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The RES-NOVA astroparticle physics observatory

Pattavina, Luca

Publisher
Zenodo
DOI
10.5281/zenodo.17815512
Repository
zenodo.org
Language
en

Abstract

Parallel talk presented at the XXI International Workshop on Neutrino Telescopes - Padova 29 September - 3 October 2025 (https://agenda.infn.it/event/44606/) Abstract: Core-collapse Supernovae (SN) represent critical astronomical events where nearly an entire star's binding energy is emitted as neutrinos. RES-NOVA addresses a significant challenge in astroparticle physics by introducing a novel neutrino detection method using cryogenic detectors constructed from ultra-pure archaeological lead (Pb). The project's key innovation lies in leveraging Coherent Elastic Neutrino-Nucleus Scattering (CEvNS), a detection mechanism with a cross-section approximately 10^4 times larger than traditional detection channels like inverse-beta decay or electron-scattering.The proposed detector array offers unprecedented sensitivity through its unique design. With a compact volume of just (30 cm)^3, RES-NOVA can survey approximately 90% of potential galactic SNe. The cryogenic detectors utilize Pb with extremely low intrinsic radioactivity, optimized for a low energy threshold and minimal background interference. This approach enables comprehensive measurement of SN neutrino signals while eliminating uncertainties related to neutrino flavor oscillations.Beyond SN research, the technology presents broad applications in astroparticle physics. The low-energy threshold and advanced background reduction techniques make these detectors promising for multi-messenger astronomy, Dark Matter searches, and fundamental neutrino property studies.In this contribution, we will present the current experimental efforts focused on the realization of this new technology. Results on the first prototype detectors will be presented, as well as sensitivity projections for the full detector operations. RES-NOVA represents a significant technological advancement, potentially establishing the foundation for a next-generation neutrino and dark matter observatory.

Full text

Luca Pattavina University and INFN of Milano-Bicocca [email protected] Oct. 2nd, 2025 - Padova, NEUTEL 2025 res-nova.unimib.it The RES-NOVA astroparticle physics observatory Neutrinos are emitted at all times Unique neutrino signature Neutrino transport simulation of a Core-Collapse SN A. Mirizzi et al., Riv. Nuovo Cim.39, 1 (2016) Nota Bene: neutrino flavor oscillations not included MPA Supernova Archive: https://wwwmpa.mpa-garching.mpg.de/ccsnarchive LS220 27 M⦿ CC-SN @ 10 kpc 2 Neutronization Accretion Cooling Pre-SN What is the average neutrino energy? vx is the most intense component of the flux vx is the most energetic component of the flux Current SN neutrino detectors are mostly sensitive to anti-ve/ve 27 M⦿ CC-SN Supernova Neutrino signal LS220 27 M⦿ CC-SN @ 10 kpc LS220 27 M⦿ CC-SN 3 > Equally sensitive to all v-flavors > High interaction cross-section Coherent neutrino-nucleus scattering All neutrino flavors are detected cross-section Neutrino energy Nuclear Form factor CE⌫NS =G2 F 4⇡F2(q2)E2 ⌫Q2 W Weak nuclear charge 4 > Equally sensitive to all v-flavors > High interaction cross-section Coherent neutrino-nucleus scattering All neutrino flavors are detected cross-section Neutrino energy Nuclear Form factor CE⌫NS =G2 F 4⇡F2(q2)E2 ⌫Q2 W Weak nuclear charge ~5% * Spin 0 interaction * 5 > Equally sensitive to all v-flavors > High interaction cross-section Coherent neutrino-nucleus scattering All neutrino flavors are detected cross-section Neutron number CE⌫NS /N2 6 Coherent neutrino-nucleus scattering Pb ideal target Highest neutron number Highest nuclear stability All neutrino flavors are detected cross-section Neutron number CE⌫NS /N2 7 + Measured nuclear Form Factor (PRex) Coherent neutrino-nucleus scattering Pb ideal target Highest neutron number Highest nuclear stability All neutrino flavors are detected Pb ideal target Highest neutron number Highest nuclear stability cross-section Neutron number CE⌫NS /N2 8 + Measured nuclear Form Factor (PRex) Coherent neutrino-nucleus scattering All neutrino flavors are detected x1000 Pb ideal target Highest neutron number Highest nuclear stability Pb ideal target Highest neutron number Highest nuclear stability cross-section Neutron number CE⌫NS /N2 9 + Measured nuclear Form Factor (PRex) 16 RES-NOVA background predictions detector response to bkg sources Total detector energy response 0.09 c/keV/kg/d _ ~30 different bkg sources: Environmental (n, μ, γ) + Shields (Bulk+Surface) + Detector (Bulk+Surface) + CosmoActivation RES-NOVA Coll., Phys.Rev.D 111 (2025) 10, 103050 Archaeo-Pb Chemical Purity transforming archaeo-Pb into PbWO4 crystals ArchPb @ LNGS ArchPb purified @ MIB ArchPb atomized @ f3nice ArchPbWO4 @ SICCAS Pb @ 99.92%Pb @ <98% Pb @ 99.94% Pb @ >99.99% Smelting Atomization Crystal growth transforming archaeo-Pb into PbWO4 crystals 18 Raw material screening Purified ArchPb WO3 powder ArchPbWO4 crystal + = 18 mBq/kg <0.7 0.32 <39 0.11 0.11 Target mBq/kg <0.23 <0.23 <0.07 <0.07 <0.71 PbWO4 xtal WO3 ArchPb * Radionuclides segregation mBq/kg mBq/kg Th232 Th232 <0.04 <1.3 Ac228/Th228 0.046±0.02 0 2.7±0.7 U238 U238 <0.04 <39 Ra226 0.060±0.03 0 0.9±0.4 Pb210 Pb210 <0.7 0.9 * CRESST Coll., JCAP 05 (2014) 018 19 RES-NOVA background predictions detector response to bkg sources Total detector energy response 0.09 c/keV/kg/d _ ~30 different bkg sources: Environmental (n, μ, γ) + Shields (Bulk+Surface) + Detector (Bulk+Surface) + CosmoActivation RES-NOVA Coll., Phys.Rev.D 111 (2025) 10, 103050 20 RES-NOVA background predictions detector response to bkg sources Total detector energy response - Multiplicity=2 0.09 c/keV/kg/d _ ~30 different bkg sources: Environmental (n, μ, γ) + Shields (Bulk+Surface) + Detector (Bulk+Surface) + CosmoActivation RES-NOVA Coll., Phys.Rev.D 111 (2025) 10, 103050 21 RES-NOVA background predictions detector response to bkg sources Total detector energy response - Multiplicity=3 0.09 c/keV/kg/d _ ~30 different bkg sources: Environmental (n, μ, γ) + Shields (Bulk+Surface) + Detector (Bulk+Surface) + CosmoActivation RES-NOVA Coll., Phys.Rev.D 111 (2025) 10, 103050 22 RES-NOVA background predictions detector response to bkg sources ~30 different bkg sources: Environmental (n, μ, γ) + Shields (Bulk+Surface) + Detector (Bulk+Surface) + CosmoActivation Transition Edge Sensors Threshold 1 keV Bkg in RoI 10-3 c/keV/ton/s <15 kpc 90% of Galactic SNe are included L. Pattavina et al., JCAP 10 (2021) 064 30 cm RES-NOVA sensitivity to SNe 24 RES-NOVA as Solar-𝞶 observatory from DM to the 𝞶 floor RN detector response to solar neutrino flux Cryogenic experiment for solar neutrinos+ Sensitive to solar 8B Integrated flux studies Potential for NSI tests + L. Gonzalez-Mestres and D. Perret-Gallix, NIMA 279 (1989) 382 55Fe calibration RES-NOVA proofs of principle achievement of low threshold and low background Above ground @ Max Planck Munich (DE) Nuclear recoil threshold - 300 eV (PbWO4 - 20 g) total energy spectrum total energy spectrum Under ground @ LNGS (IT) Radiopurity @ μBq/kg scale (PbWO4 - 0.9 kg) RES-NOVA group of interest Eur. Phys. J. C 82, 692 (2022) N. Ferreiro Iachellini et al., J. Low Temp. Phys. 11, 184 (2022) 25 Spin Independent Spin Dependent Pb207 (I.A. 22%) 32 RES-NOVA as Dark Matter observatory SNν high-multiplicity low energy Nuclear Recoils DM multiplicity-1 low energy Nuclear Recoils Direct DM search RES-NOVA Coll., Phys.Rev.D 111 (2025) 10, 103050