Fiorenzo Vincenzo

Nitrogen and oxygen abundances in the Local Universe

FV thanks the Cavendish Astrophysics Group at the University of Cambridge for kindly supporting his visit during 2014 September. FB acknowledges funding from the United Kingdom Science and Technology Facilities Council (STFC). RM acknowledges funding from the United Kingdom STFC through grant ST/M001172/1. FM acknowledges financial support from PRIN-MIUR 2010-2011 project ‘The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies’, prot. 2010LY5N2T.

Modern yields per stellar generation: : the effect of the IMF

Gaseous and stellar metallicities in galaxies are nowadays routinely used to constrain the evolutionary processes in galaxies. This requires the knowledge of the average yield per stellar generation,

Are ancient dwarf satellites the building blocks of the Galactic halo

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The IGIMF and other IMFs in dSphs: the case of Sagittarius

, i.e. the quantity of metals that a stellar population releases into the interstellar medium (ISM), which is generally assumed to be a fixed fiducial value. Deviations of the observed metallicity from the expected value of

Evolution of N/O ratios in galaxies from cosmological hydrodynamical simulations

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The effects of the initial mass function on the chemical evolution of elliptical galaxies

are used to quantify the effect of outflows or inflows of gas, or even as evidence for biased metallicity calibrations or inaccurate metallicity diagnostics. Here we show that

A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

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Extragalactic archaeology with the C, N, and O chemical abundances

depends significantly on the Initial Mass Function (IMF), varying by up to a factor larger than three, for the range of IMFs typically adopted in various studies. Varying the upper mass cutoff of the IMF implies a further variation of

On the [alpha/Fe]-[Fe/H] relations in early-type galaxies

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The Gaia-ESO Survey: The N/O abundance ratio in the Milky Way

by an additional factor that can be larger than two. These effects, along with the variation of the gas mass fraction restored into the ISM by supernovae (