08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Julia Becker for the IceCube collaboration August 2006 by the AMANDA experiment Implications of neutrino flux limits

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison 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

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison p     …    N   casc

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Amundsen-Scott South Pole Station South Pole Dome Summer camp AMANDA road to work 1500 m 2000 m [not to scale] AMANDA/IceCube 677 PMTs on 19 strings Cherenkov light

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Detection strategies AMANDA/IceCube FoV: northern hemisphere Point source searches – significance map ?clustering of neutrinos identified photon sources Stacking strategy – sum signal of point sources of same source classSearch for a diffuse signal: use complete northern hemisphere

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Other strategies  Cascade analyses  Transient sources: Flares of permanent objects Gamma Ray Bursts  stacking approach, temporal clustering SGR  Dark matter searches WIMPs Magnetic Monopoles  CR composition (IceTop)  Atmospheric muons, charm contribution  Acoustic detection great but too short time! Talk Elisa Resconi Poster Juande Zornoza Poster Brennan Hughey Poster Tom Gaisser Talks Doug Cowen, Ty DeYoung Talks Stephan Hundertmark, Justin Vandenbroucke

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Search for single point sources 90% confidence level flux upper limits for the northern hemisphere in 0.5 deg bins (15% systematic error included) Event map – 4282 events in 5 years ( ) –effective time: 1001 daysNo significant signal – Limit map preliminary!

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison 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!

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Energy spectrum (2000) High energy limit ( ) Hill et al., Neutrino 2006 Diffuse energy spectrum&limit Nellen Poster Jessica Hodges

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison 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

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Model-dependence of limit  Not always E -2  Energy range of limits change with spectral index, E -   Higher energies for flatter spectra E-1E-1 E-3E-3 E-2E-2 log(E/GeV) log(dN/dE*E 2 ) preliminary!

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison 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

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison =  +  (TeV) =

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison =  +  (TeV) = z=0.3 z=1 ~10

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison TeV Blazars – spectrum  Total diffuse flux:  Neutrino flux up to a certain redshift:  Absorption factor:

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Absorption factor conservative estimate:

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Maximum contribution astro-ph/

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison 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!) 

08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison IceCube! South Pole Station Skiway IceCube footprint (In-ice, IceTop) SPASE array AMANDA Geographic South Pole Photograph: Forest Banks Posters Jon Dumm, Hagar Landsman Talk Kael Hanson

Construction schedule AMANDA SPASE-2 South Pole Dome Skiway 100 m Text