DUSEL 01 05

Deep Underground Science and Engineering Laboratory: 

Deep Underground Science and Engineering Laboratory Worldwide Demand & International Coordination Barry Barish Caltech University of Colorado Workshop Boulder, CO, January 4–7, 2005

My Perspectives: 

My Perspectives MACRO at Gran Sasso – 10 years of underground physics MINOS – Long Baseline Neutrinos NFAC – Neutrino Facilities Assesment Committee for the NAS/NRC (2002) NSB – National Science Board (MREFC Process for the NSF) (2002 – 2008)

Slide3: 

NFAC Neutrino Facilities Assessment Committee Barry Barish Chair 5-Nov-02 for National Research Council

Slide5: 

NFAC Membership

NFAC – Important Considerations: 

NFAC – Important Considerations NFAC is asked to address to what extent the science “can be addressed with existing, soon to be completed, or planned facilities around the world.” We had presentations at our meetings to try to understand the global context of the proposed U.S. initiatives. NFAC is asked to assess “the unique capabilities of each class of new experiments and any possible redundancy between these two types of facilities.” Our study and report are being developed with the full consideration of the recommendations in several recent reports: The NRC Report “Connecting Quarks and the Cosmos: Eleven Science Questions for the New Century,” The NSAC Long Range Report for Nuclear Physics The HEPAP Long Range Report for High Energy Physics

Why Deep Underground?: 

Why Deep Underground? A clean, quiet and isolated setting is needed to study rare phenomena free from environmental background. Such a setting can be obtained only deep underground, where we can escape the rain of cosmic rays from outer space. Why do neutrinos have tiny masses and how do they transform into one another? Are the existence and stability of ordinary matter related to neutrino properties? Are there additional types of neutrinos? What is the mysterious dark matter and how much of it is neutrinos? What role do neutrinos play in the synthesis of the elements in the periodic table? Is there a deeper simplicity underlying the forces and particles we see?

Conclusions: 

Conclusions Important future experiments on solar neutrinos, double beta decay, dark matter, long baseline neutrinos, proton decay, and stellar processes are being devised, proposed and discussed. We find that a common feature of the future experimentation in this field is the importance of depth. Most of the experiments envisaged require an overburden of about 4500 mwe or more. To optimize long baseline studies of neutrino oscillations, a new underground facility should be located at a distance greater than 1000 km from existing, high intensity proton accelerators. The breadth and quality of the potential future experimental program requiring an underground location suggests that there is a major opportunity for the United States if it can soon develop a large new underground facility with the ability to meet the requirements of the broad range of proposed experiments.

Deep Underground Laboratory: 

Deep Underground Laboratory Assessment: A deep underground laboratory can house a new generation of experiments that will advance our understanding of the fundamental properties of neutrinos and the forces that govern the elementary particles, as well as shedding light on the nature of the dark matter that holds the Universe together. Recent discoveries about neutrinos, new ideas and technologies, and the scientific leadership that exists in the U.S. make the time ripe to build such a unique facility.   It will require considerable strategic and technical guidance, in order to construct a deep underground laboratory expeditiously and in synergy with the research program. Critical decisions that are beyond the scope of this report remain: choosing between several viable site options, defining the scope of the laboratory, defining the nature of the laboratory staff and the management organization, the site infrastructure and the level of technical support that will be resident. Developing sound experimental proposals will require early access to deep underground facilities to perform necessary R&D. Therefore, it is important to complete the process of setting the scope and goals for the laboratory, soliciting and reviewing proposals, and building up the necessary infrastructure, in order to initiate the experimental program in a timely fashion.

The Science Prospects Underground : 

The Science Prospects Underground Neutrino Properties Solar Neutrinos Neutrino Oscillations Double Beta Decay Dark Matter Proton Decay etc These generally represent exciting and important identified areas of “inquiry” that typically lead to generations of investigations ----------- This should be contrasted with justifications in astronomy – an “observationally” based science

Solar n’s : the Birth of Neutrino Astrophysics: 

Solar n’s : the Birth of Neutrino Astrophysics The detection of neutrinos coming from the sun and from an exploding star, discoveries from underground experiments of the past decades, were recognized in the 2002 Nobel physics prize. Kamiokande - Koshiba Homestake - Davis 37Cl + ne  37Ar + e Solar Neutrinos Supernovae 1987a

The Sun as seen from SuperKamiokande deep underground: 

The Sun as seen from SuperKamiokande deep underground

SNO shows the deficit is due to neutrino flavor change or “neutrino oscillations” : 

SNO shows the deficit is due to neutrino flavor change or “neutrino oscillations” SNO

Reactor Neutrinos -- KamLAND: 

Reactor Neutrinos -- KamLAND Observe oscillation effects with terrestrial neutrinos Further determine the parameters of neutrino oscillations

Solar Neutrinos – The Future: 

Solar Neutrinos – The Future In the standard solar model the flux from the pp reaction is predicted to an accuracy of 1%. Further, the total flux is related directly to the measured solar optical luminosity. Such a copious and well-understood source of neutrinos is ideal for precisely determining the neutrino masses and mixings. It also affords a way to search for hypothesized sterile neutrinos as much as a million times lighter than those explored by present experiments, provided they mixed sufficiently with the active neutrinos. Unfortunately, the pp neutrinos have very low energies presenting an experimental and technical challenge

The Long Range – Solar Neutrinos: 

The Long Range – Solar Neutrinos Two types of experiment are required, both sensitive to the lowest-energy neutrinos. One experiment measures the electron-flavor component by the “charged-current” (CC) reaction The other measures a combination of electron, mu and tau neutrinos via elastic scattering from electrons (the ES reaction) Large background mitigation required, so deep sites are required. Several technologies being pursued – need underground testing XMASS – Liquid Xenon Clean – Liquid Neon

Atmospheric Neutrinos: 

Atmospheric Neutrinos      m  e  nm  ne Angular distribution of neutrino events yields neutrino rate vs path length

Angular distributions and deficit both consistent with neutrino oscillation hypothesis and with each other: 

Angular distributions and deficit both consistent with neutrino oscillation hypothesis and with each other

Long Baseline Neutrino Experiments: 

Long Baseline Neutrino Experiments

Neutrino Masses and Admixtures: 

Neutrino Masses and Admixtures Next generation neutrino oscillation experiments aim to determine the admixtures and mass differences but not their absolute scale. Experiments on the neutrinoless double beta decay would supply the crucial information on the absolute scale. The electron-type component mixed in the 3rd state, called q13, is not known The potential differences between neutrinos and antineutrinos are also unknown Two possible patterns The longer term future will involve determination of q13 and possibly measuring CP violation in the neutrino sector with another generation of long base line experiments

Acceleratorsneutrino factory – neutrinos from muon collider: 

Accelerators neutrino factory – neutrinos from muon collider muon collider neutrino beams select nm’s or anti nm’s Example 7400 km baseline CERN  DUSEL “world project”

Concept for Next GenerationProton Decay/Neutrino Oscillation Detector: 

Concept for Next Generation Proton Decay/Neutrino Oscillation Detector

Goals: Dirac or Majorana particle?: 

Goals: Dirac or Majorana particle? Ettore Majorana Majorana : The neutrino is its own antiparticle

DiracvsMajoranamass: 

Dirac vs Majorana mass Majorana mass is measured by double beta decay Use Nuclei stable under normal beta decay, but decay by a double weak interaction process. Changes charge two units Two neutrinos are emitted. If neutrinos have Majorana mass, a vertex with no external neutrinos is possible. Some models predict very low values for neutrinoless double beta decay, still allowing the physical masses of all neutrinos to be orders of magnitudes larger than the observed limit of effective Majorana mass. 2nbb 0nbbB 0nbb E1 + E2 (MeV)

Dark Matter – Direct Searches: 

Dark Matter – Direct Searches Will Require Going To A Deep Site Future Goals

Slide26: 

Andrew Hime

High Energy Cosmic Ray Spectrum: 

High Energy Cosmic Ray Spectrum protons heavy nuclei extra galactic GZK cutoff

INFN Gran Sasso National Laboratory: 

INFN Gran Sasso National Laboratory 1400 m rock overburden Flat cross-section Underground area 18 000 m2 Support facilities on the surface

Kamioka Observatory: 

Kamioka Observatory KamLAND (operated by Tohoku Univ.) Super-Kamiokande 1000 m rock overburden The mine is no more active Support facilities on the surface XMASS R&D Tokyo Dark Matter exp Plot type GW detectors 20m×20m 100m×100m (Cryogenic) 100m To mine entrance (1.8km from SK)

SNO Laboratory : 

SNO Laboratory 2000 m rock overburden Almost flat surface Support facilities on the surface Vertical access Main cavity ~10,000m3 Solar neutrino oscillation !

Slide31: 

SNO cavity + surface facilities Large Halls Small Halls

Exploiting the Future Opportunities: 

Exploiting the Future Opportunities The science is fantastic --- Some of our most fundamental questions appear within reach What is the dark matter? Is the neutrino its own antiparticle? Are baryons stable? What are the mechanisms for neutrino oscillations? Is there CP violation In the weak sector? etc. What will it take to exploit this science?

Background Suppression: 

Background Suppression A common theme to reach needed sensitivities Requires technological development Requires going deep underground But, how deep? It takes two miles of rock to absorb the most energetic of the muons created by cosmic ray protons striking the earth's atmosphere At such great depths, the only backgrounds are made by neutrinos (which easily penetrate the whole earth but, by the same token, interact very seldom) and by local radioactivity in the rock itself Some experiments do not require the greatest depths, while for other experiments there is no option but depth and extreme cleanliness.

Developing the Technologies: 

Developing the Technologies Almost all of the goals require challenging technological development and large increases in scale Dark matter --- larger scale, new technologies Double Beta Decay – larger scale, technological demonstrations Proton Decay / CP Violation with n’s – neutrino beam, distance, much larger scale, cost effectiveness Solar Neutrinos – background suppression, new technologies How do we organize the effort, resources, engineering, tests to develop the best technologies to enable reaching the science goals?

Does One Depth Suits All?: 

Does One Depth Suits All? Variation of the flux of cosmic-ray muons with overburden. The horizontal bar indicates the range of depths that would be available for experiments in a multipurpose underground laboratory.

Does One Laboratory Suits All?: 

Does One Laboratory Suits All? A new multipurpose underground laboratory should be able to provide a range of depths for experiments, allowing an optimized cost benefit for each experiment Would a distributed laboratory or set of underground experiments, each optimized for its own needs, with an overall coordinating management be a better solution?

Collaborations, Resources and a Coordinated Worldwide Program : 

Collaborations, Resources and a Coordinated Worldwide Program The scale and technical demands of the experiments that will confront the science goals will require – Ambitious technical development Large collaborations Significant resources Professional engineering Management To meet these demands poses many questions?

Collaborations, Resources and a Coordinated Worldwide Program : 

Collaborations, Resources and a Coordinated Worldwide Program More coordination and resources will be required, without inhibiting the variety of ideas and approaches New underground facilities will be needed – A next generation p decay experiment and/or n CP violation will require large new space and support deep underground Ultimate dark matter experiments will require (a) well supported deep site(s). etc. The New SNOLAB facilities will be only a partial answer

Final Thoughts - Questions: 

Final Thoughts - Questions The Worldwide Underground Program How can we increase level of the R&D toward future detectors? How can we set up mechanisms to coordinate and set priorities for large international initiatives? PaNAGIC?? How can we get the larger resources needed to reach the exciting science goals? U.S. Deep Underground Laboratory Initiative Should we propose a large multipurpose laboratory or a distributed laboratory? Should the huge proton decay / neutrino experiment be treated as the center piece or a possible option? What mechanisms can be put into place to bring the level of engineering and project management for large underground experiments up to “accelerator” standards?