AGB stars Galactic evolution models self-enrichment in Globular Clusters SED of high-redshift quasar Infrared luminosity of galaxies Gas from AGBs contaminated.

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AGB stars Galactic evolution models self-enrichment in Globular Clusters SED of high-redshift quasar Infrared luminosity of galaxies Gas from AGBs contaminated by TDUHBB Flavia Dell’Agli Marcella Di criscienzo Observatory of Rome Paolo Ventura Raffaella Schneider

Gas yields from AGB stars: highly uncertain!!! TDU HBB mixing Convection modelling C N O

A laboratory for AGBs: the LMC

SILICATES CARBON DUST Z HBB TDU WHICH DUST FROM AGBs ? Di Criscienzo +, 2013, MNRAS, 433, 313

Rome Heidelbergh Unfortunately, the uncertainties affecting the evolution of AGBs reflect into the dust formation process.. SILICATES CARBON DUST

CARBON STARS HBB Understanding the colour-colour plane of AGBs in the LMC Can we understand how convection works in AGBs, based on photometric arguments? Dell’Agli , MNRAS, 447, 2992

Ventura+ 2015, MNRAS, 450, 3181

IR colours of obscured AGBs unaffected by convection modelling !!

C/O ≈ 0.03 C/O ≈ 0.4 IR spectroscopy of obscured stars crucial to understand convection in AGBs

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