Neutrino2002 Poster Session L arge V olume D etector at LNGS a nd n eutrino oscillation Marco Selvi Bologna University & INFN On behalf of the LVD collaboration. The observable neutrino reactions are:
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Large Volume Detector at LNGSandneutrino oscillation
Marco Selvi Bologna University & INFN
On behalf of the LVD collaboration
Number of events expected in LVD, in CC interactions with 12C, due to both ne andne, as a function of : the dashed line represents the no-oscillation case, while full and dotted lines represent the oscillation case, adiabatic and non adiabatic, respectively. The mixing results in an increase of the number of events, either for adiabatic or for non adiabatic conditions: in case of adiabaticity the increase is larger, and this is solely due to ne interactions.
Number of events expected in LVD, in the reaction ne p,n e+, as a function of . The dashed line represents the no-oscillation case, while full and dotted lines represent the oscillation case, adiabatic and non adiabatic, respectively. A large increase due to n mixing is clearly visible, with respect to the no-oscillation case. It should be noted that the number of ne p,n e+ events is practically the same both for adiabatic and non-adiabatic conditions, since, for normal mass hierarchy, MSW effect takes place in the neutrino sector only. Quite a different picture would appear, if we were to assume inverse mass hierarchy.
Number of events expected in LVD, in NC interactions with 12C, as a function of . They are, of course, insensitive to n mixing. However, the number of carbon de-excitations can test the temperature of neutrinospheres at the source, and therefore could be used in combination with CC data to overcome theoretical uncertainties on the temperature.
Physics with Supernovae
In spite of the lack of a “standard'' model of the gravitational collapse of a massive star, some features of its dynamics and, in particular, of the correlated neutrino emission appear to be well established.
At the end of its burning phase a massive star (M > 8 Mo) explodes into a supernova (SN), originating a neutron star which cools emitting its binding energy EB ~ 3 x 1053 erg mostly in neutrinos.
The largest part of this energy, almost equipartitioned among neutrino and antineutrino species, is emitted in the cooling phase: Eanti-ne ~ Ene ~ Enx ~ EB/6 (nx denotes generically nm , anti-nm , nt , anti-nt).
The energy spectra are approximatively Fermi-Dirac, but with different temperatures, since ne , anti-ne , nx have different couplings with the stellar matter: Tne, < Tanti-ne < Tnx .
These features are common to all existing stellar collapse models, and lead to rather model independent expectations for supernova neutrinos. The observable signal is then sensitive to intrinsic n properties, as oscillation of massive neutrinos. Indeed, oscillations change significantly the expected number of events in LVD.
In the study of supernova neutrinos nm , nt are indistinguishable, both in the star and in the detector, because their energy is below the charge lepton production threshold; consequently, in the frame of three-flavor oscillations, the relevant parameters are just (Dm2sol , Ue22) and (Dm2atm , Ue32).
We will adopt the following numerical values: Dm2sol ,= 5 x 10-5 eV2, Dm2atm = 2.5 x 10-3 eV2, Ue22 = 0.33; the selected solar parameters (Dm2sol , Ue22) describe a LMA solution, favored by recent analyses.
For a normal mass hierarchy scheme, neutrinos (not anti-neutrinos) cross two resonance layers: one at higher density (H), which corresponds to Dm2atm , and the other at lower density (L), corresponding to Dm2sol , (for inverted mass hierarchy, transitions at the higher density layer occur in the anti-neutrino sector, while at the lower density layer they occur in the neutrino sector. Anyway, both in case of normal and inverted mass hierarchy, the dynamics of collapse is not affected, since these layers are located far outside the core of the star).
Given the energy range of supernova neutrinos (5 MeV En 50 MeV), and considering a star density profile r 1/r3, the adiabaticity condition is always satisfied at the L resonance for any LMA solution, while at the H resonance, this depends on the value of Ue32.
When Ue32 5 x 10-4the conversion is completely adiabatic, meaning that ne are completely converted into the mass eigenstate n3 (detected at the Earth mainly as nm and nt).
Therefore, the SN neutrino signal could feel the effect of Ue32 (and could also help to discriminate the type of mass hierarchy).
ne p,n e+
CC with 12C
NC with 12C
F. Vissani, G. Nurzia & LVD collaboration
Reference paper: see TAUP 2001 Proceedings (astro-ph/0112312)
The possibility to detect neutrinos in different channels makes LVD sensitive to different scenarios for n properties, such as normal or inverted n mass hierarchy, and adiabatic or non adiabatic MSW resonances associated to Ue3.
CNGS beam Monitor
The CNGS beam from CERN to the Gran Sasso Underground Laboratory (LNGS), over a distance of 732 km, is a wide-band high-energy nm beam optimized for tappearance experiments. Such a beam provides a large number of interactions at Gran Sasso (about 2600 CC/kt/year at nominal beam intensity).
In principle the experiments forseen at LNGS could provide monitor informations by counting the number of nm CC interactions. Unfortunately, this could take months to accumulate due to their limited mass.
In order to monitor the performance of the CNGS beam, it has been suggested to implement, in one of the LNGS halls, a wide area simple apparatus capable of detecting the muons induced by neutrino interactions in the upstream rock and emerging into the experimental hall.
In this analysis we show the capabilities, in this respect, of the LVD detector whose beam-orthogonal surface is 13 x 10 m2 , greately much larger than the other forseen CNGS experiments.
Experimental background measured in the fiducial volume of LVD and expected e+ spectrum. In a 10 s burst, about 5-10 background events are expected.
Energy spectrum of muons when they reach LVD. The energy loss in rock, from the interaction point and the detector, has been subtracted using a full 3-d MonteCarlo simulation in which ionization, pair production and bremsstrahlung are taken into account.
LVD is member of SNEW: Supernova Early Warning System
A full simulation of the n interaction, the muon transport in rock and the LVD detector response has been developed, in order to estimate muon tagging efficiencies (nm CC interactions have been uniformly generated in a rock volume larger than the transverse LVD dimensions, in order to take into account also laterally impinging m).
The time-coincidence with the CNGS beam spill, makes this measurement pratically background free.
The main background sources are cosmic muons. The rate in the full LVD detector (3 towers) is 8600 muons/day (6 per minute).
If we ask an energy loss greater than 200 MeV per tank, 22% of them survive, that is 1900 per day.
The use of the informations from the CNGS beam spill (10.5 ms of spill lenght and 50 ms inter-spill gap) allows a reduction of the number of cosmic muons of a factor 104, i.e. about 0.5 cosmic muons per day.
Thanks to its large area (~130 m2) LVD could act as a very efficient muon monitor for the CNGS beam. A mean number of 120 muons per day is expected at nominal beam intensity. A 3% statistical error is achievable in 9 days. The measurement is pratically background free.
Event display of a CNGS muon in LVD. Side and top view of the detector are shown. The green area means energy loss in scintillator between 200 and 300 MeV (mean muon loss in LVD tanks), while yellow area stands for E between 300 and 500 MeV , i.e. muon has undergone some radiative energy loss.
The mean m energy loss in LVD scintillator is 1.56 Mev/cm, the tank lenght is 1.5 m, so the mean energy loss in each tank is about 230 MeV. This allow to define a muon criteria, requiring at least one tank with energy > 200 MeV. The resulting efficiency is 72%.