We have estimated magnitudes corrected to mean intensity for LMC type II Cepheids found in the OGLE‐III survey. Period‐luminosity relations (PLRs) are derived in as well as in a reddening‐free VI parameter. The BL Her stars and the W Vir stars ( to 20 d) are co‐linear in these PLRs. The slopes of the infrared relations agree with those found previously for type II Cepheids in globular clusters within the uncertainties. Using the pulsation parallaxes of V553 Cen and SW Tau, the data lead to an LMC modulus of uncorrected for any metallicity effects. We have now established the PLR of type II Cepheids as a distance indicator by confirming that (almost) the same PLR satisfies the distributions in the PL diagram of type II Cepheids in (at least) two different systems, i.e. the LMC and Galactic globular clusters, and by calibrating the zero point of the PLR. RV Tau stars in the LMC, as a group, are not co‐linear with the shorter‐period type II Cepheids in the infrared PLRs in marked contrast to such stars in globular clusters. We note differences in period distribution and infrared colors for RV Tau stars in the LMC, globular clusters and Galactic field. We also compare the PLR of type II Cepheids with that of classical Cepheids.
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Research Article| September 16 2009
Period‐Luminosity Relation for Type II Cepheids
Michael W. Feast;
AIP Conf. Proc. 1170, 96–98 (2009)
Noriyuki Matsunaga, Michael W. Feast, John W. Menzies; Period‐Luminosity Relation for Type II Cepheids. AIP Conf. Proc. 16 September 2009; 1170 (1): 96–98. https://doi.org/10.1063/1.3246584
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