In order to test the calibration technique to be used on the GOLF solar oscillation resonant scattering spectrometer on the SOHO mission, observations with a modified instrument have been carried out at Izana, Tenerife since 1989. Different methods of analysing data are compared. These show that calibration by means of a magnetic modulation

B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy

Comet Lulin was observed in July 2008, when the comet was in-bound at 1.7 AU from the Sun. Analysis of the images showed that the comet had a very intense and anomalous enhancement of the column density of the solid components in the inner coma. This effect was before interpreted as due to the presence of sublimating grains (Tozzi et al, 2004, AA

The observations of the low-mass x ray binary, Cyg X-2, taken with the International Ultraviolet Explorer (IUE) in a campaign conducted in June and October of 1988 are reported. A direct relationship between the strength of the UV continuum and line emission and the placement of the x ray spectrum in one of three branches of the so-called Z-shaped

A sensitive observing system for observing the cosmic microwave background on an angular scale of 8 deg is described. This angular scale is appropriate for studies of intrinsic fluctuations in the CMB generated by gravitational potential fluctuations (the Sachs-Wolfe effect). The beam-switching system employs low-noise and broadband cryogenically

An automatic and fast procedure was implemented to determine Te and log g from the comparison of the UV S 2/68 spectra with the Kurucz models. The method has been applied to all A and F stars with (B-V)0 greater than or equal to 0 and luminosity classes III, IV, IV-V, and V, included in the Ultraviolet Bright-Star Spectrophotometric Catalogue. From