1. HiRes 5Y Operations – Program and Context What Physics Will be Done? How Does it Compare With Other Projects?

2. General Goals Stereo Spectrum from 10 18 eV on – Stereo Spectrum from 10 18 eV on – Study ankle, pileup and GZK cutoff Study ankle, pileup and GZK cutoff Confirmed energy resolution using E pull ( E1- E2/Eav) Confirmed energy resolution using E pull ( E1- E2/Eav) Confirmed atmospheric parameters using energy balance and detailed laser studies. Confirmed atmospheric parameters using energy balance and detailed laser studies. Statistical strength and energy reach for 5 years Statistical strength and energy reach for 5 years

3. Stereo Aperture and Dependence on Atmospheric Parameters

4. Monocular Spectrum

5. Preliminary Look at Stereo Data – Energy Resolution

6. Event Energy Distribution (> 10 EeV) – 800 hours of stereo operation

7. Preliminary Stereo Spectrum above 10 EeV

8. Predicted Event Statistics for 5Y OP

9. Event Rate Prediction – Based on Current Reconstructed Event Rates (conservative) 5Y op = ~ 5000 hours 5Y op = ~ 5000 hours Expect ~ 500 events > 10 19 eV Expect ~ 500 events > 10 19 eV Expect ~ 5 events > 10 20 eV (based on NSF event) ~ E -3 spectrum Expect ~ 5 events > 10 20 eV (based on NSF event) ~ E -3 spectrum Expect ~ 30 events if AGASA flux is correct.(~ 5 sigma discrepancy) Expect ~ 30 events if AGASA flux is correct.(~ 5 sigma discrepancy) > 10 20 eV are “golden” – high signal, highly constrained. > 10 20 eV are “golden” – high signal, highly constrained.

10. NSF Event

11. “Golden” Events Very strong signals ( aperture cut-off due to track-length, not S/N at Xmax). Very strong signals ( aperture cut-off due to track-length, not S/N at Xmax). If Xmax seen in both eyes, Smax balance can constrain/test atmospheric parameters. If Xmax seen in both eyes, Smax balance can constrain/test atmospheric parameters. Events typically seen with one Rp much smaller than other – atmospheric effects mitigated. Events typically seen with one Rp much smaller than other – atmospheric effects mitigated. If fluorescence efficiency well understood, very hard to significantly shift event energies. If fluorescence efficiency well understood, very hard to significantly shift event energies.

12. MEASURING FLUORESCENCE AT SLAC Extensive Air Showers (EAS) are predominantly a superposition of EM sub- showers. Extensive Air Showers (EAS) are predominantly a superposition of EM sub- showers. Important N 2 transition (2P) not accessible by proton excitation; only e-beam can do it. Important N 2 transition (2P) not accessible by proton excitation; only e-beam can do it. FFTB beam-line provides energy equivalent showers from ~10 15 to ~10 20 eV. FFTB beam-line provides energy equivalent showers from ~10 15 to ~10 20 eV. 10 8 -10 10 electrons/pulse at 28.5 GeV. 10 8 -10 10 electrons/pulse at 28.5 GeV. 2% of electron pulse bremsstrahlung option. 2% of electron pulse bremsstrahlung option.

13. Significance of pileup No-pileup ( E -3 ) flux implies order of magnitude decrease in integral flux between 10 19 and 3 x10 19 eV. (81 events – 8.1x1.7 =13 events expected ) No-pileup ( E -3 ) flux implies order of magnitude decrease in integral flux between 10 19 and 3 x10 19 eV. (81 events – 8.1x1.7 =13 events expected ) Observe 29 Stereo events above 3 x10 19 eV. Observe 29 Stereo events above 3 x10 19 eV. 2.9 sigma. 2.9 sigma. After 5Y, expect 500 events above 10 19. Expect 50x1.7=85 events above 3 x10 19 eV if ( E -3 ) flux. If present data is correct, would see 179 events. This is a 7 sigma effect. After 5Y, expect 500 events above 10 19. Expect 50x1.7=85 events above 3 x10 19 eV if ( E -3 ) flux. If present data is correct, would see 179 events. This is a 7 sigma effect.

14. Significance of ankle ( dip structure) Dip structure can be used to cross-calibrate energy scale of various experiments. Dip structure can be used to cross-calibrate energy scale of various experiments. What is the physics of this structure? e+e- energy loss? Appearance of extragalactic spectrum? What is the physics of this structure? e+e- energy loss? Appearance of extragalactic spectrum? Expect ~ 3000 events above 10 18.3 eV and ~10,000 events above 10 18 eV. Statistics will not be an issue. Expect ~ 3000 events above 10 18.3 eV and ~10,000 events above 10 18 eV. Statistics will not be an issue.

15. Second Knee Second knee seen in many experiments. Simple energy scale shift can bring them into good agreement. Second knee seen in many experiments. Simple energy scale shift can bring them into good agreement. Physics of transition between galactic and extragalactic flux? Composition is changing in this energy region. Physics of transition between galactic and extragalactic flux? Composition is changing in this energy region. Can be accessed with HiRes II mono data. Can be accessed with HiRes II mono data. Propose to push thresholds down to near 10 16 eV. Continuous measurement of composition over second knee, ankle and pileup region of spectrum is then possible. Propose to push thresholds down to near 10 16 eV. Continuous measurement of composition over second knee, ankle and pileup region of spectrum is then possible.

16. Second Knee, showing correlation between knee energy and spectral normalization

17. Second Knee Spectrum, Shifted to make knee come out at same energy

18. General Goals, cont. Composition of Cosmic Rays from 10 18 eV Composition of Cosmic Rays from 10 18 eV Xmax method – preliminary stereo results confirm earlier Fly’s Eye results. Xmax method – preliminary stereo results confirm earlier Fly’s Eye results. Preliminary stereo results consistent with hadronic model predictions – sensitivity to composition. Preliminary stereo results consistent with hadronic model predictions – sensitivity to composition. Expected statistics for one and two view Xmax determination. Expected statistics for one and two view Xmax determination. Xmax resolution confirmed by Xmax pull for two view events. Xmax resolution confirmed by Xmax pull for two view events. Search for gamma ray flux using LPM and mag. Brem. Search for gamma ray flux using LPM and mag. Brem. Expected statistical reach. Expected statistical reach.

19. Resolution After All Cuts Energy X max 723 Events

20. Pull Distribution – Data and MC ) (XmaxI-XmaxII)/(XmaxI+XmaxII

22. Comparison of gamma ray Xmax distribution with LPM and magnetic brem effects taken into account

23. General Goals, cont. Anisotropy Anisotropy Small-scale anisotropy – stereo data has symmetric error boxes and excellent angular resolution ~ 1 deg. Small-scale anisotropy – stereo data has symmetric error boxes and excellent angular resolution ~ 1 deg. Is the AGASA auto-correlation result correct? HiRes I monocular data does not support it, but suffers from assymetric errors Is the AGASA auto-correlation result correct? HiRes I monocular data does not support it, but suffers from assymetric errors Sensitivity to putative point sources for 5 Y of operation. Sensitivity to putative point sources for 5 Y of operation.

24. Xmax viewing efficiency Integrated over energy range Integrated over energy range ~60% of triggered events have Xmax well reconstructed in at least one view. ~60% of triggered events have Xmax well reconstructed in at least one view. ~40% of triggered events have Xmax well reconstructed in both views. ~40% of triggered events have Xmax well reconstructed in both views. Composition above 10 19 eV will be based on Composition above 10 19 eV will be based on ~ 300 events. Resolution function based on ~200 events.

25. HiRes Monocular Error Boxes

26. HiRes monocular simulated data

27. HiRes Stereo simulated data

28. Akeno/AGASA result on anisotropy near 10 18 eV

29. General Goals, cont. Measurement of total inelastic p-Air cross- section. Measurement of total inelastic p-Air cross- section. Composition above few x 10 18 appears to be proton dominated. Composition above few x 10 18 appears to be proton dominated. Cut on deeper events to increase proton fraction. Cut on deeper events to increase proton fraction. Xmax distribution decrement is sensitive to p-Air. Xmax distribution decrement is sensitive to p-Air. Because result comes from tail of distribution, understanding of resolution and reconstruction is essential- requires tightly cut stereo data. Because result comes from tail of distribution, understanding of resolution and reconstruction is essential- requires tightly cut stereo data.

30. General Goals, cont Neutrino search Neutrino search Search for unusual shower development Search for unusual shower development

31. Other Experiments and Proposals AGASA AGASA Pierre Auger SOUTH Pierre Auger SOUTH Telescope Array Telescope Array Pierre Auger NORTH Pierre Auger NORTH EUSO EUSO OWL OWL

32. AGASA 100 km 2 ground array. Ran for ~ 12 years. To be decommissioned ( another two years possible). 100 km 2 ground array. Ran for ~ 12 years. To be decommissioned ( another two years possible). Quoted accumulated aperture ~ HiRes I mono. Quoted accumulated aperture ~ HiRes I mono. No further significant data expected. No further significant data expected.

33. Pierre Auger SOUTH 3000 km 2 ground array + Fluorescence detector. 3000 km 2 ground array + Fluorescence detector. Ground array aperture is 7000 km 2 str near 10 20 eV. Probable completion data 2005. Ground array aperture is 7000 km 2 str near 10 20 eV. Probable completion data 2005. Hybrid aperture is 10% or ~700 km 2 str. Hybrid aperture is 10% or ~700 km 2 str. If HiRes runs for 5 years and stops in 2007, Auger hybrid will have equal statistics in ~7 years, or 2012. If HiRes runs for 5 years and stops in 2007, Auger hybrid will have equal statistics in ~7 years, or 2012. Southern and Northern spectra may be different Southern and Northern spectra may be different

34. Pierre Auger SOUTH, cont. Ground array will have similar statistics to HiRes in 2006. Ground array will have similar statistics to HiRes in 2006. Issues of ground array vs. fluorescence energy scale will not be settled until hybrid data becomes significant, perhaps in 2007. Issues of ground array vs. fluorescence energy scale will not be settled until hybrid data becomes significant, perhaps in 2007.

35. Telescope Array Full – scale proposal for 8 stations + 2 HiRes stations still pending at Monkasho. Full – scale proposal for 8 stations + 2 HiRes stations still pending at Monkasho. If approved, five year construction is expected. If approved, five year construction is expected. TA phase I ( three partial eyes + ground array) proposal submitted to …. TA phase I ( three partial eyes + ground array) proposal submitted to …. HiRes group is collaborating on both proposals. HiRes group is collaborating on both proposals.

36. Pierre Auger North Originally proposed for Millard County, UT. Originally proposed for Millard County, UT. Current status unclear – may be in Europe. Current status unclear – may be in Europe. Unlikely to start construction before 2006. Unlikely to start construction before 2006. MOU exists between HiRes, Auger and TA to work together if built in Utah. MOU exists between HiRes, Auger and TA to work together if built in Utah.

37. EUSO Phase A ESA approval for deployment on ISS in ~ 2009. Phase A ESA approval for deployment on ISS in ~ 2009. Aperture ~ order of magnitude larger than Auger ground array. Aperture ~ order of magnitude larger than Auger ground array. Two to three year operational life. Two to three year operational life. Similar to Auger over expected life of detectors. Similar to Auger over expected life of detectors. Detector threshold near 10 19 eV. Detector threshold near 10 19 eV.

38. OWL Next generation ( post-EUSO) proposal. Next generation ( post-EUSO) proposal. Two 1000 km orbit free-flyer satellites. Two 1000 km orbit free-flyer satellites. Stereo observation – ~10 6 km 2 str instantaneous aperture. Stereo observation – ~10 6 km 2 str instantaneous aperture. Unlikely to fly before 2014. Unlikely to fly before 2014.