All observations listed in Tables 2 and 3 were carried out at the Bochum 61 cm and the ESO 50 cm telescopes at La Silla, Chile, from November 1990 to January 1994. A complete journal of observations is given in Table 1 (click here). Details on the technical realization of the UBV photometric systems (photomultipliers and filters) can be found in Paper I. The equipment used at the Bochum Telescope for the periods 1992/93 and 1993/94 is identical to that introduced in November 1991 (EMI 9789 B photomultiplier).
Photometric standard stars, and first and second order atmospheric extinction coefficients were always
measured as described in Paper I. In 1993/94 no second order extinction
coefficients were determined at the Bochum Telescope, but the values taken
from the 1992/93 observations (
, 
,
). After the Mt. Pinatubo volcanic eruption in June
1991, always daily first order extinction coefficients were applied to reduce
the data in order to account for intermittently ocurring large fluctuations
of the atmospheric extinction (cf. Paper I). A clear trend of the
extinction could be noticed from 1991 to 1994 due to the ``fall-out" of
Pinatubo volcanic dust from the atmosphere, with the average first
order extinction coefficients, 
, decreasing from 
in
1991/92, over 
in 1992/93, to finally 
in 1993/94.
The last value is still larger than the average coefficient of 
found in 1990, before the eruption (Paper I; Grothues
& Gochermann 1992).
Transformations of the photometries to the Johnson and Cousins UBV systems, averaging of all measurements of each star from different nights, and the determination of errors and qualities, were also performed exactly in the way described in Paper I.
Table: 1 Journal of Observations (Photometric systems:
J = Johnson,
C = Cousins)