Cosmic Ray Physics with the ARGO-YBJ experiment
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1 Cosmic Ray Physics with the ARGO-YBJ experiment Ivan De Mitri University of Salento and Istituto Nazionale di Fisica Nucleare Lecce, Italy On behalf of the ARGO-YBJ Collaboration Second Roma International Conference on AstroParticle Physics Rome, May 13-15, 2009
2 The ARGO-YBJ experiment ARGO-YBJ High Altitude Cosmic Ray YangBaJing,Tibet, China Site Altitude: 4,300 m a.s.l., ~ 600 g/cm 2 RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 2
3 ARGO-YBJ physics goals Cosmic ray physics: spectrum and composition (E th few TeV), study of the shower space-time structure, p-air cross section measurement, anti-p / p ratio at TeV energies,.. VHE γ-ray Astronomy: See S.Vernetto s talk search for point-like (and diffuse) galactic and extra-galactic sources at few hundreds GeV energy threshold Search for GRB s (full GeV / TeV energy range) Sun and Heliosphere physics through the See R. Iuppa s talk Observation of Extensive Air Showers produced in the atmosphere by primary γ s and nuclei RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 3
4 The ARGO-YBJ detector 99 m 74 m 111 m 78 m 1 CLUSTER = 12 RPC ( 43 m 2 ) 10 Pads (56 x 62 cm 2 ) for each RPC 8 Strips (6.5 x 62 cm 2 ) for each Pad RPC Strip = space pixel Pad = time pixel + Analog charge read-out on Big Pads Time resolution ~1 ns cm lead converter (2008) RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 4
5 EAS reconstruction Event Rate ~ 4 khz for N hit >20 High space/time granularity + Full coverage + High altitude detailed study on the EAS space/time structure with unique capabilities 3-D view of a detected shower Top view of the same shower RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 5
6 The Moon Shadow Size of the deficit angular resolution Position pointing accuracy West displacement Energy calibration (Geomagnetic bending 1.57 / E (TeV) ) Antiprotons should give a shadow on the opposite side (see R. Iuppa s talk) RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 6
7 The Sun Shadow Exploring the interplanetary and solar magnetic fields The deficit significance and position correlates with the sunspot distribution, even in a quite period ( ) RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 7
8 Measurement of CR energy spectrum Extract the primary energy spectrum starting from the measured particle multiplicity spectrum at ground P( M ) = N( M ) N tot Choose an initial value for P(E) P 0 (E) Use the Bayes theorem P(E M) = P(M E)P(E) P(M) P(M E) eval. from Monte Carlo events P(E) = N(E) N tot N(E) = N(M)P(E M) Iterate this procedure until variations on P(E) are neglegible RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 8
9 The measured differential all particle spectrum RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 9
10 Proton-air cross section measurement Use the shower frequency vs (secθ -1) I ( θ ) = I ( 0 ) e h o Λ ( sec( θ ) 1 ) for fixed energy and shower age. h 0 θ However Λ = k λ int mainly because of collision inelasticity, shower fluctuations and detector resolution. It is determined by simulations and depends on: hadronic interactions detector features and location (atm. depth) actual set of experimental observables analysis cuts energy,... Then: σ p-air (mb) = / λ int (g/cm 2 ) Warning Take care of shower fluctuations Constrain X DO = X det X 0 or X DM = X det X max Select deep showers (large X max, i.e. small X D0 or X DM ) Exploit detector features (spacetime pattern) and location (depth). RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 10
11 Data selection Event selection based on: (a) shower size on detector, N strip (strip multiplicity) (b) core reconstructed in a fiducial area (64 x 64 m 2 ) (c) constraints on Strip density (> 0.2/m 2 within R 70 ) and shower extension (R 70 < 30m) R 70 : radius of circle including 70% of hits N strip is used to get defferent E sub-samples Full Monte Carlo simulation: Corsika showers QGSJET I and II, SYBILL int. models GEANT detector simulation RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 11
12 Experimental data Wheather effects, namely the atmospheric pressure dependence on time, have been shown to be at the level of 1 % h 0 MC = g/cm 2 (4300m a.s.l. standard atm.) h 0 MC / h 0 = ± ( 4200 m a.s.l. ) RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 12
13 Heavy primaries contribution proton Hoerandel AP 19 (2003) 193 taken as reference. JACEE and RUNJOB for the evaluation of systematic error dn de = Φ( E) = Φ 0 Z E TeV γ Z helium RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 13
14 The proton-air cross section arxiv: RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 14
15 The total p-p cross section arxiv: RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 15
16 Summary and Outlook The all particle energy spectrum has been measured in an energy region typically covered by experiments on balloon/satellite. The proton-air cross section has been measured, giving results in agreement with previous works, done with totally different techniques The total proton-proton cross section, in an energy region so far unexplored by particle accelerators, has been inferred by using the Glauber theory. The result favours the log 2 (s) asymptotic behaviour. More accurate shower age and energy determinations will be performed, by the use of timing, rise time, front curvature,.,,, and topological information (see dedicated poster) In the future, the analyses will be extended to larger energies (up to the PeV region), by using the analog RPC readout. RICAP-09 I.De Mitri et al. : Cosmic Ray Physics with the ARGO-YBJ experiment 16
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