"The formation and evolution of dust in core-collapse supernovae (CCSNe) has been much debated following the suggestion that CCSNe could be the source of the large masses of dust observed in some very early Universe galaxies at redshifts z > 6. Observations in the far-IR by Herschel and ALMA of a few CCSNe have yielded high cold dust masses (0.1 – 1.0 M⊙), which, if representative of the wider CCSN population, could potentially account for the dust masses seen in the early Universe. Redshifted radiation that emanates from the receding regions of a CCSN must traverse a potentially dusty interior causing it to be more greatly attenuated than blueshifted emission from the approaching regions. This can result in asymmetrical, blueshifted optical and NIR line profiles which can be modelled in order to infer the mass and properties of the newly-formed dust within the supernova.

SN 2005ip is a Type IIn CCSN that provides a unique opportunity to study the formation and evolution of dust in CCSNe. It has been regularly observed, both photometrically and spectroscop- ically, since its outburst 13 years ago. The appearance of dust-affected asymmetrical optical line profiles and an IR excess at early times allow the mass, nature and location of dust within SN 2005ip to be investigated. I present models of the progressively blueshifted, broad Hα line that arises in the ejecta at early times (< 200 d) along with models of the evolving intermediate width Hα and HeI λ7065 A lines that arise in a post-shock region at later times (∼400 d – ∼4000 d). I determine the dust masses that have formed and discuss the location of the dust and the clumpy structure of the post-shock region. I discuss how these newly-formed dust masses relate to previous dust mass estimates from SED fitting for SN 2005ip and compare my SN 2005ip dust mass estimates to dust mass estimates for other CCSNe.

This work was supported by ERC Grant 694520 SNDUST."