  We revisited the short period Type II Cepheids (T2Cs), called the BL Herculis
(BLHs), in the Galactic Field to derive a homogeneous analysis of their Fourier
parameters. Only V-band data were compiled to make sure that it was directly
comparable between the known variables of the OGLE-III catalogue and the 59
individual objects classified as short period Type II Cepheids in the General
Catalogue of Variable Stars (GCVS) we had in our sample. The derived Fourier
parameters were used to make the distinction between different classes of
variables. From the 59 stars we found 19 BLHs, 19 fundamental mode Anomalous
Cepheids (ACs) (8 of them were already known from the Catalina Sky Survey
(CSS)), 1 first overtone AC, 2 were found to be possible peculiar W Virginis
(pWVir), 11 classical Cepheids (DCEPs), and 7 stars were not pulsating
variables at all. As a result we created a list of bright BLH stars in the
Galactic Field, and separated the ACs, as well as other objects that were
misclassified. The number of true BLHs decreased in our sample by more than
50%. We gathered the metallicity from spectroscopic measurements published in
the literature. While the number of actual measurements is low, it is highly
suggestive that ACs are metal poor. The mean metallicity from 8 measurements in
4 stars (UY Eri having 5 different [Fe/H] data points) is -1.12 dex, but if the
higher value metallicity outliers of UY Eri are left out the mean metallicity
becomes -1.88 dex, regardless if the AC is in the Milky Way itself or in a
cluster. On the other hand, BLHs seem to have a Solar-like metallicity of 0 dex
averaged from 21 measurements of 10 stars.
