We examine the errors in the atmospheric parameters recovered from the inversion of spectro-polarimetric data with limited wavelength sampling. We suggest that response functions evaluated in Milne-Eddington atmospheres may be useful as diagnostic tools that allow, for instance, the selection of the optimum wavelength positions to be observed by

We have used the Mambo instrument on the IRAM 30m telescope to observe at 1.2mm 63 Spitzer-selected z>1 hyperluminous infrared galaxy candidates (HLIRGs) with starburst-dominated mid-infrared (MIR) spectral energy distributions from the SWIRE Legacy survey. The primary selection criteria are a peak in the IRAC 5.8μm band due to the rest frame near

The triplet of the He I transitions around 10830 Å not only shows a rich variety of Stokes profiles, but also allows the full magnetic vector in the upper chromosphere to be probed, thus revealing the magnetic structure of loops, current sheets, finely structured supersonic downflows, the chromospheric layers of sunspots (supporting the presence of

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 present a method to combine magnetic field

EL ESTUDIO DE LA GENERACION Y LA PROPAGACION DE ONDAS EN LA ATMOSFERA SOLAR ES UN TEMA CANDENTE EN LA INVESTIGACION ASTROFISICA ACTUAL, YA QUE PROPORCIONA INFORMACION SOBRE LA ESTRUCTURA Y LA DINAMICA DE LAS ATMOSFERAS DE LAS ESTRELLAS DE TIPO SOLAR AL MISMO TIEMPO QUE NOS AYUDA A COMPRENDER LOS MECANISMOS DE CALENTAMIENTO CROMOSFERICO Y CORONAL

We present an analysis of simultaneous observations of a sunspot in two different spectral ranges (630 nm and 1565 nm). The dataset was acquired with the POlarimetric LIttrow Spectrograph (POLIS) and the Tenerife Infrared Polarimeter (TIP) at the German Vacuum Tower Telescope (VTT) of Observatorio del Teide. Inversions of both sets of lines are