Modeling the dust Spectral Energy Distribution of NGC 4214

TL;DR

This paper models the dust spectral energy distribution of NGC 4214, distinguishing between emission from HII regions and diffuse dust, using extensive multi-wavelength data and realistic geometry-based templates.

Contribution

It introduces a detailed modeling approach that separates dust emission sources in a starburst dwarf galaxy using radiation transfer templates and comprehensive data analysis.

Findings

Achieved a good fit for NGC 4214's total dust SED

Utilized multi-wavelength data to constrain model parameters

Demonstrated the effectiveness of separating emission components

Abstract

We have carried out a detailed modeling of the dust Spectral Energy Distribution (SED) of the nearby, starbursting dwarf galaxy NGC 4214. A key point of our modeling is that we distinguish the emission from (i) HII regions and their associated photodissociation regions (PDRs) and (ii) diffuse dust. For both components we apply templates from the literature calculated with a realistic geometry and including radiation transfer. The large amount of existing data from the ultraviolet (UV) to the radio allows the direct measurement of most of the input parameters of the models. We achieve a good fit for the total dust SED of NGC 4214. In the present contribution we describe the available data, the data reduction and the determination of the model parameters, whereas a description of the general outline of our work is presented in the contribution of Lisenfeld et al. in this volume.