High energy bremsstrahlung emission during spontaneous fission of 252Cf is observed. The new experimental method to detect rare coincident events by digital storage oscilloscope is used. The γ-rays with energies up to 60 MeV have been measured (by a BGO detector) in coincidence with neutrons detected by a plastic scintillator. The determination of

We are presenting new empirical fitting functions for the Lick/IDS line-strength indices as measured in MILES (Medium-resolution INT Library of Empirical Spectra). Following previous work in the field, these functions describe the empirical behaviour of the line-strength indices with the atmospheric stellar parameters (T eff, logg, [Fe/H]). In

The OTELO (OSIRIS Tunable Emission Line Object Survey project) is an emission line survey using the OSIRIS Tunable Filters on the GTC 10.4m telescope (Cepa et al. 2008). Observing in selected atmospheric windows relatively free of sky emission lines, and with a total survey area of 0.1square degree distributed in different fields, it is expected to

We present a study of the metallicity of 20268 galaxies from the Sloan Digital Sky Survey—Data Release 6 (SDSS-DR6)—using the R 23 method, and derive analytical calibrations from several metallicity-sensitive line ratios: [Nii] λ6583/Hα, [Oiii] λ5007/[Nii] λ6583, [Nii] λ6583/[Oii] λ3727, [Nii] λ6583/ [Sii] λλ6717, 6731, [Sii] λλ6717, 6731/Hα, and

The mixing of the quasifission component to the fissionlike cross section causes ambiguity in the quantitative estimation of the complete fusion cross section from the observed angular and mass distributions of the binary products. We show that the partial cross section of quasifission component of binary fragments covers the whole range of the

The theory of radiatively-driven winds successfully explains the key points of the stellar winds of hot massive stars. However, it has been recently found that some O- and B-type stars do not exhibit as strong wind as predicted by theory. In this work we explain the main issues concerning this topic. We also describe our analysis of the UV spectra