gamma astrophysics in the 50 gev – 50 tev domain
DESCRIPTION
Gamma astrophysics in the 50 GeV – 50 TeV domain. Great results from Cherenkov telescopes (IACTs): number of VHE sources increased by more than one order of magnitude in 3 years Another factor of 3 expected with MAGIC2, HESS2 And crucial improvement in resolution - PowerPoint PPT PresentationTRANSCRIPT
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Gamma astrophysics in the 50 GeV – 50 TeV domain
• Great results from Cherenkov telescopes (IACTs): number of VHE sources increased by more than one order of magnitude in 3 years
• Another factor of 3 expected with MAGIC2, HESS2– And crucial improvement in resolution
• Subjects of fundamental physics become accessible, e.g.– Lorentz violation– Dark matter– Transparency of the Universe (related to M, )
• Another order of magnitude can be gained with CTA– And more: room for new ideas…
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• IACT results:– From 3 VHE
gamma sources in 2003, we went to ~40 in 2007
– ~100 is expected with MAGIC2, HESS2, synergy with GLAST
• HESS much more successful on galactic sources, MAGIC a bit more successful in extragalactic
2003
2006
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Present IACTs: the “Big Four”
Roque delos Muchachos, Canary Islands
VERITAS (USA,UK1…)
1: Oct ’032: 2006100 m2
(4)
Montosa Canyon,Arizona
Windhoek, Namibia
HESS (Germany & France)2: Sum ’024: Early ’04
100 m2
(4+1)
Woomera, Australia
CANGAROO III(Japan & Australia)2: Dec. ’02, 3: Early ’0457 m2 (4)
MAGIC MAGIC (Germany, Italy & (Germany, Italy & Spain)Spain)1: Autumn ‘031: Autumn ‘03236 m236 m22
((2)2)
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HESS2• New 28m telescope.
• 2048 pixel camera.
• Lower energy threshold (30 GeV?)
• First light in 2008.
MAGIC2• Improved 17m telescope.
• Faster FADCs and a high-QE camera.
• First light in 2007.
What’s next - 1
VERITAS• 4x 12m telescopes at Whipple site end
2007? (now operating at basecamp)
MAGIC2
HESS2
VERITAS
Truephotos!
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What’s next – 2 : the Cherenkov Telescope Array
And: Factor 2 better angular resolution (~0.03 deg), Energy resolution ~15%
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The CTAaims to explore the sky in the 10 GeV to 100 TeV energy range
builds on demonstrated technologies (?)
combines guaranteed science with significant discovery potential
is a cornerstone towards a multi-messenger exploration of the nonthermal universe
2 sites: N ans S hemispheres
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few 1000 m
High-energy section~0.05% area coverage
Eth ~ 1-2 TeV
250 m
Medium-energy section~1% area coverage
Eth ~ 50-100 GeV
70 m
Low-energy section~10% area coverage
Eth ~ 10-20 GeV
Array layout: 2-3 Zones
FoV increasingto 8-10 degr.
in outer sections
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8Not to scale !
Option “off the shelf”: Mix of telescope types
Modes of operation• Deep wide-band mode: all
telescopes track the same source• Survey mode: staggered fields of
view survey sky• Search & monitoring mode:
subclusters track different sources• Narrow-band mode: halo
telescopes accumulate high-energy data, core telescopes hunt pulsars
…
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Proven:H.E.S.S. 12 m dish
Proven:MAGIC rapid-slewing 17 m dish(and new MAGIC, started)
Construction started:H.E.S.S. II 28 m dish0 10 m 20 m 30 m
Dish size
Cost /Dish Area
Cameracost dominates
Dish costdominates
Telescope structure “off the shelf” (but new ideas for large-field welcome)
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Strong support from EU: European lead
VERITAS
MAGIC
H.E.S.S.
CTA involves scientists fromCzech RepublicGermanyFranceItalyIrelandUKPolandSpainSwitzerlandArmeniaSouth AfricaNamibia
from several communitiesastronomy & astrophysicsparticle physicsnuclear physics
about 250-300 scientists workingcurrently in the field will bedirectly involved,user community significantly larger
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(Very optimistic) Schedule(to have a superposition w/ GLAST)
06 07 08 09 10 11 12 13Site exploration
Array design
Component prototypes
Telescope prototypes
Array construction
Partial operation
Full operation GLAST
FP 7 Design Study
“Letter of Intent”(100 pages, physics
+ conceptual design)Technicalproposal
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Tight deadlines• Working groups started meeting in June 06
– Physics: A. De Angelis and L. Drury (convenors), L. Maraschi, A. Treves, M. Persic, G. Lamanna, F. Aharonian, M. Teshima, K. Mannheim, D. Torres, G.F. Bertone, M. Punch, B. Giebels, …
– MC: K. Bernloher and E. Carmona (conv.), G. Hermann, G. Lamanna, S. Nolan, C. Bigongiari, A. Moralejo, W. Rhode, …
– Photon detector: T. Schweizer and P. Vincent (conv.), P. Goret, M. Punch, M. Teshima, E. Lorenz, N. Turini, INAF Palermo, …
– Choice of the site: B.K. and M. Teshima (conv.), G. Vasiliades, J. Cortina, …
– Mechanics and mirrors: M. Mariotti and M. Panter (conv.), Brera people, E. Lorenz, A. Biland, P. Chadwick, O. de Jager, …
– DAQ and computing: A. Biland and U. Schwanke (conv.), F. Goebel, L. Drury, T. Brez, R. Paoletti, N. Turini, G. Cabras, …
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~3000 sourcesby GLAST
~1000 sourcesby CTA
Guess confirmedby logN-logS studies
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CTA - conclusions
• A 100-150 MEUR FP7 project possibly going to be posted in May 2007– Italy (INFN+INAF) weights ~ 10-15%
• Mirror technology, advanced electronics, R&D for new telescope design?
• Science: AGN +… (INAF), astroparticle topics (INFN): Dark Matter, Lorentz Invariance Violation, Cosmological Constants, …
• Design study: ~5 MEUR now for R&D (big project re-posted in 2010 if it does not go thru?)