(gamma et neutrino) au TeV - LUTH

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CTA : Cerenkov Telescope Array ● Aims to explore the sky in the few 10 GeV to 100 TeV energy range, with “core” regime from ~100 GeV to ~ 10 TeV with milliCrab sensitivity ● Through larger array area, improved shower imaging, More Cherenkov photons per shower, more “golden” multi-telescope events ● “Survey mode” using sub-arrays can follow several sources simultaneously ● Higher sensitivity at TeV energies (x 10) using large sub-arrays or full array, finer variability measurements for known sources ● Lower threshold (few 10s GeV) with the large telescopes, for distant AGN detection, source mechanisms ● Higher detection rates ● Much finer transient phenomena measurements ● Systematic studies how performance changes with single parameters – dish size, field of view, pixel size, spacing, height 13 . 11 . 08 Yvonne Becherini, APC Paris 46
Cleaning 5/10, no cuts Blue Hillas, Red Model3D CTA : gain in angular resolution 13 . 11 . 08 Yvonne Becherini, APC Paris 47
Page 1 and 2: Séminaire du LUTh, Meudon État de
Page 3 and 4: 1ES1959 CasA 12 sources, 6 firm det
Page 5 and 6: Galactiques: Un grande nombre de so
Page 7 and 8: Accélérateur cosmique gammas phot
Page 9 and 10: VERITAS VERITAS HESS-II Télescopes
Page 11 and 12: Situé en Namibie, 23°S, 15°E Alt
Page 13 and 14: Utilité de la couverture du ciel :
Page 15 and 16: 200 m Le télescope à neutrinos Ba
Page 17 and 18: Amanda/IceCube 13 . 11 . 08 Yvonne
Page 19 and 20: 5line data (MayDec. 2007) 121 d
Page 21 and 22: Neutrinos dans Antares Antares prê
Page 23 and 24: Sensibilité du KM 3 aux sources po
Page 25 and 26: Résultats de Amanda II : analyse f
Page 27 and 28: ● Sources galactiques ● Young S
Page 29 and 30: Contour lines: ASCA X-rays Y. Uchiy
Page 31 and 32: ● On suppose π 0 γ et on calcu
Page 33 and 34: W28 @ 2-3 kpc 35 - 150 kyr age TeV
Page 35 and 36: MGRO J 1908+06: Bright extended sou
Page 37 and 38: Sensibilité pour MGRO J1908+06 ●
Page 39 and 40: The Extragalactic Catalogue Object
Page 41 and 42: Centaurus A, Distance =3.4 Mpc Radi
Page 43 and 44: γ π0 π ± 1:2:0 à la source p p
Page 45: 2048 pixel camera, 0.07° pixel siz
Page 49 and 50: CTA : gain en sensibilité “small
Page 51 and 52: ● L'astronomie plus mure par rapp
Page 53 and 54: Taux de neutrinos attendus pour les

(gamma et neutrino) au TeV - LUTH

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