# Presentation: 340463

##            How guaranteed are GZK ’s ?

- Carlos Pena Garay
- IAS, Princeton

**~**

- Somewhat soon ...
- Icecube international collaboration is working on the contruction of the detector.
- PY06, november 5, 03:12.
- Neutrino event is observed with energy of 1018 eV
- Direction : =60o ,  =10 h
- Madison, we’ve got a GZK
- Does it make sense?

- GZK neutrinos

**N + ********N ********Standard scenario: proton propagation through ********CMB**** ****Energy losses : photoproduction, pair production, and adiabatic losses.****  ****Propagation well understood. Uncertainties are in the inputs :****- Uniformly distributed sources****- Energy at CRs extragalactic dominance****- Maximum CR energy****- Injected spectrum****- Source evolution****- Other photon targets, other hadron sources**

**Greisen, Zatsepin, Kuzmin, 1966**

- Calculations

**C++ Code : ****Event generator : minimum bias photohadron interactions (a la sophia)****Extensions  (in progress. Scheduled for june, implemented with current propag. in Earth)****- higher nucleus****Oscillations are included in the output**

**Mucke, Engel, Rachen, Protheroe, Stanev, astro-ph/9903478 **

## Formulae : Input parameters

**Astrophysical UHECRs j by uniformly distributed sources**

## Is SFR tracing the UHECRs sources?

**Smail, Ivison, Blain, Kneib,  MNRAS 2002 **

**Inferences of :****(1+z)****n****f(z,z****min****,z****max****)**

## HiRes vs AGASA data ?

**Inferences of :****E****-********g(E,E****min****,E****max****)****Use compatibility****of data samples****(2********)****Use uniform****source distribution****Use  composition**

## HiRes data

## HiRes data

**Engel, Seckel, Stanev, astro-ph/0101216 **

**Waxman, Bahcall, hep-ph/9807282 **

**Waxman, 1995**

## HiRes data

**Ahlers, Anchordoqui, Goldberg, Halzen, Ringwald, Weiler, astro-ph/0503229 **

**Seckel, Stanev, astro-ph/0502244      ********+n>2.5 dominance at higher z**

**Berezinsky, Gazizov, Grigorieva, 1988, astro-ph/0204357, astro-ph/040347, astro-ph/0502550**

**Different models****fit the CR spectrum : ****2.0<******** <2.8****0<n<4.5**

**Fodor, Katz, Ringwald, Tu, hep-ph/0309171 **

## HiRes data

**Ahlers, Anchordoqui, Goldberg, Halzen, Ringwald, Weiler, astro-ph/0503229 **

**Seckel, Stanev, astro-ph/0502244      ********+n>2.5 dominance at higher z**

**Berezinsky, Gazizov, Grigorieva, 1988, astro-ph/0204357, astro-ph/040347, astro-ph/0502550**

**Different models****fit the CR spectrum : ****2.0<******** <2.8****0<n<4.5**

**Fodor, Katz, Ringwald, Tu, hep-ph/0309171 **

- More with Auger :
- Confirm GZK feature : Guaranteed
- Improved spectrum and composition

- A short trip : Wave packets , Neutrino osc.

- Same result

## The Neutrino Matrix :SM + mass

- The Neutrino Matrix :SM + mass

**Gonzalez-Garcia, Maltoni, PG, 2004**

## Neutrino mixing

****** ****decay :  Mass neutrino ratios at the Earth **

****************** **

**         ****pdf**** **

## Neutrino mixing

****** ****decay :  Flavor neutrino ratios at the Earth **

**************e**** **

**         ****pdf**** **

## Predicted GZK spectra : minimal ?

**                   ****_****    E****2************************GeVcm****-2****s****-1**** sr****-1**

**                   ****    ****E**** (****GeV)**

**If cosmic rays are mainly p (>50%) and uniformly distributed sources following the star formation rate, the total muon neutrinos ****at the Earth peaks 10****-8**** ****GeVcm****-2****s****-1**** sr****-1**** at 6 10****9**** GeV**

## Predicted GZK spectra :

**                   ****_****    E****2************************GeVcm****-2****s****-1**** sr****-1**

**                   ****    ****E**** (****GeV)**

**If cosmic rays are mainly p (>50%) and uniformly distributed sources following the star formation rate, the total muon neutrinos ****at the Earth peaks at 10****-8**** ****GeVcm****-2****s****-1**** sr****-1**** at 6 10****9**** GeV**

**Model dependent : goes up to experimental limits**

- Conclusion

**If IceCUBE sees a GZK neutrino soon : a big surprise****If GZK neutrinos are measured somewhere above the conservative calculation, GZK neutrinos have a lot to say of the main inputs needed in the calculation:****How large is the extragalactic component in the UHECRs ****Information on the source evolution of the UHECRs sources**

**Ahlers, Anchordoqui, Goldberg, Halzen, Ringwald, Weiler, astro-ph/0503229 **

**Seckel, Stanev, astro-ph/0502244     **