Up: Broad-band JHK(L') photometry of
The precise relationships which link the physical parameters of stellar atmospheres (i.e.
, log(g) and
[Fe/H]) with measured colours, photometric indices or
spectral features of stars play a central role connecting several areas of stellar physics.
In particular, the accurate calibration of
the scale of stellar effective temperatures is of increasing importance
in spectroscopic studies since
-colour or -spectral type
calibrations are usually adopted in deriving chemical abundances.
On the one hand, noteworthy differences in the
derived ratios between different elements are obtained when
analysing the same spectra with different temperature scales
(e.g. King 1994), thus implying quite
different scenarios for the chemical evolution of the galaxy. On the other hand, non-negligible variations in primordial abundances may be deduced from
the adoption of diverse temperature scales in spectroscopic analysis
(e.g. Bonifacio & Molaro 1997). Stellar effective temperatures are also a
most influential consideration in the observed differences of the giant branch and
main sequence slopes
when comparing empirical lines of globular clusters with theoretical
isochrones (e.g. Bell 1992). Here a part of the discrepancy might be induced by the
adoption of an incorrect temperature scale (since this is crucial in the
transformation of the HR diagram from the theoretical
to the observational plane).
Furthermore, the effective temperature scale is necessary
for the analysis of the global behaviour of stellar atmosphere
models (e.g. Castelli et al 1997),
in particular it is a relevant parameter for the modelling of
molecular bands in the synthesis of infrared
colours (e.g. Bell & Gustafsson 1989). Finally,
it is also important for the overall colour synthesis of stellar populations
(e.g. Vazdekis et al. 1996).
We have carried out these observations as a part of a continuing programme
aimed at the (semi-)empirical calibration of
as a function of
photometric colours, [Fe/H] and
for population I and II stars. The
part of the programme concerning stars with
(i.e.
the main sequence and the blue part of subgiant branch) has been recently
accomplished, and is described in
Alonso et al. (1996a,b; Papers III and IV respectively).
As for the part of the programme devoted to the giant branch temperature scale, we
have selected a sample of
400 stars
with spectral types from F0 to K5 covering a wide range in metal
content (+0.5 > [Fe/H] > -3.0). In order to obtain their
effective temperatures, we will apply the Infrared Flux Method
(Blackwell et al. 1990), which has proved useful for deriving stellar effective temperatures of
metal-poor giants of globular clusters
(Arribas & Martínez-Roger 1987a;
Arribas et al. 1991). Furthermore, this method relies only weakly on theoretical models and its main requirement from
the observational side is
the measurement of accurate photometry needed to derive near infrared
monochromatic fluxes. In this paper, we present and discuss the results of the observational
campaign of near-IR photometry for the stars of the sample lacking previously measured JHK(L') magnitudes, and also for stars common to other systems
which will be necessary to homogenize the photometric measurements taken
from the literature. The infrared magnitudes will be used in a later stage
of the work to derive IR monochromatic fluxes for the application of the
Infrared Flux Method.
Up: Broad-band JHK(L') photometry of
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