In the context of interferometric integral field spectroscopy at the LBT, we have investigated the physics of coupling light from a double pupil into optical fibers. Previous fiber-fed astronomical instruments solved the problem of coupling light from a single dish into single- and multi-mode fibers. However, this is an unexplored territory for a

We have explored radial color and stellar surface mass density profiles for a sample of 85 late-type spiral galaxies with deep (down to ~27 mag arcsec-2) SDSS g'- and r'-band surface brightness profiles. About 90% of the light profiles have been classified as broken exponentials, exhibiting either truncations (Type II galaxies) or antitruncations

A number of outstanding scientific problems require a high resolution, visual spectrograph at the E-ELT. Measuring the dynamics of the universe, finding earth-like planets with radial velocity techniques, determining the chemical evolution of the intergalactic medium and if physical constants varied in the past, all require a superior capability of

Context: L-type ultra-cool dwarfs and brown dwarfs have cloudy atmospheres that could host weather-like phenomena. The detection of photometric or spectral variability would provide insight into unresolved atmospheric heterogeneities, such as holes in a global cloud deck. Indeed, a number of ultra-cool dwarfs have been reported to vary. Additional

CLÉS is an evolution code recently developed to produce stellar models meeting the specific requirements of studies in asteroseismology. It offers the users a lot of choices in the input physics they want in their models and its versatility allows them to tailor the code to their needs and implement easily new features. We describe the features

As part of our ongoing Chandra/HST M31 transient program we report on Chandra ACIS observations of M31 containing the new transient sources reported by Pietsch et al. (2008, ATel #1647). Two 5ks observations were performed on 2008-05-31.47 UT (Obs. 1) and 2008-07-15.70 UT (Obs. 2), both prior to the observation of Pietsch et al. (2008, Obs. 3)