A complex kinematical structure is inferred from the analysis of high resolution spectra of the nuclear region of the galaxy NGC 6946. The spatial resolution of...
Gas motions in the plane of the spiral galaxy NGC 3631
The velocity field of the nearly face-on galaxy NGC 3631, derived from observations in the Hα line and Hi radio line, is analysed to study perturbations related...
Gas physical conditions and kinematics of the giant outflow Ou4
Context. The recently discovered bipolar outflow Ou4 has a projected size of more than one degree in the plane of the sky. It is apparently centred on the young...
Gas-phase Fe/O and Fe/N abundances in star-forming regions: Relations between nucleosynthesis, metallicity, and dust
Context. In stars, metallicity is usually traced using Fe, while in nebulae, O serves as the preferred proxy. Both elements have different nucleosynthetic...
Gas-phase metallicity for the Seyfert galaxy NGC 7130
Metallicity measurements in galaxies can provide valuable clues about galaxy evolution. One of the mechanisms postulated for metallicity redistribution in...
Gasdynamics in NGC 5248: Fueling a Circumnuclear Starburst Ring of Super-Star Clusters
Through observations and modeling, we demonstrate how the recently discovered large-scale bar in NGC 5248 generates spiral structure that extends from 10 kpc...
GATOS: missing molecular gas in the outflow of NGC 5728 revealed by JWST
The ionisation cones of NGC 5728 have a deficit of molecular gas based on millimetre observations of CO (2-1) emission. Although photoionisation from the active...
Gauss-Seidel and Successive Overrelaxation Methods for Radiative Transfer with Partial Frequency Redistribution
The linearly polarized solar limb spectrum that is produced by scattering processes contains a wealth of information on the physical conditions and magnetic...
Gaussian covariance matrices for anisotropic galaxy clustering measurements
Measurements of the redshift-space galaxy clustering have been a prolific source of cosmological information in recent years. Accurate covariance estimates are...