The solar chromosphere is a vigorously dynamic region of the sun, where waves and magnetic fields play an important role. To improve chromospheric diagnostics, we present new observations in Ca II 8542 carried out with the SST/CRISP on La Palma, working in full-Stokes mode. We measured Stokes line profiles in active regions. The line profiles

X-ray binaries are excellent laboratories to study collapsed objects. On the one hand, transient X-ray binaries contain the best examples of stellar-mass black holes while persistent X-ray binaries mostly harbor accreting neutron stars. The determination of stellar masses in persistent X-ray binaries is usually hampered by the overwhelming

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