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We present new ALMA observations of the [OIII]88$\mu$m line and high angularresolution observations of the [CII]158$\mu$m line in a normal star forminggalaxy at z$=$7.1. Previous [CII] observations of this galaxy had detected[CII] emission consistent with the Ly$\alpha$ redshift but spatially slightlyoffset relative to the optical (UV-rest frame) emission. The new [CII]observations reveal that the [CII] emission is partly clumpy and partly diffuseon scales larger than about 1kpc. [OIII] emission is also detected at highsignificance, offset relative to the optical counterpart in the same directionas the [CII] clumps, but mostly not overlapping with the bulk of the [CII]emission. The offset between different emission components (optical/UV anddifferent far-IR tracers) is similar to what observed in much more powerfulstarbursts at high redshift. We show that the [OIII] emitting clump cannot beexplained in terms of diffuse gas excited by the UV radiation emitted by theoptical galaxy, but it requires excitation by in-situ (slightly dust obscured)star formation, at a rate of about 7 M$_{\odot}$/yr. Within 20 kpc from theoptical galaxy the ALMA data reveal two additional [OIII] emitting systems,which must be star forming companions. We discuss that the complex propertiesrevealed by ALMA in the z$\sim$7.1 galaxy are consistent with expectations byrecent models and cosmological simulations, in which differential dustextinction, differential excitation and different metal enrichment levels,associated with different subsystems assembling a galaxy, are responsible forthe different appearance of the system when observed with different tracers.

Extended ionised and clumpy gas in a normal galaxy at z=7.1 revealed by ALMA