Overview of the Jiangmen Underground Neutrino Observatory (JUNO)

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Overview of the Jiangmen Underground Neutrino Observatory (JUNO)

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Overview of the Jiangmen Underground Neutrino Observatory (JUNO) Yu-Feng Li (李玉峰) Experiment Physics Center, Institute of High Energy Physics, Chinese Academy of Sciences, YuQuan Road 19B, 100049, Beijing, P. R. China Email: liyufeng@ihep.ac.cn 1. Introduction 5. Detector Concept (one option) After the discovery [PRL 108, 171803 (2012)] of non-zero theta(13) in the Daya Bay Reactor Neutrino Experiment, the neutrino mass hierarchy (MH) and lepton CP violation (CPV) are the central concerns in neutrino oscillation experiments. The neutrino MH is crucial for the measurements of CPV, the neutrinoless double beta decay and the supernova neutrinos. The neutrino MH is also fundamental to distinguish among different neutrino mass models. The neutrino MH can in principle be determined in the oscillations of accelerator neutrinos, reactor neutrinos and atmospheric neutrinos. The Jiangmen Underground Neutrino Observatory (JUNO), which is located at Kaiping, Jiangmen in South China, is designed to determine the neutrino MH using reactor neutrino oscillations [PRD 78, 111103 (2008)]. It is extremely difficult to build both the stainless steel tank and the acrylic tank. There are other options: (a) No steel tank (b) Acrylic box (c) Balloon (d) Steel tank only R&D are still ongoing for these options. Muon tracking Liquid Scintillator 20 kt Acrylic sphere: φ34.5m SS sphere: φ37 .5m Water Seal ~15000 20” PMTs optical coverage: 70-80% Stainless steel tank Oil buffer 6kt Water Buffer 10kt VETO PMTs 2. Baseline 6. Technical Challenges KamLAND JUNO LS mass ~1 kt 20 kt Energy Resolution 6%/E 3%/E Light yield 250 p.e./MeV 1200 p.e./MeV Requirements: Large detector: 20 kt LS Energy resolution: 3%/E  1200p.e./MeV Ongoing R&D: Low cost, high QE “PMT” Highly transparent LS: 15m  30m Daya Bay 60 km JUNO KamLAND More Photoelectrons – PMT: High QE photocathode MCP PMT with reflection photocathode (c) More coverage The optimum baseline is required to be at the oscillation maximum of , where the fine structure of oscillations is used to determine the MH. Dm212 Dm213 3. Experiment Site Daya Bay Huizhou Lufeng Yangjiang Taishan Status Operational Planned approved Under construction Power 17.4 GW 18.4 GW More Photoelectrons – LS: (d) Longer attenuation length (purification, e.g., Al2O3) (e) Higher light yield (Low temperature or fluor concentration optimization) Daya Bay Huizhou Lufeng Yangjiang Taishan Current site Previous site ~53 km A closer look: In granite 270 m high Mountain The interference oscillation effects due to baseline differences are crucial. Baseline differences from reactor cores should be less than 500 m. Therefore, the current site is better than the previous one [PRD 88, 013008 (2013)] . 7. Project Status 4. Physics Potentials Nominal setups: 20 kt liquid scintillator (LS) detector 3% energy resolution 52-53 km baselines 36 GW and 6 years MH sensitivity with 6 years' data of JUNO [PRD 88, 013008 (2013)]： 3 with relative measurement, 4 with absolute Δm2 measurement (if accelerator neutrino experiments can measure Δm2 to ~1% level), after taking into account the spread of reactor cores, the uncertainties in reactor neutrino fluxes and from the energy scale and non-linearity. Other physics: Precision measurement Supernova neutrinos Solar neutrinos Geo-neutrinos etc. (1) Funding Great support from CAS: “Strategic Priority Research Program” Approved on Feb.1, 2013 (2) Brief schedule Construction: 2013-2019 Filling & data taking: 2020 (3) Collaboration Two get-together meetings in Jan. and Jul. 2013 Next meeting in Jiangmen (experimental site), Jan. 2014. Welcome collaborators 8. Conclusion Current JUNO Dm212 ~3% ~0.6% Dm223 ~5% sin2q12 ~6% ~0.7% sin2q23 ~20% N/A sin2q13 ~14% ~4% ~ 15% (1) JUNO is designed to determine the neutrino MH and measure 4/6 of the oscillation parameters by using reactor neutrinos. It can also detect the neutrino sources from astrophysics and geophysics. (2) The idea of JUNO was proposed in 2008, now boosted by the large theta(13). Funding is approved from CAS. (3) JUNO has strong physics potentials, meanwhile contains significant technical challenges.