De_Angelis_Alessandro.pdf
De_Angelis_Alessandro.pdf De_Angelis_Alessandro.pdf
• • • – Alessandro De Angelis • extend E range beyond 50 TeV • better angular resolution • larger FOV • monitor many objects simult. • extend E range under 50 GeV •10x sources • better flux sensitivity • lower threshold 34
2 arrays: north+south all-sky coverage low energy section E thresh ~ 10 GeV 4 23 m telescopes Alessandro De Angelis core array 100 GeV-10 TeV ~ 23 12 m telescopes high energy section ~35 tel. on 10 km 2 area 35
- Page 1 and 2: • • • 1
- Page 3 and 4: • - • - - • - μ μ
- Page 5 and 6: hadronic cascades p + (>>TeV) matte
- Page 7: edshift z 30 GeV 100 GeV > 1 regio
- Page 10: c ~ 1º e Threshold @ sl: 21 MeV Ma
- Page 13 and 14: VERITAS: 4 telescopes (~12m) in Ari
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- Page 17 and 18: W51: gamma rays come from a molecul
- Page 19 and 20: Alessandro De Angelis 19
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- Page 27 and 28: (t) obs 3 2 E E s2 2 1 H0
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- Page 33: • LHC may find candidates but can
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- Page 41 and 42: Marvel 1961 • • 4
- Page 43 and 44: Colours: 0.2 - 6 keV (Chandra) Cont
- Page 45 and 46: • • dN dE 1 2 dN dE
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- Page 52 and 53: Design study phase concluded in Fal
- Page 54 and 55: 100 m 2 dish area 1.2 m mirror face
- Page 56 and 57: Wavelenght range 300 - 600 nm Mirro
- Page 58 and 59: Hardware key elements: - O(100) Tel
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- Page 62 and 63: 65 2008 2009 2010 2011 2012 2013 2
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- Page 66 and 67: DARMA 3C279 Note: if conversion “
- Page 68 and 69: 1st order (t) obs E H0 E s1
- Page 70 and 71: • z = 0.903 ± 0.003 • prompt s
- Page 72 and 73: Better bkgd reduction Better angula
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<strong>Alessandro</strong> <strong>De</strong> <strong>Angelis</strong><br />
• extend E range beyond 50 TeV<br />
• better angular resolution<br />
• larger FOV<br />
• monitor many objects simult.<br />
• extend E range under 50 GeV<br />
•10x sources<br />
• better flux sensitivity<br />
• lower threshold<br />
34
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