Long-Baseline Neutrino Experiment James Strait LBNE Project Director Public Information Meetings June 25-26, 2013 LBNE-doc-7321

What are neutrinos? LBNE Public Information Meeting -- June 25-26, Neutrinos are particles with no electric charge and almost no mass. They are among the most abundant particles in the universe. They are produced in great quantities by the sun and other stars, in the earth, by cosmic ray interactions in the atmosphere. Trillions of neutrinos pass through your body each second. Neutrinos hardly ever interact – a typical neutrino could travel through more than 100 million miles of lead unscathed. There are three (known) types of neutrinos: electron neutrinos, muon neutrinos and tau neutrinos. Once produced, they can change (“oscillate”) from one type to another and then back again.

Why are neutrinos important? Neutrinos play an important role in natural processes that are crucial to why we exist. The reactions in the core of the sun. The explosions of supernova stars in which the heavy elements are created and expelled into space to form planets and provide the building blocks for life. Small differences between neutrinos and their anti-particle counterparts could help explain why more matter than anti- matter was produced in the Big Bang. Understanding if neutrinos behave differently from anti- neutrinos is one of the main goals of LBNE. Because neutrinos hardly interact, they can tell us what happens in places we cannot “see” otherwise: In the core of the sun In the center of a supernova at the moment it explodes. LBNE Public Information Meeting -- June 25-26,

Why do we need a new neutrino experiment? Since we built MINOS a decade ago, we have learned many things about the properties of neutrinos. To learn more, we need to let the neutrinos and anti-neutrinos travel farther through the earth to understand how they oscillate. New detector technologies enable more precise measurements LBNE Public Information Meeting -- June 25-26,

LBNE Neutrino Beamline and Near Detector LBNE Public Information Meeting -- June 25-26, ft. 680 ft. not to scale

LBNE Neutrino Beamline LBNE Public Information Meeting -- June 25-26,

7 Far Detector at Sanford Underground Research Facility in the Black Hills of South Dakota Massive Liquid Argon Time Projection Chamber Detector – 19,000 tons 95’ 50’

Surface or Underground? The Department of Energy has given us a budget that allows us to build the detector on the surface. However, we would like to place the detector deep underground at SURF, to shield it against cosmic rays. ̶ Higher precision for the neutrino measurements ̶ Measure cosmic-ray produced neutrinos ̶ See neutrinos from a supernova (if one goes off during the lifetime of the experiment) ̶ Search for the decay of protons into lighter particles We are developing new partnerships, both domestic and foreign, which could provide the resources to move the detector underground. LBNE Public Information Meeting -- June 25-26,

9 Underground Detector Location 4550 ft not to scale

J.Strait, IOP 2013, 10 April Surface R&D facility MAJORANA Electroforming Lab 0.6 mi Majorana Demonstrator LUX Davis Campus Experiments LBNE Base of the Yates Shaft Sanford Underground Research Facility 4850 Level (4550’ depth)

LBNE Collaboration LBNE Public Information Meeting -- June 25-26, collaborators, 63 institutions, 5 countries Fermilab, March 2013 AlabamaArgonneBostonBrookhavenCambridgeCataniaColumbiaChicagoColorado Colorado State Columbia Dakota State DavisDrexelDukeDuluthFermilabHawaii Indian Universities Indiana Iowa State Irvine Kansas State Kavli/IPMU-Tokyo Lawrence Berkeley NL Livermore NL London UCL Los Alamos NL Louisiana State Maryland Michigan State Minnesota MITNGA New Mexico Northwestern Notre Dame OxfordPennsylvaniaPittsburghPrincetonRensselaerRochester Sanford Lab SheffieldSLAC South Carolina South Dakota South Dakota State SDSMT Southern Methodist SussexSyracuseTennessee Texas, Arlington Texas, Austin TuftsUCLA Virginia Tech Washington William and Mary WisconsinYale