“the cosmic ray composition in the knee region and the hadronic interaction models” g. navarra
DESCRIPTION
“The Cosmic Ray composition in the knee region and the hadronic interaction models” G. Navarra INFN and University, Torino, Italy For the EAS-TOP Collaboration. XIII International Symposium on Very High Energy Cosmic Ray Interactions Pylos Greece, 6 -12 September 2004. EAS-TOP at LNGS - PowerPoint PPT PresentationTRANSCRIPT
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“The Cosmic Ray composition in the knee region and the hadronic interaction models” G. NavarraINFN and University, Torino, ItalyFor the EAS-TOP Collaboration
XIII International Symposium on Very High Energy Cosmic Ray InteractionsPylos Greece, 6 -12 September 2004
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EAS-TOP at LNGSCampo Imperatore 2000 m a.s.l. 820 g.cm-2 data taking: 1989-2000
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The Cosmic
Ray primary
spectrum
THE HIGH ENERGY GALACTIC RADIATION
KNEEDIRECT EXP.
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EAS-TOP
Energy range from the direct measurements up to above the knee:Cosmic Ray primary spectrum & compositionVerification of the hadronic physics
DETECTORS:HADRONS ATMOSPHERIC C.l.ELECTROMAGNETICMUONS (E > 1 GeV)+ MUONS (E > 1.3 TeV)Deep underground GS labs.: MACRO, LVD
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EAS-TOP: THE CALORIMETER& MUON TRACKER
8 x 13 cm Fe layers; 144 m2 streamer + q. proportional tubes
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DETECTORS & METHODS
Hadrons p-spectrum @ E0 ~ 0.5 - 50 TeV
Cherenkov light + TeV muons p, He, CNO fluxes @ E0 ~ 100 TeV
e.m. spectrum in “knee” region E0 ~ 103 - 104 TeV
e.m. + GeV muons composition in “knee” region
e.m. + TeV muons composition in “knee” region
Verifications of methods and HE physics used
e.m. anisotropies & search for gamma primaries
CORSIKA-QGSJET
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Size and energy spectra:
Ne Eo
Astrop. Phys. 10 (1999) 1
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Ne-N distributions
3-component fit: L, CNO, H in LogNe = 0.2 intervals of Ne
2 = i (fci – fexp
i)2/i2 fci = wLfsL
i + wCNOfsCNOi + wHfsH
i
Simulations with = 2.75 spectraL = “p” or “50%p + 50% He” ; CNO = N; H = Fe
Frac
tion
of
even
ts
Frac
tion
of
even
ts
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The composition in the ‘knee’ region
Mass group Heavier primary spectra harder Ek Z ?
l > 3.1
CNO ~ 2.75
Fe = 2.3 – 2.7
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TeV muon multiplicity fits in MACRO (TeV )
L = p + He
H = Mg + Fe
L+H
Measured
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EAS-TOP & MACRO (TeV )
L = p + He H = Mg + Fe
Astrop. Phys., 20 (2004) 641
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< ln A > vs. E0
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particle and energy flux in p-p
MACRO EAS-TOP
E. M.
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The hadronic interaction models (CORSIKA)
Primary protons:
N Ne
= 0.820 ± 0.007
= 0.792 ± 0.007
= 0.789 ± 0.008
= 0.77 ± 0.02
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Evolution of composition< Ne-N
EXP= 0.907 ± 0.004
EXTRCMP= 0.79 ± 0.02
MAX-VENUS= 0.820 ± 0.007
QGSJET: agreement with extrapolated direct measurements!
NO INTERACTION MODEL CAN ACCOUNT FOR THE INCREASING N vs. Ne WITHOUT INCREASING PRIMARY MASS
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Component dominating at the “knee”?
He – p spectra similar RUNJOB
He spectrum harder JACEE
From “direct” measurements:JACEE
RUNJOB
JACEERUNJOBEAS-TOP
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THE EAS-TOP CHERENKOV DETECTOR
2 wide angle detectors per telescope(MIRROR: A = 0.5 m2 , f.l. = 40 cm , f.o.v. = 0.16 sr)
equipped with 7 photomultipliers (d = 6.8 cm , f.o.v. = 0.023 sr)
Trigger threshold: Nphe,th = 120 phe / mirror (Ethr 40 TeV at r = 130 m) Trigger rate: 7 Hz/telescopeCherenkov event: coincidence in T = 30 ns , between any 2 corresponding PMs.
5
MACRO UndergroundGran Sasso Labs.depth: 3100 m w.e. Eth ~ 1.3 TeV 76.6 x 12 x 4.8 m
< 1o
20 m at surface level
Astrop. Phys., 21 (2004) 223
Proc. 28th ICRC, 1 (2003) 115
A different approach: EAS-TOP & MACRO
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EAS-TOP (Cherenkov detector):
total energy through the amplitude
of the detected Cherenkov light signal.
MACRO (muondetector):
EAS primaries with En > 1.3 TeV/n
EAS geometry through the track
( r ~ 20 m, ~ 10 uncertainties)
MACRO and EAS-TOP are separated by 1100-1300 m of rock: E 1.3 - 1.6 TeV
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DATA SET
t = 7s
September 1998 – May 2000
Tot. Time T = 208 h
5 telescopes
exposure 830 day m2 sr
angular window:
: 16 < < 58 , 127 < <
210
MACRO events in T and :
35814
with EAS-TOP in t = 7s:
3830
(expected accidental events < 3.0)
Event coincidence is established
off-line (GPS system - T < 1s)
Coincidence Peak
tMACRO–t Cherenkov (s)
t = 7s
7
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E ≈ 80 TeV Np ≈ N
He
E ≈ 250 Tev Np ≈ N
He ≈ NCNO
C.l. yield: p ~ He ~ CNO
p
He
CNO
Fe
C.l. + TeV muon analysis
Mg
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p, He, CNO @ ~ 100-200 TeVInformation EAS-TOP
& MACROJACEE RUNJOB
Jp+He
(80 TeV)
18 ± 4 12 ± 3 8 ± 2
Jp+He+CNO
(250 TeV)
1.1 ± 0.3 0.7 ± 0.2 0.5 ± 0.1
Jp/ Jp+He
(80 TeV)
0.29 ± 0.09 0.45 ± 0.12 0.63 ± 0.20
Jp+He/ Jp+He+CNO
(250 TeV)
0.78 ± 0.17 0.70 ± 0.20 0.76 ± 0.25
JHe
(80 TeV)
12.7 ± 4.4 6.4 ± 1.4 3.1 ± 0.7
x 10-7 m-2s-1sr-1TeV-1
EAS-TOP & MACRO data
EAS-TOP & MACRO data + p-flux
p+He p+He+CNO
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The Cherenkov light LDF
WITH JACEE FLUX
Test of energy release in the atmosphere of QGSJET:
R = (42 m) / (134 m)
= Ne (370 g/cm2) / Ne (505 g/cm2)
(Rexp – Rth)/Rth = 0.14 ± 0.09
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Ne and N spectra
Ne N
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Sec Ik*107 Nk chi**2/df m-2s-1sr-1
1.00-1.05 2.56 2.96 0.06 1.1 0.1 6.08 0.03 7.8/111.05-1.10 2.56 2.86 0.05 1.3 0.2 5.95 0.04 8.4/111.10-1.15 2.56 2.84 0.04 1.0 0.1 5.95 0.04 5.3/111.15-1.20 2.56 2.82 0.08 0.8 0.2 5.92 0.06 7.6/111.20-1.25 2.56 2.92 0.09 0.5 0.1 5.94 0.05 4.6/111.25-1.30 2.56 2.75 0.07 1.4 0.4 5.62 0.07 2.8/11
chi**2/df (1slope)1.00-1.05 3.21 0.06 3.42 0.10 1.2 0.3 4.65 0.10 10.4/10 18.7/121.05-1.10 3.18 0.08 3.45 0.10 1.4 0.2 4.65 0.10 9.3/10 20.7/121.10-1.15 3.18 0.09 3.40 0.20 0.6 0.2 4.75 0.15 6.9/10 9.9/121.15-1.20 3.12 0.15 3.4 0.10 1.6 0.5 4.55 0.15 5.9/10 14/12
Agreement inside errors (~ 30%)
2 slopes
Decreasing with increasing zenith angle
Ne
N
N Ne
= (e –1) /(-1) = 0.7 – 0.8
In agreement with models SAME BENDING COMPONENT ?
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IFSAME BENDING COMPONENTin Ne and N spectra
We can identify it.
We construct for each component (p, He, CNO, Mg, Fe) the energy spectrum fitting the size spectrum in the region of the knee.
From such energy spectra we construct for each component the corresponding N spectrum, to be compared with the measured one.
The result of such comparison
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Muon size spectrum: measured and expected for different primaries
on the base of the Ne spectrum
If “Knee” on Helium primaries
Ek (He) = (3.5 0.3) 1015 eV
VENUS
QGSJET
NEXUS
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The primary spectrum from EAS-TOP
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Natural evolution…..
KASCADE-Grande
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KASCADE-Grande
If : E k,Z = Z * E k,1
SEARCH FOR IRON “KNEE” AT ~ 1017 eV
PRIMARY COMPOSITION: 1016 - 1018 eV
STUDY OF C.R. INTERACTIONS AT UHE
N (> 1018 eV) ~ 250 (3 y data taking)
At the threshold of Auger (High Resolution)
P,He
iron
Eknee = 3 – 4 PeV
EAS-TOP/KASCADE
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Hadron spectrum at 820 g/cm2 & comparison with sea level (1033 g/cm2)
Calculated QGSJET
Exp. KASCADE/EAS-TOP
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E0 = 0.5 – 50 TeVProton spectrum at TOP
Astrop. Phys. 19 (2003) 329 He contribution subtracted
S(Eo) = (9.8 1.1stat 1.6sys) 10–5 (Eo/1000) –2.80 0.06 m-2 s-1 sr-1 GeV-1