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We present ultraviolet, optical and infrared photometry and opticalspectroscopy of the type Ic superluminous supernova (SLSN) Gaia16apd (= SN2016eay), covering its evolution from 26 d before the $g$-band peak to 234.1 dafter the peak. Gaia16apd was followed as a part of the NOT Unbiased TransientSurvey (NUTS). It is one of the closest SLSNe known ($z = 0.102\pm0.001$), withdetailed optical and ultraviolet (UV) observations covering the peak. Gaia16apdis a spectroscopically typical type Ic SLSN, exhibiting the characteristic blueearly spectra with O II absorption, and reaches a peak $M_{g} = -21.8 \pm 0.1$mag. However, photometrically it exhibits an evolution intermediate between thefast- and slowly-declining type Ic SLSNe, with an early evolution closer to thefast-declining events. Together with LSQ12dlf, another SLSN with similarproperties, it demonstrates a possible continuum between fast- andslowly-declining events. It is unusually UV-bright even for a SLSN, reaching anon-$K$-corrected $M_{uvm2} \simeq -23.3$ mag, the only other type Ic SLSN withsimilar UV brightness being SN 2010gx. Assuming that Gaia16apd was powered bymagnetar spin-down, we derive a period of $P = 1.9\pm0.2$ ms and a magneticfield of $B = 1.9\pm0.2 \times 10^{14}$ G for the magnetar. The estimatedejecta mass is between 8 and 16 $\mathrm{M}_{\odot}$ and the kinetic energybetween 1.3 and $2.5 \times 10^{52}$ erg, depending on opacity and assumingthat the entire ejecta is swept up into a thin shell. Despite the earlyphotometric differences, the spectra at late times are similar toslowly-declining type Ic SLSNe, implying that the two subclasses originate fromsimilar progenitors.

Gaia16apd -- a link between fast-and slowly-declining type I superluminous supernovae