Baseline Optimization Studies D. Reyna Argonne National Lab.

Slides:

Advertisements

Similar presentations

Oscillation formalism

Advertisements

Happiness comes not from material wealth but less desire. 1.

MINOS+ Sterile Neutrino Studies J.Thomas UCL J.Evans (UCL), A.Gavrilenko (W&M), M.Matthis (W&M)A.Sousa(Harvard) UCL.

Neutrinos Louvain, February 2005 Alan Martin Arguably the most fascinating of the elementary particles. Certainly they take us beyond the Standard Model.

Atmospheric Neutrinos Barry Barish Bari, Bologna, Boston, Caltech, Drexel, Indiana, Frascati, Gran Sasso, L’Aquila, Lecce, Michigan, Napoli, Pisa, Roma.

Midwest critical mass 2010 Measurement of two-particle correlations in pp collisions at sqrt(s) = 900 GeV as well as at sqrt(s) = 7 TeV with ALICE The.

Takaaki Kajita ICRR, Univ. of Tokyo Nufact05, Frascati, June 2005.

Sinergia strategy meeting of Swiss neutrino groups Mark A. Rayner – Université de Genève 10 th July 2014, Bern Hyper-Kamiokande 1 – 2 km detector Hyper-Kamiokande.

Measuring CP violating phase from long baseline neutrino experiments Naotoshi Okamura (YITP, Kyoto Univ.) ICFP2005 Oct. 07, NCU.

July 2001 Snowmass A New Measurement of  from KTeV Introduction The KTeV Detector  Analysis of 1997 Data Update of Previous Result Conclusions.

Cosmic Induced Backgrounds D. Reyna Argonne National Lab.

Error Propagation. Uncertainty Uncertainty reflects the knowledge that a measured value is related to the mean. Probable error is the range from the mean.

Blessed Plots 2005 The current set of Blessed plots available from the MINOS website are taken from the 5 year plan exercise that occurred in mid-2003.

1 Beam e ’s from antineutrinos using the pME and LE beams David Jaffe, Pedro Ochoa December 8 th 2006  Part 1: Reminder and update  Part 2: Change in.

1 CC analysis update New analysis of SK atm. data –Somewhat lower best-fit value of  m 2 –Implications for CC analysis – 5 year plan plots revisited Effect.

An Alternate Perspective Most development on ton detectors –~500 GW-ton-years –Systematics limited for rate measurement Lots of thought about systematics.

Atmospheric Neutrino Oscillations in Soudan 2

Shoei NAKAYAMA (ICRR) for Super-Kamiokande Collaboration December 9, RCCN International Workshop Effect of solar terms to  23 determination in.

1 Super-Kamiokande atmospheric neutrinos Results from SK-I atmospheric neutrino analysis including treatment of systematic errors Sensitivity study based.

1 The Daya Bay Reactor Electron Anti-neutrino Oscillation Experiment Jianglai Liu (for the Daya Bay Collaboration) California Institute of Technology APS.

Recent Results from Super-Kamiokande and Sudbury Neutrino Observatory R. D. McKeown California Institute of Technology January 17, 2004 IHEP Beijing.

© 2002 Thomson / South-Western Slide 8-1 Chapter 8 Estimation with Single Samples.

Solar neutrino measurement at Super Kamiokande ICHEP'04 ICRR K.Ishihara for SK collaboration Super Kamiokande detector Result from SK-I Status of SK-II.

Caren Hagner CSTS Saclay Present And Near Future of θ 13 & CPV in Neutrino Experiments Caren Hagner Universität Hamburg Neutrino Mixing and.

The Earth Matter Effect in the T2KK Experiment Ken-ichi Senda Grad. Univ. for Adv. Studies.

Monday, Feb. 24, 2003PHYS 5326, Spring 2003 Jae Yu 1 PHYS 5326 – Lecture #11 Monday, Feb. 24, 2003 Dr. Jae Yu 1.Brief Review of sin 2  W measurement 2.Neutrino.

Using Reactor Anti-Neutrinos to Measure sin 2 2θ 13 Jonathan Link Columbia University Fermilab Long Range Planning Committee, Neutrino Session November.

Sterile Neutrino Oscillations and CP-Violation Implications for MiniBooNE NuFact’07 Okayama, Japan Georgia Karagiorgi, Columbia University August 10, 2007.

Karsten M. Heeger US Reactor  13 Meeting, March 15, 2004 Comparison of Reactor Sites and  13 Experiments Karsten Heeger LBNL.

Sensitivity to New Physics using Atmospheric Neutrinos and AMANDA-II John Kelley UW-Madison Penn State Collaboration Meeting State College, PA June 2006.

Basic Business Statistics, 11e © 2009 Prentice-Hall, Inc.. Chap 7-1 Developing a Sampling Distribution Assume there is a population … Population size N=4.

The NOvA Experiment Ji Liu On behalf of the NOvA collaboration College of William and Mary APS April Meeting April 1, 2012.

Wednesday, Feb. 14, 2007PHYS 5326, Spring 2007 Jae Yu 1 PHYS 5326 – Lecture #6 Wednesday, Feb. 14, 2007 Dr. Jae Yu 1.Neutrino Oscillation Formalism 2.Neutrino.

Kr2Det: TWO - DETECTOR REACTOR NEUTRINO OSCILLATION EXPERIMENT AT KRASNOYARSK UNDERGROUND SITE L. Mikaelyan for KURCHATOV INSTITUTE NEUTRINO GROUP.

New Results from the Salt Phase of SNO Kathryn Miknaitis Center for Experimental Nuclear Physics and Astrophysics, Univ. of Washington For the Sudbury.

Search for Electron Neutrino Appearance in MINOS Mhair Orchanian California Institute of Technology On behalf of the MINOS Collaboration DPF 2011 Meeting.

Performance Comparisons of Safeguard Detector Designs D. Reyna (Argonne National Laboratory) with help from R.W. McKeown (Drexel University)

Ralf Averbeck Stony Brook University Hot Quarks 2004 Taos, New Mexico, July 19-24, 2004 for the Collaboration Open Heavy Flavor Measurements with PHENIX.

Preliminary results for the BR(K S  M. Martini and S. Miscetti.

Optimizing the green-field beta beam NuFact 08 Valencia, Spain June 30-July 5, 2008 Walter Winter Universität Würzburg.

Search for Sterile Neutrino Oscillations with MiniBooNE

Karsten Heeger Beijing, January 18, 2003 Design Considerations for a  13 Reactor Neutrino Experiment with Multiple Detectors Karsten M. Heeger Lawrence.

Double Chooz Near Detector Guillaume MENTION CEA Saclay, DAPNIA/SPP Workshop AAP 2007 Friday, December 14 th, 2007

Jun Cao Jan. 18, 2004 Daya Bay neutrino experiment workshop (Beijing) Detector Module Simulation and Baseline Optimization ● Determine module geometric.

Daya Bay Reactor Neutrino Experiment On behalf of the DayaBay collaboration Virginia Polytechnic Institute and State University Joseph ykHor YuenKeung,

Measuring  13 with Reactors Stuart Freedman HEPAP July 24, 2003 Bethesda Reactor Detector 1Detector 2 d2d2 d1d1.

2005 Unbinned Point Source Analysis Update Jim Braun IceCube Fall 2006 Collaboration Meeting.

CP phase and mass hierarchy Ken-ichi Senda Graduate University for Advanced Studies (SOKENDAI) &KEK This talk is based on K. Hagiwara, N. Okamura, KS PLB.

A monochromatic neutrino beam for  13 and  J. Bernabeu U. de Valencia and IFIC NO-VE III International Workshop on: "NEUTRINO OSCILLATIONS IN VENICE"

Sensitivity to New Physics using Atmospheric Neutrinos and AMANDA-II John Kelley UW-Madison IceCube Collaboration Meeting Baton Rouge, LA April 10, 2006.

News from the Sudbury Neutrino Observatory Simon JM Peeters July 2007 o SNO overview o Results phases I & II o hep neutrinos and DSNB o Update on the III.

Neutrino physics: The future Gabriela Barenboim TAU04.

1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.

PHENIX J/  Measurements at  s = 200A GeV Wei Xie UC. RiverSide For PHENIX Collaboration.

Referee Report on Open charm production results for summer conferences, 2010 Peter Clarke Marcel Merk “Observations” and “Comments” The referees thank.

IBD Detection Efficiencies and Uncertainties

Donato Nicolo` Pisa University & INFN,Pisa

Jim Marie Advisor: Richard Jones University of Connecticut

Observation of Diffractively Produced W- and Z-Bosons

 Results from KTeV Introduction The KTeV Detector

High g Li/B b-Beam Enrique Fernández-Martínez, MPI für Physik Munich

T2KK sensitivity as a function of L and Dm2

T2KK Sensitivity of Resolving q23 Octant Degeneracy

f  K+K- analysis in Run4 Au+Au collisions

T2KK (without reactor) solves 8-fold degeneracy

Daya Bay Neutrino Experiment

Naotoshi Okamura (YITP) NuFact05

Determination of Neutrino Mass Hierarchy at an Intermediate Baseline

Fitting Systematics Sensitivity of overall fitting to ratio fit

Observation of Diffractively Produced W- and Z-Bosons

Presentation transcript:

Baseline Optimization Studies D. Reyna Argonne National Lab

D. Reyna – Argonne National Lab2 1 May 2003 Some Basic Questions Does sensitivity to θ 13 survive under complete 3 flavor mixing? How can we best use all of the information in the energy spectrum? What are the optimal locations for 2 identical detectors? Bottom line: Can we achieve the desired sensitivity?

D. Reyna – Argonne National Lab3 1 May 2003 Independence of ∆m 2 solar atmospheric

D. Reyna – Argonne National Lab4 1 May 2003 Total Rate vs. Baseline E ν = 3.5 MeV Full Reactor Spectrum

D. Reyna – Argonne National Lab5 1 May 2003 Shape Comparison 1 km 100 m Make  2 Comparison Of Distributions Each bin normalized to total at that location Errors are statistical only

D. Reyna – Argonne National Lab6 1 May 2003  2 Comparisons Combined: Shape Test:  Minimizes Detector Specific Systematics  Loss of overall rate information  Assumes Identical Detectors  More Statistical Power

D. Reyna – Argonne National Lab7 1 May 2003 Optimizing 2 Locations  2 Identical Detectors  Fix 1 Detector Baseline  Sweep the Other

D. Reyna – Argonne National Lab8 1 May 2003 Optimizing 2 Locations (cont’d) 100m 500m 1km 1.5km2km

D. Reyna – Argonne National Lab9 1 May 2003 Statistical Power of Combined  2 Test Combined (stat only) Combined (+ 1% sys) Shape Only (stat only) Shape Only (+ 1% sys)

D. Reyna – Argonne National Lab10 1 May 2003 Secondary Maxima? Combined (stat only) Combined (+ 1% sys) Shape Only (stat only) Shape Only (+ 1% sys)

D. Reyna – Argonne National Lab11 1 May 2003

D. Reyna – Argonne National Lab12 1 May % Confidence Limits

D. Reyna – Argonne National Lab13 1 May 2003 Short and Long Solutions

D. Reyna – Argonne National Lab14 1 May 2003 Final Thoughts It is possible to get the desired sensitivity Optimal near detector location should be as close as possible A Detector should be at the first oscillation minimum (900 – 1400m) A farther location (~2.5km) yields almost as much statistical power  Could be effective if a very near detector is not possible  Possible 3 rd detector?