The behavior of the observed polarization amplitudes with spatial resolution is a strong constraint on the nature and organization of solar magnetic fields below the resolution limit. We study the polarization of the very quiet Sun at different spatial resolutions using ground- and space-based observations. It is shown that 80% of the observed

Aims: In this paper we study the feasibility of inferring the magnetic field from polarized multi line spectra using two methods: The pseudo line approach and The PCA-ZDI approach. Methods: We use multi line techniques, meaning that all the lines of a stellar spectrum contribute to obtain a polarization signature. The use of multiple lines

Following the SuperAGILE detection of an X-ray burst from the neutron star transient and atoll source 4U 1608-522 (ATel #2461), on 3 March 2010 at 06:33:25 UT, marking the beginning of a new outburst, as confirmed by the MAXI (ATel #2462) and INTEGRAL (ATel #2464) detection of increased persistent emission, we obtained Swift and RXTE target of

To interpret the UVEX observations, simulations of the colours of stars and the effect of reddening are a very powerful and important tool. In obtaining the simulated colours, we follow the procedure as outlined in Drew et al. (2005MNRAS.362..753D) for the IPHAS. (6 data files).

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