Outline

1. DUSEL Experiment Development and Coordination (DEDC)Internal Design ReviewJuly 16-18, 2008Steve Elliott, Derek Elsworth, Daniela Leitner, Larry Murdoch, Tullis C. Onstott and Hank Sobel

2. Outline • Introduction - DEDC, who, what, why, when • Physics Experiments • Science Themes • Superset of ISExperiments • Biology-Geoscience-Engineering Experiments • Science Themes • Superset of ISExperiments • PHYS-BGE Linking Themes • Science Themes • Superset of ISExperiments • Summary

3. The Path Ahead – ISE Preparation Timetable Anticipated October July 16 2008 Anticipated December

4. Physics Experiments at DUSEL • Long Baseline Neutrino Beam/Nucleon Decay • Dark Matter • Neutrino-less Double Beta Decay • Solar Neutrinos • Nuclear Astrophysics • Energetic particle effects Exploratory programs • Gravity Waves • 1- km Vertical Space

5. Three Neutrino Picture The physical neutrino eg. nm is a mixture of eigenstates such that: nm = Um1n1 + Um2n2 + Um3n3etc. MNS Maki-Nakagawa-Sakata mixing matrix Flavor States Mass eigenstates 3 independent parameters + 1 complex phase q12, q23, q13, d

6. Remaining Questions Small ne allowed Solar ~7.9x10-5ev2 m1 Atmospheric ~2.5x10-3eV2 Atmospheric ~2.5x10-3eV2 Solar ~7.9x10-5ev2 • Mass hierarchy? • How small is q13? • CP Violation? • Absolute mass scale? • Dirac or Majorana? LB-L bb

7. Neutrino Beam From Fermilab(Strongly indorsed by P5) NUMI/MINOS 1300km To DUSEL NUMI/HOMESTAKE New Target Hall, Shaft, and Service Building

8. Long Baseline Physics Program Why DUSEL? Can probe remaining unknown neutrino parameters. • Neutrino interactions in the Earth probe the hierarchy. Need long travel distance 1300 km distance offers a significantimprovement. • CP violation may be observable with intense neutrino and anti-neutrino beams. • CP violation may explain matter/anti-matter asymmetry of the Universe Rates are low, need very large detectors. • Large detectors and great depth allows additional rich physics program. Nucleon decay, Relic supernovae detection, Solar neutrinos

9. Water Cherenkov/Liquid Argon LAANDD: modular cubic evacuated Super-Kamiokande 50,000 ton Water Cherenkov Detector in Japan Too small, too close (295 km) • Scale existing water detector up to >100kt modules • Initial Argon proposal is for 5kt • Staged approach investigating development issues • Triggering, purification, TPC design, vessel design, electronics, depth

10. Sensitivity q13 Hierarchy CP Violation Initial sensitivity of 100 kt water detector The DUSEL 100kt detector is almost an order of magnitude better than NOnA for mass hierarchy determination for same running. Additionally, High Precision (~1%) Measurement of Sin22q23, dm223 with Muon CC Events

11. S-4 Issues / Facility Needs Most important is identifiable rock mass for excavation. This information drives the designs. Need coring & engineering. For LAr: Risk analysis for underground siting. Ventilation Controlled release studies Freeze-thaw mitigation Egress plan Vessel/cavern configuration For Water: Shape and size optimization Geo-textile design PMT size/number optimization PMT pressure testing PMT mounting Top down power estimate for water detector- First module: 50,000 channels at 10 W/channel, plus 40% for HVAC and 20% other power, for total of 840kW.

12. The Direct Detection of Dark Matter

13. Breakthroughs in cosmology have transformed our understanding of the Universe. • Spiral galaxies • rotation curves • Clusters & Superclusters • Weak gravitational lensing • Strong gravitational lensing • Galaxy velocities • X rays • Large scale structure • Structure formation • CMB anisotropy: WMAP Evidence for Dark matter now overwhelming – amount becoming precisely known

14. Despite this progress, the identity of dark matter remains a mystery • Constraints on dark matter properties the bulk of dark matter cannot be any of the known particles. • One of the strongest pieces of evidence that the current theory of fundamental particles and forces, is incomplete. • Because dark matter is the dominant form of matter in the Universe, an understanding of its properties is essential to attempts to determine how galaxies formed and how the Universe evolved. • Dark matter therefore plays a central role in both particle physics and cosmology, and the discovery of the identity of dark matter is among the most important goals in basic science today.

15. Experimental Challenges TheoreticalModels Xe or Ge rate(Ar ~1/5 rate/mass) Existing Limits Pre DUSEL Goal 1 evt/10 kg/month 4850ft DUSEL Goal 7400ft DUSEL Goal 1 evt/1 ton/month 1 evt/10 ton/month In many supersymmetric models, the lightest supersymmetric particle is, stable, neutral, weakly-interacting, mass ~ 100 GeV. All the right properties for WIMP dark matter! Overall expected rate is very small • Large low-threshold detector to discriminate against various backgrounds. • WIMPs and neutrons scatter off nuclei. • Photons scatter off electrons. • Minimize radioactive contamination. • Minimize external incoming radiation. • Deep underground location The WIMP “signal” is a low energy (10-100 keV) nuclear recoil.

16. Dark Matter Working Group (DMWG)Co-Chairs: Akerib, Gaitskell + Sadoulet Candidate Experiments For list of groups associated with each experiment see presentations posted at http://dmtools.brown.edu/DMWiki/index.php/DMWG_DUSEL_Lead_Meeting_080424

17. Double Beta Decayrequires massive Majorana neutrinos 1-tonne Ge EXO At least one neutrino has a mass >50 meV. These experiments will have a sensitivity below 50 meV. • Two detectors proposed for DUSEL: EXO and GERDA/MAJORANA, which use isotopes of 136Xe and 76Ge with very different and complementary techniques. More than one experiment is required because: • backgrounds are different • possible gamma lines will not produce false detection in multiple isotopes • Nuclear matrix elements are different for different isotopes • The underlying physics of neutrinoless double beta decay can only be elucidated by studying more than one isotope

18. Solar Neutrinos Is 13 different from zero? Time dependencies in the Sun’s opacity or energy production? Is there a subdominant energy source in the sun? Is the MSW mechanism correct? Do nuclear reactions fully account for the Sun’s energy output today? LENS 125 t Liquid scint. 10 t In Scintillation readout 10 tons for CC study CLEAN Liquid Ne Scintillation readout 10 tons for pp search eBubble 40-atm Ne gas Low-E track readout S4 proposal for prototype 20 tons for pp search

19. Accelerator Laboratory for Nuclear Astrophysics (ALNA) Collaborators Matthaeus Leitner LBNL Paul Vetter LBNL Peggy McMahan LBNL Daniela Leitner LBNL Damon Todd LBNL Ani Aprahamian Notre Dame Philippe Collon Notre Dame Manoel Couder Notre Dame Joachim Goerres Notre Dame Francesco Raiola Notre Dame Daniel SchuermannNotre Dame Ed Stech Notre Dame Michael Wiescher Notre Dame Xiao-Dong Tang Notre Dame Jose Alonso Sanford Lab Arthur ChampagneUNC Claudio Ugalde UNC Michael Famiano WMU Peter Parker Yale International interest Pietro Corvisiero INFN Genova, IT Paulo Prati INFN Genova, IT Heide Costantini INFN Genova, IT Lucio Gialanella Naples, IT Gianluca Imbriani Naples, IT Christina Bordenau HH-NIPNE, RO Two accelerators 400 kV CLAIRE350 kV-3 MV (Dynamitron, other option being studied) ECR ion source for extended energy range (1MeV/u) Energy overlap allows to consistently measure cross section over a wide energy range and allow reliable extrapolations Address a wide range of nucleosynthesis cross sections Flexibility would make it a unique facility world wide S-4 500k$/year for 3 years ISE Project cost 20-30 M$

20. ScienceStellar evolution, Origin of Elements, Stellar Neutrino Sources, Nucleosynthesis 10 Si-ignition O-ignition Ne-ignition 9 C-ignition log (Tc) He-ignition 8 H-ignition 7 0 2 4 4 6 8 10 log (c) Challenge: Reaction rates at stellar energy are tiny, Extrapolation carry substantial uncertainties Underground Shields cosmic ray backgrounds Unprecedented beam intensities will allow to push level of accuracy • Proposed initial experiments • 3He()7Bestringent benchmark of the facility • Constrain “invisible energy production” • Constrain solar metallicity and temperature Determines solar neutrino flux measured by current and proposed neutrino oscillation experiments Neutron sources Large uncertainty in s-process element production and subsequent nucleosynthesis e.g. 22Ne(,n)25Mg, 25Mg(,n)28Si… • Cannot be addressed in the LUNA facility

21. Astrophysics facility requirements • Facilities Underground (4850 ft level) Standard Experimental Cavity of 45x20x20m3, low background rock, external shielding • 2 Accelerators with energy overlap (50keV to 3MeV), auxiliary beams lines and power supplies • Experimental hall, control area, counting area • Target preparation and low background counting • Utilities • Power estimate about 500 kW • SF6 storage, LCW Cooling water, Cryogenic equipment/cryogenics • Climate control of the cave environment (humidity) • Above ground areas • Machine shop area • Above ground office space and counting areas • Laboratory space for general use (experiment and target preparation, detector testing)

22. Science: Low Background Counting A Dedicated Facility for the Assay, Control, and Production of Low Radioactivity Materials has been recognized as an essential shared task from the beginning of the DUSEL process. Facility will need to be defined and supported by the various experiments S-4 Process will further define the facility

23. Exploratory ISE proposals 1km Vertical Space Extensive feasibility studies are still to be done • Gravity Wave Exploring 1-Hz region (outside the LIGO frequency band) of gravitational waves (merger of white dwarfs and massive black hole) • Why Underground? Seismic noise and gravity gradient noise are among the major obstacles for reaching 1-Hz scale. Unique vertical Laboratory space • Evacuated tube required • NNbar Collaboration • Gravity waves by Atomic Interferometry • Mirror Matter Transition Search • Study of Diurnal Earth rotation • 1km Vertical Space (clean room and climate control required) • Facility for physics of Cloud Formation

24. Final Thoughts – The Physics program is very rich and requires a deep underground laboratory • DUSEL is a vital component of a continuing neutrino program. • The distance from Fermilab and the depth make for a world-leading program. • The mega-tonne scale detector will significantly advance the search for nucleon decay and evidence for grand unification. • Dark Matter experiments are growing larger and more sensitive. DUSEL depth, space and infrastructure are necessary components in this program. • Double-beta decay experiments will be sensitive to the atmospheric neutrino mass scale. • Solar neutrinos provide a unique window into the Sun. • A Nuclear astrophysics underground accelerator experiment will help us to understand the origin of the elements.

25. ARMA-NSF-NeSS Workshop Biology-Geoscience-EngineeringScience Plan & Societal Imperatives • Resource Recovery • Petroleum and Natural Gas Recovery • In Situ Mining • HDR/EGS • Potable Water Supply • Mining Hydrology • Waste Containment/Disposal • Deep Waste Injection • Nuclear Waste Disposal • CO2 Sequestration • Cryogenic Storage/Petroleum/Gas • Site Restoration • Aquifer Remediation • Underground Construction • Civil Infrastructure • Mining • Underground Space • Secure Structures Both GeoHydrology and GeoMechanics Mainly GeoHydrology Mainly GeoMechanics

26. 4D - Experiments within a block of rock (~km-scale) at depth and at in situ temperature and stress. Access to fluids and gas with minimal contamination for molecular studies. Capabilities to characterize the rock block at multiple scales. Access to controlled energy sources. Proximal access to clean laboratory, fabrication facilities and unique technologies. Why DUSEL for BGE? Time, t Spatial scale, x,y,z Depth, z -> Ds; DT

27. BGE – Science Questions • Dark Life (Biology) • How deep does life go? • Do biology and geology interact to shape the world underground? • How does subsurface microbial life evolve in isolation? • Did life on earth originate beneath the surface? • Is there life on earth as we don’t know it? • Restless Earth (Geosciences) • What are the interactions among subsurface processes? • Are underground resources of drinking water safe and secure? • Can we forewarn of earthquakes? • Can we view complex underground processes in action? • Ground Truth (Geoengineering) • What lies between boreholes? • How can technology lead to a safer underground? • How do water and heat flow deep underground?

28. The Path Ahead - Initial Suite of Experiments, Bio-Geo-Eng • Baseline characterization (NSF-SGER: no S-4) Larry Stetler (SDSMT), Cynthia Anderson (BHSU) • Ambient rock deformation processes/Ambient flow, transport, biodiversity and microbial and geochemical activity/Ultra-deep biological observatory David Boutt (U Mass), Tom Kieft (NM Tech), Herb Wang (U Wisc) • Induced flow, transport and activity/Induced rock deformation Leonid Germanovich (Georgia Tech) and Eric Sonnenthal (LBNL) • Underground construction and mining Charles Fairhurst (UMN) and Joe Labuz (UMN) • CO2sequestration/Resource extraction Joe Wang (LBNL) and Jean-Claude Roegiers (U Oklahoma) • Subsurface imaging and sensing Steven Glaser (UC Berkeley)

29. Facility Needs - Summary Summary of Facilities and Infrastructure Active Processes Labs Fracture and Transport Lab Yates Ross 300 L Ambient Transport Fiber Optic Strain Network 2000L 3650L Ultra-deep Borehole Exploration borehole 4850L 7400L Relocatable sensing arrays 8000L ~16000+ LB Caverns Level

30. Ambient Behavior and Ultra-Deep Biological Observatory – Scale Effects Lab scale Field scale Regional scale 10-10 ? Permeability, m2 10-14 10-18 10-1 100 102 103 101 [e.g. Dershowitz, 2004] Spatial Scale, m

31. Compelling Research Questions Connecting Geomechanics, Geohydrology, and Geomicrobiology What controls deep life? • How do geomechanical, hydrologic, thermal and geologic conditions control the distribution of life in the deep subsurface? • How do those factors control microbial diversity, microbial activity and nutrients? • How do state variables (stress, strain, temperature, and pore pressure) and constitutive properties (permeability, porosity, modulus, etc.) vary with scale (space, depth, time) in crystalline rock?

32. Proposed Experiments • Ultra-deep Drilling • What factors control the distribution of life as functions of depth, temperature, and rock type? • What are the patterns in microbial diversity, microbial activity and nutrients as a function of depth? • Scale Effects Experiment (SEE) • How are stress state and strength related to geologic heterogeneity and anisotropy, fracture geometry, the pressure and flow of fluids? • How do the fracture network, stress state, and constitutive properties of crystalline rocks affect the stability of tunnels, shafts, wellbores, and large, room-sized excavations? • Dark Flow • What controls porosity and permeability with depth in crystalline rock? • What are the characteristics of fracture networks that conduct water? • Do patterns of microbial diversity reflect connectivity of fractures (e.g. can microorganisms be used as a new type of particulate tracer)? • 4-D Hydromechanical Simulator • To synthesize observations for site selection of cavern construction, borehole locations, and bioaugmentation/biostimulation experiments.

33. An Overarching Hypothesis: Fluid flow in a rock mass can be predicted if both the stress field and the fracture network are characterized at a range of spatial scales. • What is the stress state and are some fractures critically stressed? • How is the transmissivity of fractures affected by stress state? • How have mining excavations altered the stress field and hydrology? • How does stress state affect stability of tunnels, shafts, wellbores, and large, room-sized excavations? • How do the stress and flow environment affect microbial identity, activity, and diversity?

34. Induced Displacements Due to Dewatering K: 5E-10 m/s

35. Conceptual diagram of fiber-optic displacement sensor network Distributed Strain and Temperature (DST) measurements can be made over kilometers of distance in the mine. However, development work must be done to establish clamping techniques to the rock mass and compared with fiber-optic displacement sensors, such as those shown in the figures.

36. Induced Flow, Transport and Activity/Induced Rock DeformationThe Active Processes Laboratory • Objective - to evaluate how • Fractures propagate and deform during fluid flow and changes in stress in rock • Faults initiate, heal, seal, and reactivate • Fractures interact to create networks • Scaling laws can apply to rock fracture processes • Heat, mass, and microbes are transported through fractures and the adjacent rock matrix • Chemical and microbially-mediated reactions are controlled by heat and mass transport • New technologies can improve the imaging of fractures and faults • Why is DUSEL the best or only place this experiment can be done? Objectives can only be achieved by manipulating in situ conditions at large scales and depths, and then directly observing results. Such experiments require • Substantial and specialized sub-surface infrastructure over many years • Excavating host rock in the vicinity of created faults and fractures • Expected results and their significance • Improved understanding of seismicity • Advanced understanding of fractures and fracture networks • Why is it important to do these experiments in the near future? • public safety • water supply • hydrocarbon production and geothermal energy recovery • waste remediation and disposal • CO2sequestration and climate change

37. FRACTURE PROCESSES LAB Create fractures in highly instrumented setting to characterize deformation processes, then use for transport experiments

38. Example: FAULT EXPERIMENT s1 Approach Utilize large, natural in-situ stresses – currently, the only option Create failure by reducing existing load s1 t s3 s3 s1

39. Ds3 s1 Concept • Create a pair of parallel lines of boreholes or slots normal to s3 • Cooling by DT reduces s3 and allows controlled modification of stress state between lines • Reduce s3 between boreholes until failure occurs s3

40. Fault experiments at 300 ft level s1 Ds3 Cooling s3

41. Fault experiments at 300 ft level s1 t s1 s3 Heating Fracture surface

42. SUITE OF EXPERIMENT – RUPTURE & TRANSPORT • Fracture propagation • Fluid flow in networks • Deformation of fractures • Faulting • Scaling of fracture energy • Transport and geochemical reactions in fractures • Pressure solution at fracture asperities • Hydrothermal convection - permeability changes from mechanical and chemical processes • Microbiological processes during fracturing

43. Relation to Some DOE Grand Challenges Focus Areas • Multiphase fluid transport in geologic media • Chemical migration processes • Subsurface characterization • Modeling and simulation of geologic processes Grand Challenges • Computational Thermodynamics of Complex Fluids and Solids • Integrated characterization, modeling and monitoring of geologic systems • Simulation of multi-scale systems for ultra long times Priority Research Directions • Mineral-water interface complexity and dynamics • Nanoparticle and colloid physics and chemistry • Dynamic imaging of flow and transport • Transport properties and in situ characterization of fluid trapping, isolation and immobilization • Fluid-induced rock deformation • Biogeochemistry in extreme subsurface environments [DOE, BES, 2007]

44. Underground Construction & MiningScale Effects in Geomechanics – Space and Time [Elsworth and Fairhurst, NSF-S1, 2007] [Fairhurst, 2004] [Courtesy: C. Fairhurst]

45. Science Objectives: 1. Fully integrate knowledge into the design and construction of a cavern 2. Develop methods of ground control to accommodate the large cavity design – e.g. control fracture of rock through preconditioning and blasting studies Why DUSEL? Large in-situ stress, fractured rock mass, and large scale excavation

46. Proposed Experiments (Describe A+ Experiments in multiple slides: maybe 1 to 5 slides) Cavern Design • Predesign • Construction including mitigation for stresses • Long-term performance

48. Towards a Transparent Earth S.D. Glaser, UC, Berkeley W. Roggenthen, SDSMT L.R. Johnson, E.L. Majer, LBNL Install an acoustic “microscope” surrounding the Homestake workings – 1st NSF funded DUSEL research signal Deep is Quiet, and Quiet is Good noise • Develop deep in-situ seismic observatory for rapid imaging of dynamical geo-processes at depth. • Provide rock mass dynamics and safety information to miners and tunnelers • Provide an infrastructure for all earth scientists • Improve ability to detect and characterize underground structures and activity

49. Seismic Imaging of Subsurface Stress • The time-varying stress field at depth is perhaps the most crucial parameter for understanding the earthquake triggering process. • The Speed of Seismic Waves is a Measures of Stress in Rocks. This holds at seismogenic depth and can be used as a “stress meter”. Why at Homestake? Stress changes at seismogenic depth could be more difficult to observe with conventional surface instruments. Temperature variation at surface is a large noise source in the electronics. Deep observation could avoid surface environmental effects, such as precipitation. Need a deep natural experiment site that bridges laboratory study and large scale seismic experiment. FenglinNiu, Rice University P. G. Silver, Carnegie Institution of Washington T. Daley, Lawrence Berkeley National Lab

50. PHYS-BGE Linking Themes • Geoneutrinos [GRAFG] • Whole body counting [NORM] • Cross-cutting Applications [CCA] • Petrology, ore deposits and structure [PODS]