  Over the last decade, choked jets have attracted particular attention as
potential sources of high-energy cosmic neutrinos. Testing this hypothesis is
challenging because of the missing gamma-ray counterpart, hence the
identification of other electromagnetic signatures is crucial. A choked-jet
source is expected harboring in core-collapse supernovae with extended hydrogen
envelopes, leading to the release of ultraviolet and optical emission for a few
days. The ultraviolet band will be visible with an unprecedentedly large field
of view by the future mission satellite ULTRASAT, for which we investigate the
detection prospects in relation to the chocked source visibility in the optical
band with the currently operating telescope ZTF. As these sources can produce
neutrinos via hadronic and photohadronic interactions in choked jets, we also
investigate how neutrino observations by existing Cherenkov high-energy
neutrino telescopes (as IceCube and KM3NeT) can be used in association with
electromagnetic signals coming from shock breakout events. By considering
fiducial parameters of the source population and instruments performances, we
estimate the maximum redshift up to which ULTRASAT and ZTF are able to detect
ultraviolet and optical signals from these explosions, respectively.
Furthermore, we discuss coordinated multi-messenger observations among those
instruments and high-energy neutrino telescopes. ULTRASAT will be able to
double the volume of sky currently visible by ZTF for the same emitting sources
enlarging the sample of observed Type II supernovae by around 60%. For
optimized multi-messenger detections, the delay between neutrino produced at
the shock breakout occurrence (during the jet propagation inside the stellar
envelope) and ULTRASAT observations should be of around 4(5) days, with a
subsequent follow-up by instruments like ZTF about one week after.
