BV(Rl) KC light curves are presented for 27 type la supemovae discovered during the course of the Calán/Tololo Survey and for two other SNe la observed during the same period. Estimates of the maximum hght magnitudes in the B, V, and I bands and the initial decline rate parameter Am 15 (B) are also given.

We present a compilation of UBVRIz light curves of 51 type II supernovae discovered during the course of four different surveys during 1986-2003: the Cerro Tololo Supernova Survey, the Calán/Tololo Supernova Program (C&T), the Supernova Optical and Infrared Survey (SOIRS), and the Carnegie Type II Supernova Survey (CATS). The photometry is based on template-subtracted images to eliminate any potential host galaxy light contamination, and calibrated from foreground stars. This work presents these photometric data, studies the color evolution using different bands, and explores the relation between the magnitude at maximum brightness and the brightness decline parameter (s) from maximum light through the end of the recombination phase. This parameter is found to be shallower for redder bands and appears to have the best correlation in the B band. In addition, it also correlates with the plateau duration, being shorter (longer) for larger (smaller) s values.

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The proper motion of the Large Magellanic Cloud (LMC) relative to three background quasi-stellar objects has been determined using 125 CCD frames taken from 1989.0 to 1997.2 at the Cassegrain focus of the CTIO 1.5 m telescope. The observation and reduction methods are fully described. The results are compared with those obtained by other authors who use di †erent methods and reference systems for the proper motions. This comparison results in a good agreement for and a rather large discrepancy k a cos d for Our LMC proper motion seems to indicate that the LMC is not leading the Magellanic Stream. k d . Finally, from the newly determined proper motion, the LMC spatial velocity vector is calculated, which in turn is used to determine the lower limit of the mass of the Galaxy contained within 50 kpc from its center. The possible consequences of our results on the dynamical status of the LMC are discussed.

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