Evolutionary tracks are of key importance for the understanding of star formation. Unfortunately, tracks published by various groups differ so that it is fundamental to test them observationally. In order to do this, we derived the masses of the two components of the Pre-Main Sequence (PMS) binary HD113449 by combining radial velocity (RV)

Mid-infrared (mid-IR) imaging at resolutions of 300mas of the central kpc region of 13 nearby, well-known active galaxies is presented. The bulk of the mid-IR emission is concentrated on an unresolved central source within a size of less than 5-130pc, depending on the object distance. Further resolved emission is detected in 70 per cent of the

Context. CoRoT, the pioneer space-based transit search, steadily provides thousands of high-precision light curves with continuous time sampling over periods of up to 5 months. The transits of a planet perturbed by an additional object are not strictly periodic. By studying the transit timing variations (TTVs), additional objects can be detected in

NGC 2808 is one of the globular clusters containing multiple stellar populations in our Galaxy. The cluster color-magnitude diagram contains two extra sequences blueward of the main cluster ridge-line. Stars on these sequences appear to be enhanced in Helium up to Y=0.40. The origin of these stars is still mysterious although they are believed to

We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm with the Spitzer Infrared Array Camera (IRAC). Our measured occultation depths are 0.510±0.042% at 4.5 and 0.41±0.11% at 8 μm. In addition to the CoRoT optical measurements, these planet/star flux ratios indicate a poor heat distribution on the

This study is an investigation of the stellar density profile of the Galactic disc in the anticentre direction. We select over 40000 early A stars from INT/WFC Photometric Hα Survey of the Northern Galactic Plane (IPHAS) photometry in the Galactic longitude range 160° l 200° close to the equatorial plane (-1° b +1°). We then compare their