The evolution of CNO elements in galaxies

Abstract

After hydrogen and helium, oxygen, carbon, and nitrogen - hereinafter, the CNO elements - are the most abundant species in the universe. They are observed in all kinds of astrophysical environments, from the smallest to the largest scales, and are at the basis of all known forms of life, hence, the constituents of any biomarker. As such, their study proves crucial in several areas of contemporary astrophysics, extending to astrobiology. In this review, I will summarize current knowledge about CNO element evolution in galaxies, starting from our home, the Milky Way. After a brief recap of CNO synthesis in stars, I will present the comparison between chemical evolution model predictions and observations of CNO isotopic abundances and abundance ratios in stars and in gaseous matter. Such a comparison permits to constrain the modes and time scales of the assembly of galaxies and their stellar populations, as well as stellar evolution and nucleosynthesis theories. I will stress that chemical evolution models must be carefully calibrated against the wealth of abundance data available for the Milky Way before they can be applied to the interpretation of observational datasets for other systems. In this vein, I will also discuss the usefulness of some key CNO isotopic ratios as probes of the prevailing, galaxy-wide stellar initial mass function in galaxies where more direct estimates from starlight are unfeasible.

arXiv comment83 pages, 19 figures. Invited review to appear in Astronomy and Astrophysics Review

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• Direct measurements of carbon and sulfur isotope ratios in the Milky Way
• Explaining the ${}^{12}\text{C}{/}^{13}\text{C}$ ratio in the Galactic halo: the contribution from shell mergers in primordial massive stars
• The earliest phases of CNO enrichment in galaxies
• Ariel stellar characterisation II. Chemical abundances of carbon, nitrogen, and oxygen for 181 planet-host FGK dwarf stars
• Infrared fine-structure lines at high redshift
• Sulfur isotope ratios in the Large Magellanic Cloud
• Metallicity dependence of the CO-to-H${}_2$ and the [CI]-to-H${}_2$ conversion factors in galaxies
• The ESO SupJup Survey VIII. Chemical fingerprints of young L dwarf twins
• PRODIGE - envelope to disk with NOEMA: V. Low 12C/13C ratios for CH3OH and CH3CN in hot corinos
• Molecular isotopologue measurements toward super star clusters and the relation to their ages in NGC253 with ALCHEMI
• Chemical evolution imprints in the rare isotopes of nearby M dwarfs
• Nitrogen Abundance Distribution in the inner Milky Way
• Exploring giant barium stars: ${}^{12}\mathrm{C}{/}^{13}\mathrm{C}$ ratio and elemental abundances of carbon, nitrogen, and oxygen
• ${}^{18}$O${/}^{17}$O abundance ratio toward a sample of massive star forming regions with parallax distances
• Yields from massive stars in binaries. Chemical evolution of the Milky Way disk
• Assessing stellar yields in Galaxy chemical evolution: observational stellar abundance patterns
• The Missing Link: Testing Galactic Chemical Evolution Models with the First Multi-Isotopic Abundances in Solar Twin Stars
• Carbon from massive binary-stripped stars over cosmic time: effect of metallicity
• The Wanderer: Charting WASP-77A b's Formation and Migration Using a System-Wide Inventory of Carbon and Oxygen Abundances
• ${}^{14}$N${/}^{15}$N abundance ratio toward massive star-forming regions with different Galactic distances
• A Census of Sun's Ancestors and their Contributions to the Solar System Chemical Composition
• The challenging first direct measurement of the 65 keV resonance strength in the ${}^{17}$O(p,$\gamma$)${}^{18}$F reaction at LUNA