Context. The Kepler spacecraft is providing time series of photometric data with micromagnitude precision for hundreds of A-F type stars. Aims: We present a first general characterization of the pulsational behaviour of A-F type stars as observed in the Kepler light curves of a sample of 750 candidate A-F type stars, and observationally investigate

In Planetary Nebulae (PNe) and HII regions ionic abundances can be derived by using collisionally excited lines (CELs) or recombination lines (ORLs). Such abundances do not coincide for the same ion and usually abundances from ORLs are larger than those from CELs by factors of 2 or larger. The origin of the discrepancy, known as the Abundance

Hubble Space Telescope (HST) and ground-based [O II] and [N II] images obtained in the period 1996-1999 reveal a complex, ionized optical nebula around the symbiotic binary CH Cyg extending out to 18" or 5000 AU from the central stars. The observed velocity range of the nebula, derived from long-slit echelle spectra, is 130 km s-1. In spite of its

Radial velocities of 40 intracluster planetary nebulae (ICPNs) in the Virgo Cluster were obtained with the new multifiber FLAMES spectrograph on UT2 at the Very Large Telescope. For the first time, the λ4959 line of the [O III] doublet is seen in a large fraction (50%) of ICPNs spectra, and a large fraction of the photometric candidates with m(5007

Context. The VISTA Variable Survey (VVV) is able to map the Galaxy at l ≤ 0° with an unpaired depth (at least 3 mag deeper than 2MASS), opening new possibilities for studying the inner structure of the Milky Way. Aims: In this paper we concentrate on the exploitation of these data to better understand the spatial disposition and distribution of the

We report the results of a CCD investigation of stars in a selected region near the center of the intermediate age galactic cluster NGC 7789. A CM diagram is presented for a sample of 1122 stars, which should be complete down to V=20. On the ground of recent theoretical evolutionary models, simulations of both the colour-magnitude diagram and the