The study of cool atmospheres is currently a fruitful field of interaction between theorists developing better atmosphere models and observers discovering new cool objects and analysing their emission spectrum. Save for a few close binaries with known parallax and a dynamical mass determination, comparison of spectra to models is the only method

We triggered a Chandra ToO observation of the ongoing outburst of a transient source in the globular cluster Terzan 5 (ATel #2919, #2920, #2922, #2924, #2929, #2932, #2933, #2937, #2939, #2940, #2946, #2952, #2958). The 9.9 ks observation was taken with the ACIS S3 chip in imaging mode and began on 2010-10-24 at 19:30:29 UTC. Inspection of the new

CARMENES, Calar Alto high-Resolution search for M dwarfs with Exo-earths with a Near-infrared Echelle Spectrograph, is a study for a next-generation instrument for the 3.5 m Calar Alto Telescope to be designed, built, integrated, and operated by a consortium of nine German and Spanish institutions. Our main objective is finding habitable exoplanets

Transiting planet systems offer a unique opportunity to observationally constrain proposed models of the interiors (radius, composition) and atmospheres (chemistry, dynamics) of extrasolar planets. The spectacular successes of ground-based transit surveys (more than 60 transiting systems known to-date) and the host of multi-wavelength, spectro

The -beam asymmetry Σ in the photoproduction of negative pions on quasi-free neutrons in a deuterium target was measured at the Grenoble Anneau Accelerateur Laser in the energy interval 700-1500 MeV and over a wide angular range, using polarized and tagged photons. Results are compared with recent partial-wave analyses.

We use ACS data from the HST Treasury survey of the Coma cluster (z˜0.02) to study the properties of barred galaxies in the Coma core, the densest environment in the nearby Universe. This study provides a complementary data point for studies of barred galaxies as a function of redshift and environment. From ˜470 cluster members brighter than MI =