  The infrared flux method (IRFM) has been applied to a sample of 135 dwarf and
36 giant stars covering the following regions of the atmospheric parameters
space: 1) the metal-rich ([Fe/H]>0) end (consisting mostly of planet-hosting
stars), 2) the cool (Teff<5000 K) metal-poor (-1<[Fe/H]<-3) dwarf region, and
3) the very metal-poor ([Fe/H]<-2.5) end. These stars were especially selected
to cover gaps in previous works on Teff vs. color relations, particularly the
IRFM Teff scale of A. Alonso and collaborators. Our IRFM implementation was
largely based on the Alonso et al. study (absolute infrared flux calibration,
bolometric flux calibration, etc.) with the aim of extending the ranges of
applicability of their Teff vs. color calibrations. In addition, in order to
improve the internal accuracy of the IRFM Teff scale, we recomputed the
temperatures of almost all stars from the Alonso et al. work using updated
input data. The updated temperatures do not significantly differ from the
original ones, with few exceptions, leaving the Teff scale of Alonso et al.
mostly unchanged. Including the stars with updated temperatures, a large sample
of 580 dwarf and 470 giant stars (in the field and in clusters), which cover
the ranges: 3600 K<Teff<8000 K, -4.0<[Fe/H]<+0.5, have Teff homogeneously
determined with the IRFM. (Abridged)
