(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
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- 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 :
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- Page 17 and 18: Amanda/IceCube 13 . 11 . 08 Yvonne
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- Page 21 and 22: Neutrinos dans Antares Antares prê
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- Page 43 and 44: γ π0 π ± 1:2:0 à la source p p
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W28 @ 2-3 kpc<br />
35 – 150 kyr age<br />
<strong>TeV</strong> emission coincident with<br />
molecular clouds is revealed by HESS<br />
Index varies 2.3-2.7<br />
OH masers trace shocks<br />
Expected B-field high <br />
First evidence for p-p<br />
in SNR/ cloud interaction<br />
If @ 2kpc,<br />
Implies 10-30 times<br />
CR enhancement wrt Solar System<br />
These CRs may be supplied by W28<br />
Older Shell-type SNRs: W28<br />
NANTEN CO<br />
10-20 km/s<br />
20/90 cm VLA<br />
MSX 8 micron<br />
13 . 11 . 08 Yvonne Becherini, APC Paris 33