Implications of neutrino flux limits
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1 Implications of neutrino flux limits by the AMANDA experiment Julia Becker for the IceCube collaboration August 2006
2 Contents I. Detection principle and detector II. Analysis methods and results I. point sources II. stacking of point sources III. diffuse signal III. Interpretation of the diffuse signal IV. Summary
3 p γ Δ π ν... ν N...μ, casc
4 AMANDA/IceCube road to work South Pole Dome AMANDA 1500 m Summer camp 2000 m Amundsen-Scott South Pole Station 08/2006 [not Julia to Becker, scale] Universität Dortmund TeV particle astrophysics, Madison
5 AMANDA/IceCube 677 PMTs on 19 strings Cherenkov light road to work South Pole Dome AMANDA 1500 m Summer camp 2000 m Amundsen-Scott South Pole Station 08/2006 [not Julia to Becker, scale] Universität Dortmund TeV particle astrophysics, Madison
6 Detection strategies Point source searches significance map?clustering of neutrinos identified photon sources AMANDA/IceCube FoV: northern hemisphere
7 Detection strategies Stacking strategy sum signal of point sources of same source class AMANDA/IceCube FoV: northern hemisphere
8 Detection strategies Search for a diffuse signal: use complete northern hemisphere AMANDA/IceCube FoV: northern hemisphere
9 Other strategies Talks Doug Cowen, Ty DeYoung Cascade analyses Talk Elisa Resconi Transient sources: Flares of permanent objects Poster Brennan Hughey Gamma Ray Bursts stacking approach, temporal clustering Poster Juande Zornoza SGR Dark matter searches WIMPs Magnetic Monopoles great but too short time! Poster Tom Gaisser CR composition (IceTop) Atmospheric muons, charm contribution s Stephan Hundertmark, Justin Vandenbroucke, Buford Price Acoustic detection
10 Searchforsinglepoint sources Event map 4282 events in 5 years ( ) effective time: 1001 days preliminary!
11 Searchforsinglepoint sources Event map 4282 events in 5 years ( ) effective time: 1001 days No significant signal Limit map 90% confidence level flux upper limits for the northern hemisphere in 0.5 deg bins (15% systematic error included) preliminary!
12 Stacking of AGN GeV blazars (EGRET) GeV Unidentified EGRET sources unidgev Infrared sources IR HAEO-A-detected kev sources kev(h) ROSAT-detected kev sources kev(r) TeV blazars - TeV Compact Steep Spectrum and Giga-Hertz peaked sources CSS/GpS FR-I galaxies including M87 FR-I(M) FR-I galaxies without M87 FR-I FR-II galaxies FR-II Radio-weak quasars QSO preliminary!
13 Stacking of AGN preliminary!
14 Diffuse energy spectrum&limit Energy spectrum (2000) Nellen High energy limit ( ) 2 E φ GeVcm = sr 8 1 Hill et al., Neutrino 2006 s Poster Jessica Hodges
15 X-ray AGN (I) Nellen,Mannheim&Biermann Phys.Rev.D (1993) Stecker&Salamon Space Science Rev. (1996) Limits&IceCube sensitivity Hill et al., Neutrino 2006 Limit strongly restrictive Favoring IC scenario
16 Model-dependence of limit E - 3 E - 1 log(dn/de*e 2 ) E - 2 log(e/gev) Not always E -2 Energy range of limits change with spectral index, E -γ Higher energies for flatter spectra preliminary!
17 X-ray AGN (II) Nellen,Mannheim&Biermann Phys.Rev.D (1993) Stecker&Salamon Space Science Rev. (1996) Limits&IceCube sensitivity Hill et al., Neutrino 2006 Limit adjusted to model 1 order of magnitude below flux
18 = ν + γ(tev) = ν
19 = ν + γ(tev) = ν z= ~10 z=0.3
20 TeV Blazars ν spectrum Total diffuse ν flux: Neutrino flux up to a certain redshift: Absorption factor:
21 Absorption factor eta(z max ) conservative estimate: z max
22 Maximum contribution astro-ph/
23 Summary Point source analysis no significant signal Source stacking: increase of sensitivity limits to flux from source classes Diffuse flux: strong constraints X-ray AGN: most likely X-rays from Inverse Compton TeV-sources: limit to contribution of TeV-photon observable sources Limits adjusted to different flux models Very near future (9 strings working already!)
24 IceCube! South Pole Station Geographic South Pole SPASE array AMANDA IceCube footprint (In-ice, IceTop) Talk Kael Hanson Photograph: Forest Banks Skiway Posters Jon Dumm, Hagar Landsman
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