RES-NOVA sensitivity to core-collapse and failed core-collapse supernova neutrinos. (arXiv:2103.08672v3 [astro-ph.IM] UPDATED)

RES-NOVA sensitivity to core-collapse and failed core-collapse supernova neutrinos. (arXiv:2103.08672v3 [astro-ph.IM] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Pattavina_L/0/1/0/all/0/1">L. Pattavina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iachellini_N/0/1/0/all/0/1">N. Ferreiro Iachellini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pagnanini_L/0/1/0/all/0/1">L. Pagnanini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canonica_L/0/1/0/all/0/1">L. Canonica</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Celi_E/0/1/0/all/0/1">E. Celi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clemenza_M/0/1/0/all/0/1">M. Clemenza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferroni_F/0/1/0/all/0/1">F. Ferroni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fiorini_E/0/1/0/all/0/1">E. Fiorini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garai_A/0/1/0/all/0/1">A. Garai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gironi_L/0/1/0/all/0/1">L. Gironi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mancuso_M/0/1/0/all/0/1">M. Mancuso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nisi_S/0/1/0/all/0/1">S. Nisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petricca_F/0/1/0/all/0/1">F. Petricca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pirro_S/0/1/0/all/0/1">S. Pirro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pozzi_S/0/1/0/all/0/1">S. Pozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puiu_A/0/1/0/all/0/1">A. Puiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rothe_J/0/1/0/all/0/1">J. Rothe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schoenert_S/0/1/0/all/0/1">S. Schoenert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shtembari_L/0/1/0/all/0/1">L. Shtembari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strauss_R/0/1/0/all/0/1">R. Strauss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wagner_V/0/1/0/all/0/1">V. Wagner</a>

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 (CE$nu$NS) 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 $> 3 sigma$ 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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