2017/01/09 by G. Domínguez-Guzmán, M. Rodríguez, Domínguez-Guzmán, G. +5
Physics and Astronomy · #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1701.02326
openalex publication_date 2017/01/09 · openalex created_date 2019/12/26 · openalex updated_date 2026/07/28
We use very deep spectra obtained with the Ultraviolet-Visual Echelle\nSpectrograph in the Very Large Telescope in order to determine the physical\nconditions, the chemical abundances and the iron depletion factors of four H II\nregions of the Large Magellanic Cloud and four H II regions of the Small\nMagellanic Cloud. The spectral range covered is 3100-10400 mathringA with\na resolution of \Δ\λ \∼ \λ / 8800. We measure the intensity\nof up to 200 emission lines in each object. Electron temperature and electron\ndensity are determined using different line intensity ratios. The ionic and\ntotal abundances are derived using collisionally excited lines for O, N, S, Cl,\nNe, Ar, and Fe. The uncertainties are calculated using Monte Carlo simulations.\nThis is the largest available set of high quality spectra for H II regions in\nthe Magellanic Clouds. Thus, we can derive chemical abundances and depletion\nfactors and constrain their variations across each galaxy with better accuracy\nthan previous studies. In particular, we find that the amount of Fe depleted on\nto dust grains in the H II regions of the Magellanic Clouds is similar to that\nfound in Galactic H II regions.\n