The planetary nebula TS 01 (also called PN G 135.9+55.9 or SBS 1150+599A) with its record-holding low oxygen abundance and its double degenerate close binary core (period 3.9 h) is an exceptional object located in the Galactic halo. We have secured observational data in a complete wavelength range to pin down the abundances of half a dozen elements

Context. Recent accurate abundance analyses of B-type main sequence stars in the solar vicinity has shown that abundances derived from these stellar objects are more homogeneous and metal-rich than previously thought. Aims: We investigate whether the inhomogeneity of abundances previously found in B-type stars in the Ori OB1 association is real

We have used observations obtained as part of the Hubble Space Telescope/ACS Survey of Galactic Globular Clusters to construct global present-day mass functions for 17 globular clusters utilizing multi-mass King models to extrapolate from our observations to the global cluster behavior. The global present-day mass functions for these clusters are

Spectral data are presented for comets 2006 VZ13 (LINEAR), 2006 K4 (NEAT), 2006 OF2 (Broughton), 2P/Encke and 93P/Lovas I, obtained with the Cerro Tololo Inter-American Observatory 1.5-m telescope in 2007 August. Comet 2006 VZ13 is a new Oort cloud comet and shows strong lines of CN (3880 Å), the Swan band sequence for C2 (4740, 5160 and 5630 Å)

The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other ground-based instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR

Located at the Canary island of La Palma, MAGIC is the world-wide largest Imaging Atmospheric Cherenkov telescope. MAGIC-I has been in operation since 2004. Currently, two twin telescopes can take data in stereo mode. Both in single or stereo mode, the telescopes deliver a wealth of exciting physics results in the Very High Energy (VHE) region of