Measure of low radioactive contamination and nuclear recoil quenching factor using cryogenic particle detectors

Alessandrello, A.; Brofferio, C.; Bucci, C.; Camin, D. V.; Caspani, P.; Colling, P.; Cremonesi, O.; Fiorini, E.; Giuliani, A.; Nucciotti, A.; Pavan, M.; Pessina, G.; Pirro, S.; Previtali, E.; Zanotti, L.

doi:10.1016/s0920-5632(98)00395-8

“…The crystals are operated as cryogenic calorimeters, a detector technology which demonstrated high energy resolution over a wide energy range [42], and most importantly limited uncertainties in event energy reconstructions due to energy quenching [43]. These aspects are particularly relevant for CEνNS investigations, where the neutrino signal is expected to lie at the detector energy threshold.…”

Section: Jcap10(2021)064mentioning

confidence: 99%

RES-NOVA sensitivity to core-collapse and failed core-collapse supernova neutrinos

Pattavina

¹

,

Iachellini

²

,

Pagnanini

³

et al. 2021

J. Cosmol. Astropart. Phys.

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RES-NOVA is a new proposed experiment for the investigation of astrophysical neutrino sources with archaeological Pb-based cryogenic detectors. RES-NOVA will exploit Coherent Elastic neutrino-Nucleus Scattering (CEνNS) as detection channel, thus it will be equally sensitive to all neutrino flavors produced by Supernovae (SNe). RES-NOVA with only a total active volume of (60 cm) 3 and an energy threshold of 1 keV will probe the entire Milky Way Galaxy for (failed) core-collapse SNe with > 3 σ detection significance. The high detector modularity makes RES-NOVA ideal also for reconstructing the main parameters (e.g. average neutrino energy, star binding energy) of SNe occurring in our vicinity, without deterioration of the detector performance caused by the high neutrino interaction rate. For the first time, distances < 3 kpc can be surveyed, similarly to the ones where all known past galactic SNe happened. We discuss the RES-NOVA potential, accounting for a realistic setup, considering the detector geometry, modularity and background level in the region of interest. We report on the RES-NOVA background model and on the sensitivity to SN neutrinos as a function of the distance travelled by neutrinos.

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“…The crystals are operated as cryogenic calorimeters, a detector technology which demonstrated high energy resolution over a wide energy range [37], and most importantly limited uncertainties in event energy reconstructions due to energy quenching [38]. These aspects are particularly relevant for CEνNS investigations, where the neutrino signal is expected to lie at the detector energy threshold.…”

Section: Ptfe Holdermentioning

confidence: 99%

RES-NOVA sensitivity to core-collapse and failed core-collapse supernova neutrinos

Pattavina,

Iachellini,

Pagnanini

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

RES-NOVA is a new proposed experiment for the investigation of astrophysical neutrino sources with archaeological Pb-based cryogenic detectors. RES-NOVA will exploit Coherent Elastic neutrino-Nucleus Scattering (CEνNS) as detection channel, thus it will be equally sensitive to all neutrino flavors produced by Supernovae (SNe). RES-NOVA with only a total active volume of (60 cm) 3 and an energy threshold of 1 keV will probe the entire Milky Way Galaxy for (failed) core-collapse SNe with > 3 σ detection significance. The high detector modularity makes RES-NOVA ideal also for reconstructing the main parameters (e.g. average neutrino energy, star binding energy) of SNe occurring in our vicinity, without deterioration of the detector performance caused by the high neutrino interaction rate. For the first time, distances < 3 kpc can be surveyed, similarly to the ones where all known past galactic SNe happened. We discuss the RES-NOVA potential, accounting for a realistic setup, considering the detector geometry, modularity and background level in the region of interest. We report on the RES-NOVA background model and on the sensitivity to SN neutrinos as a function of the distance travelled by neutrinos. Contents 1 Introduction 1 2 Supernovae as neutrino sources 3 3 The RES-NOVA detector 4 4 Detector background model 6 5 Detector response to SN neutrinos 10 6 RES-NOVA detection significance 11 6.1 SN neutrino signals at close distances (d < 3 kpc) 12 6.2 SN neutrino signals in absence of pile-up (d > 3 kpc) 13 7 Conclusions 14

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