Characterising the Spatial Variation of Dust Attenuation in Galaxies

Given advances in integral-field spectroscopy (IFS), which allows spectroscopy to be obtained simultaneously over a large region, it is now practical to examine the structural nature of dust attenuation within individual galaxies in the local Universe (e.g., Sydney-AAO Multi-object Integral-field spectrograph survey (SAMI; Bryant et al. 2015); Mapping Nearby Galaxies at APO (MaNGA; Bundy et al. 2015)). You will perform an analysis of nearby galaxies imaged with IFS that are resolved in imaging data from Ultraviolet to Infrared wavelengths. By performing a region-by-region analysis of the dust attenuation inferred from the ionised gas (via IFS data) and the emission from stars and dust, we will gain a better understanding of the factors giving rise to its spatial variation (see above Figure). The full spectral range of data available for these galaxies will also be used to explore the amount of variation in commonly adopted dust correction diagnostics. To perform this study, you will utilise archival IFS data from the SAMI and/or MaNGA surveys. 

This project will provide you with expertise in the analysis of IFS and other multi-wavelength data that are highly desired skills in the field. You will also gain knowledge of new astrophysical software and improve your coding ability. For more information about this potential research topic or activity, or to discuss any related research area, please contact the supervisor.