We took simultaneous observations in Fe I 1.5 µ and Fe I 630 nm of an internetwork region. We discuss the compatibility of the data in the two spectral ranges, and present results for the magnetic field distribution. We show that the larger contribution comes from hG field strengths.

¿Como se forman las galaxias?, ¿Cómo evolucionan?. Éstas son cuestiones fundamentales que las cartografiados profundos de galaxias a alto desplazamiento al rojo tratan de resolver. Una segunda aproximación es reconstruir la historia de la formación estelar a través de sus poblaciones estelares resueltas. La Historia de formación estelar de una

We present first comparisons between high resolution observations of the quiet photosphere, obtained with the Interferometric BIdimensional Spectrometer (IBIS) in the non-magnetic Fe I 7090.4 Å spectral line, and the synthetic spectrum calculated for a 3D snapshot of a radiation-hydrodynamical simulation of the solar atmosphere. Together with

We present a discussion of efforts to obtain external validation of the estimated atmospheric parameters (Teff, log g, [Fe/H]) obtained from medium-resolution (R = 2000) SDSS spectroscopy and ugriz photometry, which are being employed for both the completed SDSS-I and the ongoing SEGUE survey. The SDSS/SEGUE spectroscopic pipeline makes use of a

The huge star formation events that occur at some galactic centers do not provide enough clues as to their origin, since the morphological signatures of the triggering mechanism are smeared out in the timescale of a few orbital revolutions of the galaxy core. Our high spatial resolution three-dimensional near-infrared spectroscopy for the first

Aims.We present multiwavelength observations of the gamma-ray burst GRB 051028 detected by HETE-2 in order to derive its afterglow emission parameters and to determine the reason for its optical faintness when compared to other events. Methods: .Observations were taken in the optical (2.0 m Himalayan Chandra Telescope, 1.34 m Tautenburg, 4.2 m