Transcript Where to Build a Neutrino Factory

f Axis
The NOA Experiment:
Phase 2 of the Fermilab NuMI Program
NOA
Workshop on Physics with Atmospheric Neutrinos and
Neutrinos from Muon Storage Rings
Maury Goodman, Argonne National Lab
(most slides courtesy of Gary Feldman, Harvard)
The NOA Experiment
(NuMI Off-Axis e Appearance Experiment)


NOA is an approved Fermilab experiment
optimized for measuring e appearance with the
goal of improving the sensitivity to q13 from the
current CHOOZ limit by more than a factor of 20.
The NOA far detector will be
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a 30 kT “totally active” liquid scintillator detector
located 15 mrad (12 km) off the NuMI beamline axis near
Ash River, NM, 810 km from Fermilab
The uniqueness of NOA is the long baseline,
which is necessary for determining the mass
ordering of the neutrino states.
Maury Goodman
IIT Mumbai
1-2 August 2005
2
2004 APS  study
 One of (two) high priority
recommendations is for a
concerted program to
measure q13 including:


A reactor experiment
An accelerator experiment
(with NOA in mind).
Maury Goodman
IIT Mumbai
1-2 August 2005
3
Maury Goodman
IIT Mumbai
1-2 August 2005
4
Ash River; 810 km
200 x 40 m labs shown
Maury Goodman
IIT Mumbai
1-2 August 2005
5
P(me)
(in Vacuum)

P(me) = P1 + P2 + P3 + P4

P1 = sin2(q23) sin2(2q13) sin2(1.27 Dm132 L/E)
“Atmospheric”

P2 = cos2(q23) sin2(2q12) sin2(1.27 Dm122 L/E)
“Solar”

P3 =

P4 = J cos(d) cos(1.27 Dm13 L/E)
J sin(d) sin(1.27 Dm132 L/E)
2

Atmosphericsolar interference
where J = cos(q13) sin (2q12) sin (2q13) sin (2q23) x
sin (1.27 Dm132 L/E) sin (1.27 Dm122 L/E)
Maury Goodman
IIT Mumbai
1-2 August 2005
6
P(νμ → νe)
(in Matter)

In matter at oscillation maximum, P1 will be approximately
multiplied by (1 ± 2E/ER) and P3 and P4 will be approximately
multiplied by (1 ± E/ER), where the top sign is for neutrinos
with normal mass hierarchy and antineutrinos with inverted
mass hierarchy
ER 

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2
Dm13
2 2GF e
 11 GeV for the earthÕ
s crust.
About ±30% effect for NuMI
About ±11% effect for T2K
The effect is reduced for energies above the oscillation
maximum & increased for energies below
Maury Goodman
IIT Mumbai
1-2 August 2005
7
Off-Axis Rationale

Both Phase 2 experiments, NOA and T2K are sited off the
neutrino beam axis. This yields a narrow band beam:

More flux and less background (e’s from K decay and higherenergy NC events)
E 
0.43  m
1  2q 2

Maury Goodman
IIT Mumbai
1-2 August 2005
8
NOA Far Detector
“Totally Active”
30 kT:
24 kT liquid scintillator
6 kT PVC
32 cells/extrusion
12 extrusions/plane
15.7m
1984 planes
Cell dimensions:
3.9 cm x 6 cm x 15.7m
(0.15 X0 thickness)
Extrusion walls:
3 mm outer
2 mm inner
U-shaped 0.8 mm WLS
fiber into APD
Maury Goodman
132 m
32-plane
block
15.7m
IIT Mumbai
Admirer
1-2 August 2005
9
30 kton NOA detector
Maury Goodman
IIT Mumbai
1-2 August 2005
10
Light collection
Maury Goodman
IIT Mumbai
1-2 August 2005
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Far Detector Assembly
1-cm expansion gap
One 8-plane sub-block
assembled per day
Detector has 248 subblocks
8-plane
sub-block
Maury Goodman
IIT Mumbai
32-plane
block
1-2 August 2005
32-plane
block
12
Half-scale NOA Prototype in
Bldg 366
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Unprecedented plastic
structure of this scale
Measure mechanical
properties
Compare to FEA
calculations
Try out assembly
procedures
Mounting/gluing tests
Maury Goodman
IIT Mumbai
1-2 August 2005
13
Structural Analysis

Rigid PVC

ASTM D1784 “Standard Specification
for Rigid PVC Compounds”
Defines 6 grades with allowable design
stresses from 1000 PSI to 2000 PSI

NOvA design working limit of 1500
PSI
Well before creep onset
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Good resistance to catastrophic
failure
Creep before crack
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FEA model
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Results baselined with bench tests
Maximum internal stress of 1400 PSI
for vertical cell from hydrostatic
pressure
Maximum transferred stress of 560
PSI for horizontal to vertical cells
70 PSI in sheer
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Safety factor of 2.9 for buckling
10C temperature change
Force generated of 4.3 PSI
Length of detector increased by 9cm
Include expansion gaps between blocks
Maury Goodman
IIT Mumbai
1-2 August 2005
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Near Detector
8-plane block
10.6 T full
1.6 T empty
262 T
145 T totally active
20.4 T fiducial
(central 2.5 x 3.25 m)
9.6 m
5m
Muon catcher
1 m iron
Shower containment region
3.5 m
Maury Goodman
Target region
Veto region
IIT Mumbai
1-2 August 2005
15
Near Detector in
MINOS Surface Building
6.5 x 1020 pot in 75 mrad off-axis beam
Kaon peak
45,000 m CC events
Maury Goodman
IIT Mumbai
2,200 e CC events
1-2 August 2005
16
1.87 GeV eN  ep+0
x-z View
Accepted
Maury Goodman
IIT Mumbai
1-2 August 2005
17
2.11 GeV mN  mp0
x-z View
Accepted!
Maury Goodman
IIT Mumbai
1-2 August 2005
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1.86 GeV eN  ep+
x-z View
Not accepted
Maury Goodman
IIT Mumbai
1-2 August 2005
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Electron ID & Energy Resolution
Electrons
10%
Muons
E
Electron
resolution
Also use RMS of pulse height per plane,
gapsIIT&Mumbai
energy cuts
Maury Goodman
1-2 August 2005
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Post-Collider Proton Plan
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Proton Plan with Collider
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Post-Collider Proton Plan
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9/11 Slip-stacked Booster batches at 5.51012 p/batch
Repetition rate = 0.8 s (Booster) + 1.4 s (Ramp) = 2.2 s
10% for Collider shot setup + 5% for antiproton transfer
 3.4 1020 protons/yr
11 batches for neutrinos  11/9 = 1.22 factor
Hide Booster filling time in Recycler  0.8 s  0.067 s
 2.2 s  1.467 s = 1.50 factor
Save 10% shot setup and 5% antiproton transfer = 1.17 factor
 (3.4 1020 protons/yr)(1.22)(1.50)(1.17) = (7.3 1020
protons/yr)
Negotiated rate is 90% of this: (6.51020 protons/yr)
Proton Driver rate taken as 251020 protons/yr
Maury Goodman
IIT Mumbai
1-2 August 2005
21
Parameters Consistent with
a 2% m  e Oscillation
Maury Goodman
IIT Mumbai
1-2 August 2005
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Parameters Consistent with
Other Oscillation Probabilities
Maury Goodman
IIT Mumbai
1-2 August 2005
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3 s Sensitivity to q13  0
5 year
 only
run
Maury Goodman
IIT Mumbai
1-2 August 2005
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3 s Sensitivity to q13  0
2.5 yr each
 and  run
Maury Goodman
IIT Mumbai
1-2 August 2005
25
3 s Sensitivity to q13  0
Comparison with Proton Driver
2.5 yr each
 and  run
Maury Goodman
IIT Mumbai
1-2 August 2005
26
Importance of the Mass Ordering
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Window on very high energy scales: grand unified
theories favor the normal mass ordering, but other
approaches favor the inverted ordering.
If we establish the inverted ordering, then the next
generation of neutrinoless double beta decay
experiment can decide whether the neutrino is its
own antiparticle. However, if the normal ordering
is established, a negative result from these
experiments will be inconclusive.
To measure CP violation, we need to resolve the
mass ordering, since it contributes an apparent CP
violation that we must correct for.
Maury Goodman
IIT Mumbai
1-2 August 2005
27
Role of NOA in Resolving
the Mass Ordering
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The mass ordering can be resolved only by matter
effects in the earth over long baselines.
NOA is the only proposed experiment with a
sufficiently long baseline to resolve the mass
ordering.
The siting of NOA is optimized for this
measurement.
NOA is the first step in a step-by-step program
that can resolve the mass ordering in the region
accessible to conventional neutrino beams.
Maury Goodman
IIT Mumbai
1-2 August 2005
28
95% CL Resolution of the
Mass Ordering
Maury Goodman
IIT Mumbai
1-2 August 2005
29
95% CL Resolution of the
Mass Ordering
Maury Goodman
IIT Mumbai
1-2 August 2005
30
95% CL Resolution of
the Mass Ordering
Scenario:
2 years into the PD
run, realize the need
for the 2nd off-axis
detector. Build in 4
years, run for 6 years.
Thus, 12 years running
of NOA with PD and
6 years of running the
second detector.
Several technologies
possible for the 2nd
detector. Use SK as
a model for the
calculation.
Maury Goodman
IIT Mumbai
1-2 August 2005
31
Other Physics


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Better Dm231 & sin22q23
Study a possible MiniBooNE signal
Supernova
Maury Goodman
IIT Mumbai
1-2 August 2005
32
Cost
Contingency Total Cost M$
Far Detector
Active detector
30%
79.5
Electronics and DAQ
55%
13.4
Shipping
21%
7.0
Installation
43%
13.5
Near Detector
44%
3.1
Building and outfitting
58%
29.3
Project management
25%
4.7
Additional contingency
Total
Maury Goodman
14.1
50%
IIT Mumbai
1-2 August 2005
164.7
33
Schedule
(10 of 29 Milestones)
Project start
Oct 2006
R&D prototype Near Detector complete
Mar 2007
Start Far Detector Building construction
Jul 2007
Start receiving packaged APDs
Oct 2007
Start extrusion module factories
Oct 2007
Start construction of Near Detector
Dec 2007
Start operation of Near Detector
Jul 2008
Start Far Detector assembly
May 2009
First kiloton operational
Oct 2009
Full 30 kilotons operational
Jul 2011
Maury Goodman
IIT Mumbai
1-2 August 2005
34
NOA Status

Approved by Fermilab April 2005: Letter from Mike
Witherell
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“The Committee found that NOA …is the best approach to
address the compelling neutrino physics questions ahead of us.
They judged NOA to be well designed, fully competitive, and
complementary to other efforts. They also consider it to be the
right platform for further steps in the evolving neutrino program
worldwide. The Committee recommended Stage I approval.”
“Organizing the best program of neutrino research with
Fermilab’s accelerators is critical to the strength of the particle
physics program in the US and worldwide. I agree with the
Committee’s judgment that NOA is the right experiment to
anchor this program, and I agree that now is the time to act. I
therefore grant Stage I approval to the NOA experiment.”
Maury Goodman
IIT Mumbai
1-2 August 2005
35
NOA Status


Approved by Fermilab April 2005 (see letter)
Ed Temple has set out a schedule of critical
decisions and reviews that will allow a Oct 2006
construction start (see timeline)
Maury Goodman
IIT Mumbai
1-2 August 2005
36
Sensitivity vs. Time
3 s Sensitivity to sin 22q13
0.05
0.045
NOA
0.04
sin2(2q23) = 1.0
typical d
0.035
sin2(2q13)
Dm322 = +0.0025 eV2
0.03
0.025
0.02
0.015
Start of Far
Detector
Assembly
0.01
0.005
0
2007
2008
2009
2010
2011
2012
2013
2014
2015
2016
2017
Start of Fiscal Year
Maury Goodman
IIT Mumbai
1-2 August 2005
37
Conclusion

NOA provides a flexible approach to studying all
of the parameters of neutrino oscillations

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A long baseline approach is crucial in the context of the
world program.
NOA is the first stage of a flexible program where each
stage can be planned according to what has been learned
in previous stages.
The NOA physics reach is greater than other
experiments being contemplated for the next few years.
Maury Goodman
IIT Mumbai
1-2 August 2005
38
Backup Slides
Maury Goodman
IIT Mumbai
1-2 August 2005
39
3 s Sensitivity to q13  0
Maury Goodman
IIT Mumbai
1-2 August 2005
40
95% CL Resolution of the
Mass Ordering: Summary
Maury Goodman
IIT Mumbai
1-2 August 2005
41
3 s Determination of
CP Violation
Maury Goodman
IIT Mumbai
1-2 August 2005
42
95% CL Resolution of
the Mass Ordering
NOA with T2K Phase 1
Maury Goodman
IIT Mumbai
NOA/PD with T2K Phase 2
1-2 August 2005
43
95% CL Resolution of the
Mass Ordering
Maury Goodman
IIT Mumbai
1-2 August 2005
44
Ed Temple’s Timeline of
Critical Decisions and Reviews
11 reviews in 22 months exclusive of NuSAG, P5, and the PAC
Maury Goodman
IIT Mumbai
1-2 August 2005
45
Assumed T2K Beam Power
vs. Time
From S. Nagamiya,
Feb 2005
Maury Goodman
IIT Mumbai
1-2 August 2005
46
Sensitivity vs. Time
Comparison to T2K
3 s Sensitivity to sin 2(2q13)
0.05
T2K assuming a 50 GeV
synchrotron and completion
of the 400 MeV Linac in
JFY2010
0.045
0.04
sin2(2q13)
0.035
NOA assuming
project start in
FY2007
0.03
0.025
0.02
0.015
0.01
0.005
0
2007
Dm322 = +0.0025 eV 2
sin2(2q23) = 1.0
typical d
2008
2009
2010
2011
2012
2013
2014
2015
2016
2017
Start of Fiscal Year
Maury Goodman
IIT Mumbai
1-2 August 2005
47
Sensitivity vs. Time
Comparison to a reactor experiment
3 s Sensitivity to sin 2(2q13)
0.05
0.045
0.04
Medium reactor assuming
2 yr construction starting
in FY2007
sin2(2q13)
0.035
0.03
0.025
0.02
Dm322 = +0.0025 eV2
sin2(2q23) = 1.0
typical d
0.015
NOA assuming
project start in
FY2007
0.01
0.005
0
2007
2008
2009
2010
2011
2012
2013
2014
2015
2016
2017
Start of Fiscal Year
Maury Goodman
IIT Mumbai
1-2 August 2005
48
P(me)
(in Matter)

In matter at oscillation maximum, P1 will be approximately
multiplied by (1 ± 2E/ER) and P3 and P4 will be approximately
multiplied by (1 ± E/ER), where the top sign is for neutrinos
with normal mass hierarchy and antineutrinos with inverted
mass hierarchy.
ER 
2
Dm13
2 2GF e
 11 GeV for the earthÕ
s crust.
About a ±30% effect for NuMI, but only a ±11% effect for
JPARC .
However, the effect is reduced for energies above the
oscillation maximum and increased for energies below.
Maury Goodman
IIT Mumbai
1-2 August 2005
49
3 s Sensitivity to q13  0
Comparison with Proton Driver
5 year
 only
run
Maury Goodman
IIT Mumbai
1-2 August 2005
50
3 s Sensitivity to q13  0
Comparison with T2K
5 year
 only
run
Maury Goodman
IIT Mumbai
1-2 August 2005
51
3 s Sensitivity to q13  0
Comparison with a reactor experiment
5 year
 only
run
Maury Goodman
IIT Mumbai
1-2 August 2005
52
95% CL Resolution of the Mass
Ordering: with a Reactor Expt.
Maury Goodman
IIT Mumbai
1-2 August 2005
53
3 s Determination of
CP Violation: with a Reactor Expt.
Maury Goodman
IIT Mumbai
1-2 August 2005
54
95% CL Resolution of
the q23 Ambiguity
Maury Goodman
IIT Mumbai
1-2 August 2005
55
3 s Determination of
CP Violation
Maury Goodman
IIT Mumbai
1-2 August 2005
56
3 s Determination of
CP Violation
Maury Goodman
IIT Mumbai
1-2 August 2005
57
3 s Determination of
CP Violation
Maury Goodman
IIT Mumbai
1-2 August 2005
58
3 s Determination of
CP Violation
Maury Goodman
IIT Mumbai
1-2 August 2005
59
3 s Determination of
CP Violation
Maury Goodman
IIT Mumbai
1-2 August 2005
60
95% CL Resolution of
the Mass Ordering
Maury Goodman
IIT Mumbai
1-2 August 2005
61
95% CL Resolution of
the Mass Ordering
Maury Goodman
IIT Mumbai
1-2 August 2005
62
Far Detector Assembly
1-cm expansion gap
One 8-plane sub-block
assembled per day
Detector has 248 subblocks
8-plane
sub-block
Maury Goodman
IIT Mumbai
32-plane
block
1-2 August 2005
32-plane
block
63
Far Detector Building
Proposal Design
Bathtub for full
containment
Maury Goodman
IIT Mumbai
1-2 August 2005
64
Far Detector Building
Design with Overburden
Maury Goodman
IIT Mumbai
1-2 August 2005
65
Near Detector
8-plane block
10.6 T full
1.6 T empty
262 T
145 T totally active
20.4 T fiducial
(central 2.5 x 3.25 m)
9.6 m
5m
Muon catcher
1 m iron
Shower containment region
3.5 m
Maury Goodman
Target region
Veto region
IIT Mumbai
1-2 August 2005
66
Near Detector:
Modular and Mobile
MINOS Surface Building
M Test
NuMI Access Tunnel
Maury Goodman
IIT Mumbai
1-2 August 2005
67
Near Detector in
MINOS Surface Building
6.5 x 1020 pot in 75 mrad off-axis beam
Kaon peak
45,000 m CC events
Maury Goodman
IIT Mumbai
2,200 e CC events
1-2 August 2005
68
Near Detector in the
Access Tunnel
Far Detector x 800
Site 1.5
Site 2
m CC events
Maury Goodman
IIT Mumbai
e CC events
1-2 August 2005
69
Sensitivity to m  e
Vs. Off-Axis Distance
Maury Goodman
IIT Mumbai
1-2 August 2005
70
Sensitivity to m  e
Vs. Off-Axis Distance
Maury Goodman
IIT Mumbai
1-2 August 2005
71
Sensitivity to the Mass Ordering
Vs. Off-Axis Distance
Maury Goodman
IIT Mumbai
1-2 August 2005
72
3 s Sensitivity to q13  0
2.5 yr each
 and  run
Maury Goodman
IIT Mumbai
1-2 August 2005
73
3 s Sensitivity to q13  0
2.5 yr each
 and  run
Maury Goodman
IIT Mumbai
1-2 August 2005
74
3 s Sensitivity to q13  0
2.5 yr each
 and  run
Maury Goodman
IIT Mumbai
1-2 August 2005
75
3 s Sensitivity to q13  0
2.5 yr each
 and  run
Maury Goodman
IIT Mumbai
1-2 August 2005
76
Measurement of
Dm322 and sin2(2q23)
5-year  run
5-year  run
with Proton Driver
Maury Goodman
IIT Mumbai
1-2 August 2005
77
Study MiniBooNE Signal
Site 1.5
Site 3
1-year
 run
Maury Goodman
1-year
 run
IIT Mumbai
1-2 August 2005
78
Sensitivity to a Galactic
Supernova
Signal in 100 ms bins
for a galactic supernova
assuming a 3 m overburden
1500 signal events
Maury Goodman
IIT Mumbai
1-2 August 2005
79