(gamma et neutrino) au TeV - LUTH
(gamma et neutrino) au TeV - LUTH (gamma et neutrino) au TeV - LUTH
IceCube unbinned analysis 13 . 11 . 08 Yvonne Becherini, APC Paris 26
● Sources galactiques ● Young Shell-type Supernova Remnants (RXJ 1713.7-3946) ● Older and/or Interacting SNRs (W28) ● Composite SNRs ● Pulsar Wind Nebulae (Vela X) ● Binary Systems (LS 5039, PSR B1259) ● Open Stellar Clusters ● Galactic Centre ● Galactic diffuse emission Principaux résultats en gamma par H.E.S.S. ● MILAGRO sources and “hot spots” C. Stegmann ICRC 2007 ●Sources extra-galactiques ●Blazars (8 discoveries by H.E.S.S., several confirmations) PKS 2155-304 ● Radiogalaxies (Centaurus A) ● Extragalactic Background Light (EBL) – H.E.S.S. demonstrated that EBL is lower than previously thought (Nature, 2006) ● Limit on Quantum Gravity thanks to measurements of rapid flares (submitted 2008) ● Multiwavelength campaigns (e.g. PKS 2155- 13 . 11 . 08 Yvonne Becherini, APC Paris 27 304) ● Starburst Galaxies (UL) ● GRBs (UL)
- 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: Résultats de Amanda II : analyse f
- 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 and 46: 2048 pixel camera, 0.07° pixel siz
- Page 47 and 48: Cleaning 5/10, no cuts Blue Hillas,
- 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
IceCube unbinned analysis<br />
13 . 11 . 08 Yvonne Becherini, APC Paris 26
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