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Implications of aperture choice on ELT performance. A case study of stellar populations
Mysterious UV Lines of Fe II in the Blob Spectrum of Eta Carinae
Distance-effects in the census of binaries with GAIA: principles and qualitative results
The present contribution describes some simulations of the observation of binaries with GAIA. The results do not differ fundamentally from earlier estimates, e.g. in GAIA's Concepts and Technology Study Report (ESA-2000-SCI-4), but they are based on more realistic assumptions and much more extensive numerical work.
Ulysses Dust Detection System V3.1
This data set contains the data from the Ulysses dust detector system (UDDS) from start of mission through the end of mission, 1990-2007. (As the dust detector was turned off after Nov. 30, 2007, this is the last date for which UDDS data is recorded.) Included are the dust impact data, noise data, laboratory calibration data, and location and orientation of the spacecraft and instrument.
Photon correlation spectroscopy for observing natural lasers
ELSA - Training the Next Generation of Space Astrometrists
Cr II Fluorescence in Eta Carinae due to H Lyman Alpha Pumping
Classification of Wolf-Rayet stars in NGC 595 in M 33 through high-spatial resolution observations
Astronomical quantum optics with Extremely Large Telescopes
On the Lanthanides and Broad Spectrophotometric Depressions in Magnetic CP Star Spectra
Binarity of Hipparcos Main Sequence Survey Stars
Hipparcos observations of double stars, mainly A and F primaries, aremodelled in order to check the statistics of double-star solutions inthe Hipparcos Catalogue and to set quantitative limits on binarydistributions. The number of companions per primary is estimated to 0.25+/-0.05 for semi-major axes from 1 to 10 AU, and to 0.43 +/-0.20 for therange 10--100 AU. The total multiplicity found is betw
Sampling distant stellar populations on the evolution of galaxies
Preparation of the Gaia Data Processing: First Astrometric Results
The Gaia mission of the European Space Agency (ESA) will produce high-precision astrometry for 10^9 objects up to 20th magnitude. The volume of data generated (about 150TB of compressed raw data) and the complexity of the relationships between them make the scientific processing a challenging task. This paper presents the basic concepts of the core of the astrometric data reduction, the AGIS syste