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Aims: Using 2D Mgii h&k solar prominence modelling, our aim is to understandthe formation of complex line profiles and how these are seen by the InterfaceRegion Imaging Spectrograph (IRIS). Additionally, we see how the properties ofthese simulated observations are interpreted through the use of traditional 1Dprominence modelling.  Methods: We used a cylindrical non-local thermodynamic equilibrium (NLTE) 2Dcomplete redistribution (CRD) code to generate a set of cylindrical prominencestrands, which we stacked behind each other to produce complex line profiles.Then, with the use of the point spread functions (PSFs) of IRIS, we were ableto predict how IRIS would observe these line profiles. We then used the 1D NLTEcode PROM in combination with the Cross Root Mean Square method (xRMS) to findthe properties recovered by traditional 1D prominence modelling.  Results: Velocities of magnitude lower than 10 km/s are sufficient to produceasymmetries in the Mgii h&k lines. However, convolution of these with the PSFsof IRIS obscures this detail and returns standard looking single peaks. Byincreasing the velocities by a factor of three, we recover asymmetric profileseven after this convolution. The properties recovered by xRMS appear adequateat first, but the line profiles chosen to fit these profiles do notsatisfactorily represent the line profiles. This is likely due to the largeline width of the simulated profiles.  Conclusions: Asymmetries can be introduced by multithread models withindependent Doppler velocities. The large line width created by these modelsmakes it difficult for traditional 1D forward modelling to find good matches.This may also demonstrate degeneracies in the solution recovered bysingle-species 1D modelling.

Mgii h&k fine structure prominence modelling and the consequences for observations