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Observations of high‐redshift supernovae (SNe) open a novel opportunity to study the massive star population in the early Universe. We study the detectability of superluminous SNe with upcoming optical and near‐infrared (NIR) surveys. Our calculations are based on the cosmic star‐formation history, the SN occurrence rate, the characteristic colour and the light curve of the SNe, which are all calibrated using available observations. We show that 15–150 SNe up to  z ∼ 4 will be discovered by the proposed Subaru/Hyper Suprime‐Cam deep survey, a 30‐deg 2  survey with 24.5 AB mag depth in the  z  band for 3 months. With its ultradeep layer (3.5 deg 2  with 25.6 AB mag depth in the  z  band for 4 months), the highest redshift can be extended to  z ∼ 5. We further explore the detectability by upcoming NIR surveys utilizing future satellites such as  Euclid ,  WFIRST  and  WISH . The wide‐field NIR surveys are very efficient at detecting high‐redshift SNe. With a hypothetical deep NIR survey for 100 deg 2  with 26 AB mag depth, at least ∼50 SNe will be discovered at  z  &gt; 3 in half a year. The number of detected SNe can place a strong constraint on the stellar initial mass function or its slope, especially at the high‐mass end. Superluminous SNe at high redshifts can be distinguished from other types of SNe by the long time‐scale of their light curves in the observer’s frame, optical colours redder than other core‐collapse SNe and NIR colours redder than any other type of SNe.

Detectability of high‐redshift superluminous supernovae with upcoming optical and near‐infrared surveys