Balloons, driven by hot air or some gas lighter than air, were the first artificial machines able to lift payloads (including humans) from the ground. After some pioneering flights the study of the physical properties of the terrestrial atmosphere constituted the first scientific target. A bit later astronomers realized that the turbulence of the

We describe the results of a search for diffuse sources in the 0.4 deg2 area of the XMM-Newton 770 ks survey of the Lockman Hole. An abundant population of sources is revealed, which is likely to stem from low-mass galaxy clusters at redshift near 1. We present the optical images in the K′ and R-bands for our candidates, suggesting a concentration

The main aim of JIS (Joint Information System) is to overcome the present lack of detailed knowledge amongst the European Solar Physics community. This lack of knowledge occurs at several levels: groups of researchers, institutions, scientific activities, running programs, resources, new opportunities, observational campaigns etc. JIS will not be

We present the first results obtained recently with Gemini GMOS MOS spectroscopy of Ly-alpha emitters at redshift z = 5.7 - 6.0. We are carry out a spectroscopic study using Gemini GMOS of our sample of 259 candidates to galaxies at redshifts up to 6.0. The sample comprises: (i) 17 Ly-alpha (LAE) candidates at redshift 5.7, (ii) 4 LAE candidates at

In this work we present the first results of a study of BAL QSOs (at low and high redshift), based on very deep Gemini GMOS integral field unit (IFU) spectroscopy. In particular, new Gemini results obtained for the nearest BAL IR-QSO Mrk 231 are presented. The very deep Gemini GMOS 3D spectra clearly show that the BAL I system (in the lines Na ID

Results are presented of a large-scale imaging photometric study of the stellar population in the northern part of NGC 3372 with a wavelength coverage from 0.33 to 2.5 μ m. All observations were made at Las Campanas Observatory. The sizes of the three stellar clusters, Tr 14, Tr 15 and Tr 16, were determined by means of star counts. Two-colour and