RES-NOVA: archaeological Pb observatory for astrophysical neutrino sources
L. Pattavina Laboratori Nazionali del Gran Sasso Technical University of Munich
Magnificent CEvNS @ Cyberspace
!1 Latin for revolution, political change
RES - NOVA
thing - new
➜ new experiment/approach
L. Pattavina, N. Ferreiro Iachellini, I. Tamborra, Phys. Rev. D 102, 063001 (2020) [ArXiv]
!2 Neutrino source zoo
!3 Why SNe?
interplay between black-hole & neutron star nucleosynthesis of elements cosmic-ray accelerator neutrinos and GW properties
What do we know: only 1 observation with underground instrumentation + hydrodynamical simulations of the explosions
!4 SN neutrino signal 1D Hydro-dynamical simulation of a 27 M SN (LS220 EoS) occurring at 10 kpc
Neutronization Accretion Cooling Neutronization Accretion Cooling
vx is the most intense component of the flux vx is the most energetic component of the flux
Current SN neutrino detectors are sensitive to anti-ve/ve Need for a flavor independent channel sensitive also to anti-vx/vx !5 The solution Form factor Neutrino energy
Electroweak-charge Cross-section is target-dependent ➜ target "tuning" Neutral current process ➜ equally sensitive to all flavours High cross-section ➜ >104 than NC Threshold-less process ➜ sensitive to the entire v emission
CEvNS ideal channel for SN neutrinos
!6 A. Drukier and L. Stodolsky, Phys. Rev. D 30, 2295 (1984) Pb as a target material
Pb is the element with the highest CEvNS x-section Cross-section >102 (104) than IBD (ES) process
Pb has with the highest nuclear stability Low background
Highly efficient target for SN neutrinos Coherency
Pb: ideal target for SN neutrino detection
"Pb coherence Small volume detectors are possible limit" !7 RES-NOVA: Pb-based CRYO DETECTORS
Cryogenic detectors are a leading technology: Heat Absorber Neutrinoless ββ decay: low background level bath 10 mK crystal Direct dark matter: low energy threshold thermal (0.5-5 kg) coupling thermometer Highly sensitive
↑ Easily scalable technology ↑ Ultra-low energy thresholds ↑ No quenching
↓ Fully active detectors ➜ low bkg pure-Pb PbWO4 L. Pattavina et al., PbMoO4 Eur. Phys. J. A (2019) 55: 127 J.W. Beeman, LP et al., L. Pattavina et al., Eur. Phys. J. A (2013) 49: 50 Eur. Phys. J. A 56, (2020) 38 8 RES-NOVA design
RN-1 @ LNGS Size: (60 cm)3 RN2 Threshold: 1 keV SN @ 10 kpc: ~100 counts
RN1 RN-2 @ LNGS 3 Size: (140 cm) Threshold: 1 keV SN @ 10 kpc: ~1000 counts
RN-3 (RN2 x10) Size: (RN-2) x10 facilities Threshold: 1 keV SN @ 10 kpc: ~10000 counts
!9 RES-NOVA design
RN-1 @ LNGS Size: (60 cm)3 RN2 Threshold: 1 keV SN @ 10 kpc: ~100 counts
RN1 RN-I small volume cryogenic facility Detector mass: 2.4 tons Array of 500 cryo-detectors Particle ID: feasible
!10 Which Pb?
Low-background/Commercial Pb: high 210Pb concentration (Qβ--value: 63 keV, T1/2= 22.3 y): 100 Bq/kg Archaeological Pb is “old enough” (e.g. Roman Pb) to ensure a negligible 210Pb concentration: < 1 mBq/kg
[1] G. Heusser, Ann.Rev.Nucl.Part.Sci. 45 (1995) 543. [2] L. Pattavina et al., Eur. Phys. J. A (2019) 55: 127. [3] CUORE Coll., Eur. Phys. J. C (2017) 77: 543. from passive material to active detector component
N. Nosengo, Nature (2010), 10.1038/news.2010.186
Archaeological Pb is already available !11 RES-NOVA detector response
SN signal from 1D Hydro-dynamical simulation of a 27 M⊙ (LS220 EoS) occurring at 10 kpc Time integrated (over 10 s) detector response
!12 Detector background model MC simulation of the detector response (no veto included) to radioactive background sources Total anti-coincidence energy spectrum (M=1) Signal significance
preliminary
2 crystals-coincidence energy spectrum (M=2) preliminary
A segmented detector enables: Effective background suppression through multiplicity preliminary Stand high interaction rate
!13 RN: neutrino energy reconstruction Normalization Neutrino fluence factor ↵T 0 E (1 + ↵T )E • We parametrized the neutrino energy spectrum: f (E; E , ↵T )=AT ⇠T exp h i E E ✓h i◆ ✓ h i ◆ • ⟨E⟩ and AT are inferred by a maximum likelihood analysis Pinching parameter
• αT is the time average over the relevant time interval
Neutronization phase Accretion phase Cooling phase
!14 RN: total reconstructed energy Normalization Neutrino fluence factor ↵T 0 E (1 + ↵T )E • We parametrized the neutrino energy spectrum: f (E; E , ↵T )=AT ⇠T exp h i E E ✓h i◆ ✓ h i ◆ • ⟨E⟩ and AT are inferred by a maximum likelihood analysis Pinching parameter
• αT is the time average over the relevant time interval
Precision: RN-I 30% SK - IBD only 25% RN-2 8% SK - IBD+ES+NCR 11% RN-3 4% A. Gallo Rosso et al., JCAP 04 (2018) 040
!15 RN: non-standard intercations
If we consider a CC-SN (27 M⊙) and a failed-SN (40 M⊙) @ 10 kpc
COHERENT + CONNIE + Δaμ COHERENT + CONNIE A. Suliga, I. Tamborra ArXiv:2010.14545
!16 Conclusions BH properties
Total SN Energy RES-NOVA is a newly proposed underground experiment @ LNGS: CEvNS + Archeo-Pb + Cryo-detectors DSNB sensitivity The technology for the experiment realization is already established
RES-NOVA (and CEvNS) can provide a Deep space exploration complementary approach to the current SN neutrino observatories Solar neutrinos Archaeological Pb is an ideal material for CEvNS applications
L. Pattavina, N. Ferreiro Iachellini, I. Tamborra, Phys. Rev. D 102, 063001 (2020) [ArXiv] !17 !18