To be published in "The Spectral Energy Distribution of Gas-Rich Galaxies: Confronting Models with Data", Proceedings of the International Workshop held 4-8 October 2004 in Heidelberg, 4-8 Oct. 2004, Edited by Cristina C. Popescu and Richard J. Tuffs, AIP Conf. Ser.

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Abstract. We give an overview of the factors shaping the ultraviolet (UV)/optical - far-infrared (FIR)/submillimeter (submm) spectral energy distributions (SEDs) of normal (non-starburst) galaxies. Particular emphasis is placed on the influence of the geometry of dust and stars on the propagation of light through the interstellar medium. Although strong constraints can be placed on the amount and large scale distribution of dust in disks from the appearance of the galaxies in the optical/UV range, this dust does not account for the observed amplitude and colour of the FIR/submm radiation. Additional, optically thick components of dust associated with the young stellar population on large and small scales are required to account for the complete UV/optical - FIR/submm SEDs. Self-consistent models for the calculation of SEDs of spiral galaxies are reviewed, and their predictions for the dust emission and the attenuation of starlight are compared and contrasted.

Table of Contents

INTRODUCTION

WHAT SHAPES THE SEDS OF GALAXIES?

MODELS WHICH ACCOUNT FOR THE OPTICAL APPEARANCE OF GALAXIES

MODELS WHICH ACCOUNT FOR THE ENTIRE OPTICAL/FIR/SUBMM SEDs

Choice of intrinsic distributions of stars and dust

Testing the models

The origin of dust heating

Application to statistical samples

A CLOSER LOOK AT THE ROLE OF CLUMPS IN SHAPING THE SEDS OF GALAXIES

MODELLING THE ATTENUATION OF STELLAR LIGHT IN GALAXIES

OUTLOOK

REFERENCES