New UBV photometry for 878 luminous member stars of the Large Magellanic Cloud (LMC) and 13 stars of uncertain membership is presented. The data will be available at Centre de Données astronomiques de Strasbourg. Including former observations now UBV data are available for altogether 2470 luminous LMC stars and 2106 foreground stars plus 65 stars of uncertain membership. The observations have been used already for several investigations dealing e.g. with interstellar reddening lines and intrinsic colours, the dust distribution and the calibration of charge‐coupled device exposures.

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Abstract. In addition to the list of UBV photometries of 955 galactic foreground stars in the direction to the Large Magellanic Cloud published by Gochermann et al. (1993a), a supplement of 545 stars is presented, which have been measured with the same photometric accuracy. Moreover, less reliable photometries of 379 further foreground stars are listed in a separate table. The homogeneous data base of more than 1 500 high accuracy photometries represented by these stars has been used to construct a reddening distribution map of the galactic foreground towards the LMC by .

Abstract. In order to construct a comprehensive HRD of early type stars in the Large Magellanic Cloud (LMC) in the first step the reddenings of individual stars and the LMC reddening law have been investigated. 1942 LMC member stars with good UBVphotometries from the Bochum photometry data base have been first corrected individually for galactic foreground reddening. From stars with good spectral classification the slope of the LMC internal reddening line E U−B E B−V was calculated for each spectral subclass between O3 and A4. A remarkable difference to the galactic reddening law was found. The slope of the reddening line first decreases for stars from O3 to B0, and then increases rapidly between B0 and B3 from ∼0.7 to ∼1.1. For later type stars it remains higher than for early type stars. This effect has important consequences for all extinction corrections. We checked this using different methods. Because no evidence for systematically wrong classifications was found, the differences in the reddening slopes must be caused by the ISM of the LMC itself. Four possible causes are considered.