The ongoing and future searches for diffuse supernova neutrinos and sterile neutrinos carried out with large water-Cherenkov detectors require a precise determination of the backgrounds, especially those involving γ rays. Of great importance, in this context, is the process of neutron knockout through neutral-current scattering of atmospheric neutrinos on oxygen. Nuclear reinteractions of the produced neutron may in fact lead to the production of γ rays of energies high enough to mimic the processes of interest. In this article, we focus on the kinematical range suitable for simulations of atmospheric-neutrino interactions and provide the neutron-knockout cross sections computed using the formalism based on the realistic nuclear spectral function. The role of the strange-quark contribution to the neutral-current axial form factor is also analyzed. Based on the available experimental information, we give an estimate of the associated uncertainty. The detection of the antineutrino burst from the 1987A core-collapse supernova in the Large Magellanic Cloud by three independent experiments [1-3] marked the dawn of a new era in observational astronomy. That measurement, totaling 24 events, was feasible owing to not-too far distance from the collapsing star and to the extreme nature of supernova explosions. While the gravitational energy released in the act of collapse is ∼200-300 times higher than that produced by the Sun over its entire lifetime, ∼99% of it is radiated over a time scale of a few tens of seconds in the form of an immense flux of low-energy neutrinos [4].Supernovae have long been recognized as unique laboratories to study a number of fundamental physics issues [5]. The scarcity of the available data seems, however, to be an insuperable problem, because the frequency of the core-collapse events within our Galaxy is estimated to be 1.9 ± 1.1 per century [6].On the other hand, during the lifetime of the Milky Way, those phenomena have occurred approximately 100 million times, and the Universe witnesses them at the rate of approximately one per second [7]. All the past core-collapse supernovae have contributed to a diffuse supernova-neutrino (DSN) flux, which is expected to be tiny but continuous in time. Its detection may provide a great deal of information, complementary to that from the future neutrino bursts.Although its detailed features show some model dependence, it is rather well established that the predicted DSN spectrum has a peak at the value of 4-7 MeV with an exponential drop at higher energy [8]. In the low-energy region, E ν 8-12 MeV, the DSN signal is not accessible owing to an overwhelming flux of reactorν e . On the other hand, in the high-energy region, E ν 30-40 MeV, it is covered by the ν andν flux of atmospheric origin [8- * Present address: Department of Physics, Okayama University, Okayama 700-8530, Japan; Artur.Ankowski@roma1.infn.it † Omar.Benhar@roma1.infn.it 10]. Moreover, at E ν 16 (19) MeV, the solar neutrino flux from the 8 B (hep) chain dominates over the DSN flux. Therefor...