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The Galactic Cepheid period-luminosity relation revisited using bona fide cluster Cepheids

Anderson, Richard I. ; Mowlavi, Nami ; Eyer, Laurent

In: Proceedings of the International Astronomical Union, 2012, vol. 8, no. S289, p. 153-156

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    Title
    • The Galactic Cepheid period-luminosity relation revisited using bona fide cluster Cepheids
    Author
    • Anderson, Richard I.. Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, CH-1290 Versoix, Switzerland email: richard.anderson@unige.ch
    • Mowlavi, Nami. Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, CH-1290 Versoix, Switzerland email: richard.anderson@unige.ch
    • Eyer, Laurent. Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, CH-1290 Versoix, Switzerland email: richard.anderson@unige.ch
    Document Type
    • Postprint
    Language
    • English
    Published in
    • Proceedings of the International Astronomical Union, 2012, vol. 8, no. S289, p. 153-156. Cambridge University Press
    Other Version
    OAI-PMH Identifier
    • oai:doc.rero.ch:291760
    Summary
    Classical Cepheids in Galactic open clusters (cluster Cepheids: CCs) have been studied extensively for multiple decades, thanks to their importance as calibrators of the Galactic Cepheid period-luminosity relation (PLR). Here we revisit the calibration of the Galactic PLR using a new sample of CCs, since even recent calibrations show significant discrepancies. The CC sample employed for the calibration is based on the preliminary results of a self-consistent, eight-dimensional all-sky census. This census is based mostly on literature data, supplemented with high-precision radial-velocity observations from both hemispheres. New CCs are identified from our census and the degree of confidence in membership is quantified for known candidates. Using only bona fide CCs, we obtain MV = (−3.08 ± 0.50) log P + (−0.94 ± 0.42) mag, which is in perfect agreement with the results by Sandage, Tammann, and Reindl, albeit with larger error bars and an rms of 0.21 mag. The key to obtaining a meaningful calibration is to employ accurate cluster distance moduli and space reddening values. A homogeneous study of all bona fide host clusters would be desirable to increase precision and confidence in the calibration