Using broad band photometry, a new method is derived to evaluate relative (arm with respect to the interarm disk) star formation rates and relative star formation efficiencies together with spiral arm amplitudes, as a function of the galactocentric radius. The classical method to obtain star formation rates from Hα photometry is discussed, and a

Infrared observations taken during the major outburst seen in 1993 show strong evidence of rapid variability in 3C 66A on a time scale of a few hours, with associated variability of the spectral slope on the same time scale. A strong (P>>99%) correlation is seen between the flux at 2.2-microns and the spectral index, with the spectrum steepening as

First results of a cosmic microwave background (CMB) anisotropy experiment conducted at the Observatorio del Teide (Tenerife, Spain) are presented. The instrument is a four channel (3.1, 2.1, 1.3, and 1.1 mm) 3He bolometer system coupled to a 45 cm diameter telescope. The resultant configuration is sensitive to structures on angular scales ~1 deg-

We have studied the signal received by a distant observer from a pulsar orbiting a stellar black hole. The binary system has a non-eccentric orbit and the most favourable configuration (edge-on) for observing the influence of the black hole on the signal emitted by the pulsar. In particular, the influence of the spin of the black hole on the

We discuss the multi-Gaussian decomposition of the [O III] λλ 4959,5007 emission line profiles from 2-D spectroscopy. We found that a model based on five main gaseous components can reproduce the observed line profiles consistently. The morphology of the intensity maps of some of these gaseous subsystems seems bipolar. This is in better agreement

From 2-D spectroscopy of the [O III] λλ 4959,5007 and [S III] λ 9069 lines we have studied the ionized gas-velocity field in the central regions of NGC 1068. The existence of a strong bipolar outflow of ionized gas is confirmed. The origin of this outflow, which is probably related to the active nucleus, is about 1.4″ NE of the optical nucleus