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[Abridged] We present an integrated photometric spectral energy distribution(SED) of the Magellanic-type galaxy NGC 4449 from the far-ultraviolet (UV) tothe submillimetre, including new observations acquired by the Herschel SpaceObservatory. We include integrated UV photometry from the Swift Ultraviolet andOptical Telescope using a measurement technique which is appropriate forextended sources with coincidence loss. In this paper, we examine the availablemultiwavelength data to infer a range of ages, metallicities and star formationrates for the underlying stellar populations, as well as the composition andthe total mass of dust in NGC 4449.  We present an iterative scheme, which allows us to build an in-depth andmulticomponent representation of NGC 4449 `bottom-up', taking advantage of thebroad capabilities of the photoionization and radiative transfer code MOCASSIN(MOnte CArlo SimulationS of Ionized Nebulae). We fit the observed SED, theglobal ionization structure and the emission line intensities, and infer arecent SFR of 0.4 Msolar/yr and a total stellar mass of approximately 1e9Msolar emitting with a bolometric luminosity of 5.7e9 Lsolar. Our fits yield atotal dust mass of 2.9e6 Msolar including 2 per cent attributed to polycyclicaromatic hydrocarbons. We deduce a dust to gas mass ratio of 1/190 within themodelled region. While we do not consider possible additional contributionsfrom even colder dust, we note that including the extended HI envelope and themolecular gas is likely to bring the ratio down to as low as ~ 1/800.

monthly notices of the royal astronomical society

A multiwavelength study of the Magellanic-type galaxy NGC 4449 - I.  Modelling the spectral energy distribution, the ionization structure and the  star formation history