The results of the photometries are arranged in two tables. Table 2 contains a supplement of UBV photometries of 545 galactic foreground stars in front of the LMC, which have been measured with the same accuracy as the data presented in Table 7 of Paper I. The criterion for the selection to this list demands at least two independent measurements of a star in different photometric nights, and a photometric accuracy corresponding to quality 2 for V and B-V as defined by Nicolet (1978), i.e. errors smaller than 006.
In a second table (Table 3), all photometries of foreground stars are
collected for which only one measurement exists, or the qualities
for V or B-V are 1 (
). Despite their ``bad
photometries" (most of the stars were measured only once, but have small
photometric errors), these 379 stars are published here, because no
further photometric observations are planned. Two more stars (one
in Table 2 and one in Table 3) turned out to be identical with stars already
published in Paper I. Nevertheless, their additional photometries have
been published here (cf. the remarks to the tables).
Contrary to Paper I, where the stars were ordered by FD-numbers (catalogues of )FD70, Tables 2 and 3 list the entries according to their HD/HDE numbers. Stars which do not appear in the HD/HDE catalogues, are given the designation of the catalogues they were taken from. These designations are listed subsequent to the HD/HDE entries in numerical and alphabetical order (Col. 2). Also included in both tables are those foreground stars which have been measured erroneously instead of others that should have been observed. These stars are listed under the designation of the catalogued star nearby and marked by an ending ``F" (= false), e.g. ``HDE 268841F" if HDE 268841 should have been measured. All 35 erroneous stars are identified in Fig. 3.2 (click here) on finding charts reproduced from the Southern Digitized Sky Survey (ESO-SERC).
Figure 1: a) Histogram of 1604 LMC foreground stars with
high quality UBV photometries taken from Papers I and II, and the
literature (see text). Plotted are absolute numbers, 
,
per magnitude interval, 
. b) Cumulative
star numbers, log
, as a function of V with the
cut-off magnitude, 
, and the slopes indicated
(see text). The class interval is again 
Following, is a description of the columns of Tables 2 and 3:
) indicates a remark
at the end of the table, while a
number refers to a finding chart
number in Fig. 3.2 (click here).
The histogram in Fig. 1 (click here)a plots the star numbers, 
, as a function
of V magnitudes for all stars with reliable photometries (as defined in
Sect. 3.1), i.e. all stars from Paper I (Table 7) and Paper II (Table 2),
together with 104 stars of equivalent qualities from the literature. The
cut-off of the exponential increase in the star numbers, 
(Fig. 1 (click here)a),
and the linear slope of the cumulative star numbers, log
(Fig. 1 (click here)b), as a function of V, at 
suggest that
the sample can be taken as a statistically representative subsample of LMC
galactic foreground stars for 
(cf. Paper I). In their
different catalogues, Fehrenbach & Duflot selected the foreground stars by
means of objective-prism radial-velocities, leaving out all those objects
that showed overlapping spectra, especially in the crowded LMC bar. This
makes the sample of photometries presented in Fig. 1 (click here) a magnitude limited
subsample of all LMC galactic foreground stars. However, Fehrenbach
& Duflot do not give any statements on the completeness of their selections.
A detailed analysis carried out by Oestreicher & Schmidt-Kaler
(1995) suggests that the limit of completeness for
the G to M type stars which comprise the majority of the objects
listed in Papers I and II is indeed given by an apparent V
magnitude of about 115. For the fewer B to F type stars, the
limit is even shifted to fainter magnitudes of 125 to 135.
The cumulative star numbers, for the representative sample (
) display a slope of (
) mag
as a function of V
which is compatible with the average all-sky value of 0.40 at 
(cf. Paper I). There is, however, a significant difference between the slopes
for 
with 
mag
and 
with 
mag
which cannot be explained by
an incomplete selection of stars, nor it is caused by the influence of
interstellar extinction (dark clouds), as the galactic foreground reddening
in the field is generally low (
; see below). Rather,
the change of the slope points to different stellar populations in the
galactic foreground (cf. Oestreicher & Schmidt-Kaler
1995).
Figure 2: Color-color diagram for the same stars as Fig. 1. The
ZAMS and the respective line for the giants taken from
Schmidt-Kaler () are plotted for comparison
Figure 2 (click here) presents a color-color diagram for the same 1604 stars as plotted
in Fig. 1 (click here). Most of the stars belong to the main sequence and show only
small to moderate reddenings. A detailed investigation by Oestreicher
et al. (1995) gives 
to 
, and an
average of 
. Furthermore, a
substantial number of K-type giants (luminosity class III)
populate the lower right part of the diagram (cf. Paper I).
Figure 3: Identification charts for all stars marked by a
number in column ``Remarks" in Tables 2 and 3. These numbers
are given in brackets below each chart. All charts are
reproduced as a gnomonic projection from the Digitized Sky
Survey (ESO-SERC) with an effective passband between 400 and
550 nm. The field of view is a 
square at a resolution of about 2''. North is always up, East
to the left
Acknowledgements
We gratefully acknowledge the Deutsche Forschungsgemeinschaft (DFG) for supporting the project under grants nos. Schm 160/39-1 and 2.