Highlights from the ARGO-YBJ Experiment Ivan De Mitri University - PowerPoint PPT Presentation

Highlights from 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 12th International Conference on Topics in Astroparticle and Underground Physics TAUP 2011, 5 – 9 September 2011, Munich, Germany

The ARGO-YBJ experiment ARGO-YBJ �������������������������������������������������������������� Site Altitude: 4,300 m a.s.l. , ~ 600 g/cm 2 TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 2

ARGO-YBJ physics goals � VHE γ γ -Ray Astronomy : γ γ ( search for)/(study of) point-like (and diffuse) galactic and extra-galactic sources at few hundreds GeV energy threshold � Cosmic ray physics : spectrum and composition (E th few TeV), study of the shower space-time structure, flux anisotropies at different angular scales (see Di Sciascio’s talk) p-Air cross section measurement and hadronic interaction studies anti-p / p ratio at TeV energies, ….. � Search for GRB’s (full GeV / TeV energy range) � … through the… Observation of Extensive Air Showers produced in the atmosphere by primary γ γ ’s and nuclei γ γ TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 3

�������� ������������ 99 m 74 m 8 Strips 10 Pads 1 CLUSTER = 12 RPC (6.5 x 62 cm 2 ) (56 x 62 cm 2 ) ( ∼ 43 m 2 ) for each Pad for each RPC 78 m 111 m RPC Strip = space pixel Pad = time pixel + Analog charge read-out on “Big Pads” Time resolution ~1.7 ns TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 4

EAS reconstruction 86% duty cycle Event Rate ~ 3.5 kHz for N hit >20 High space/time granularity detailed study on the + Full coverage EAS space/time structure + High altitude with unique capabilities 3-D view of a detected shower Top view of the same shower TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 5

The Moon Shadow ARGO-YBJ coll., PRD 84 (2011) 022003 Number of standard deviations � 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 ⇒ Upper limit TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 6

VHE gamma-ray astronomy � up to 70 10 � All sky survey (from - -10 up to 70° ° in declination) above 0.1TeV in declination) above 0.1TeV All sky survey (from 4 sources with significance >5 σ σ in σ σ Crab 17 σ σ , Mrk421 12 σ σ σ σ , MGRO J1908+06 6 σ σ σ σ σ , MGRO J2031+41 6.3 σ σ σ σ σ Interesting results on long term variabilities, correlation with Xrays, spectra,…. The CRAB All sky survey 3.5 yrs Excluding regions close to Crab, Mrk421, 17 s.d. MGRO J1908+06 , MGRO J2031+41 All directions TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 7

CRAB flaring at TeV energies ? AGILE discovered a flare at E > 100 MeVin 19th-21st September 2010 (ATel#2855) Fermi LAT confirmed (ATel#2861). Sept. TeV emission enhancement (~3 -4 times) observed with 4.1 s.d. by ARGO-YBJ in ~54 h observation from 2010 18th to 27th Sep. 2010 (ATel#2921). Not confirmed by MAGIC and VERITAS with short observations from 17th to 20th Sep. 2010 (ATel#2967, 2968). AGILE light curve (E > 100 MeV) ARGO-YBJ significance map in the same 6 days April Expected 0.62 s.d. 2011 Observed 3.5 s.d At E ≈ 3 TeV TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 8

MGROJ1908+06 Observed for 3 yrs above 1 TeV 6 s.d. excess above background Extended source: gaussian profile with σ = (0.5 � ±0.35)° � ���������� 0.34±0.04° ) ��������� ���� �������� ������������������ ���� �������� ����������������� ���� ���������� ����������� !"�#$�%�& ���' �������� &�����(����)*+ �,-�� .��&/&� ± 0.4)10 -13 (E/7TeV) -2.3±0.3 photons/cm -2 s -1 TeV -1 Flux in agreement with Milagro but a factor 3 larger than HESS measurement Complex source morphology ? Diffuse galactic flux contamination ? Flux variability ? Observation times: MILAGRO (2000-2007), ARGO-YBJ(2007- 2011), HESS (27hours in 2005-2007) TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 9

Mrk421 Observations Source detected with more than 12 s.d. Flaring activity, continuously monitored since 2008 Good correlation with X and gamma rays No other continuous observation at TeV energies ARGO-YBJ coll., ApJ 734 (2011) 110 TeV g rays ARGO X- rays 2-12 KeV RXTE/AMS X –rays 15-30 KeV SWIFT/BAT 2008 2009 2010 2011 TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 10

Mrk421 Observations Both X-ray and TeV spectra are observed to harden as the flux increases Observations are compatible with a SSC model with ARGO-YBJ coll., ApJ 734 (2011) 110 flares being due to hardening of the electron Feb 16, 2010 injection spectrum Apr 28, 2010 Feb 16, 2010 Apr 28, 2010 TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 11

Light- -component spectrum of component spectrum of CRs CRs Light Measurement of the light-component (p+He) spectrum of primary CRs in the energy region (5 – 250) TeV via a Bayesian unfolding procedure. The contribution of heavier nuclei to the trigger is a few % ARGO data agree with CREAM results For the first time direct and ground- -based measurements overlap for a wide based measurements overlap for a wide For the first time direct and ground energy range thus making possible the cross- -calibration of the experiments. calibration of the experiments. energy range thus making possible the cross TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 12

Proton-air cross section measurement Use the shower frequency vs (sec θ -1) X 0 rise h ( ) X o − θ − sec 1 θ = ⋅ I I e Λ h 0 ( ) ( 0 ) for fixed energy and shower age. X max X DM The lenght Λ Λ is not the p interaction lenght θ Λ Λ mainly because of collision inelasticity, shower fluctuations and detector resolution. It has been shown that Λ Λ Λ Λ = k λ λ λ λ int , where k is determined by simulations and depends on: � hadronic interactions � detector features and location (atm. depth) � actual set of experimental observables � analysis cuts � energy, ... σ p-Air (mb) = 2.4 10 4 / λ σ λ int (g/cm 2 ) σ σ λ λ Then: TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 13

The total p-p cross section � No p-p (and pbar-p) accelerator data available at these energies � The log 2 (s) asymptotic behaviour is favoured ARGO-YBJ Coll. Phys. Rev D 80, 092004 (2009) Extending the energy range with the analog readout TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 14

Info from the analog readout Real event Strips (digital) 4000 0 3500 BigPads 3000 � Extend the covered energy range (analog) 2500 2000 � Access the LDF down to the shower core 1500 � Sensitivity to primary mass 1000 � Info/checks on Hadronic Interactions 500 TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 15

Summary and Outlook � Full detector in stable data taking since Nov. 2007 (first data in 2006) � Trigger Rate ~3.5 kHz - Dead time 4% � 220 GB/day transferred to IHEP (China) / CNAF (Italy) data centers � Detailed analysis of the Moon shadowing effect (pointing, energy scale) � Long-term monitoring of Crab and Mrk421 � MGRO J1908+06 and MGRO J2031+41 observed above 5s.d. Fluence upper limits on 110 GRB ( Δ E=1-100GeV) � � Measurement of CR light component energy spectrum below 100TeV � Study of the CR anisotropy at different angular scales � Measurement of the CR antip/p flux ratio in TeV energy range � Monitoring of the IMF by the Sun shadow displacement � Measurement of the p-air and p-p cross sections up to 100TeV � Data taking planned up to December 2012 Updating current results and data reprocessing with γ /h discrimination � � Extending the energy range to the CR knee region by the RPC charge readout � LDF near the shower core and hadronic interactions and primary mass sensitivity TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 16

More stuff…. TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 17

RPC performance and linearity range By means of the RPC analog readout TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 18

ARGO-YBJ angular resolution and sensitivity to gamma ray sources The cumulative sensitivity to the Crab like source is 28% Crab unit. � TAUP2011 I.De Mitri: Highlights from the ARGO-YBJ experiment 19