(gamma et neutrino) au TeV - LUTH
(gamma et neutrino) au TeV - LUTH (gamma et neutrino) au TeV - LUTH
Vela X : hadrons vs. leptons mean atm. flux (Volkova, 1980, Sov.J.Nucl.Phys., 31(6), 784) - leptonic models favoured in other PWN (e.g. HESS J1825-137) due to observation of change in spectral index with distance from pulsar → cooling/aging of electrons) - 1 sigma errors include systematic errors (20% norm., 10% index & cut-off) - 5 years livetime in a KM 3 detector → 2.6 sigma ! Vela X (PWN) expected neutrino flux – in reach for KM3NeT measured γray flux (H.E.S.S.) 13 . 11 . 08 Yvonne Becherini, APC Paris 32
W28 @ 2-3 kpc 35 – 150 kyr age TeV emission coincident with molecular clouds is revealed by HESS Index varies 2.3-2.7 OH masers trace shocks Expected B-field high First evidence for p-p in SNR/ cloud interaction If @ 2kpc, Implies 10-30 times CR enhancement wrt Solar System These CRs may be supplied by W28 Older Shell-type SNRs: W28 NANTEN CO 10-20 km/s 20/90 cm VLA MSX 8 micron 13 . 11 . 08 Yvonne Becherini, APC Paris 33
- 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: ● On suppose π 0 γ et on calcu
- 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
Vela X : hadrons vs. leptons<br />
mean atm. flux<br />
(Volkova, 1980,<br />
Sov.J.Nucl.Phys.,<br />
31(6), 784)<br />
- leptonic models favoured in other PWN (e.g. HESS J1825-137) due to observation<br />
of change in spectral index with distance from pulsar → cooling/aging of electrons)<br />
- 1 sigma errors include systematic errors (20% norm., 10% index & cut-off)<br />
- 5 years liv<strong>et</strong>ime in a KM 3 d<strong>et</strong>ector → 2.6 sigma !<br />
Vela X<br />
(PWN)<br />
expected<br />
<strong>neutrino</strong> flux –<br />
in reach for KM3NeT<br />
measured<br />
γray flux<br />
(H.E.S.S.)<br />
13 . 11 . 08 Yvonne Becherini, APC Paris 32
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