We observed surface images of the Au islands periodically deposited on a Ta sheet by means of an energy-filtered XPEEM using a retarding Wien-filter energy analyzer and a high energy X-ray. By changing the passing photoelectron kinetic energy (Ekin), we had a brighter Au island image at the Ekin=0 eV and 60 eV while we had a brighter Ta substrate image at Ekin=102 eV, corresponding to a Ta 3p3/2 photoelectron peak.
We estimate how well we will know the parameters of solar neutrino oscillations after KamLAND and Borexino. The expected error on ∆m 2 is few per-mille in the VO and QVO regions, few per-cent in the LMA region, and around 10% in the LOW region. The expected error on sin 2 2θ is around 5%. KamLAND and Borexino will tell unambiguously which specific new measurement, dedicated to pp solar neutrinos, is able to contribute to the determination of θ and perhaps of ∆m 2 . The present data suggest as more likely outcomes: no measurement, or the total pp rate, or its day/night variation.
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