ORCA with e J. Brunner. Step 1 Oscillation probabilities – Values from Fogli et al. (arxiv:1205.5254) –  23 =45˚ (avoid octant problem) – CP-phases :

Slides:



Advertisements
Similar presentations
V.L. Kashevarov. Crystal Collaboration Meeting, Edinburg,13-15 Sept Photoproduction of    on protons ► Identification of  p →  o.
Advertisements

P u t y o u r h e a d o n m y s h o u l d e r.
MINOS+ Starts April 2013 for three years April
The effect of turbulence upon supernova neutrinos Jim Kneller NC State University NOW 2010.
11-September-2005 C2CR2005, Prague 1 Super-Kamiokande Atmospheric Neutrino Results Kimihiro Okumura ICRR Univ. of Tokyo ( 11-September-2005.
GZK Horizons and the Recent Pierre Auger Result on the Anisotropy of Highest-energy Cosmic Ray Sources Chia-Chun Lu Institute of Physics, National Chiao-Tung.
X The values of all neutrino oscillation parameters in the 3ν scheme can now be extracted from global fits of available data with a precision better than.
T2K neutrino experiment at JPARC Approved since 2003, first beam in April Priorities : 1. search for, and measurement of,   e appearance  sin.
Searching for the footprint of prompt atmospheric neutrino flux and beyond Guey-Lin Lin National Chiao-Tung U. Taiwan With N. Tung and F.-F. Lee KEKPH.
Some answers to the questions/comments at the Heavy/Light presentation of March 17, Outline : 1) Addition of the id quadrant cut (slides 2-3); 2)
The Nightglow Spectrum of Jupiter as seen by the Alice UV Spectrograph on New Horizons A. J. Bayless 1, G. R. Gladstone 1, J.-Y. Chaufray 2, K. D. Retherford.
Zero-point Energy Minimum energy corresponds to n=1
Probing the X-ray Universe: Analysis of faint sources with XMM-Newton G. Hasinger, X. Barcons, J. Bergeron, H. Brunner, A. C. Fabian, A. Finoguenov, H.
Arie Bodek, Univ. of Rochester1 Vector and Axial Form Factors Applied to Neutrino Quasi-Elastic Scattering Howard Budd University of Rochester
1 Latest CC analysis developments New selection efficiencies: –Based on C++ reco + PDFs rather than old (Fortran+reco_minos) cuts –Attempt to optimise.
1 Recent developments on sensitivity calculations Effect of combined le and me running –Is there a statistical advantage over pure le running? Discrimination.
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.
High-energy electrons, pulsars, and dark matter Martin Pohl.
Motivation. Why study ground state hyperon electroproduction? CLAS detector and analysis. Analysis results. Current status and future work. M. Gabrielyan.
V.L. Kashevarov. Crystal Collaboration Meeting, Mainz, September 2008 Photoproduction of    on protons ► Introduction ► Data analysis.
Walid DRIDI, CEA/Saclay n_TOF Collaboration Meeting, Paris December 4-5, 2006 DAPNIA Neutron capture cross section of 234 U Walid DRIDI CEA/Saclay for.
Counting Electrons to Measure the Neutrino Mass Hierarchy J. Brunner 17/04/2013 APC.
Extrapolation Neutrino Flux measured at Near Detector to the Far Detector Near Detector Workshop, CERN, 30 July 2011 Paul Soler, Andrew Laing.
Steve Geer IDS Meeting CERN March Neutral Currents and Tests of 3-neutrino Unitarity in Long-Baseline Exeriments Steve Geer Barger, Geer, Whisnant,
MEASUREMENT OF THE NEUTRINO MASS HIERARCHY IN THE DEEP SEA J. Brunner.
Study of neutrino oscillations with ANTARES J. Brunner.
Study of neutrino oscillations with ANTARES J. Brunner.
Study of γd --> K + Λn through 3-track detected events with the NKS2 HONDA Kazuhisa Tohoku University.
Λ and Σ photoproduction on the neutron Pawel Nadel-Turonski The George Washington University for the CLAS Collaboration.
ORCA simulations - First steps J. Brunner 06/09/2012.
The ORCA Letter of Intent Oscillation Research with Cosmics in the Abyss ORCA Antoine Kouchner University Paris 7 Diderot- AstroParticle and Cosmology.
KM3NeT – ORCA Measuring Neutrino Oscillations and the Neutrino Mass Hierarchy in the Mediterranean Sea J. Brunner CPPM.
Russian Aviation and Space Agency Institute for Space Research NASA 2001 Mars Odyssey page 1 Workshop HEND Radiation environment on Odyssey and.
Thoughts on the optimization of the VLENF VLENF meeting at Fermilab, USA September 1, 2011 Walter Winter Universität Würzburg TexPoint fonts used in EMF:
DIJET STATUS Kazim Gumus 30 Aug Our signal is spread over many bins, and the background varies widely over the bins. If we were to simply sum up.
Photoproduction of the  (1385) resonance at LEPS K. Hicks & D. Keller, Ohio U. LEPS Collaboration Meeting May 1, 2008.
1 Luca Stanco, INFN-Padova (for the OPERA collaboration) Search for sterile neutrinos at Long-BL The present scenario and the “sterile” issue at 1 eV mass.
Alternative Code to Calculate NMH Sensitivity J. Brunner 16/10/
Search for the  + in photoproduction experiments at CLAS APS spring meeting (Dallas) April 22, 2006 Ken Hicks (Ohio University) for the CLAS Collaboration.
Recent b physics results from OPAL David Waller, Carleton University for the OPAL Collaboration EPS Conference HEP2003 Heavy Flavour Physics Session Aachen,
Atom-molecule energy transfer and dissociation processes for nitrogen and oxygen Fabrizio Esposito IMIP-CNR, Bari Section (Institute of Inorganic Methodologies.
Aart Heijboer ● ORCA * catania workshop sep statistical power of mass hierarchy measurement (with ORCA) Aart Heijboer, Nikhef.
K* photoproduction from g11 K. Hicks Ohio University HSG meeting, 12 June 2009.
The KASCADE-Grande Experiment: an Overview Andrea Chiavassa Universita’ di Torino for the KASCADE-Grande Collaboration.
Recent Results from Super-K Kate Scholberg, Duke University June 7, 2005 Delphi, Greece.
ORCA from ANTARES modules J. Brunner 06/10/2012. Detector Hexagonal layout a la IceCube 37 lines, distance 20m 25 ANTARES storeys  z = 4.5m Equipped.
Neutral Current Contributions J. Brunner 22/04/2015.
15 cm Plots of missing mass spectrum and 90% interval for width of 0.5 and 10 MeV. Color lines show upper limit, lower limit and sensitivity. Search for.
Alternative Code to Calculate NMH Sensitivity J. Brunner 16/10/
Study of the Differential Luminosity Spectrum Measurement using Bhabha Events in 350GeV WANG Sicheng 王 思丞 Supervisor: André Sailer.
Shih-Hao Wang 王士豪 Graduate Institute of Astrophysics & Leung Center for Cosmology and Particle Astrophysics (LeCosPA), National Taiwan University 1 This.
T2K Experiment Results & Prospects Alfons Weber University of Oxford & STFC/RAL For the T2K Collaboration.
E. W. Grashorn, for the MINOS Collaboration Observation of Shadowing in the Underground Muon Flux in MINOS This poster was supported directly by the U.S.
Jixie’s Analysis Status Jixie Zhang Sep. 22th, 2010.
Polarization of final electrons/positrons during multiple Compton
Figure 1. Three light curves of IRAS 13224–3809 in 600-s bins
SOLAR ATMOSPHERE NEUTRINOS
Measurement of the Neutrino Mass hierarchy in the deep sea
KM3NeT Collaboration meeting, Marseille, January 2013
SOLAR ATMOSPHERE NEUTRINOS
COMPTON ANALYSIS REPORT
Volume 111, Issue 2, Pages (July 2016)
Demonstration of MT sorting by integrating the top-down design of PDMS device with the bottom-up design of MT properties. Demonstration of MT sorting by.
by Haiming Zhu, Kiyoshi Miyata, Yongping Fu, Jue Wang, Prakriti P
Simulations of the response of the Mars ionosphere to solar flares and solar energetic particle events Paul Withers EGU meeting Vienna,
DUNE as the Next-Generation Solar Neutrino Experiment
Demonstration of MT sorting by integrating the top-down design of PDMS device with the bottom-up design of MT properties. Demonstration of MT sorting by.
Christian Madelaire et al. JCHF 2018;6:
Discriminating IR light with visual cortex.
Presentation transcript:

ORCA with e J. Brunner

Step 1 Oscillation probabilities – Values from Fogli et al. (arxiv: ) –  23 =45˚ (avoid octant problem) – CP-phases : colored bands (NH : red, IH : blue) Averaged over fluxes (Honda) and cross sections All components taken into account – µ  µ e  e Perfect flavour identification NC ignored  ignored

Flavour average P osc (µ) cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

Flavour average P osc (e) cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

Step 2 Event Numbers for 6 years of data taking – Numbers are per bin (0.1) in cos  – Uncertainties are from width of CP-band Averaged over fluxes and cross sections All components taken into account – µ  µ e  e Perfect flavour identification NC ignored  ignored

N ev (µ) perfect resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85 NH : 4266  21 IH : 4197  2 NH : 3345  30 IH : 3395  2 NH : 3033  5 IH : 3145  2 NH : 2948  15 IH : 3005  3

N ev (e) perfect resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85 NH : 3781  47 IH : 3789  8 NH : 2776  51 IH : 2709  6 NH : 2241  12 IH : 2088  4 NH : 1852  27 IH : 1677  5

Step 3 Event Numbers for 6 years of data taking Averaged over fluxes and cross sections All components taken into account – µ  µ e  e Perfect flavour identification NC ignored  ignored Energy resolution 25% Gaussian in E

N ev (µ) perfect resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

N ev (µ) 25% E resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

N ev (e) perfect resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

N ev (e) 25% resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

Step 4 Event Numbers for 6 years of data taking Averaged over fluxes and cross sections All components taken into account – µ  µ e  e Flavour misidentification from P2O note NC added  added Energy resolution 25% Gaussian in E

N ev (µ) 25% E resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

Flavour misidentification cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

N ev (e) 25% resolution cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

Flavour misidentification cos  = 0.25cos  = 0.45 cos  = 0.65cos  = 0.85

Significance Cross check : Perfect conditions Ok w.r.t. V.L. & Smirnov 6 years (~ 10 Mton*years) µe

Significance Resolution included : 25% E ;  : 0.5  m/E Perfect particle ID, no NC,  ignored 6 years (~ 10 Mton*years) µe

Significance Resolution included : 25% E ;  : 0.5  m/E Imperfect particle ID, NC,  included 6 years (~ 10 Mton*years) trackscascades

Significance Resolution included : 25% E ;  : 0.5  m/E NO particle ID, NC,  included 6 years (~ 10 Mton*years) All events

Significance – time dependence Electrons are better !! Measurement still possible without particle ID Absolute values here are too good, comparison among curves counts – Solid : only resolution – Dashed : also misreco e µ No particle ID

Event Ratios Resolution included : 25% E ;  : 0.5  m/E Perfect particle ID, no NC,  ignored µe

Event Ratios Resolution included : 25% E ;  : 0.5  m/E Imperfect particle ID, NC,  included trackscascades

Event Ratios Resolution included : 25% E ;  : 0.5  m/E NO particle ID, NC,  included All events