In this paper we adopt a chemical evolution model, which is an improved version of the
Chiappini, Matteucci, & Gratton model, assuming two main accretion episodes for the …

The problem of oxygen abundance determination in H II regions based on the" strong
oxygen line intensities-oxygen abundance" empirical calibration is revisited. A compilation …

We present the first results from Chemical Evolution Constrained Using Ionized Lines in
Interstellar Aurorae (CECILIA), a Cycle 1 JWST NIRSpec/MSA program that uses ultra …

Abstract We present Very Large Telescope (VLT) UVES echelle spectrophotometry of the
Orion nebula in the 3100–10 400 Å range. We have measured the intensity of 555 emission …

We discuss the evolution of oxygen, carbon and nitrogen in galaxies of different
morphological type by adopting detailed chemical evolution models with different star …

This is our second paper devoted to the problem of line intensity-oxygen abundance
calibration starting from the idea of McGaugh ([CITE]) that the strong oxygen lines (and) …

The absolute integrated fluxes that we obtained (Paper I) for 34 H ii regions, with
Galactocentric distances RG in the 6.6–17.7 kpc range, in the emission lines [O ii] λλ 3726 …

The origin of the abundance discrepancy, ie, the fact that abundances derived from
recombination lines are larger than those from collisionally excited lines, is one of the key …

Using ab-initio photoionization models of giant H ii regions, we test methods for abundance
determinations based on a direct measurement of the electron temperature, now possible …

The problem of the line intensities--oxygen abundance calibration has been considered. We
confirm the idea of McGaugh (1991) that the strong oxygen lines ([OII] 3727, 3729 and [OIII] …