1 E Extreme U Universe S Space O Observatory Sergio Bottai INFN Firenze on behalf of the EUSO Collaboration DETECTING NEUTRINOS WITH EUSO Paris neutrino2004
Jan 11, 2016
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EExtreme UUniverse SSpace OObservatory
Sergio Bottai
INFN Firenze
on behalf of the EUSO Collaboration
DETECTING NEUTRINOS WITH EUSO
Paris neutrino2004
2#2
EUSO Consortium - Institutes
Participant Nations and Institutions
Brazil Germany Spain USA Japan Switzerland PortugalItaly France
– APC, Paris– CdF, Paris– IAP, Paris– LPSC, Grenoble– LPTHE, Paris– OdP, Paris
– IASF, Palermo– ISAC-CNR, Bologna– INFN & Univ. Genova– INFN & Univ. Firenze– INFN & Univ. Torino– INFN & Univ. Trieste– INFN Catania & Univ. Palermo– Univ. Roma “La Sapienza”– Scuola Normale Sup. Pisa– Oss. Astrofisico Arcetri– Oss. Astrofisico Catania– CARSO– INOA
– LIP, Lisbon
– MSFC & NSSTC, Huntsville– UAH, Huntsville– UCB, Berkeley– UCLA, Los Angeles– Vanderbilt Univ.
– Obs. Neuchatel
– RIKEN– ICRR– Konan Univ.– ISAS– Rikkyo– KEK– NAO– Tokyo Univ.– Saytama– Aoyama– Kinki– Seikei– Kanazawa
– MPIfP, Munich– MPIHLL, Munich– MPIfRA, Bonn– Univ. Wuerzburg
– IAG, Univ Sao Paulo
– IAA-CSIC, Granada– Dpt.FTC & CAFPE,
Univ. Granada
The EUSO instrument consortium is truly global in nature with >150 researchersin 50 institutions in 6 countries in Europe, the USA, Japan and Brazil.
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BASIC GUIDELINE
EUSO is an experiment devoted to measure the cosmic ray spectrum above 1020eV with high statistic
EUSO is at present in a phase of ‘feasibility study’
EUSO has also some potentiality to detect extraterrestrial neutrinos of energy close to 1020eV. The sensitivity for such neutrino discover will be discussed in the presentation
4#4
UHECR Observational Situation as today E>1020eV particles hit the atmosphere at a rate of <1/(100km2•year). A great experimental challenge.
P
γ3K
Δ
N
π
GZK mechanism
WE NEED NEW EXPERIMENTS :
CONTROLL SYSTEMATICS -> AUGER INCREASE STATISTICS -> AUGER-EUSO
AGASA - HIRES
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Exposure
1
10
100
1000
10000
1990
1992
1994
1996
1998
2000
2002
2004
2006
2008
2010
2012
2014
Year
Expo
sure AGASA
HiResAugerEUSO
Exposure (AGASA unit)
EUSO
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EHECR FROM SPACEPhotons per misotropic
330 – 400 nm
Euso Area vs Auger
EUSO
Pierre-Auger
7#7
• Geometrical Factor (A · ) 6 · 105 km2 sr (FoV=±30° at ISS mean distance hISS430km)
• rather constant signal attenuation ~0.5
• Negligible Proximity Effect
(Dist./Dist. < 1%)
(acceptance not depending on energy)
• Full Sky Coverage
• Cerenkov “footprint” of shower
Advantage of a space-based fluorescence detector for EECR
ATMOSPHERE
8#8
ELECTRONICS :PHOTON COUNTINGTIME INFORMATION
FOCAL SURFACELIGHT SENSORS
LENSES
The instrument
9#9
Optics Requirements–FoV 30° –Pupil entrance pupil 2 m–F/# 1.15–Spot dimension ~ 0.1°–Spectral range 300-400 nm– Limited mass !!
11:26:05
EUSO:f/1.25 Monochromatic Double Fresnel Scale: 0.05 DJL 01-Nov-01
490.20 MM
EUSO -The Optical System
VERY challenging
2 Double sided Fresnel lens !Pupil diameter 2.3m
10#10
Support Structure
Focal Surface assembly
Microcell
Macrocell
EUSO – The Focal Surface 200.000 pixels at single PE
R8900 – M36
Filters
MAPMT R8900 – M36
FILLING>0.9
11G. D’Alì Staiti, Bologna, May 24, 2004 #11#11
The Atmosphering sounding
Cloud topology surveyAtmospheric transmission calibration
LIDAR
+
IR camera
LIDAR
12#12
The detected signal FOR 1020eV
SIMULATION : The Detector Light Sensitivity
The trigger efficiency
Random Noise 0.5-0.8
Signal ~10
The trigger efficiency
for a subsample
20%
Threshold reach ~5*1019eV
13#13
The Real Atmosphere
no triggerno triggerclearclear
MCM’02
14#14
The EUSO AcceptanceIn clear sky… …and in real atmosphere
GoldenCerenkov only
Fmax only
The EUSO statistics E>1020eV
~1000 events/year in SuperGZK mode>70 events/year in GZK-suppressed mode
REALISTIC CLOUDS SCENARIO KILL ~40% OF SHOWERS
15#15
EUSO resolution
Angular res = 1o – 4o
Energy res = 20% (RMS)+..(with Lidar info)
Xmax res = 50 g/cm2
(with Lidar info)
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SHOWERS
NEUTRINO EVENTS IN ATMOSPHERE
(e)
2000 km3we of target for EUSOBut : duty cycle, efficiency, very high energy threshold
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Proton – neutrino discrimination
The probability of neutrino interaction in atmosphere is proportional to the atmospheric density.
NEUTRINOSCC INTERACTIONS(LPM effect included)
P+
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DOWNWARD NEUTRINO ACCEPTANCE FOR EUSO
Rejection > 10-4
Golden events Fluorescence only events
XmaxSelect.
ShapeSelect.
P+
P+
1600g/cm2
Neutrinodomain
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TOP ATMOSPHERE
P+
NEUTRINO
Ground level
Showers
The probability of a neutrino interaction in a volume element dV is proportional to density
NEUTRINO
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EFFECTIVE ACCEPTANCE (g*sr) FOR NEUTRINOS
Clear skyWith clouds
(duty cycle not contained)
CC
CC
NC NC~300 km3we
+ Shower max visibleTrigger + Selection
~50 km3we
dutycycle
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log(E2 Flux)
log(E/GeV)TeV PeV EeV
3 6 9
pp core AGN
p blazar jet
Top-Down models
GRB (W&B)
Classes of UHE Models
GZK neutrinos
EUSO
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Neutrino sensitivity
Auger
EUSO
Sensitivity1 events/decade/year
EUSO has 10 times largerAperture than Auger aboveGZK energy
EUSO is sensitive Z-Burst, Top Down Models and High (MAXIMUM) GZK flux.
~ 10 events/year detected
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EUSOthreshold
UPWARD TAU SHOWERS
EUSO X 20
S. Bottai , S. Giurgola ICRC 2001S. Bottai,S.Giurgola Astr. Phys. 18 2003
24#24
EUSO2003 2004 2005 2006 2007 2008 2009 2010 201320122011
A C/DB
Just wishful thinking?
on June 2004 ESA ‘SCIENCE DIRECTORATE’ DID NOT INCLUDED EUSO IN THE PRIORITY LIST OF CANDIDATE EXPERIMENT UP 2012 . (“wait AUGER results”)
The possibility to mantain the time schedule is under investigation
ESA-EUSO STARTED A PHASE A STUDY FOR ISS
PHASE A UFFICIALLY CLOSE IN JULY 2004
LAUNCH 2010
25#25
Conclusion
EUSO is a pioneering experiment for studying EAS from space:
An instantaneous aperture of 6×105km2sr with a duty cycle ~20% is a technically achievable goal with up-to-date technology;The acceptance reduction due to cloud effect has been evaluated to be ~0.5.
50.000 km2sr effective acceptance
~103 events/year can be expected according to AGASA findings;~102 events/year can be expected according to GZK-suppressed spectrum due to uniform source distribution.
for with E>5*1019eV EUSO will have a competitive sensitivity (50 km3 we effective) TOP DOWN MODELS CAN BE SEEN IF THEY EXISTS
TIME SCHEDULE 2010 ???????
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Design of a mirror optics, based on the Schmidt camera principle, with FOV up to 25°
A proposed large mirror system
correcting plate and/or filter
mirrorlight shield
focal plane
FEATURES
3 identical DETECTORS ASSEMBLED INSIDETHE ISS ?
Solid state detectors ?
5-7 m
27GZK(A)~0.3 events/year in EUSO
EUSO
AUGER
q.e=50%Eth=3EeVD=7.5mFOV= EUSO X 3
GZK(A)~ 40 events/year
S. Bottai, P. Spillantini, “ FROM THE EXTREME UNIVERSE SPACE OBSERVATORY(EUSO) TO THE EXTREME ENERGY NEUTRINO OBSERVATORY “ prooceedings of the XIth Lomonosov Conferenceq
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