Vía Láctea (VVV) ESO Public Survey is a variability survey of the Milky Way bulge and an adjacent section of the disk carried out from 2010 on ESO Visible and Infrared Survey Telescope for Astronomy (VISTA). The VVV survey will eventually deliver a deep near-IR atlas with photometry and positions in five passbands (ZY JHK S ) and a catalogue of 1−10 million variable point sources -mostly unknown -that require classifications. Aims. The main goal of the VVV Templates Project, which we introduce in this work, is to develop and test the machine-learning algorithms for the automated classification of the VVV light-curves. As VVV is the first massive, multi-epoch survey of stellar variability in the near-IR, the template light-curves that are required for training the classification algorithms are not available. In the first paper of the series we describe the construction of this comprehensive database of infrared stellar variability. Methods. First, we performed a systematic search in the literature and public data archives; second, we coordinated a worldwide observational campaign; and third, we exploited the VVV variability database itself on (optically) well-known stars to gather high-quality infrared light-curves of several hundreds of variable stars. Results. We have now collected a significant (and still increasing) number of infrared template light-curves. This database will be used as a training-set for the machine-learning algorithms that will automatically classify the light-curves produced by VVV. The results of such an automated classification will be covered in forthcoming papers of the series.

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Pulsating Stars

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A comprehensive study of the SX Phoenicis star BL Camelopardalis

Cited by 20 publications

References 34 publications

The field high-amplitude SX Phoenicis variable BL Camelopardalis: results from a multisite photometric campaign

The field high-amplitude SX Phoenicis variable BL Camelopardalis: results from a multisite photometric campaign

The VVV Templates Project Towards an automated classification of VVV light-curves

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