Aldo Morselli, INFN & Università di Roma Tor Vergata, 1. Scineghe07. Aldo Morselli

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1 Aldo Morselli, INFN & Università di Roma Tor Vergata, 1 Scineghe07 Aldo Morselli

2 Proceedings in Frascati Physics series Deadline 25 of July 8 pages (4 pages for posters ) in 5 days macros in the web site (as Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 2

3 PAMELA Launch 15/06/06 Aldo Morselli, INFN & Università di Roma Tor Vergata, 3

4 23 April 12 o clock Roma time : Launch Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 4

5 First Results:the VELA pulsar The picture shows a preliminary count map (Galactic coordinates) of photons with energy above 100 MeV of the Vela Pulsar region. The observation duration is approximately half a day (7 orbits) between May 29 and 30, This image represents only the central part of the AGILE gamma-ray imager field of view and was built from data with a preliminary background rejection taken with an instrument configuration that is not yet optimized.

6 GLAST SciNeGHE Frascati June R.Dubois 6/25

7 2008 Agile PAMELA GLAST Aldo Morselli, INFN & Università di Roma Tor Vergata, 7

8 High Energy Gamma Experiments ~1993

9 Aldo Morselli, INFN & Università di Roma Tor Vergata, 9

10 Aldo Morselli, INFN & Università di Roma Tor Vergata, 10

11 High Energy Gamma Experiments

12 Gamma -ray mission deadtime Aldo Morselli, INFN & Università di Roma Tor Vergata, 12

13 Gamma -ray mission deadtime Aldo Morselli, INFN & Università di Roma Tor Vergata, 13

14 High Energy Gamma Experiments

15 Sensitivity of γ-ray detectors AMS trk AMS Cal High galactic latitudes(φ b = γ cm -2 s -1 sr -1 (100 MeV/E) 1.1 ). Cerenkov telescopes sensitivities (Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations.large field of view detectors sensitivities (AGILE, GLAST, Milagro, ARGO, AMS) are for 1 year of observation. Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 15

16 ARGO-YBJ Yangbajing village Vernetto

17 Moon shadow ARGO data Number of PAD > 500 Median energy 5 TeV 10 standard deviations Position of the maximum deficit: x = 0.04 West East y = 0.14 Simulations x = y = 0.0 Geomagnetic shift time 500 hours (from July 2006 to February 2007)

18 preliminary Crab Nebula - ARGO data degrees Number of PAD > standard deviations Excess distribution Crab time 290 hours (July 2006 March 2007) Equivalent time 50 days Standard deviations

19 preliminary Mrk ARGO data degrees Number of PAD > 60 > 5 standard deviations Excess distribution Mrk421 Standard deviations time 80 hours (July - August 2006)

20 Next step: Magic II 85 m A second telescope is under construction De Lotto

21 Highlights in Galactic source observation New source Galactic Center HESS J1813 HESS J1834 LSI Crab Nebula New source MAGIC J Cygnus X1 + several in queue

22 Highlights in Extragalactic source observation MAGIC discovery Mrk421 (z=0.031) Mrk501 (z=0.034) 1ES2344 (z=0.044) Mrk180 (z=0.045) MAGIC discovery 1ES1959 (z=0.047) BL-Lacertae (z=0.069) 1ES1218 (z=0.18) PG 1553 (Z>0.25) + 3 more in press

23 New readout system Sampling frequency: 2 GHz Receiver boards Trigger L1 based on Domino ring sampler Readout Electronics Trigger L2 Magic-I DAQ STORAGE Trigger L3 DAQ Readout Electronics Trigger L2 Magic-II Receiver boards Trigger L1

24 New camera Total ~1000ch Central ~500ch: High Q.E. Photo Detectors (50-55% Q.E.) 17m telescope becomes equivalent with 24m telescope γ shower events (MC simulation)

25 H.E.S.S. Galactic survey HESS J HESS J HESS J HESS J HESS J G Gal. Centre 30 Tens of established associations of VHE γ-ray sources with MWL observed astrophysical sources 0 HESS J LS 5039 Original VHE emission discoveries puzzling the leptonic / hadronic acceleration mechanisms and sites HESS J HESS J HESS HESS J HESS J RX J HESS J HESS J HESS J The Sources survey > recently 6 sigma was (9 extended, new, 11 total) covering the regions l = 280 deg deg and l = 30 deg - 60 deg, leading Sources to the > 4 discovery sigma (7 of new) several previously unknown sources with high statistical significance. G. LAMANNA SciNeGHE07 June 18-20, 2007 Lamanna

26 What next? Plenty of data from HESS I and.. Lower threshold and higher sensibility with HESS II G. LAMANNA SciNeGHE07 June 18-20, 2007

27 Source creation acceleration injection Cosmic rays: about 10 Myears in the Galaxy (6-7 g/cm2) further acceleration? Cosmic Rays Propagation γ Modulation ν Space experiments ~ 400 km Atmosphere 40 km 23 Xo High Montain Detectors Direct detection Balloons ~ 40 km ~3 g/cm 2 residual atmosphere Extensive Air Shower Detectors Particle Astrophysics Experiments Cherencov Detectors Underground, Under-ice, Underwater Particle Aldo Morselli, Accelerators INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 27

28 Vernetto Camarri De Lotto Doro Vitale Gaug Cosmic Giebles rays: about 10 Myears in the Galaxy (6-7 Cusumano g/cm2) Di Ciaccio Glicenstein Lamanna Gavin Atmosphere 40 km 23 Xo Source γ ν High Montain Detectors Cherencov Detectors further acceleration? Cosmic Rays creation acceleration injection Propagation Modulation Space experiments ~ 400 km Direct detection Balloons ~ 40 km ~3 g/cm 2 residual atmosphere Extensive Air Shower Detectors Tavani Barbiellini Feroci Del Monte Marisaldi Particle Astrophysics Experiments Underground, Under-ice, Underwater DuBois do Couto e Silva Moiseev Conrad Di Falco Sparvoli Carboni Costa Bernabei Schlenstedt Particle Aldo Morselli, Accelerators INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 28

29 Cosmic rays: about 10 Myears in the Galaxy (6-7 g/cm2) Atmosphere 40 km 23 Xo Source γ ν High Montain Detectors Cherencov Detectors further acceleration? Cosmic Rays creation acceleration injection Propagation Modulation Space experiments ~ 400 km Direct detection Balloons ~ 40 km ~3 g/cm 2 residual atmosphere Extensive Air Shower Detectors Particle Astrophysics Experiments Underground, Under-ice, Underwater Pizzella Muñoz Schelke Bambi Bringmann Sellerholm Regis Casanova Caraveo Protheroe Massaro Moskalenko Donato Ullio Pieri Lavalle Fargion Particle Aldo Morselli, Accelerators INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 29

30 at least 1 mystery solved Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 30

31 What we can do in the future? Aldo Morselli, INFN & Università di Roma Tor Vergata, 31

32 CTA : The Cherenkov Telescope Array facility aims to explore the sky in the 10 GeV to 100 TeV energy range Not to scale!

33 C TA An / V e T [ Possible CTA sensitivity advanced facility for ground-based high-energy gamma ray astronomy GLAST E. F(>E) ] ) E s ~3000 m [TeV/cm 2 2 s] 2 mirror area > ( F MAGIC ~5000 m x 2 mirror area few E m with H.E.S.S. dense coverage (5-10%) O(10 7 m 2 ) with low coverage 1% Crab ( %) few 10 5 m 2 with medium 1000coverage E [GeV] (1-2%) Crab 10% Crab x 1.5 ~4000 m 2 mirror area

34 Aldo Morselli, INFN & Università di Roma Tor Vergata, 34

35 many tanks to all the Villa Mondragone Staff many tanks to Vincenzo Buttaro for the web page many tanks to Marta Solinas and Gabriella Ardizzoia from all of us Aldo Morselli, INFN & Università di Roma Tor Vergata, 35

36 2008 Agile PAMELA GLAST Scineghe 08 Aldo Morselli, INFN & Università di Roma Tor Vergata, 36