Kellogg Lab Overview

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Kellogg Lab Overview
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KamLAND
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Outline

• Neutrino Oscillations
• Overview and history

• Reactor Neutrinos
• KamLAND Experiment
• Future outlook

Reference McKeown Vogel, Phys. Rep. 394, 315
(2004) hep-ph/0402025
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Two Generation Model
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Length Energy Scales
Super-K
En 1 GeV, Dm210-3 eV2 , L 1240 km
Chooz, Palo Verde
En 1 MeV, Dm210-3 eV2 , L 1.2 km
En 1 MeV, Dm210-5 eV2 , L 125 km
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30 kton H20 Cherenkov 11000 20 PMTs
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Super-Kamiokande Results
Wn gt 0.001
g K2K, MINOS
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Solar Neutrino Energy Spectrum
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More missing neutrinos
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Neutrino Oscillations?
Rorbit
Just So ???
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Matter Enhanced Oscillation (MSW)
Mikheyev, Smirnov, Wolfenstein
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Open circles combined best fit Closed circles
experimental data
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Results from Solar and Atmospheric Neutrino
Experiments

• ns transform flavor

• Atmospheric n data explained extremely well by
  oscillations

• looks like primarily nm to nt conversion
• mixing angle q23 is very large, possibly maximal
• Dm2 2 x 10-3 eV2

• looks like primarily nm to nt conversion
• mixing angle q23 is very large, possibly maximal
• Dm2 2 x 10-3 eV2

• Solar ne change primarily to other active ns

• if oscillations, mixing angle q12 is large but
  not maximal
• if oscillations, Dm2 7 x 10-5 eV2
• matter predicted to play a role in transformation

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W.A. Fowler Nobel Lecture, 1983
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???
Is it really an OSCILLATION effect ??
Or is it a HELICITY-FLIP effect ??
Or possibly a SOURCE GENERATION effect ??
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Enter

• Long Baseline (180 km)
• Calibrated source(s)
• Large detector (1 kton)
• Deep underground (2700 mwe)

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Designed to test solar neutrino oscillation
parameters on Earth (!) KamLAND has a much
longer baseline than previous (reactor)
experiments
Statistical errors only
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Reactor Neutrino Experiments

• ne from n-rich fission products
• detection via inverse beta decay (nepgen)
• Measure flux and energy spectrum
• Variety of distances L 10-1000 m

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Detection Signal
Liquid Scintillator can measure lower energies
than water Cherenkov detectors

• Coincidence signal detect
• Prompt e annihilation g
  EnEpromptEn0.8 MeV
• Delayed n capture 180 ms capture time

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Previous Measurements
Flux and Energy Spectrum g 1-2
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Previous Oscillation Searches
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Distance (m)
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Only a few places in the World could host an
experiment like KamLAND
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KamLAND uses the entire Japanese nuclear
power industry as a longbaseline source
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Baseline is limited 85.3 of signal has 140 km
lt L lt 344 km

• The total electric power produced as a
• by-product of the ns is
• 60 GW or...
• 4 of the worlds manmade power or
• 20 of the worlds nuclear power

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Total expected signal from reactors 2
ev/day S/N ratio 20 _at_ 10-14 U, Th,
40K contamination in the scintillator
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Spectrum Distortion
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KamLAND Detector
1000 Ton
(135 mm)
1879
(Cosmic veto)
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KamLANDphysics on a shinkansen

• Summer 2000 PMT installation
• Winter 2000-01 Veto counter installation
• Feb 2001 Balloon insertion
• Mar-Apr 2001 Balloon inflation and test
• Apr-May 2001 Plumbing for fill
• Jun-Sept 2001 Fill MO and LS
• Aug-Sept 2001 Eng. runs with Macro Elec.
• Sept 2001 FEE/DAQ/Trigger int. (LBL)
• end Sept 2001 First data taking with FEE
• Jan 22, 2002 Begin Data Taking

• Dec. 6, 2002 Report 1st Physics Results

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Sphere Construction
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PMT Installation
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PMT Installation
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Filling the Detector
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Minimizing Radioactivity (Background)
Balloon Film

• Certification of materials
• Caltech low-background
• counting facilities
• Mass spectroscopy
• Neutron activation analysis

Ge Detector
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Front End Electronics
Waveforms are recorded using Analogue Transient
Waveform Digitizers (ATWDs), allowing multi p.e.
resolution
Blue raw data red pedestal green pedestal
subtracted

• The ATWDs are self launching with a threshold
  1/3 p.e.
• Each PMT is connected to 2 ATWDs, reducing
  deadtime
• Each ATWD has 3 gains (20, 4, 0.5), allowing a
  dynamic range of 1mV to 1V

ADC counts (120 mV)
Samples (1.5ns)
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68Ge 1.012 MeV (g g) 65Zn
1.116 MeV (g) 60Co 2.506 MeV (g g) AmBe
2.20 , 4.40, 7.6 MeV (g)
-5m
5m
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Anti-Neutrino Candidate
(color is time)
Delayed Signal E 2.22 MeV
Prompt Signal E 3.20 MeV
Dt 111 ms DR 34 cm
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There is a clean signal
npgdg
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Correlation with reactor power variation
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Observed Event Rates
2002-4 dataset 766.3 tonyr, Eprompt
gt 2.6 MeV Observed 258
events No-oscillation 365.2 23.7
events Background 17.6 7.2 events
accidental 2.69 0.02 9Li/8He (b, n) 4.8
0.9 fast neutron lt 0.89 13C(a,n) 10.0
7.1
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Evidence for Reactor ne Disappearance!!
99.998 C.L.
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Ratio of Measured and Expected ne Flux from
Reactor Neutrino Experiments
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Measurement of Energy Spectrum
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Oscillation Effect
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KamLAND best fit Dm2 7.9 x 10-5 eV2 tan2q
0.45
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Combined fit with solar neutrino data
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KamLAND Future

• Precision Reactor Neutrino Measurements
• - 4p calibration system
• - refine analysis methods
• - more statistics
• Geoneutrinos
• Supernova detection
• Precision Solar Neutrino Measurements
• - radiopurity
• - low energy threshold

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Maki Nakagawa Sakata Matrix
Future Reactor Experiment!
CP violation
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Implications for Theory

• Right-handed Dirac neutrinos
• - weakly-interacting (10-12)
• - extra dimensions?
• Majorana neutrinos
• - heavy right-handed neutrinos
• (M1016 GeV, GUT scale)
• - mlight mD2/M (see-saw)
• - CP violation, leptogenesis?

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Why so different???
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The Mass Puzzle
Seesaw mechanism
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Why havent we seen nR?Extra Dimension

• All charged particles are on a 3-brane
• Right-handed neutrinos SM gauge singlet
• ? Can propagate in the bulk
• Makes neutrino mass small
• (Arkani-Hamed, Dimopoulos, Dvali, March-Russell
• Dienes, Dudas, Gherghetta)
• Barbieri-Strumia SN1987A constraint
• ?Warped extra dimension (Grossman, Neubert)
• or more than one extra dimensions
• Or SUSY breaking
• (Arkani-Hamed, Hall, HM, Smith, Weiner
• Arkani-Hamed, Kaplan, HM, Nomura)

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Mass Hierarchy and Mixing
Normal Inverted
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Goals for the future

• Establish q13 non-zero
• Measure CP violation
• Determine mass hierarchy

Also Majorana or Dirac Sterile species?
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Maki Nakagawa Sakata Matrix
Future Reactor Experiment!
CP violation
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ne Disappearance
Dominant ?12 Oscillation
P(?e??e)
Distance (m)
Subdominant ?13 Oscillation
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Previous q13 Experiments
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New q13 Experiment

• Powerful reactor plant
• Identical near/far detectors
• Larger detector mass (100 Ton)
• Far distance 2km

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New Reactor Proposals
Daya Bay, China

• 1.5 km baseline
• Deeper/bigger
• Near/Far

Chooz, France
Diablo Canyon, Calif
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Diablo Canyon - An Ideal Site?
( Other possible site options Japan, France,
Brazil, China )
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Another Option Daya Bay, China
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Reactor (/- 0.01)
normal
dCP
inverted
NOnA (5 yr n)
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Other Future Studies

• Double beta decay (mlt0.1 eV)
• (Majorana only!)
• Direct measurements (mlt 1 eV)
• (KATRIN)
• Cosmological Input (mlt0.2 eV)
• (Planck satellite)

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A collaboration of LA Area High Schools, Caltech,
CSUN, and UCI
to develop a distributed array of detectors to
study ultra-high energy cosmic rays.
Research Director  Prof. R. D. McKeown, Caltech
Education Director Prof. R. Seki, CSU
Northridge Project Coordinator Dr. T. Lynn,
Caltech
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Ultra-high Energy Cosmic Rays
Extended Air Showers
UHECR
Terrestrial Accelerators
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Source of UHECR??
HiRes AGASA Controversy
Supernova acceleration
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• GPS Timing
• Power, shelter
• Data transfer
• via internet
• Cost effective

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A Large Air Shower
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A Large Air Shower
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Search for Correlated Showers
All Sites
Separation gt 1 km
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A closer look
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Maybe Interesting!
Need More Data!
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Future Plans

• Complete deployment of 90 sites in SG and SF
  valleys in 2004 collect data
• Raise funds to expand to 200-300 sites
• Develop new detector concepts
• Improve instrumentation