The absolute spectral energy distribution data for 60 stars of the southern hemisphere in the range 310-1105 nm with a step of 2.5 nm are given. The observations were made in the Chilean and the Bolivian expeditions. The absolute calibration of the data is based on Vega. For variable stars L2 Pup, V806 Cen and RR Seo, the individual spectral distributions in the range 495-1105 nm at different Julian Days are given. Spectrophotometric catalogue of 60 selected southern stars 363 The catalogue A

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... st of the observed stars is given in Table 1 . The following information about the stars is given: HR and HD numbers, the Bayer's name, the number of independent scans of the spectrum (Chilean/Bolivian), the equatorial coordinates for 2000.0, the spectral type from the 1982 version of the HR catalogue, the magnitude V and the color index B-V from the same source. Data on binarity and variability are given in the remarks following the table. For the visual binaries, separation and Am are taken from the same source. For the variables, the variability type and magnitudes at the maximum and minimum light and the period are from the General Catalogue of Variable Stars (Kholopov et al. 1985(Kholopov et al. -1990. The final energy distribution data in the range 310-1105 nm with a step of 2.5 nm, expressed in m = -2.5 log E (E is in erg/s-cm 2 -cm), are given in Tables 2, 3 and 4. Table 2 contains the combined data covering the wavelengths 310-1105 nm, Table 3 contains only the Bolivian data covering 495-1105 nm and Table 4 (a, b, c) contains three variable stars (L2 Pup, V806 Cen and RR Seo) for which the individual energy distribution curves are given at different Julian Days. The standard deviations σ of the data differ in different spectral regions: < 0.02 mag for the zones of the continuous spectrum and < 0.05 to 0.07 mag for the border zones and within the spectral lines. Acknowledgments. The authors would like to express their deep gratitude to K.V. Rumyantsev for his participation in updating and maintaining the observational facilities and for his assistance in the observations in Bolivia, to A.V. Mikhailov for writing a software, to D.D. Polozhentsev, the head of the Bolivian Expedition, for ensuring good working conditions during the expedition and to many other colleagues in the Pulkovo Observatory and in Bolivia for their real and useful assistance in our work.