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|Title:||The VMC Survey - XIII. Type II Cepheids in the Large Magellanic Cloud||Authors:||RIPEPI, Vincenzo
Moretti, Maria Ida
Cioni, M. -R. L.
de Grijs, R.
Emerson, J. P.
Groenewegen, M. A. T.
Ivanov, V. D.
Piatti, A. E.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||446||Issue:||3||First Page:||3034||Abstract:||The VISTA (Visible and Infrared Survey Telescope for Astronomy) survey of the Magellanic Clouds System (VMC) is collecting deep K<SUB>s</SUB>-band time-series photometry of the pulsating variable stars hosted in the system formed by the two Magellanic Clouds and the Bridge connecting them. In this paper, we have analysed a sample of 130 Large Magellanic Cloud (LMC) Type II Cepheids (T2CEPs) found in tiles with complete or near-complete VMC observations for which identification and optical magnitudes were obtained from the OGLE III (Optical Gravitational Lensing Experiment) survey. We present J and K<SUB>s</SUB> light curves for all 130 pulsators, including 41 BL Her, 62 W Vir (12 pW Vir) and 27 RV Tau variables. We complement our near-infrared photometry with the V magnitudes from the OGLE III survey, allowing us to build a variety of period-luminosity (PL), period-luminosity-colour (PLC) and period-Wesenheit (PW) relationships, including any combination of the V, J, K<SUB>s</SUB> filters and valid for BL Her and W Vir classes. These relationships were calibrated in terms of the LMC distance modulus, while an independent absolute calibration of the PL(K<SUB>s</SUB>) and the PW(K<SUB>s</SUB>, V) was derived on the basis of distances obtained from Hubble Space Telescope parallaxes and Baade-Wesselink technique. When applied to the LMC and to the Galactic globular clusters hosting T2CEPs, these relations seem to show that (1) the two Population II standard candles RR Lyrae and T2CEPs give results in excellent agreement with each other; (2) there is a discrepancy of ̃0.1 mag between Population II standard candles and classical Cepheids when the distances are gauged in a similar way for all the quoted pulsators. However, given the uncertainties, this discrepancy is within the formal 1σ uncertainties.||Acknowledgments:||We wish to thank our referee, Dr C. D. Laney, for his helpful and competent review of the manuscript. VR warmly thanks Roberto Molinaro for providing the program for the spline interpolation of the light curves. Partial financial support for this work was provided by PRIN-INAF 2011 (PI: Marcella Marconi) and PRIN MIUR 2011 (PI: F. Matteucci). We thank the UK's VISTA Data Flow System comprising the VISTA pipeline at the Cambridge Astronomy Survey Unit (CASU) and the VISTA Science Archive at Wide Field Astronomy Unit (Edinburgh) (WFAU) for providing calibrated data products supported by the STFC. This work was partially supported by the Gaia Research for European Astronomy Training (GREAT-ITN) Marie Curie network, funded through the European Union Seventh Framework Programme ([FP7/2007- 1312 2013] under grant agreement no. 264895). RdG acknowledges research support from the National Natural Science Foundation of China (NSFC) through grant 11373010. This work was partially supported by the Argentinian institutions CONICET and Agencia Nacional de Promoción Científica y Tecnológica (ANPCyT).||URI:||http://hdl.handle.net/20.500.12386/24639||URL:||https://academic.oup.com/mnras/article/446/3/3034/2892558||ISSN:||0035-8711||DOI:||10.1093/mnras/stu2260||Bibcode ADS:||2015MNRAS.446.3034R||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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