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The emission from shock breakouts (SBOs) represents the earliestelectromagnetic (EM) signal emitted by cataclysmic events involving theformation or the merger of neutron stars (NSs). As such, SBOs carry uniqueinformation on the structure of their progenitors and on the explosion energy.The characteristic~SBO emission is expected in the UV range, and its detectionis one of the key targets of~the ULTRASAT satellite. Among SBO sources, wefocus on a specific class involving the formation of fast spinning magnetars inthe core-collapse (CC) of massive stars. Fast spinning magnetars are expectedto produce a specific signature in the early UV supernova light curve, poweredby the extra spin energy quickly released by the NS. Moreover, they areconsidered as optimal candidates for the emission of long-transientgravitational wave (GW) signals, the detection of which requires early EMtriggers to boost the sensitivity of dedicated GW search pipelines. Wecalculate early supernova UV light curves in the presence of a magnetar centralengine, as a function of the explosion energy, ejecta mass and magnetarparameters. We then estimate the ULTRASAT detection horizon (z < 0.15) as afunction of the same physical parameters, and the overall expected detectionrate finding that magnetar-powered SBOs may represent up to 1/5 of the totalevents detected by ULTRASAT. Moreover, at the expected sensitivity of theLIGO/Virgo/Kagra O5 science run, one such event occurring within 5 Mpc willprovidean ideal trigger for a GW long transient search. Future GW detectorslike the Einstein Telescope will push the horizon for joint EM-GW detections to35-40 Mpc.

UV signatures of magnetar formation and their crucial role for Gravitational Wave detection