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Properties of bars and bulges in the Hubble sequence |
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A Connection between Star Formation in Nuclear Rings and Their Host Galaxies |
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Do Bars Drive Spiral Density Waves? |
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The Hα Galaxy Survey. VIII. Close Companions and Interactions, and the Definition of Starbursts |
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The Hα galaxy survey. VII. The spatial distribution of star formation within disks and bulges |
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Galactic evolution of nitrogen |
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Evidence for the Naphthalene Cation in a Region of the Interstellar Medium with Anomalous Microwave Emission |
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On the action of UV photons on hydrogenated fulleranes C60H36 and C60D36 |
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A survey for pulsating subdwarf B stars with the Nordic Optical Telescope |
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Testing Intermediate-Age Stellar Evolution Models with VLT Photometry of Large Magellanic Cloud Clusters. I. The Data |
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The Chemical Enrichment History of the Fornax Dwarf Spheroidal Galaxy from the Infrared Calcium Triplet |
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Spectroscopy of QUEST RR Lyrae Variables: The New Virgo Stellar Stream |
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On the Extended Structure of the Phoenix Dwarf Galaxy |
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Astronomical site selection: on the use of satellite data for aerosol content monitoring |
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GRB 080913 at Redshift 6.7 |
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The SAURON project - VI. Line strength maps of 48 elliptical and lenticular galaxies |
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The SAURON project - X. The orbital anisotropy of elliptical and lenticular galaxies: revisiting the (V/σ, ɛ) diagram with integral-field stellar kinematics |
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The SAURON project - XI. Stellar populations from absorption-line strength maps of 24 early-type spirals |
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Neutral oxygen spectral line formation revisited with new collisional data: large departures from LTE at low metallicity |
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Deep echelle spectrophotometry of S 311, a Galactic HII region located outside the solar circle |
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Faint emission lines in the Galactic HII regions M16, M20 and NGC 3603* |
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The Localized Chemical Pollution in NGC 5253 Revisited: Results from Deep Echelle Spectrophotometry |
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The chemical composition of the Galactic H II regions M8 and M17. A revision based on deep VLT echelle spectrophotometry |
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Pre-main sequence spectroscopic binaries suitable for VLTI observations |
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