  The IceCube Neutrino Observatory, a cubic-kilometer-scale neutrino detector
at the geographic South Pole, has reached a number of milestones in the field
of neutrino astrophysics: the discovery of a high-energy astrophysical neutrino
flux, the temporal and directional correlation of neutrinos with a flaring
blazar, and a steady emission of neutrinos from the direction of an active
galaxy of a Seyfert II type and the Milky Way. The next generation neutrino
telescope, IceCube-Gen2, currently under development, will consist of three
essential components: an array of about 10,000 optical sensors, embedded within
approximately 8 cubic kilometers of ice, for detecting neutrinos with energies
of TeV and above, with a sensitivity five times greater than that of IceCube; a
surface array with scintillation panels and radio antennas targeting air
showers; and buried radio antennas distributed over an area of more than 400
square kilometers to significantly enhance the sensitivity of detecting
neutrino sources beyond EeV. This contribution describes the design and status
of IceCube-Gen2 and discusses the expected sensitivity from the simulations of
the optical, surface, and radio components.
