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Next-generation neutrino telescopes with substantially improved sensitivity are required to pinpoint the sources of the diffuse astrophysical neutrino flux detected by IceCube and uncover the century-old puzzle of cosmic-ray origins. A detector near the Equator will provide a unique viewpoint of the neutrino sky, complementing IceCube and other neutrino telescopes in the Northern Hemisphere. Here we present results from an expedition to the northeastern region of the South China Sea, in the western Pacific Ocean. A favourable neutrino telescope site was found on an abyssal plain at a depth of ~3.5 km. At depths below 3 km, the sea current speed, water absorption and scattering lengths for Cherenkov light were measured to be vc < 10 cm s−1, λabs ≈ 27 m and λsca ≈ 63 m, respectively. Accounting for these measurements, we present the design and expected performance of a next-generation neutrino telescope, Tropical Deep-sea Neutrino Telescope (TRIDENT). With its advanced photon-detection technology and large dimensions, TRIDENT expects to observe the IceCube steady source candidate NGC 1068 with 5σ significance within 1 year of operation. This level of sensitivity will open a new arena for diagnosing the origin of cosmic rays and probing fundamental physics over astronomical baselines.A South China Sea expedition in 2021 identified a 3.5-km-deep site close to the Equator for a next-generation neutrino telescope: TRIDENT. A large array of advanced detectors will be arrayed on the seabed to probe fundamental physics and explore the extreme Universe.

The SNO + collaboration reports its first spectral analysis of long-baseline reactor antineutrino oscillation using 114 tonne-years of data. Fitting the neutrino oscillation probability to the observed energy spectrum yields constraints on the neutrino mass-squared difference Δ m 21 2 . In the ranges allowed by previous measurements, the best-fit Δ m 21 2 is ( 8 . 85 - 1.33 + 1.10 ) × 10 - 5 eV 2 . This measurement is continuing in the next phases of SNO+ and is expected to surpass the present global precision on Δ m 21 2 with about three years of data.

The SNO+ collaboration reports its first spectral analysis of long-baseline reactor antineutrino oscillation using 114 tonne-years of data. Fitting the neutrino oscillation probability to the observed energy spectrum yields constraints on the neutrino mass-squared difference \\( m^2_21\\). In the ranges allowed by previous measurements, the best-fit \\( m^2_21\\) is (8.85\\(^+1.10_-1.33\\)) \\(\\) 10\\(^-5\\) eV\\(^2\\). This measurement is continuing in the next phases of SNO+ and is expected to surpass the present global precision on \\( m^2_21\\) with about three years of data.

The direction of individual \\(^8\\)B solar neutrinos has been reconstructed using the SNO+ liquid scintillator detector. Prompt, directional Cherenkov light was separated from the slower, isotropic scintillation light using time information, and a maximum likelihood method was used to reconstruct the direction of individual scattered electrons. A clear directional signal was observed, correlated with the solar angle. The observation was aided by a period of low primary fluor concentration that resulted in a slower scintillator decay time. This is the first time that event-by-event direction reconstruction in high light-yield liquid scintillator has been demonstrated in a large-scale detector.

The SNO+ Collaboration reports the first evidence of reactor antineutrinos in a Cherenkov detector. The nearest nuclear reactors are located 240~km away in Ontario, Canada. This analysis uses events with energies lower than in any previous analysis with a large water Cherenkov detector. Two analytical methods are used to distinguish reactor antineutrinos from background events in 190 days of data and yield consistent evidence for antineutrinos with a combined significance of 3.5\\(\\sigma\\).

This paper reports results from a search for single and multi-nucleon disappearance from the \\(^{16}\\)O nucleus in water within the \\snoplus{} detector using all of the available data. These so-called \"invisible\" decays do not directly deposit energy within the detector but are instead detected through their subsequent nuclear de-excitation and gamma-ray emission. New limits are given for the partial lifetimes: \\(\\tau(n\\rightarrow inv) > 9.0\\times10^{29}\\) years, \\(\\tau(p\\rightarrow inv) > 9.6\\times10^{29}\\) years, \\(\\tau(nn\\rightarrow inv) > 1.5\\times10^{28}\\) years, \\(\\tau(np\\rightarrow inv) > 6.0\\times10^{28}\\) years, and \\(\\tau(pp\\rightarrow inv) > 1.1\\times10^{29}\\) years at 90\\% Bayesian credibility level (with a prior uniform in rate). All but the (\\(nn\\rightarrow inv\\)) results improve on existing limits by a factor of about 3.

The SNO+ Collaboration reports new results on reactor antineutrino oscillations using data acquired from May 2022 through July 2025. The spectral analysis of a flux dominated by nuclear reactors at 240, 350, and 355 kilometers yields the mass-squared difference \\(\\Delta m^2_{21}=(7.93^{+0.21}_{-0.24})\\times 10^{-5}\\) eV\\(^2\\). This result is compatible with and approaches the precision of the only other long-baseline reactor antineutrino measurement, by KamLAND. Combining these measurements, along with those from solar neutrino experiments, the global values of the neutrino mixing parameters become: \\(\\Delta m^2_{21}\\) = \\((7.63\\pm0.17)\\times 10^{-5}\\) eV\\(^2\\) and \\(\\sin^2{\\theta_{12}}=0.310\\pm0.012\\). The analysis of geoneutrinos at SNO+ is also improved, with a measured signal of 49\\(^{+13}_{-12}\\) TNU.

SNO+ is a large-scale liquid scintillator experiment with the primary goal of searching for neutrinoless double beta decay, and is located approximately 2 km underground in SNOLAB, Sudbury, Canada. The detector acquired data for two years as a pure water Cherenkov detector, starting in May 2017. During this period, the optical properties of the detector were measured in situ using a deployed light diffusing sphere, with the goal of improving the detector model and the energy response systematic uncertainties. The measured parameters included the water attenuation coefficients, effective attenuation coefficients for the acrylic vessel, and the angular response of the photomultiplier tubes and their surrounding light concentrators, all across different wavelengths. The calibrated detector model was validated using a deployed tagged gamma source, which showed a 0.6% variation in energy scale across the primary target volume.

Next-generation neutrino telescopes with significantly improved sensitivity are required to pinpoint the sources of the diffuse astrophysical neutrino flux detected by IceCube and uncover the century-old puzzle of cosmic ray origins. A detector near the equator will provide a unique viewpoint of the neutrino sky, complementing IceCube and other neutrino telescopes in the Northern Hemisphere. Here we present results from an expedition to the north-eastern region of the South China Sea, in the western Pacific Ocean. A favorable neutrino telescope site was found on an abyssal plain at a depth of \\(\\sim\\) 3.5km. At depths below 3km, the sea current speed, water absorption and scattering lengths for Cherenkov light, were measured to be \\(v_{\\mathrm{c}}<\\)10cm/s, \\(\\lambda_{\\mathrm{abs} }\\simeq\\) 27m and \\(\\lambda_{\\mathrm{sca} }\\simeq\\) 63m, respectively. Accounting for these measurements, we present the design and expected performance of a next-generation neutrino telescope, TRopIcal DEep-sea Neutrino Telescope (TRIDENT). With its advanced photon-detection technology and large dimensions, TRIDENT expects to observe the IceCube steady source candidate NGC 1068 with 5\\(\\sigma\\) significance within 1 year of operation. This level of sensitivity will open a new arena for diagnosing the origin of cosmic rays and probing fundamental physics over astronomical baselines.