This article presents a statistical-mechanical treatment of a relationship (the force equation) between the gravitational potential for two particles and the correlation functions in a relaxed distribution of particles with different masses. This relationship is used in the case of galaxies interacting through a Newtonian potential in a Universe in

We have observed the spectral regions around the LiI resonance 670.8nm and subordinate 610.4nm lines of V471 Tau. This is an eclipsing post common-envelope (CE) binary system. A revision of several independent measurements of the parallax and proper motion of V471 Tau allow us to argue that this system is indeed a Hyades cluster member by examining

GOLF in-flight commissioning and calibration was carried out during the first four months, most of which represented the cruise phase of SOHO towards its final L1 orbit. The initial performance of GOLF is shown to be within the design specification, for the entire instrument as well as for the separate sub-systems. Malfunctioning of the polarising

We have acquired narrow and broad band imaging, together with high and low resolution spectroscopy for the source IRAS 09371+1212. As a result, we are able to show the presence of systematic colour gradients within the interior and exterior envelopes. Whilst the interior bright lobes are characterised by relatively high values of V-R (a regime of

We present the optical and UV emission-line properties of 160 X-ray-selected active galactic nuclei (AGN) taken from the RIXOS survey (including Hα, Hβ, [Oiii] lambda5007, Mgii lambda2798 and Ciii] lambda1909). This sample is believed to contain a mixture of absorbed and unabsorbed objects, with column densities up to ~4x10^21cm^-2. Although the

In the context of a more extensive project, a study of the structural components of the barred spiral galaxy NGC 5850 is presented here, using U, B, V, R, and I photometry. After subtracting a bulge+disk model from the observed image, we obtain the bars, rings and other non-axisymmetric structures. We fit two-dimensional analytic functions for each