POLITECHNIKA WARSZAWSKA WYDZIAŁ BUDOWNICTWA, MECHANIKI...
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POLITECHNIKA WARSZAWSKAPOLITECHNIKA WARSZAWSKAWYDZIAŁ BUDOWNICTWA, MECHANIKI I WYDZIAŁ BUDOWNICTWA, MECHANIKI I
PETROCHEMII W PŁOCKUPETROCHEMII W PŁOCKU
XIII INTERNATIONAL SYMPOSIUM ON VERY HIGH ENERGY COSMIC RAY INTERACTIONS
Pylos 2004Nuclear Physics B (Proc. Suppl.) 151 (2006)
XXIX INTERNATIONAL COSMIC RAY CONFERENCE
Pune 2005Proceedings 29th ICRC 2005
Mapa z lat 1950 - ok. 7 tysięcy gwiazd
EGRET instrument onboard the Compton Gamma Ray Observatory
zdjęcie w promieniach gamma
DROGA MLECZNA
MILAGRO (Los Alamos 2630 m n.p.m)
• Staw 80 m x 60 m x 8 m• ok. 20 mln litrów wody
oglądanej przez 723 fotopowielacze (450+273) w siatce 2,8m x 2,8 m
HAWC > 4000 m n.p.m
Cosmic-ray muons and neutrinos originate from the decay of pions and kaons produced by the interactions of high-energy primary nuclei Acr with atmospheric ones Aair. Acr + Aair → π
± , K ± ,K0
π + → µ + + νµ
π -→ µ - +νµ
µ +→ e+ + νe +νµ
µ -→ e - + νe + νµ..
EAS Array at Moscow State University
✔ The array consists of 77 detection points for determining the density of charged particles and individual showers; the detectors are Geiger counters of various areas: S1= 330 cm2, S2 = 100 cm2, S3= 21 cm2. An interval of measured density - from 0.5 up to 1500 particles per m2.
✔ The total number of detectors in the array is 8160
✔ Each detector of the ground-based points located at the distance more than 60 m from the center and the central point of the array had scintillators for measuring the direction of shower axis arrival, the shower particle density and for triggering the array.
✔ There are 13 independent triggering systems in the array.
✔ Accuracy for determining of different parameters of individual EAS: the zenith angle ~ 3O, ∆Ne/ Ne ~ 0.30, ∆s / s ~ 0.11, ∆R / R~0.05.
Rankin et al, 2001 formula:
ρ = Ne • 0.28/R2m.s
• (r/R m.s)-1.2 • (1+r/R m.s)-3.33 • [1+(r/R m.s)2]-0.6
R m.s - mean square radius,
Ne - total number of electrons
The formula of the lateral distribution of electrons in EAS
0 1 2 3
-6
-5
-4
-3
-2lg (ρ R) [m-1]
lg R [m]
1234
Normalized LDF’s:
LDF NKG, s=1.2 (1)
LDF Raikin Eo, eV R m.s,m et al 1015 153 (2)
1016 141 (3)
1017 129 (4)
Examples of the shape of the lateral distribution functions LDF’s
0 1 2 30
1
2
3
4
lg R [m]
lg (ρ .R) [m-1]
1
2
3
4
LDF’s for different Ne . LDF Raikin et al - solid green line; LDF NKG - dashed red line.1 - 1g Ne = 5.2 - 5.4, 2 - 1g Ne = 5.6 - 5.83 - 1g Ne = 6.0 - 6.2, 4 - 1g Ne = 6.4 - 6.6
Shapes of the lateral distribution functions for showers with different number of particles
Phenomenological characteristics of EAS at sea level:EAS size spectra and fluctuations of EAS
S.N. Vernov, G.B. Khristiansen et al.Proc 10th ICRC, Calgary, 1967 S197 - S200
The integral size spectra of EAS:, size determined taking into account the s parameter of a single shower ; •, size determined taking into account the mean electron lateral distributions.
5 6 7 87
8
9
θ < 18o
lg [ I(Ne).Ne2.4 ] , arb. units
lg Ne
The differential size spectra for near vertical showers
+ - LDF Raikin et al 2001 • - LDF NKG
( ) γ−⋅=Φ EAE
KONWOLUCJA WIDMJeżeli różniczkowe widmo ma postać:
a prawdopodobieństwo, że energię E’ zarejestrujemy jako E:( )
2
2
2
21),( σ
′−−
σπ=′
EE
eEEp
( ) ( )
( )
+σ+γγ+⋅=Φ
′′Φ⋅′=Φ
γ−
∝
∫
2
2
exp
0exp
211)(
,)(
EEAE
EdEEEpE
to:
Dla rozkładu log-normal:
2exp
22
)(γσ
γ− ⋅⋅=Φ eEAE
ROZKŁADY MC W SKALI LOGARYTMICZNEJ
E0=1 EeV
Ne
ρ(600)
Nµ
Escobar et all 2002
Antoni et all 2005
E0=0,5 PeV
( ) CEE
eEAE−
γ− ⋅⋅=Φ
KONWOLUCJA WIDM
Jeżeli widmo ma postać:
To z rozkładem log-normal:
CEE
eeEAE~
2exp
22
)(−γσ
γ− ⋅⋅⋅=Φ
gdzie:2~ γσ⋅= eEE CC
905 surface detector stations deployed
Three fluorescence buildings complete each
with 6 telescopes
AUGER - CONSTRUCTION PROGRESS
Collection period – 1 January 2004 to 5 June 2005
Zenith angles - 0 - 60ºTotal acceptance – 1750km2 sr yr
(~ AGASA)Surface array events (after quality
cuts)Current rate - 18,000 / monthTotal ~180,000
Hybrid events (after quality cuts) Current rate – 1800 / monthTotal ~ 18000
Cumulative number of eventsJa
nuar
y 04
July
04
Janu
ary
05
THE FIRST DATA SET
A Big Event - One that got away!
Shower/detector plane Fluorescence Mirror
Energy Estimate
>140 EeV
A BIG EVENT – ONE THAT GOT AWAY!
The detector signal size at 1000 meters from the shower core - called the ground parameter or S(1000) - is determined for each surface detector event using the lateral density function. S(1000) is proportional to the primary energy.
The energy scale is based on fluorescence measurements without reliance on a specific interaction model or assumptions about the composition.
Zenith angle ~ 48º
Energy ~ 70EeV
ENERGY DETERMINATION AND THE SPECTRUM
The energy converter:
Compare ground parameter S(1000) with the fluorescence detector energy.
Transfer the energy converter to the surface array only events.
Log S(1000)
Log
(E/E
eV) 10EeV
1 EeV
Hybrid EventsStrict event selection:
track length >350g/cm2 Cherenkov contamination
<10%
ENERGY DETERMINATION AND THE SPECTRUM
1) M. Takeda et al. Astroparticle Physics 19, 447 (2003)
2) R.U. Abbasi et al. Phys Lett B (to be published)
PORÓWNANIE Z HiRes 1 i AGASA
Żółtym kolorem zaznaczono dolną część aparatury.
Mylnie korelowano grupę kaskad (A) z kliszy I12 z grupą (B) w górnej części
aparatury - klisza S55.W granicach błędu w części
górnej obszar zakreskowany pokazuje gdzie powinna
znajdować się kontynuacja przypadku.
Aparatura na Mt. Chacaltaya (widok z góry)
W rzucie (C) widać niezgodność w kącie
azymutalnym, natomiast w rzucie (D) widać zgodność
kąta zenitalnego.Kontynuacja z I12 powinna znajdować się w kliszy S42,
S28 lub S29 a nie w S55.
Aparatura na Mt. Chacaltaya Widok z boku (C) oraz (D)
HALO EVENT at Mt. CHACALTAYA
detection threshold 2 TeV
( )TeVE
TeVETeVE
sN
h
halo
e
8,278
5,632850
59,0,107 7
=
=
==
⋅=
∑∑
γ
γ
50 tys. lat świetlnych
Słońce
Zdjęcie w podczerwieni,COBE SATELITE
30 tys. lat świetlnych
Cosmic Background Explorer
DROGA MLECZNA