The energy emission involved in a Gamma-Ray Burst evidently can be estimated only provided that we know the distance to the source. The same is true for the peak energy of the event in the source rest frame. Redshifts have been actually measured only for about 40 events. In order to check if it is possible to extend the Epeakrest E relation

The quiet-Sun photospheric plasma has a variety of magnetic field strengths going from zero to 1800 G. The empirical characterization of these field strengths requires a probability density function (PDF), i.e., a function P(B) describing the fraction of quiet Sun occupied by each field strength B. We show how to combine magnetic field strength

Exoplanetary transits produce a double-horned color signature that is distinct from both binaries and blends and can thus be used to separate exoplanets from false positives in transit searches. Color photometry with precision sufficient to detect this signal in transits of HD 209458 is available in the literature. Analysis of these observations

We describe the latest results and future prospects of the QUEST survey for RR Lyrae stars in the halo of the Milky Way. Because RR Lyrae variables are excellent standard candles, they are very useful tools for finding sub-structures in the halo that may be tidal tails from dwarf galaxies or globular clusters. Also, we show that observations of the

We have determined spectroscopic ages of elliptical galaxies in the Virgo Cluster using spectra of very high signal-to-noise ratio (S/N>100 Å-1). We observed eight galaxies with the Subaru Telescope and have combined this sample with six galaxies previously observed with the WHT. To determine their ages, we have used a new method based on the Hγσ

We summarise the results and achievements of integral-field spectroscopy of early-type galaxies, observed as part of a survey using both the SAURON and OASIS spectrographs. From the perspective of integral-field spectroscopy, these otherwise smooth and featureless objects show a wealth of structure, both in their stellar kinematics and populations