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JHKs  magnitudes corrected to mean intensity are estimated for Large Magellanic Cloud (LMC) type II Cepheids in the OGLE‐III survey the third phase of the Optical Gravitational Lensing Experiment (OGLE). Period–luminosity (PL) relations are derived in  JHK  s  as well as in a reddening‐free  VI  parameter. Within the uncertainties, the BL Her stars  ( P  &lt; 4 d)  and the W Vir stars (  P = 4  to 20 d) are colinear 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  κ  Pavonis 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  &gt; 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 colinear 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.

Period–luminosity relations for type II Cepheids and their application