Experimental Methods in HEP

Salasa A. Nawang Iligan Institute of Technology of Mindanao State University Iligan City OUTLINE

● Introduction/Overview ● Principles of detection ● Important aspects in measurement ● : Physics motivation and Measurement ● Our Work

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 2 Introduction/1

Physics [Theory]

Expt Detectors Methods

Accurate/Precise Getting meaningful Measurement results

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 3 Experimental Design

confirmation

THEORY EXPERIMENT

validation

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 4 Introduction/2 ● Experimental Goal – We want to detect its presence – Look at its tracks/pattern. – Measure its energy deposit, etc...

● Procedure [what forms?] – Depends on the type of particle, mass, charge, etc... ● Motivation – Guided by theory...

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 5 Detection Principle [too primitive]

Path of the positron in a CLOUD ELECTROSCOPE Chamber [C. D. Anderson, Phys. Rev. 43 (1933 492)]

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 6 Detection Principle [w/ photons]

Scintillator

Light Guide

PMT 3/31 - 4/9,2014, Nawang, S. CERN School Philippines 7 Detection Principle [e.g. charge particles]

They interact via multiple Coulomb scattering via the Stopping power dE/dx.

dE/dx is described by the Bethe-Bloch equation

About (1/500) of Etotal is transferred per collision with the electron 3/31 - 4/9,2014, Nawang, S. CERN School Philippines 8 dE/dx for electrons/positrons

(dE/dx)(dE/dx)TOTAL == (dE/dx)(dE/dx)collision ++ (dE/dx)(dE/dx)radiation

Due to the Total Due to Radiation

Due to collision Proton's

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 9 Detection Principle [DAQ]

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 10 Detection Principle [e.g. spectrum]

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 11 Range

Phenomenon: RANGE STRAGGLING

Energy loss is Statistical in nature

−1 T O dE S T 0=∫ dE NUMERICAL INTEGRATION 0 [ dx ]

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 12 But, wait a minute...

Why spend so much money and put such great effort into studying particles which are so short-lived and which are created only under special circumstances?

Why not confine our studies only to Protons, neutrons and electrons...

...a...a detectivedetective agent?agent?

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 13 Via Cosmic-rays

Only 14 particles known in 1947: 4 pioneers (γ, p, n, & e), and anti-neutrino, 3 pions, 2 , & Anti-p,n, & positron

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 14 From Cosmic-rays to Accelerators

● 1928-1932: Cockcroft-Walton

● 1930: Robert J. Van de Graaff

● 1930: Ernest O. Lawrence [circular type]

● 1950s: In the US, Cosmotron(~3 GeV @ BNL), Bevatron (~6 GeV @ UC Berkeley), 10-Gev (in Russia)

● 1960: 28-GeV PS @ CERN

● 1961: 33 GeV BNL

● 1967: 76 GeV in Russia

● 1972,1975: 400,500 GeV at Fermi Lab

● 1976: CERN SPS

● 1980s: Tevatron at Fermi-Lab

● Colliders, storage ring, and so on 3/31 - 4/9,2014, Nawang, S. CERN School Philippines 15 So,

do we have an accelerator in the

Philippines?

If Yes, where?

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 16 Mesons of spin zero known in 1960

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 17 ...a Detective work...

3/31 - 4/9,2014, Nawang, S. CERN School Philippines Courtesy: BNL 18 Nucleons and known in 1960

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 19 Typical Scenario

PUZZLE THEORIST EXPERIMENTALISTS

Beta Decay Pauli, Fermi, ... Reines, Cowan,..

Solar Neutrino John Bahcall Raymond Davis [SOLVED?]

Atmospheric Neutrino ??? SuperKamiokande

Any Puzzle ...it can be anyone here ???

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 20 Problem in Nuclear Beta Decay

CONTINUOS

Pauli proposal (1930) New particle exist.

Continuous Energy spectrum of Beta electrons!!!

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 21 Neutrino particle Observed… Reines and Cowan (1956)

Detector at the Savanna River υ + → + + Nuclear Reactor e p n e

Frederick Reines received in 1995 …We are happy to announce to you [Pauli] that we have definitely Detected neutrinos …

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 22 Solar Neutrino Problem

Sudbury Neutrino Observatory RESULT

RATIO

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 23 Raymond Davis Jr.’s Perseverance: 30 years pioneering solar neutrino detection (1969-1999)

Homestake mine tank: 20 feet in diameter, 48 feet long, held 100,000 gallons of perchloroethylene . It was located 4,900 feet below ground surface 4/5/14 24 Atmospheric Neutrinos

Expect an isotropic flux of neutrinos at High energies

For E > a few GeV, and a given neutrino flavor, (Up-going/Down-going) ~ 1.0

Expected uncertainty less than 1%

4/5/14 25 Did the neutrinos change to another kind? 4/5/14 26 Atmospheric Neutrinos

4/5/14 27 Atmospheric Neutrinos

Eν>1.3 GeV

PUZZLE: Evidence for oscillation of atmospheric neutrinos, Where did the other Phys. Rev. Lett. 81 (1998) 1562-1567 muon neutrinos go?

4/5/14 28 Motivation to perform an experiment/measurement ● It depends if you are a: ● Student ● Newly working Researcher ● Administrator ● Government ● etc...

4/5/14 29 ...OR

● Science propagation of knowledge ● Confirmation ● Search for truth...

4/5/14 30 K2K (KEK to KAMIOKA) Search for NEUTRINO OSCILLATIONS using accelerator-produced neutrinos (April 1999-November 2004)

Far Detector(Super-Kamiokande) Near Detector(KEK) ● Detect neutrino signal after possible ● Measure neutrino flux oscillation ● Study Neutrino interactions ● 250km from KEK, Tsukuba ● Located, 200m downstream

Neutrino Beam ● 99% νμ beam ● Average energy ~ 1.3 GeV ● Produced by 12 GeV PS accelerator at KEK 4/5/14 31 4/5/14 32 ’s Vision (Neutrino Oscillation, 1957) Other neutrino flavors were not yet know at that time

J. Exptl. Theoret. Phys. 33, 1957, 549 Pontecorvo’s idea: ν⇒ ν In analogy to K O ⇒ K O oscillation

Neutrino Flavor Mechanism

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 33 Different Neutrino species exists (1962)

νe ,μ , τ +N →{e ,μ ,ν }+ X

Leon M. Lederman, Melvin Schwartz , The 1988

For the neutrino beam method and the demonstration of the doublet structure of the through the discovery of the 4/5/14 34 Neutrino Mixing

Neutrino Flavors Mass eigenstates MIXING

Flavor states NOT EQUAL TO Mass Eigenstates ν = ν = µ τ i ∑ Uiα α i e, , α 4/5/14 35 Unitary matrix U Mixing angle

Maki-Nakagawa-Sakata Matrix: sij = sin θ ij cij = cos θij

Mixing pattern borrowed from Cabibbo-Kobayashi-Maskawa Matrix in quark sector

 U U U   e1 e2 e3  = = θ = θ U  U µ 1 U µ 2 U µ 3  sij sin ij cij cos ij    U τ 1 U τ 2 U τ 3   c s 0  1 0 0   1 0 0   c 0 s   12 12       13 13  = − U  s12 c12 0  0 c23 s23   0 1 0   0 1 0     −   − iδ   −   0 0 1   0 s23 c23   0 0 e   s13 0 c13 

4/5/14 36 Two Flavor state

In the two-flavor neutrino oscillation framework, the probability that a neutrino of energy E with a flavor state νμ will later be observed In the νμ eigenstate after traveling a distance L in vacuum is given by

  2 2 L(km) 2 P(ν µ → ν τ ) = sin 2θ sin 1.27 ∆ m  23  E(GeV) 23 

sin 2 2θ = 1, ∆ m2 = 3.0x10− 3 eV2 ,L = 250 km (Values taken from Solar neutrino data)

4/5/14 37 Physics/Neutrino Interaction

CCQE ● ~100% efficiency for NSK ● reconstruct Eν from(θμ,Pμ)

CC nQE ● ~100% efficiency for NSK ● Bkg for Eν measurement

NC ● Less 50% efficiency for NSK ● Bkg for CCQE tracks 4/5/14 38 Typical νμ production

From Accelerator machine

detector

4/5/14 39 Principle of Measurement

● Measurement of neutrino flux with CCQE interactions between two identical (except the size) detectors [water Cerenkov Detector]

● Measurement of Disappearance at SK

● Same Target and technique, but different spectra

4/5/14 40 Overview of Detectors

MUMON ND

4/5/14 41 Phys Rev D 74 (2006) pp072003 Nature of Measurement

● PRESENCE or ABSENCE ● Confirmation thru its signature or decay mode, or interactions, if there are any. ● If present, ● How many?...its like counting how many fish in the net. ● If absent, ● (Keep it secret first) …...repeat again, and again...

4/5/14 42 Cherenkov Radiation

Cherenkov Light ring

4/5/14 43 Detection Principle

Charged particles travelling In water at speed greater than c/n emit Cherenkov light

υ + → + − e n p e υ + → + + e p n e − υ µ + n → p + µ + υ µ + p → n + µ

The cone aperture determines Cherenkov light is detected by an Velocity. If we can identify the array of light sensitive PMTs. The image Particle then we know the is in the form of a ring (red tubes) energy

4/5/14 44 Long Track

4/5/14 45 Stopping Track

Cherenkov LIGHT

4/5/14 46 Particle Identification Cherenkov Light

4/5/14 48 Tracking Detector

TOP View

Side View

4/5/14 49 CCQE Candidate

ν+n⇒ p+μ 4/5/14 50 CCQE Candidate

ν+n⇒ p+μ 4/5/14 51 CC-pπ Candidate

ν+n⇒ p+μ+π 4/5/14 52 πo Candidate

O 4/5/14 π ⇒ γ+γ 53 νe CCQE Candidate

−❑ 4/5/14 νe +n⇒ e + p 54 Event Selection

● Criteria (decide to accept/reject an event) ● Cuts ● Time cut ● Energy Cut ● etc... ● Error Estimation ● Systematic Error ● Statistical Error ● MC role (EGS4, Geant4, etc...) ● Estimates agreement between expected and observed

4/5/14 55 Time Event Selection GPS

TSpill TSK

Observed Events

4/5/14 56 SuperK Study Solar/Atmospheric Neutrino

4/5/14 57 Particle Detectors

● Features: good resolution sufficient enough to enable particles to be separated in space and time

● Identify each particle and measure its energy and momentum – NO single detector optimized – combination of other detectors ● Usually HUGE, integrates other sub-detectors – fast electronics – Need many computer units (control and monitoring

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 58 4/5/14 59 K2K Result Phys. Rev D 74 (2006) pp072003

SK obs N MC N exp= N KT⋅ KT N MC

Without Oscillation

Expected with Oscillation With Oscillation +9.2 158−8.6

Observed events 112

4/5/14 60 Cosmic Ray Flux Measurement setup

4/5/14 Cosmic rays 61 Cosmic Ray Flux (from MS theses)

Place No. of Counts per min

MSU-Marawi 16.64 +/- 0.84 (Lanao-SUR)

ADZU-Zamboanga 10.41 +/- 0.31 [2 independent measurements done at different times] 10.84 +/- 0.18

10.30 +/- 0.16 Iligan [3 independent 10.64 +/- 0.12 measurements done at different times] 10.52 +/- 0.41

4/5/14 Estimate: ~30 cosmic rays per meter square per62 minute Summary

● Theoretical motivation ● Experimental Design – Optimization, budget, manpower,etc... ● Set of criteria or cuts ● Error Analysis

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 64 Acknowledgement

● The cosmic ray flux measurements were done under the supervision of Dr. Angelina M. Bacala ● Neutrino event samples are owned by neutrino group {under scibar, K2K-II}.

3/31 - 4/9,2014, Nawang, S. CERN School Philippines 65