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Our current knowledge of star formation and accretion luminosity athigh-redshift (z>3-4), as well as the possible connections between them, reliesmostly on observations in the rest-frame ultraviolet (UV), which are stronglyaffected by dust obscuration. Due to the lack of sensitivity of past andcurrent infrared (IR) instrumentation, so far it has not been possible to get aglimpse into the early phases of the dust-obscured Universe. Among the nextgeneration of IR observatories, SPICA, observing in the 12-350 micron range,will be the only facility that can enable us to make the required leap forwardin understanding the obscured star-formation rate and black-hole accretion ratedensities (SFRD and BHARD, respectively) with respect to what Spitzer andHerschel achieved in the mid- and far-IR at z<3. In particular, SPICA will havethe unique ability to trace the evolution of the obscured SFRD and BHARD overcosmic time, from the peak of their activity back to the reionisation epoch(i.e., 3<z<6-7), where its predecessors had severe limitations. Here we discussthe potential of both deep and shallow photometric surveys performed with theSPICA mid-IR instrument (SMI), enabled by the very low level of impact of dustobscuration in a band centred at 34 micron. These unique unbiased photometricsurveys that SPICA will perform will be followed up by observations both withthe SPICA spectrometers and with other facilities at shorter and longerwavelengths, with the aim to fully characterise the evolution of AGNs andstar-forming galaxies after re-ionisation.

Tracing the evolution of dust obscured star-formation and accretion back to the reionisation epoch with SPICA