1. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 MAGPOP ESR at the Institut d’Astrophysique de Paris MAGPOP Mid Term Review La Palma, 7 – 8 December 2006 Elisabete da Cunha (Early Stage Researcher)

2. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 SHORT PROFILE 1  Nationality: Portuguese  Previously at the Faculty of Sciences of the University of Porto (Portugal): degree (July 2005) in Physics/Applied Mathematics (Astronomy)  Broad background in Physics and Mathematics  Cosmology, Extragalactic Astronomy, Observational Astronomy, …  MAGPOP Research Training Network:  3 year PhD project (10.2005 – 10.2008)  Node: Institut d’Astrophysique de Paris, CNRS, Université Pierre et Marie Curie – Paris VI, France  Supervisor: Stéphane Charlot  Modelling and interpreting galaxy spectral energy distributions

3. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 SCHOOLS 2 École Doctorale d’Île de France (Doctoral School):  1st year:  Numerical simulations and parallel calculus  Evolution of local and distant galaxies  Dynamics of galaxies  2nd year:  Data analysis  Cosmology  Introduction to telescope time proposals MAGPOP Budapest Summer School (08.2006):  Observational Astronomy (ground- and space-based)  Stellar population synthesis models  Galaxy formation and evolution models  Practical sessions:  Virtual Observatory  Telescope time proposals

4. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 ACTIVITIES & CONFERENCES 3 IAP activities:  Annual Thesis Day : where PhD students present their work to other researchers and students in the IAP.  Weekly seminars on several subjects.  Weekly Jornal Club with the Galaxy Group at the IAP. Conferences & Meetings:  MAGPOP Network Meeting in Toledo, Spain (02.2006)  ENAA 2006 : National Meeting of Portuguese Astronomical Society in Espinho, Portugal (07.2006)

5. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 RESEARCH PROJECTS 4  Simple model for the infrared emission by dust in galaxies: with S. Charlot (IAP), D. Elbaz (CEA Saclay).  Simple model for the full spectral energy distributions of galaxies from the ultraviolet to infrared: with S. Charlot (IAP), D. Elbaz (CEA Saclay).  Infrared cosmological background /first stars and galaxies: with S. Charlot (IAP), E. Vangioni (IAP), K. Olive (Univ. Minnesota), F. Daigne (IAP). Current projects and collaborators:

6. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 MODELLING GALAXY SPECTRA 5 Modelling the SED:  Star formation history  Dust content PhD Thesis: Modelling and interpretation of the spectral energy distributions (SEDs) of galaxies from ultraviolet to infrared wavelengths with simple models. UV Optical DUST Infrared STARS ULIRG Starburst Disk Elliptical

7. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006

8. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 MODELLING GALAXY SPECTRA 6 We are developing a simple, versatile model to interpret consistently the spectra of galaxies at ultraviolet, optical and infrared wavelengths in terms of a set physical parameters describing the star formation history and the dust content. This model will be applied to the analysis of large samples of galaxies. Ultraviolet and optical emission: Stellar populations synthesis models (Bruzual & Charlot) to describe stellar emission + simple prescription for the attenuation by dust (Charlot & Fall). Infrared emission: Develop a simple, physically motivated model for the IR emission, which allows one to interpret the mid- and far-infrared emission by dust in galaxies consistently with the emission at shorter wavelentghs. consistently connected

9. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 MODELLING GALAXY SPECTRA 7 Dust luminosity:  The total luminosity reradiated by dust grains in a galaxy equal to the total luminosity they absorb from stars.  Influence of the finite lifetimes of stellar birth clouds on the absorption of radiation: photons emitted by stars that live longer than the birth clouds (~10 Myr) propagate only through the ambient ISM before they escape from the galaxy. giant molecular clouds in which stars form: H II region (hydrogen ionized by young hot stars) + H I region (neutral hydrogen) interstellar medium (older and colder stars)

10. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 MODELLING GALAXY SPECTRA – Infrared 8 Dust components:  Polycyclic Aromatic Hydrocarbons (PAHs) Organic molecules that have a typical emission spectrum in the mid-infrared (between ~5 and 20 µm).  Very Small Grains (VSGs) Small carbonaceous grains that are heated by the absorption of single photons and reach high temperatures (several hundreds of K).  Big Grains (BGs) Composed mainly of silicates and graphite with sizes up to ~100 nm; these grains are in thermal equilibrium with the radiation field and emit as modified black bodies.

11. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 MODELLING GALAXY SPECTRA – Infrared 9 Example of a model infrared galaxy spectrum: T BGs BC f µ = L d ISM / L d total  1 = L PAH / L d BC  2 = L VSGs (200K) / L d BC  3 = L VSGs (80K) / L d BC  4 = L BGs BC / L d BC

12. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 10 NGC 5713  Spiral galaxy (SABbcp)  d=26.6 Mpc Result of the fit to ISO and IRAS infrared fluxes to the model library – model SED and comparison with observations. MODELLING GALAXY SPECTRA – Infrared

13. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 11 NGC 5713  Spiral galaxy (SABbcp)  d=26.6 Mpc Result of the fit to ISO and IRAS infrared fluxes to the model library – probability density histogram for each parameter of the model. MODELLING GALAXY SPECTRA – Infrared

14. Elisabete da Cunha (ESR – IAP) MAGPOP Mid Term Review – La Palma, 12.2006 12 NEXT...  Connect with stellar emission models and with constraints on the optical attenuation curve (O. Vince, Budapest Node ) model galaxy spectra in the ultraviolet, optical and infrared  Application of the new model to observed samples of galaxies in the UV, optical and IR (V. Buat, J. Walcher, Marseille Node ; T. Heckman, JHU Node ). Extract information about key physical parameters related to the star formation history and the interaction between stellar radiation and dust.  Implications for the evolution of the physical properties of galaxies ( MPA Node ). galaxy formation and evolution models