"Cosmogenic neutrinos detection" Round Table discussion “Exciting neutrino: from Pauli, Fermi and Pontecorvo to nowadays prospect” 16°th Lomonov conference on Elementary Particle Physics, Moscow 22‐28 August, 2013 P. Spillantini, INFN and University, Firenze 9/8/2013 1
30
Embed
Cosmogenic neutrinos detection - msu.runuclphys.sinp.msu.ru/conf/epp10/Spillantini.pdf“Ultra‐High Energy Neutrino Fluxes and Their Constraints” (Kalashek, Kuzmin, Semokov, Sigl)
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
"Cosmogenic neutrinos detection"
Round Table discussion “Exciting neutrino: from Pauli, Fermi and Pontecorvo to nowadays prospect”
11th Lomonosov Conference on Elementary Particle PhysicsMoscow, August 21‐27, 2003
Sergio Bottai, INFN, Firenze, ItalyPiero Mazzinghi, INOA, Firenze, ItalyPiero Spillantini, University and INFN, Firenze, Italy
Continu
ed from
:
9/8/2013 2
From the ‘Extreme Universe Space Observatory’(EUSO)
to the ‘Extreme Energy Neutrino Observatory’
10th Lomonosov Conference on Elementary Particle Physics,Moscow, 23‐29 August 2001
Continu
ed fro
m:
9/8/2013 3
Protons coming from distances >20-50 Mpc interactwith the CMB (GKZ effect) producing pions,
and finally neutrinos.
Protons with E>1020eV interact several times beforedegrading under the GKZ cut-off
producing many νe and νμ neutrinos.
The energy of produced neutrinos is ≈ 1018eV or more
Cosmogenic neutrinos component
9/8/2013 4
This is the “less unprobable” neutrino componentexpected at the extreme energies.
It is not “model dependent”(i.e. it only depends from UHECR Emax and the proton source distribution)
9/8/2013 5
9/8/2013 6
Fig. 2.1 – Artist view of the EUSO concept. The shower development occurs in the atmosphere layersbelow 30‐40 km a.s.l.; the isotopic fluorescence emission is proportional at any depth to the number of charged particles (mainly electrons) present in the shower front: Ne ≈ EeV / (1.4x10
9). The UV yield is ≈4 photons per meter of electron track, almost independent from air pressure and temperature. 9/8/2013 7
9/8/2013 8
The most complete work was (@<2004)
“Ultra‐High Energy Neutrino Fluxes and Their Constraints”
(Kalashek, Kuzmin, Semokov, Sigl)
[arXiv:hep‐ph/0205050 v3 13 Dec 2002]
[Model consistent with gamma’s and UHECR data (Fly’sEye, Haverah Park, Yakytsk, AGASA)]
Neutrino events per year (≈min) 0.4 1.5 4.5 10 18 40
Neutrino events per year (≈Max) 6 12 14 18 56 126
Neutrino events per year (bestfit) 0.05 0.3 1 2.5 4 9
Neutrino events per year (px100%) 0.002 0.035 0.15 0.5 0.6 1.3
Neutrino events per year (px10%) ‐ 0.0025 0.015 0.08 0.06 0.13
Neutrino events per year (px1%) ‐ 0.0002 0.003 0.025 0.012 0.027
One optical system
(EUSO like) Multi‐mirror
9/8/2013 21
sEusox 2.5ø=4ø=12
sEusox 2.5ø=10ø=30
sEusox 2.5ø=6ø=18
bestfit
Px100%
Px1% Px10%
Maxmin
‐‐1
h= 400
km
(EUSO
Φ=2m)
h= 120
0 km
‐‐10
‐‐1
‐‐100
9/8/2013 22
9/8/2013 23
Conclusions:
Cosmogenic neutrino detection is crucial for the neutrino entering the scene asa new instrument for Astrophysics, Cosmology and Particle Physics
New data have diminished their foreseen flux by at least 2 orders of magnitude
If the p component in UHECR is abundant, complex large optical systems can observecosmogenic neutrinos from space, but high altitude orbits could be necessary
If the heavy nuclei component prevails its ‘daugter’ cosmogenic neutrino flux isout of reach for any system. (also because the neutrino energy becomes too small for detection by radio‐systems)
In next few years the increase of UHECR statistics and the definition of their chargeshould help in clarifying the situation.
Could you follow me?
Thank you!
9/8/2013 24
Rejection > 10-4
golden Fluorescence only
XmaxSelect.
ShapeSelect.
9/8/2013 25
01000 1500 2000
30° 60° 65° 70°
HORIZON
5
10
15
10
20
30
40
50
60
70
80
90
100
0.5
10
distance from Nadir (Km)1/2 FoV
Area of the calotta (106 Km2 )
Area of the calotta Area seen by EUSO
Atte
nuat
ion
fact
or (r
espe
ct to
Nad
ir)attenuation due to geometry
attenuation due to atmosphere *TOTAL attenuation
*Considered from the sea level
(EUSO)
500
45°
Florescence light attenuationas a function of the FoV
(EUSO)
(EUSO=1.7x106km2)
(EUSO x 3)
9/8/2013 26
0
1
2
3
4
5
6
7
8
0,0 5,0 10,0 15,0 20,0 25,0
FOV (deg)
gres
(km
)
0
4000
8000
12000
16000
20000
24000
28000
32000
36000
40000
spot
rad
ius
size
(mic
ron)
0
1
2
3
4
5
6
7
8
0,0 5,0 10,0 15,0 20,0 25,0
FOV (deg)
gres
(km
)
0
4000
8000
12000
16000
20000
24000
28000
32000
36000
40000
spot
rad
ius
size
(mic
ron)
0
1
2
3
4
5
6
7
8
0,0 5,0 10,0 15,0 20,0 25,0
FOV (deg)
gres
(km
)
0
4000
8000
12000
16000
20000
24000
28000
32000
36000
40000
spot
rad
ius
size
(mic
ron)
0
1
2
3
4
5
6
7
8
0,0 5,0 10,0 15,0 20,0 25,0
FOV (deg)
gres
(km
)
0
4000
8000
12000
16000
20000
24000
28000
32000
36000
40000
spot
rad
ius
size
(mic
ron)
0
1
2
3
4
5
6
7
8
0,0 5,0 10,0 15,0 20,0 25,0
FOV (deg)
gres
(km
)
0
4000
8000
12000
16000
20000
24000
28000
32000
36000
40000
spot
rad
ius
size
(mic
ron)
Aspherical mirror + Schmidt corrector
Spherical mirror + Schmidt corrector optimized at marginal field angles
Spherical mirror + Schmidt corrector
Spherical mirror with ± 15° FOV
Spherical mirror with ± 25° FOV
Resolution of 5 m EDP reflecting systemINOA
9/8/2013 27
The optical surface is coupled to a structure of light rigid supports by a matrix of actuators, adjusted on the measurements of the wave front