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The importance of following the evolution of the dust in galaxies on their SEDs

Published online by Cambridge University Press:  01 June 2008

A. Schurer ,
F. Calura ,
L. Silva ,
A. Pipino ,
G. L. Granato ,
F. Matteucci  and
R. Maiolino
A. Schurer
Affiliation:
Astrophysics Sector, SISSA/ISAS, Via Beirut 2-4, I-34014 Trieste, Italy email: schurer@sissa.it INAF, Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
F. Calura
Affiliation:
INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11 I-34131 Trieste, Italy
L. Silva
Affiliation:
INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11 I-34131 Trieste, Italy
A. Pipino
Affiliation:
Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
G. L. Granato
Affiliation:
INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11 I-34131 Trieste, Italy
F. Matteucci
Affiliation:
INAF, Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11 I-34131 Trieste, Italy INAF, Dipartimento Astronomico-Universita di Trieste, Via G. B. Tiepolo 11 I-34131 Trieste, Italy
R. Maiolino
Affiliation:
INAF – Osservatorio Astronomico di Roma, via di Frascati 33, Monte Porzio Catone, Italy
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Abstract

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We present photometric evolution of galaxies in which, in addition to the stellar component, the effects of an evolving dusty interstellar medium have been included with particular care. Starting from the work of Calura, Pipino & Matteucci (2008), in which chemical evolution models have been used to study the evolution of both the gas and dust components of the interstellar medium in spiral, elliptical and irregular galaxies, it has been possible to combine these models with a spectrophotometric stellar synthesis code that includes dust reprocessing (GRASIL) (Silva 1998) to analyse the evolution of the Spectral Energy Distributions (SED) of these galaxies. We test our models against observed SEDs both in the local universe and at high redshift. The importance of following the dust evolution is investigated by comparing our results with those obtained by adopting simple assumptions to treat this component. Possible errors from assuming a Milky Way dust composition and a dust-to-gas ratio scaling with the metallicity particularly in young galaxies, ellipticals and low metallicity galaxies are highlighted.

Keywords

ISM: abundancesISM: dustextinctiongalaxies: abundancesgalaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 147 - 151
Copyright
Copyright © International Astronomical Union 2008

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