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The electromagnetic transients accompanying compact binary mergers($\gamma$-ray bursts, afterglows and 'macronovae') are crucial to pinpoint thesky location of gravitational wave sources. Macronovae are caused by theradioactivity from freshly synthesised heavy elements, e.g. from dynamic ejectaand various types of winds. We study macronova signatures by usingmulti-dimensional radiative transfer calculations. We employ the radiativetransfer code SuperNu and state-of-the-art LTE opacities for a fewrepresentative elements from the wind and dynamical ejecta (Cr, Pd, Se, Te, Br,Zr, Sm, Ce, Nd, U) to calculate synthetic light curves and spectra for a rangeof ejecta morphologies. The radioactive power of the resulting macronova iscalculated with the detailed input of decay products. We assess the detectionprospects for our most complex models, based on the portion of viewing anglesthat are sufficiently bright, at different cosmological redshifts ($z$). Thebrighter emission from the wind is unobscured by the lanthanides (or actinides)in some of the models, permitting non-zero detection probabilities forredshifts up to $z=0.07$. We also find the nuclear mass model and the resultingradioactive heating rate are crucial for the detectability. While for the mostpessimistic heating rate (from the FRDM model) no reasonable increase in theejecta mass or velocity, or wind mass or velocity, can possibly make the lightcurves agree with the observed nIR excess after GRB130603B, a more optimisticheating rate (from the Duflo-Zuker model) leads to good agreement. We concludethat future reliable macronova observations would constrain nuclear heatingrates, and consequently help constrain nuclear mass models.

Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers