Spectrophotometric observations of OQ 208 over the time period between March 1985 and February 1991 are presented. It is found that the H-beta flux varies strongly over the period of observation. The peculiar profiles of the Balmer lines are variable, and their variations make it possible to place some unambiguous constraints on the broad line

We observed the λ 4232 Å CH+ interstellar line in the direction of the Sco OB 1 association (d ≃ 2 kpc) with the aim of detecting variations of the 12C/13C ratio at large distances from the Sun. The collection of 30 high-resolution spectra (λ/δλ = 1O5) of the V-6.3 stars HD 152235 and HD 152424 by means of the ESO 3.6m telescope allowed us to

BVRI surface photometry is presented for the interacting galaxy pair Arp 86 (NGC 7753-7752). Deep high-resolution images were obtained in order to study the faint tidal features. The bridge was found to be bluer than the tail both in V - R and B - V, the V - R color probably suggesting enhanced long-term star formation in the bridge. The end of the

A 2D array of optical fibers generating simultaneous spectral and spatial information has been used to observe the central 13 arcsec of NGC 5728; on this basis, an analysis of the morphology and kinematics of the galaxy's circumstellar environment is conducted. The kinematic center coincides with the peak in radio emission, but is separated by

The B array of the VLA has observed a sample of seven H II galaxies at 325 and 1489 MHz; the radio continuum spectra thus obtained exhibit a wide variety of spectral shapes, but four show a significant flattening toward lower frequencies. A detailed discussion is conducted of this LF flattening, invoking several radio emission and absorption

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