Table 2 (click here) lists the SMC- and LMC objects, and Table 3 (click here) the galactic objects,
respectively, identified by their numbers,
the spectral type, for the SMC and LMC only the galactic foreground reddening
(see further), the adopted reddening, the mean Hp and 
magnitude,
= 
, the maximum range ever observed (only the micro
variations if an eclipse, or an SD (S Dor)-type variability is involved),
(for most of the stars derived from the spectral type
calibration of de Jager & Nieuwenhuijzen 1987) and at last 
.
For the SMC and LMC is in most cases based on the distance
moduli 19.1 and 18.6, respectively, or are based on an indirect method.
For the galactic objects is taken from various references.
The galactic foreground reddening 
of the Magellanic Cloud objects
were extracted from Figs. 7b, c of Schwering & Israel (1991). They
used the HI distribution to separate the galactic infrared emission in front
of the Clouds themselves and constructed maps of the smoothed galactic
foreground colour excess distribution towards the Clouds. It
should be emphasized that apart from local fluctuations, smaller than the
resolution of 
, these values are only a lower limit. The reddening in
the Clouds should be added, but in most cases it is unknown. If a literature
value for the total reddening is known, but lower than the galactic
foreground reddening, the latter
is used for the determination of instead of the literature
value. If no literature value is known then it is derived from the
spectrum/
relationship (Schmidt-Kaler 1982) and the
observed 
. If this reddening is lower than the galactic foreground
reddening, the latter is used. Therefore, in many cases is
presumably a lower limit.