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

A large fraction of all stars, after experiencing heavy winds at the end of the Asymptotic Giant Branch (AGB) phase, leave behind a core that is below the Chandrasekhar mass limit. This core eventually photoionizes the stellar ejecta giving birth to a planetary nebula (PN). PN and AGB stars are therefore the remnants of stars that through their

Here we present a self-consistent stationary solution for spherically symmetric winds driven by massive star clusters under the impact of radiative cooling. We demonstrate that cooling may modify drastically the distribution of temperature if the rate of injected energy approaches a critical value and that the stationary wind solution does not