In this contribution we summarise our science preparation activities to complete the CARMENES input catalogue of M dwarfs using low-resolution spectroscopy to derive spectral indices sensible to spectral type, gravity and metallicity as well as the level of chromospheric activity. We provide here all this information for 181 stars in addition to

CARMENES, the new ultra-stable high-resolution spectrograph at the 3.5 m Calar Alto telescope and the only one in its category that covers from 0.52 to 1.71μm in one shot, started its guaranteed time observations (GTO) in January 2016. Under GTO, CARMENES is monitoring approximately 300 selected M dwarfs for at least three years with the aim of

Li depletion is strongly age-dependent but currently available data have shown a complex pattern of Li depletion on the pre- and main-sequence stars that is not yet understood. The lithium abundance observed in late-type stars depend not only of the age and the temperature but also on metallicity, mixing mechanisms, convection structure, rotation

The determination of the chemical composition of extrasolar planets has been the subject of numerous studies in the last years. While the composition of the atmosphere of planets can be observed through, e.g., the absorption of the star light, the composition of the solids remains difficult to estimate. As both planetesimals and planets are formed

The existing status of our knowledge of binary central stars of planetary nebulae will be explored. Binary modeling of known systems is providing physical parameters that can be compared amongst the sample, with nebular characteristics, and with similar binaries with no associated planetary nebula. Correlations among these areas will be discussed

Massive stars in young massive clusters insert tremendous amounts of mass and energy into their surroundings in the form of stellar winds and supernova ejecta. Mutual shock-shock collisions lead to formation of hot gas, filling the volume of the cluster. The pressure of this gas then drives a powerful cluster wind. However, it has been shown that