Summary on parallel sessions: "EAS and Gamma Detection" and "Gamma Detection Aldo Morselli INFN Roma Tor Vergata RICAP07 21-06-07 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 1
23 April 12 o clock Roma time : Launch Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 2
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, 2007. 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.
GLAST SciNeGHE2007 - Frascati June 19 2007 R.Dubois 4/25
2008 Agile PAMELA GLAST Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 5
High Energy Gamma Experiments ~1993
Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 7
Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 8
High Energy Gamma Experiments
Gamma -ray mission deadtime Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 10
Gamma -ray mission deadtime Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 11
High Energy Gamma Experiments
Sensitivity of γ-ray detectors AMS trk AMS Cal High galactic latitudes(φ b =2 10-5 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 13
MAGIC Observation LS I was observed for 6 orbits between Oct 05 and March 06 In total 54 hours of data, 22% of data taken during moon Clear detection with 8.7 sigma Excess position: RA=2h 40m 34s DEC= + 61 15 25 In agreement with LS I position Possible association with variable EGRET source Tobias Jogler Max Planck Institute für Physik jogler@mppmu.mpg.de
Orbital Light Curves Phases 0.8 0.1 not observed due to bright moon Periastron Oct 2005 Albert et al. Science 312, 1771 (2006) Strong variability between phases Probability of a constant flux < 3 x 10-5 Nov 2005 Dec 2005 Jan 2006 Source is quiet at periastron and loud before apastron! Feb 2006 Mar 2006 Maximum flux 16% of Crab Nebula at 0.5-0.7 Average Tobias Jogler Max Planck Institute für Physik jogler@mppmu.mpg.de
LS I - a Microquasar? Production of γ - rays: e + γ LE e + γ VHE γ LE from synchrotron radiation or γ LE from companion star p + Ion π 0 + π ± γ γ Features: - accretion disc - jets - modulation with accretion rate Mirabel 2006 Tobias Jogler Max Planck Institute für Physik jogler@mppmu.mpg.de
LS I a Binary Pulsar? Production of γ - rays: e + γ LE e + γ VHE γ LE from companion star e from relativistic PW p + Ion π 0 + π ± γ γ Mirabel 2006 Features: - no accretion disc - no jet Tobias Jogler Max Planck Institute für Physik jogler@mppmu.mpg.de
Highlights in Galactic source observation New source Galactic Center HESS J1813 HESS J1834 LSI+61 303 Crab Nebula New source MAGIC J0617+225 Cygnus X1 + several in queue
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
Next step: Magic II 85 m A second telescope is under construction
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
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)
Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 23
Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 24
Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 25
H.E.S.S. observations of Active Galactic Nuclei PKS 2155-304 Volpe First blazar ever to show such high luminosity TeV short time variability (even shorter than for Mkn 421) No spectral variability compared to the low state Huge MWL dataset (HESS, CHANDRA, RXTE, optical...) Discovery of blazars 1ES 0347-321 & 1ES 0229+200 with significance above 5σ Results with standard analysis soon published The spectral analyses will give further constraints on the intensity of the extragalactic background light H.E.S.S. II increase the sensitivity and reduce the threshold
What next? Plenty of data from HESS I and.. Lower threshold and higher sensibility with HESS II G. LAMANNA SciNeGHE07 June 18-20, 2007
ARGO-YBJ Yangbajing village DI Girolamo
The shadow of the Moon at ARGO July 2006 to February 2007 data, with ARGO-130 reconstructed core position inside the array; 1.16 x 10 6 events in a window 6 x 6 around the moon. 560 hours of Moon observation with zenith angle < 45. and the shadow of the Sun and ~210 hours looking at the Sun, from july to Oct. 06 N pad >500 ~6σ N pad > 500, <E> = 5 TeV : A peak at 10 σ significance. Shifting: West 0.04, North 0.14 with respect to the nominal moon position
Search for point γ ray sources Some preliminary result The 2006 Markarian 421 Flare PRELIMINARY Cross Check Analysis July-August 2006 data: ~80 hours of Markarian 421 exposure Result: An observed excess with statistical significance: >5σ above the fluctuations Data reduction: Zenith angle <40 Quality cut on the event rec. based on the χ 2 of the fit. Nhit>60 (energy threshold) Window size: 1
Di Girolamo
2008 Scineghe 08 Aldo Morselli, INFN & Università di Roma 16-19 Tor Vergata, June aldo.morselli@roma2.infn.it 2008, Abano Terme, Padova32
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 33
Van Eldik Volpe Jogler Source creation acceleration injection Grasso Kryvdyk Meli Gavin Cosmic rays: about 10 Myears in the Galaxy (6-7 g/cm2) Di Girolamo:ARGO-JBJ Smith : Milagro Cao: CRTNT Atmosphere 40 km 23 Xo γ ν High Montain Detectors Cherencov Detectors further acceleration? Cosmic Rays Propagation Modulation Space experiments ~ 400 km Direct detection Balloons ~ 40 km ~3 g/cm 2 residual atmosphere Extensive Air Shower Detectors Bertania: KASCADE Grande Kokoulin : DECOR Salamida: AUGER Geenen : Particle Astrophysics Experiments Underground, Under-ice, Underwater Particle Aldo Morselli, Accelerators INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 34
KASCADE-Grande is in continuous and stable data taking since 2004 The detector has been studied and understood The performance of the detector looks promising First analysis show reasonable preliminary results Lot of physics to be explored Mario Bertaina - RICAP Conference, Rome 20-22 June 2007
General view of NEVOD-DECOR complex Kokoulin Side SM: 8.4 m 2 each; σ x 1 cm; σ ψ 1. DECOR data favor an increase of the effective primary mass up to energies 10 17 ev
What we can do in the future? Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 37
CTA : The Cherenkov Telescope Array facility aims to explore the sky in the 10 GeV to 100 TeV energy range Not to scale!
C TA An / V e T [ Possible CTA sensitivity advanced facility for ground-based high-energy gamma ray astronomy 10-11 GLAST E. F(>E) ] ) E s ~3000 m [TeV/cm 2 2 s] 2 mirror area > ( 10-12 F MAGIC ~5000 m x 2 mirror area few E10 4 10 m -13 2 with H.E.S.S. dense coverage (5-10%) O(10 7 m 2 ) with low coverage 1% Crab (0.03-0.05%) 10-14 few 10 5 m 2 with 10 100 medium 1000coverage10 4 10 5 E [GeV] (1-2%) Crab 10% Crab x 1.5 ~4000 m 2 mirror area
Gavin Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 40
The GAW Telescope Unit Each telescope is equipped with a refractive optics, a Fresnel lens, and with a focal surface detector formed by a grid of MultiAnode PhotoMultiplier Tubes, MAPMT. Each telescope will be equipped with an alt-az mounting. Cusumano SciNeGHE07 Villa Mondragone, Frascati, Rome, Italy
γ High Altitude Water Cherenkov Telescope Gus Sinnis Los Alamos National Laboratory for the HAWC Collaboration Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 42
Survey Sensitivity 1500 hrs/fov 4 min/fov 7 min/fov 1500 hrs/fov Sinnis Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 43
Through most of history, the cosmos has been viewed as eternally tranquil Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 44
` During the 20 th century the quest to broaden our view of the universe has shown us the vastness of the Universe and revealed violent cosmic phenomena and mysteries Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 45
Exploring Nature s Highest Energy Processes MAGIC, HESS, VERITAS Milagro, KASCADE- Grande, Auger in data taking April 07: AGILE in the sky First results from ARGO GLAST: Jan. 2008 launch Thank you!! Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 46