1. David Nitz Michigan Technological University Instrumentation for the Northern Site of the Pierre Auger Observatory 1 1Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

2. 2 Special thanks to my many collaborators for providing slides and photos 2Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

3. The Auger Observatory One observatory in two hemispheres [Design Report 1995] Southern site completed June 2008 First Proposals for Northern site submitted 2009 Hybrid shower measurements: Surface array + air fluorescence 3 3Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

4. Auger South Overview 4 4Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation Covers 3000 km 2 - 1660 water Cherenkov stations on 1.5 km triangular grid (SD) 3 9” Photonis XP1805 PMTs per station 4 Fluorescence Detector stations with 6 telescopes each (FD) 2 atmospheric monitoring laser facilities (CLF & XLF) Balloon launch station for atmospheric profiling (BLS) Low energy extension infill & fluorescence telescopes (AMIGA+HEAT) Wide area wireless LAN system (Comms) – 1200 bits/sec per station Auger South Quick Facts

5. Auger South Science Highlights 27 Events of November 2007 And more events keep coming 5 5Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation Observed GZK feature in the spectrum Observed anisotropic sky >60 EeV Showed that GZK sphere does have sources Find puzzling composition (or new physics?) at ~40 EeV (FD) Problem: Auger South is not big enough ~25 events/yr > 60 EeV with Surface Detector ~2 events/yr > 60 EeV with Fluorescence Detector Science, November 2007

6. Solution: Auger North 6 6Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation 7x larger than Auger South allowing: Discovery of the UHECR sources using: Much higher statistics > 60 EeV (trans-GZK) Full sky distribution of events > 60 EeV Probing >350 TeV physics scale via: Determining the primary composition > 60 EeV astrophysically Measuring shower properties (with help of FD) Detecting UHE neutrinos and photons

7. Auger North Layout 20,000 km 2 4,000 WCDs on √2-mile (2.3 km) square grid. 10% additional in-fill on 1-mile (1.6 km) grid (+400 WCDs) 39 FD telescopes at 5 buildings Permanent vertical lasers Basic technologies follow successful Auger South designs Focused on energies > 3 x10 19 eV 7 7 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

8. AN Instrumentation Challenges 8 8Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation 7x larger size Focus on higher energies than AS Increase SD station dynamic range Sparsify SD and FD to minimize cost Improve atmospheric monitoring Reduce cost per station Reduce # PMTs from 3 to 1 per SD station Simplify FD buildings Colder climate Insulate the WCD tanks More contention for the radio spectrum Use dedicated bands provided by the U.S. government Terrain not as wireless communications friendly Develop new network paradigm Advances in technology Lower power operation Faster sampling of signals Higher comms bandwidth (2400 bits/sec per station)

9. FD R&D for Auger North at Auger South HEAT enhancement serves as major FD R&D for Auger North in shutters, cost saving buildings, new electronics 9 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation High efficiency PMTs Same gain as Photonis XP3062 used in AS Similar dimension Slightly worse after-pulsing & dark current But 35% versus 27% QE Improvements to HV/LV distribution Faster sampling rate & fewer electronics boards

10. R&D at Auger North Lamar Community College – Outreach and support Prowers County building – R&D headquarters WCD’s COMMs only Auger North R&D at the Colorado Site 10 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

11. AMT Laser/ LIDAR Laser/LIDAR 355 nm Laser Raman Detector (L’Aquilla) 38.8 km 8 km AMT 3.8m 2 mirror 4 columns of 16 1 degree pixels External Trigger from GPS (NAILS-Lite) Atmospheric Monitoring 9 Distant Laser Facilities (DLFs) Calibration & Monitoring Additions Nitrogen Automated Independent Laser System (NAILS) at each FD station FD Atmospheric Monitoring & Calibration 11 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

12. SD Station Overview 12 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

13. SD WCD Tank Modifications Auger North tank: Roto-molded polyethylene 1 PMT must be insulated 3 options for insulation are being pursued: Internal molded-in insulation Internal sheets of insulation installed afterwards External sprayed on insulation Thermal studies on tanks in Lamar (also outreach) and Malargue. Red dots are temperature probes in and around tanks. 13 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

14. SD Station PMT and Electronics 14 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation Higher energy focus requires extending SD station dynamic range Studies have been done with Photonis XP1805 9” PMTs used in Auger South Looks promising to extend dynamic range to >20 bits using deep dynode(s) Now re-doing the work with comparable PMTs from remaining PMT vendors Hammamatsu R5912mod ET Enterprises 9354 Prototype front-end board Prototype DAQ board HV Anode – 3 gains 1 deep dynode Additional dynodes possible Atmel 91rm9200 ARM CPU 3 dual LTC2280 100 MHz ADCs Altera Cyclone III FPGA

15. 15 Auger North Data Communications Issues Auger North is bigger than Auger South Factor of 7 in land area Auger South terrain is very comms friendly Array area is remarkably flat Surrounded by hills Clear lines-of-sight to towers Auger North site is not nearly so friendly No convenient big hills on the periphery Many annoying little hills, ridges, and gullies in the interior Line-of-sight can be difficult But RF spectrum issues are better Radios will operate 4.65-4.70 GHz band Avoids conflict with other users Springfield Lamar Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

16. 16 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation Communications System Components V2 prototype radio board V3 prototype radio board Altera Cyclone III FPGA Baseband signal processing 2 Embedded NIOS2 CPUs TMS470 “channel guardian” CANbus interface Integrated 2.45 GHz transceiver Altera Cyclone III FPGA Baseband signal processing 2 Embedded NIOS2 CPUs TMS470 “channel guardian” CANbus interface RF daughter card (not shown) 4.65 GHz dedicated bands 2.45 GHz for initial tests Prototype 4.65 GHz ~10 dBi omni antenna

17. 17 Terrain Solution: WAHREN (Wireless Architecture for Hard Real-time Embedded Networks) Auger North uses 2 nd Order Power chains Advantage: tolerant of single node failures Start with a basic chain – nearest neighbor communications only Extend RF range to reach second-nearest neighbors 1 2 3 4 5 6 7 8 9 10 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

18. 18 – Gentle curves are no problem – But what about sharp corners? – We introduce a Mobius fold – Existence of Mobius fold is transparent to the topology 7 8 9 10 7 8 9 Turning Corners 1 2 3 4 5 6 Mobius Fold Must be Prevented by Protocol Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

19. 19 Systolic Broadcast Protocol Unidirectional Single-Source Broadcast: – Window 0: Node 0 originates a message – Window w: Node w forwards node 0’s message Redundancy: Node Red. & Path Red. & Time Red. = 2 Unidirectional Multi-Source Broadcast – Window 0: All nodes originate a message – Window w: Node k forwards node (k-w)’s message 0 Win-2 Win-1 Win-0 Win-4 Win-5 Win-3 1 264 35 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

20. 20 Auger North Comms Topology Array is partitioned into “service areas” – Each served by one Concentrator Station Each Service Area is partitioned into “sectors” – May be triangular, rectangular, or quite irregular Service Area Sector Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

21. 21 Comm. Sequence in One Sector 1.41 mi array is a square array tilted 45 degrees – Each adjacent pair of row or columns forms a 2 nd order power chain – Can be organized into Backbones & Sidechains – Intersecting at Mobius Folds Side Chains Backbone Concentrator Station Fiber to Campus PC Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

22. 22 Dynamic Rerouting A 2 nd Order Chain Is tolerant of distributed single faults But can be broken by 2 adjacent faults In that case, the system can reroute through nearby nodes Decision is made by local neighboring nodes, in real-time Hence the name “Dynamic Rerouting”. 1 2 3 4 5 6 7 8 9 10 3 4 5 6 7 8 9 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation

23. 23 Instrumentation for the Northern Site of the Pierre Auger Observatory 12th Vienna Conference on Instrumentation