Here is a state-of-the-art review of our current knowledge of brown dwarfs and very low-mass stars. The hunt for, and study of, these elusive objects is currently one of the most dynamic areas of research in astronomy. This volume presents review articles from a team of international authorities who assess the spectacular progress in this field in

We report the detections of a giant planet (MARVELS-7b) and a brown dwarf (BD) candidate (MARVELS-7c) around the primary star in the close binary system, HD 87646. To the best of our knowledge, it is the first close binary system with more than one substellar circumprimary companion that has been discovered. The detection of this giant planet was

We describe the source subtraction strategy and observations for the extended Very Small Array (VSA), a cosmic microwave background interferometer operating at 33GHz. A total of 453 sources were monitored at 33GHz using a dedicated source subtraction baseline. 131 sources brighter than 20mJy were directly subtracted from the VSA visibility data

We observed the reflection nebula NGC 7023 at various positions using wide and narrow band photometry centred on the 7.7 and 11.3μm PAH emission features and wide band photometry at 20 and 25μm. No significant variations have been detected over the nebula in the 7.3 and 20μm continuum relative to the total emission in the 6-15μm range (hereafter

We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for

VII Zw403 is a nearest BCD galaxy. This izolated system is so close (~4.5 Mp c), that it makes it possible to study it's star forming regions with unprecedently great details. recent X-ray observations (Papaderos et al. 1994) added more interest to the system, as revealed an extended, kpc-scale region of the diffuse X-ray emission. We use our