Interpretation of the Atmospheric Muon Charge Ratio in MINOS

Slides:



Advertisements
Similar presentations
Recent Results from Super-Kamiokande on Atmospheric Neutrino Measurements Choji Saji ICRR,Univ. of Tokyo for the Super-Kamiokande collaboration ICHEP 2004,
Advertisements

Correlation and regression
London Collaboration Meeting September 29, 2005 Search for a Diffuse Flux of Muon Neutrinos using AMANDA-II Data from Jessica Hodges University.
Atmospheric Neutrinos Barry Barish Bari, Bologna, Boston, Caltech, Drexel, Indiana, Frascati, Gran Sasso, L’Aquila, Lecce, Michigan, Napoli, Pisa, Roma.
Cosmic Rays with the LEP detectors Charles Timmermans University of Nijmegen.
Muon Identification Antoine Cazes Laboratoire de l’ Accelerateur Lineaire OPERA Collaboration Meeting in Frascatti Physics coordination meeting. October.
Error Propagation. Uncertainty Uncertainty reflects the knowledge that a measured value is related to the mean. Probable error is the range from the mean.
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.
May 26, 2002Thomas K. Gaisser Atmospheric neutrino fluxes Status of the calculations based on work with M. Honda.
November 1999Rick Field - Run 2 Workshop1 We are working on this! “Min-Bias” Physics: Jet Evolution & Event Shapes  Study the CDF “min-bias” data with.
RF background, analysis of MTA data & implications for MICE Rikard Sandström, Geneva University MICE Collaboration Meeting – Analysis session, October.
1 Super-Kamiokande atmospheric neutrinos Results from SK-I atmospheric neutrino analysis including treatment of systematic errors Sensitivity study based.
Introduction 2. 2.Limitations involved in West and Yennie approach 3. 3.West and Yennie approach and experimental data 4. 4.Approaches based on.
1 1.Introduction 2.Limitations involved in West and Yennie approach 3.West and Yennie approach and experimental data 4.Approaches based on impact parameter.
A new approach to EAS investigations in energy region eV R.P.Kokoulin for DECOR Collaboration Moscow Engineering Physics Institute, Russia.
PHYS 241 Exam 1 Review Kevin Ralphs. Overview General Exam Strategies Concepts Practice Problems.
PPR meeting Marcello Lunardon 1 Semi-electronic beauty detection: status and perspectives THE COLLABORATION Rosario Turrisi and Marcello Lunardon.
Photon Statistics Blackbody Radiation 1.The energy loss of a hot body is attributable to the emission of electromagnetic waves from the body. 2.The.
A statistical test for point source searches - Aart Heijboer - AWG - Cern june 2002 A statistical test for point source searches Aart Heijboer contents:
Response of AMANDA-II to Cosmic Ray Muons and study of Systematics Newt,Paolo and Teresa.
1 dE/dx  Let’s next turn our attention to how charged particles lose energy in matter  To start with we’ll consider only heavy charged particles like.
Introduction The statistical model approach is established by analysis of particle ratios of the high energy heavy ion collisions in GSI-SIS to CERN-SPS.
Calorimeters Chapter 21 Chapter 2 Interactions of Charged Particles - With Focus on Electrons and Positrons -
Properties of giant air showers and the problem of energy estimation of initial particles M.I. Pravdin for Yukutsk Collaboration Yu.G. Shafer Institute.
A Measurement of Two-Photon Exchange in Unpolarized Elastic Electron-Proton Scattering John Arrington and James Johnson Northwestern University & Argonne.
Particle Detectors for Colliders Robert S. Orr University of Toronto.
Study of the Atmospheric Muon and Neutrinos for the IceCube Observatory Ryan Birdsall Paolo Desiati, Patrick Berghaus,
Min-DHCAL: Measurements with Pions Benjamin Freund and José Repond Argonne National Laboratory CALICE Collaboration Meeting Max-Planck-Institute, Munich.
School of Cosmic-ray Astrophysics, Erice, July 4, 2004 Thomas K. Gaisser Role of particle interactions in high-energy astrophysics Uncorrelated fluxes.
A bin-free Extended Maximum Likelihood Fit + Feldman-Cousins error analysis Peter Litchfield  A bin free Extended Maximum Likelihood method of fitting.
Aart Heijboer ● ORCA * catania workshop sep statistical power of mass hierarchy measurement (with ORCA) Aart Heijboer, Nikhef.
G. Eigen, Paris, Introduction The SiPM response is non-linear and depends on operating voltage (V-V bd ) and temperature  SiPMs need monitoring.
Status of QEL Analysis ● QEL-like Event Selection and Sample ● ND Flux Extraction ● Fitting for MINOS Collaboration Meeting FNAL, 7 th -10 th December.
1 A.Fanfani – Measurement of Charge Ratio of atmospheric  with CMS – ICATPP 2010 Measurement of the charge ratio of atmospheric muons with the CMS detector.
All lepton generation and propagation with MMC Dmitry Chirkin, UCB/LBNL AMANDA meeting, Uppsala, 2004.
Heavy Quark Production in 920GeV Proton Nucleus Interactions Michael Danilov ITEP, Moscow Representing HERA-B Collaboration Outline 1.Detector and data.
Atmospheric Neutrino Fluxes Giles Barr XXIst International Conference on Neutrino Physics and Astrophysics Neutrino 2004 Paris.
Measurement of the Muon Charge Ratio in Cosmic Ray Events with the CMS Experiment at the LHC S. Marcellini, INFN Bologna – Italy on behalf of the CMS collaboration.
Chapter 7 The electronic theory of metal Objectives At the end of this Chapter, you should: 1. Understand the physical meaning of Fermi statistical distribution.
A Measurement of the Ultra-High Energy Cosmic Ray Spectrum with the HiRes FADC Detector (HiRes-2) Andreas Zech (for the HiRes Collaboration) Rutgers University.
Lecture 8: Understanding the form factor 30/9/ Why is this a function of q 2 and not just q ? Famous and important result: the “Form Factor.
An analytically solvable model of a nuclear cascade in the atmosphere M. G. Kostyuk BNO INR RAS Using sufficiently accurate uniform (that is, suitable.
The simple linear regression model and parameter estimation
Atmospheric neutrinos with Deep Core
Muons in IceCube PRELIMINARY
Rotation of 67P. Mottola et al. (2014): Lightcurve photomerty -> Spin period of h.
IceCube Collaboration Meeting
Update on Muon Flux Underground Using Geant4 Simulation
Marco Incagli – INFN Pisa
Observation of a “cusp” in the decay K±  p±pp
Andrea Chiavassa Universita` degli Studi di Torino
How to measure E-by-E fluctuations of identified particles
Newt Ganugapati and Teresa Montaruli
Linear Regression and Correlation Analysis
L/E analysis of the atmospheric neutrino data from Super-Kamiokande
Mathematical Modeling and Variation 1.10
Response of AMANDA-II to Cosmic Ray Muons and study of Systematics
Comparison Of High Energy Hadronic Interaction Models
Comparison Of High Energy Hadronic Interaction Models
kT Asymmetry in Longitudinally Polarized Collisions
HADRONIC INTERACTION MODELS AND DPMJET-CHARM MODEL
Hadronic Interaction Model Analysis Air Shower Development
Fluxes of atmosperic leptons
J/   analysis: preliminary results and status report
University of Minnesota on behalf of the CLEO Collaboration
Xiaobin Wang (for the STAR Collaboration)
kT Asymmetry in Longitudinally Polarized pp Collisions
Study of e+e- pp process using initial state radiation with BaBar
Homework Solution Draw out all 15 possible microstates for a system of three molecules with equally-spaced (1 quantum) energy levels and four quanta of.
The structure and evolution of stars
Presentation transcript:

Interpretation of the Atmospheric Muon Charge Ratio in MINOS Phil Schreiner & Maury Goodman For the MINOS collaboration July 5, 2007 presenter

Introduction & new equation July 5, 2007 m+/m- interpretation Maury Goodman, ANL m+/m- interpretation

Compare 3 things Data A new formula MINOS far 1.374  0.004 + 0.012 – 0.010 MINOS near 1.288  0.004  0.025 Other previous mostly near 1.25-1.28 A new formula Some full simulations (Cort, Honda, Lipari) One possible conclusion is that the K+/K- ratio in these simulations is too high. July 5, 2007 Maury Goodman, ANL m+/m- interpretation

With some account for energy dependence. Gaisser’s Equation Nm = Nm (from p) + Nm(from K) A new Equation Nm+ = Nm+ (from p+) + Nm+(from K+) Nm- = Nm- (from p-) + Nm-(from K-) And Nm = Nm+ + Nm- With some account for energy dependence. July 5, 2007 Maury Goodman, ANL m+/m- interpretation

New Equation Gaisser: New: fp fK -fp 0.054(1-fK) July 5, 2007 Maury Goodman, ANL m+/m- interpretation

What’s what fp is related to the m+/m- ratio from p fK is related to the m+/m- from K 0.054 ( h) is related to K/p ratio 115 GeV(850) is the critical energy above which p (K) interact before they decay fp, fK & h assumed energy independent (not true, but reasonable if Feynman scaling) July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Parameterization of muon charge ratio Gaisser sets B=1.1, η=0.054, εp=115 GeV, and εK=850 GeV July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Notice that the ratio depends only on E cos q and not separately on E or q This has a cause. This has some implications. July 5, 2007 Maury Goodman, ANL m+/m- interpretation

More Features p+/p-  rp = fp/(1-fp) & K+/K-  rK = fK/(1-fK) Equation has asymptotic values at low Ecosq & high Ecosq Both asymptotic values have m’s from both p & K MINOS is the first high statistics experiment with Ecosq > ep = 115 GeV h 0.054 rlo =(fp+hfK)/ (1-fp+h(1-fK)) rhi = (epfp+heKfK)/ (ep(1-fp)+heK(1-fK)) July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Commments on MINOS data July 5, 2007 m+/m- interpretation Maury Goodman, ANL m+/m- interpretation

Crude Approximation Our E cos q distribution is a d function This approximation isn’t used for any data analysis – it is illustrative to see why our E cos q distributions are so narrow. Zero maximum detectable momentum Flat surface Constant density In the energy loss equation, a is constant In the energy loss equation, neglect b E cos (qz) = Emin The last 4 assumptions imply the energy loss only depends (simply) on zenith angle. dE/dX = a(E) + b(E)  E July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Minimum Energy to reach MINOS Depends on zenith angle surface Emin Emin/ (cos qz) qz MINOS July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Actual ranges of E & Ecosq in MINOS Far Near July 5, 2007 Maury Goodman, ANL m+/m- interpretation

July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Data plots In the formula, r only depends on Esurfacecosq !!! For a long time we concentrate on the dependence of r with Esurface In the formula, r only depends on Esurfacecosq !!! July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Compare with Simulations July 5, 2007 m+/m- interpretation Maury Goodman, ANL m+/m- interpretation

Look at Full simulations We have predictions from CORT (from V. Naumov) Lipari Honda These all give r vs E in bins of cos(q). We can ask (independent of all data), do these calculations: Depend only on E  cos(q)? Consistent with our formula? July 5, 2007 Maury Goodman, ANL m+/m- interpretation

vs E CORT HONDA Lipari July 5, 2007 m+/m- interpretation Maury Goodman, ANL m+/m- interpretation

CORT vs E cos(q) July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Honda & Lipari vs Ecosq & fit July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Predictions with Data July 5, 2007 m+/m- interpretation Maury Goodman, ANL m+/m- interpretation

Fits with data July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Fits & conclusions July 5, 2007 m+/m- interpretation Maury Goodman, ANL m+/m- interpretation

rK & rp for fits data & simulations rK=K+/K- d(rK) rp =p+/p- d(rp) Lipari 2.87 n/a 1.25 CORT 2.39 1.26 Honda 1.63 1.28 Gaisser(91) 3.2 1.4 Agrawal10TeV (96) 2.92 1.35 MINOS PRD 2.03 1.22 MINOS N+F 2.23 0.26 1.232 0.030 MINOS + L3+C + Hebbeker-Timmermans + CosmoALEPH 2.28 0.06 1.224 0.003 July 5, 2007 Maury Goodman, ANL m+/m- interpretation

The contributions to the muon flux from p+, p-, K+, K- July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Physics not included in our formula Variations to Power law Energy dependence of K/p, p+/p- & K+/K- Non-isothermal effects (i.e. e(height)) Charm Variations in chemical composition (n/p) …but discrepancies (equation & models) not yet understood by us July 5, 2007 Maury Goodman, ANL m+/m- interpretation

Conclusions MINOS has the first high stats data with Ecosq >ep & sees a rise in charge ratio A new formula well describes the data MINOS data narrow in Ecosq Some agreement, disagreement with full simulations Possible guidance to model-builders Some K+/K- ratios too high July 5, 2007 Maury Goodman, ANL m+/m- interpretation