We present the evolution of the rest-frame optical luminosity density jrestλ, the integrated rest-frame optical color, and the stellar mass density, ρ*, for a sample of Ks band-selected galaxies in the Hubble Deep Field-South (HDF-S). We derived jrestλ in the rest-frame U, B, and V bands and found that jrestλ increases by a factor of 1.9+/-0.4, 2.9

We present the first detailed imaging polarization observations of six SMC and six LMC clusters, known to have large populations of B-type stars that exhibit excess Hα emission from 2-CD photometric studies, to constrain the evolutionary status of these stars and hence better establish links between the onset of disk formation in classical Be stars

The most energetic part of the Sun, its interior, due to its plasma parameters is hidden below the solar surface and invisible to the observer. Nevertheless, the solar interior generates the energy and provokes atmospheric magnetic activity. Despite great progress in both observational and simulational methods, the mechanism of energy transport

Aims: The physics driving features such as breaks observed in galaxy surface brightness (SB) profiles remains contentious. Here, we assess the importance of stellar radial motions in shaping their characteristics. Methods: We use the simulated Milky Way-mass cosmological discs from the Ramses Disc Environment Study (RaDES) to characterise the

Over recent decades there has been a proliferation of special-interest magazines dedicated to astronomy. In spite of the undoubted market for specialist feature articles on astronomy such articles appeal to a restricted sector of the general public and rarely appear in the daily or weekly press. I argue here that, apart from television documentary

We present the first results on the optical identification of 89 sources with S(0.5-2 keV)>=1.7x10^-14 erg s^-1 cm^-2 detected in eight ROSAT Position Sensitive Proportional Counter (PSPC) observations targeted on the second Lockman hole region. Because of the low Galactic HI column density towards this field [N_HI~(6-12)x10^19 cm^-2] the X-ray