LERMA UMR8112

Laboratoire d’Études du Rayonnement et de la Matière en Astrophysique et Atmosphères



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LERMA UMR8112

Observatoire de Paris LERMA - UMR8112
77 avenue Denfert Rochereau - 75014 Paris

5 place Jules Janssen - 92190 MEUDON

4 place Jussieu Tour 32-33 - 3eme ET - 75005 Paris

Université de Cergy-Pontoise

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Credits

This website uses a graphic template that is designed and produced as part of the project for the harmonization of CNRS websites.

Project manager

Marco Cucchi (Pôle-web, DirCom, CNRS)

Web template development (Web team, Communications Department, CNRS)

  • Pascal Verrier: web development
  • Eric Furlan: web design and integration

Development of the plugin "Seminar"

Amaury Adon

Development of the initial versions of the template

Frank de Albuquerque - Jean-Baptiste Pressac (CNRS) - Valérie Pierre (CNRS) - Benoît Chassigneux - Julien Barnier (GRS) - Jean-Christophe Monferran (LAHIC) - Stéphane Pouyllau (CRHST)

CSS drop-down menu

Eric Meyer - http://more.ericmeyeroncss.com/projects/06/

Photo credits for the default banner

© CNRS Photothèque

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5.3.15

Logo SPIPKit made with SPIP (Internet publication system), free software published under GPL licence

Séminaires à venir

Vendredi 3 juillet 2020, 14h00
,
visioconférence
Metallicity gradients of star-forming regions since cosmic noon
Patricia B. TISSERA
Universidad Andrés Bello, Santiago
résumé :
The evolution of chemical abundances in galaxies provides crucial information to study how galaxies formed and evolved. Results in the Local Universe show that on average, disc galaxies have negative metallicity gradients. As a function of redshift, the trend is not clear enough yet, although there is a significant fraction of positive ('inverted') metallicity gradients.

Using hydrodynamical cosmological simulations, we studied the metallicity gradients at z=0 and the processes that might affect them and the azimuthal metallicity distribution such as mergers, SN and AGN feedback and gas inflows.

In this talk I am going to summarize the latest results on the evolution of the metallicity gradients as a function of stellar mass, galaxy size and star formation efficiency from z~0 to z~2.5.
 
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