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Many massive star forming disc galaxies in the redshift range 3 to 0.5 areobserved to have a clumpy morphology showing giant clumps of size $\sim$1 kpcand masses of about $10^7M_{\odot}$ to $10^{10} M_{\odot}$. The nature and fateof these giant clumps is still under debate. In this work we use 19high-resolution simulations of disc galaxies from the NIHAO sample to study theformation and the evolution of clumps in the discs of high redshift galaxies.We use mock HST - CANDELS observations created with the radiative transfer codeGRASIL-3D to carry out, for the first time, a quantitative comparison of theobserved fraction of clumpy galaxies and its evolution with redshift withsimulations. We find a good agreement between the observed clumpy fraction andthe one of the NIHAO galaxies. We find that dust attenuation can suppressintrinsically bright clumps and enhance less luminous ones. In our galaxysample we only find clumps in light (u-band) from young stars but not instellar mass surface density maps. This means that the NIHAO sample does notshow clumpy stellar discs but rather a clumpy light distribution originatingfrom clumpy star formation events. The clumps found in the NIHAO sample matchobserved age/color gradients as a function of distance from the galaxy centerbut they show no sign of inward migration. Clumps in our simulations disperseon timescales of a about a hundred Myr and their contribution to bulge growthis negligible.

NIHAO XIII: Clumpy discs or clumpy light in high redshift galaxies?