Summary WG4 – Neutrino Astronomy experimental part Mieke Bouwhuis: Results from ANTARES Georgio Riccobene: Results from NEMO and KM3NeT Dave Besson: Radio detection Doug Cowen: Tau neutrino detection in IceCube Ty de Young: Novel tau signatures in neutrino telescopes Julia Becker: AMANDA flux results and interpretation Elisa Resconi: IceCube: multiwavelength approach Lutz Köpke University of Main + many posters extend reach: (sky coverage, energy coverage, -id …) improve sensitivities: (stacking, -correlation…)
22
Embed
Summary WG4 – Neutrino Astronomy experimental part Mieke Bouwhuis: Results from ANTARES Georgio Riccobene: Results from NEMO and KM3NeT Dave Besson: Radio.
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
Summary WG4 – Neutrino Astronomy experimental part
Mieke Bouwhuis: Results from ANTARESGeorgio Riccobene: Results from NEMO and KM3NeTDave Besson: Radio detectionDoug Cowen: Tau neutrino detection in IceCubeTy de Young: Novel tau signatures in neutrino telescopesJulia Becker: AMANDA flux results and interpretationElisa Resconi: IceCube: multiwavelength approach
Deep, low bioluminescence, weakcurrents, little sedimentation
full tower 2007
TDR KM3NeT 2009 cost < 200 M€
NEMO-km3 detector design study
20 m
40 m
…similar number of PMT’s, towers as IceCube… 100 km from shore
Modular, rigid structures with 4 PMTs that unfolds …
Philosophy: reduce number of structures and
underwater connections; operate by ROV
Radio detection
Points of cautions: 1) presented upper limits can `float’ horizontally (no energy resolution),2) different model parameters used for different modes, 3) 90% vs. 95% C.L. limits, 4) results depend on binning
Characteristic level (band)Depends on: source + detector
Elevated levels or flares : ~ 15 %
+ 3
Rchar
TeV- curves very sporadic, historical light curves: under construction
AMANDA
Diffuse limits
112
82 108.8
srsGeVcm
E AMANDA4 year limitassuming E-2:
Hill et al., Neutrino 2006Nellen,Mannheim & Biermann 1993
Stecker & Salamon 1996 (x-ray)
Differential limits difficult to obtain limits depend on assumed spectral index
…exclude
Stecker&Salomon 96 AGN flux, but not Stecker 2005
Stecker 2005 (-ray)
Diffuse flux of TeV Blazars
conservative estimate:
Both , visible (x < 0.3)only visible (1 < x < 10)
x
diffuse flux flux sources up to redshift zmax absorption factor
Maximum contribution from TeV blazars
astro-ph/0607427
Test
spe
cific
mod
els!
Experimental summary(summary) of WG4
Extend reach:
– Northern hemisphere detectors (Antares 2007+, TDR km3NET 2009)– Further extend energy range (radio, acoustics ….)– Ideas to identify -neutrinos in many topologies
Extend sensitivities:
– stacking techniques (assume analogous behaviour, - correlation)– Correlation with x-ray or TeV flares; -telescope triggers?– Investigate specific models