This communication presents a family of spectrographs designed for the European Solar Telescope. They can operate in four different configurations: a long slit standard spectrograph (LsSS), two devices based on subtractive double pass (TUNIS and MSDP) and one based on an integral field, multi-slit, multi-wavelength configuration. The combination of

Results from a new multi-wavelength evolutionary synthesis model including the γ-ray line emission from various radioactive isotopes (26Al, 60Fe) are presented. In particular the predicted γ-ray line observations combined with measurements of ionising fluxes can efficiently constrain the age of a stellar population, and help to identify the primary

We present new UV observations for NGC 288, taken with the WFC3 detector on board the Hubble Space Telescope, and combine them with existing optical data from the archive to explore the multiple-population phenomenon in this globular cluster (GC). The WFC3's UV filters have demonstrated an uncanny ability to distinguish multiple populations along

We present a source-plane reconstruction of a Herschel and Planck-detected gravitationally lensed dusty star-forming galaxy (DSFG) at z = 1.68 using Hubble, Submillimeter Array (SMA), and Keck observations. The background submillimeter galaxy (SMG) is strongly lensed by a foreground galaxy cluster at z = 0.997 and appears as an arc with a length of

Spatial and temporal evolution of dynamic fibrils (DF) as well as coupling with photospheric features was investigated. The main target were remnants in the active region 10997 on May 28, 2008. We used about 1 hour series of multi wavelength simultaneous observations of the DFs and corresponding photospheric features. The observations were

Context: We present observations of the GRB 080319B afterglow at optical, mm, and radio frequencies between a few hours and 67 days after the burst. Aims: We attempt to understand the nature of this extraordinarily bright explosion based on the observed properties and its comparison with afterglow models. Methods: Our observations and other