Period-Luminosity Relations for Type II Cepheids and their Application

TL;DR

This study derives period-luminosity relations for Type II Cepheids in the LMC, compares them with globular cluster stars, and discusses implications for distance measurements and stellar classification.

Contribution

It provides new infrared and optical PL relations for LMC Type II Cepheids and compares them with globular cluster stars, enhancing understanding of their properties and distance scale applications.

Findings

Infrared PL slopes agree with globular cluster stars within uncertainties.

LMC distance modulus estimated at 18.46 +- 0.10 mag.

Galactic RV Tau stars show different properties from globular cluster stars.

Abstract

JHKs magnitudes corrected to mean intensity are estimated for LMC type II Cepheids in the OGLE-III survey. Period-luminosity (PL) relations are derived in JHKs as well as in a reddening-free VI parameter. Within the uncertainties the BL Her stars (P < 4 d) and the W Vir stars (P = 4 to 20 d) are co-linear in these PL relations. 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 uncorrected for any metallicity effects of 18.46 +- 0.10 mag. The type II Cepheids in the second-parameter globular cluster, NGC 6441, show a PL(VI) relation of the same slope as that in the LMC and this leads to a cluster distance modulus of 15.46 +- 0.11 mag, confirming the hypothesis that the RR Lyrae variables in this cluster are overluminous for their metallicity. It is suggested that the Galactic variable kappa Pav is a member of the peculiar W Vir class found by the OGLE-III group in the LMC. Low-resolution spectra of OGLE-III type II Cepheids with P > 20 d (RV Tau stars) show that a high proportion have TiO bands; only one has been found showing C_2. The LMC RV Tau stars, as a group, are not co-linear with the shorter-period type II Cepheids in the infrared PL relations in marked contrast to such stars in globular clusters. Other differences between LMC, globular cluster and Galactic field type II Cepheids are noted in period distribution and infrared colours.