1. 20 May 2008, Moscow The Telescope Array and its Low Energy Extension (TA/TALE) J.N. Matthews University of Utah

2. 20 May 2008, Moscow Outline Objective and Motivation for TA/TALE TA Construction and Status TALE 6km Stereo Fluorescence TALE Fluorescence Tower TALE Infill Array TALE Muon Array Summary

3. 20 May 2008, Moscow Spring 2008 Spectral Shape –The GZK Cut-off is there! 1 st Observation by the HiRes group – Announced at the 2001 ICRC/Hamburg, PRL in print Recent confirmation by Auger –Ankle Clearly Observed by Fly’s Eye and HiRes –Second Knee Observed by HiRes-MIA among others energy not well known –Structure = Physics Composition –heavy at 10 17 eV, turning light at 10 18 eV, constant to highest energies Anisotropy – No Clear Signs –Experiment –HiRes – AGASA triplet?, BL-Lacs?, Galactic Anticenter deficit?, no correlation with AGNs, No sign of Autocorrelation –AGASA – doublets, triplet, BL-Lacs?, Galactic Center excess? – Anticenter deficit?, Positive Autocorrelation –Auger – AGNs?, No excess at Galactic Center, Positive Autocorrelation

4. 20 May 2008, Moscow There’s Work to be done! Understand the spectral shape – it tells us about sources, their distribution, and propagation Look at changes in composition in conjunction with the spectrum – try to figure out the end of the Galactic Spectrum and separate it from the Extra- Galactic part As always, search for sources/anisotropy

5. 20 May 2008, Moscow TALE Goal: Reach 10 16.5 eV Study the Transition Region from Galactic to Extra-galactic cosmic ray flux Extend the overall coverage of the TA experiment to include all three cosmic ray spectral features in the ultrahigh energy regime: 1.The GZK Suppression 2.The Ankle 3.The Second Knee It is important than we establish a single unified energy scale for the measurement of all three features

6. 20 May 2008, Moscow Xmax Tells Us Composition Measuring gives us our best handle on composition. Need to extend Xmax measurements down to 10 16.5 eV to see the galactic/extragalacti c transition with good lever arm.

7. 20 May 2008, Moscow TA Stage-1 The energy region > 10 19 eV is well-covered by the existing TA detectors Ground Array becomes fully efficient at ~5x10 18 eV The three FD stations –TA-FD0 at Black Rock Mesa –TA-FD1 at Long Ridge –TA-FD2 at Middle Drum provide ~100% coverage of the ground array at 10 19 eV and above

8. 20 May 2008, Moscow Below 10 19 eV However, Stage-1 of TA was not designed for physics below 10 19 eV. There is no overlap at all in the aperture of the three fluorescence detectors at 10 18 eV The ground array efficiency drops quickly in the 10 18 -10 19 eV decade

9. 20 May 2008, Moscow HiRes Stereo HiRes Stereo aperture falls too rapidly through the ankle region to extend flux measurements much below ~3  10 18 eV. There are two primary reasons for this: 1.The 12.6 km separation of the two stations is too large: the overlap between the two shrinks very quickly below 3  10 18 eV 2.HiRes-1 only covers elevation angles up to 17 , which further limits the aperture near and below the ankle itself

10. 20 May 2008, Moscow TALE 6km Stereo Detector TALE will deploy a 2-ring, 24 mirror detector (using HiRes FADC detectors) on Long Ridge, 6 km from TA- FD1. Site separation of ~6km: State trust land (SITLA) site available at the location shown (more flexibility in land- use than BLM land) Available SITLA locations near BRM are too close to archaeological sites and to scenic landmarks Top view projection of the viewing solid angles of the TALE telescopes

11. 20 May 2008, Moscow Stereo Overlap Aperture is much flatter than the HiRes stereo aperture. Aperture at 10 18 eV is ~6  that of HiRes stereo. Stereo detection over the ankle region provides better resolution than monocular Stereo is better than hybrid: redundant measurement of shower properties (e.g. E and Xmax) which allows DIRECT validation of MC

12. 20 May 2008, Moscow TALE 6km detector Housing Construct two (2) 6-bay buildings similar to the Middle Drum structure (which has 7 bays) –Each bay holds one ring-1 (3-17  ) and one ring-2 (17- 31  ) telescope –For 24 telescopes you need two buildings in order not to have the telescopes obscure one another HiRes2 mirrors, PMT cameras and mirror stands will provide these 24 telescopes.

13. 20 May 2008, Moscow Zero in on the Ankle The energy, angular, and Xmax resolutions of the 6km stereo pair is expected to be similar to that of the HiRes stereo pair, except that the aperture is flattened in the decade of energy containing the ankle. Will provide stereo composition measurement down to ~10 18 eV, where we expect the elongation rate to begin to change…overlapping with the “Tower” hybrid detector.

14. 20 May 2008, Moscow Additional Benefits of TALE-6km The TALE-FD (6km telescopes) will also extend the both the monocular and stereo coverage of TA at the highest energies: we will have total time-averaged FD aperture >50% that of the ground array We will also have improved stereo-hybrid (2+ FD in coincidence with ground array) coverage: essentially 2/3 stereo-hybrid coverage of the ground array above 10 19 eV

15. 20 May 2008, Moscow “31° Bias”: Can’t Measure Xmax Below 10 18 eV Xmax measurements below 10 18 eV are beyond the scope of HiRes and Auger. TA is only a little better. Two-ring (<31  elevation) configuration introduces significant trigger bias toward low Xmax (heavy composition) showers TALE will need additional elements to cover this region, which contains the Second Knee Structure

16. 20 May 2008, Moscow Previous Attempt: HiRes prototype-Mia (~1993-1996) 14 (HiRes-1) + 4 (HiRes-2) mirror prototype detector operated between 1992 and 1996 HiRes-1 field of view up to ~70 . HiRes-1 operated in hybrid mode with the MIA muon array (16 patches  64 underground scintillation counters each):

17. 20 May 2008, Moscow HiRes-MIA & TALE Designs HiRes-MIA was a experiment of opportunity and was not optimized for the overlap region: –Used the 0.25km 2 CASA-MIA array (CASA was used only for triggering): limited by limited flux over such a small (but dense) ground array –MIA was designed as a hadronic event veto and cannot actually count muons –Due to a “longitudinal bias”, HiRes-size mirrors can’t measure Xmax below 10 17 eV The TALE solution is an improvement on the HiRes-MIA hybrid design. Deploy larger mirrors in rings 3-5, plus a larger infill surface array covering ~40 km 2 with 400m spacing –~3x larger mirrors in to extend the lowest energy physics threshold to 10 16.5 eV. –Dedicated muon detector with counting capability.

18. 20 May 2008, Moscow Tower Fluorescence Detector Use ~4 m diameter mirrors to triple the collection area over those of the re-deployed HiRes mirrors in the 6km stereo detector. Lowers bias to E < 10 16.5 eV. Use scaled-up ~F1.1 optics identical to HiRes Re-use PMTs from HiRes telescopes Use Winston cones for light collection

19. 20 May 2008, Moscow Tower FD The TALE Tower FD consists of 15 telescopes in its top three “rings”: –6 (3) at 31-45  –5 (3) at 45-59  –4 (4) at 59-73  # in parenthesis shows the number of mirrors in the HiRes tower prototype at the same elevation The 6km telescopes also provide 16 telescopes directly below the top three rings compared to only 4 in the HiRes- prototype Stereo overlap with TA-FD1 at Long Ridge for direct validation of MC resolutions Top view projection of the viewing solid angles of the TALE telescopes

20. 20 May 2008, Moscow Improved Sensitivity The increased mirror size will improve substantially the sensitivity of TALE in the 10 16.5 -10 17.5 eV energy decade Note the gain in sensitivity comes from the improvement in signal. The HiRes trigger scheme is not S/N limited, but limited by having enough signal to reconstruct a reliable shower profile.

21. 20 May 2008, Moscow Hybrid Operation The tower can operate in monocular mode, but limited to Xmax resolution of ~50 g/cm 2. Stereo overlap with Long Ridge FD site is too small to have large enough stereo aperture (but enough for direct MC validation of resolutions Need infill array for hybrid operation Simulations show 400 m spacing and ~4km x 4km array to be the optimal solution for hybrid operation the 10 16.5 -10 19 eV energy range Part of the main ground array northeast of TALE-FD site suitable for infill AND muon array. Sensitive plant species are found south of that location

22. 20 May 2008, Moscow Infill Array Will place 111 additional surface array counters overlapping with main ground array: 4km x 4km 16 of the counters in the main ground array will form part of the infill One possibility: re- use the AGASA scintillators and PMTs for the infill array

23. 20 May 2008, Moscow Muon Array One of the goals of TALE is to find where the (heavy) Galactic flux gives way to the (light) extra-galactic flux An orthogonal composition measurement (in addition to shower profile) will be a valuable addition to TALE Measure the e/μ ratio. Propose a 25 detector array placed in the “inner corner” of the infill array. The current plan is to bury the counters under 3m of packed soil Negotiations under way with BLM to collaborate This 2.5km x 2.5km graded array is designed to work at 10 16.5 -10 18 eV

24. 20 May 2008, Moscow Summary TA/TALE will bring together four different detector systems with overlapping energy ranges to give continuous coverage from 10 16.5 eV to the highest energies. The cost will be shared between U.S., Japan, South Korea, and Russia. TA/TALE will be able to study all three spectral features in the UHE regime and measure the composition in each energy range. In the energy region of the Second Knee where we suspect Galactic/Extragalactic transition to occur, we will have two orthogonal composition measurements: FD shower profile + e/  ratio.

25. 20 May 2008, Moscow HiRes: 5σ Observation of the GZK Break in the Spectrum Broken Power Law Fits –Two BP with extension to test hypothesis that a break is present. Expect 43 events Observe 13 events Poisson probability: P(13;43) = 5.3  Break is at (5.6 ± 0.5) x 10 19 eV; GZK expected at 6 x 10 19 eV. The break is the GZK cutoff! E -5.1

26. 20 May 2008, Moscow HiRes and Other Experiments HiRes and Auger(2007)HiRes, AGASA, Auger(2005)

27. 20 May 2008, Moscow A New Detector in the North! The Telescope Array was approved first by the Japanese government in 2003

28. 20 May 2008, Moscow Telescope Array Surface Detector Stations covering (blue diamonds): ~800 km 2 square grid with 1.2km spacing; 3.0 m 2 plastic scintillation detectors Three fluorescence Stations: 12 x 3m dia. mirrors each at Black Rock Mesa and Long Ridge, 14x 2m dia. Mirrors at Middle Drum Central Laser Facility: atmospheric monitoring laser seen by all 3 FD Surface Detectors LR MD BRM CLF

29. 20 May 2008, Moscow A New Detector in the North! The University of Utah and began site procurement with help from the University of Utah and the State of Utah Construction of the Black Rock Fluorescence Detector began in 2004

30. 20 May 2008, Moscow A New Detector in the North! The University of Utah and began site procurement with help from the U and State Construction of the Black Rock Fluorescence Detector began in 2004 Phase-1 Approval by US NSF in 2006

31. 20 May 2008, Moscow