kastoria tei

Transcription

kastoria tei

Computing in particle physics:
The DAQ and Controls systems of the
NOvA Neutrino Oscillations Experiment.
Athanasios Hatzikoutelis
University of Tennessee Knoxville
TEI Kastorias
September 12, 2012, Kastoria, Greece.
Outline

Neutrino oscillation experiments.


Short and Long baselines.
The NOvA experiment
The NOvA detectors.
 The NOvA DAQ &DCS.
 Status and outlook.

9/12/2012
A.Hatzikoutelis,TEI Kastoria
2
Basic blocks of matter
Neutrino oscillations
Physics basics
9/12/2012
3
Neutrino Oscillations
Near
9/12/2012
4
Neutrino Oscillations
Far
9/12/2012
5
Short Baseline Reactor sources:
Double Chooz
Studies anti-νe emitted from the two nuclear reactors of the Chooz
power plant, in the French Ardennes to precisely observe the anti-νe
disappearance. (arXiv:1207.6632)
9/12/2012
6
more Short Baseline Reactor sources:
Daya Bay & RENO
Designed to measure the mixing angle
θ13 using anti-νe produced by the reactors of
the Daya Bay Nuclear Power Plant (NPP) and
the Ling Ao NPP. (PRL 108 171803(2012))
9/12/2012
Also see the RENO
experiment.
(PRL 108, 191802 (2012))
7
Long Baseline:
T2K
Flavor mixing from νe-appearance and νµ disappearance. Off axis 2.5o , 0.6 GeV peak.
First indication of
non-zero θ13 ,
PRL 107, 041801,
2011
9/12/2012
8
Long baseline:
MINOS&
MINOS
& NOvA





NO𝜈
NO
𝜈A Far Detector (Ash River, MN)
MINOS Far Detector (Soudan, MN)
Powerful accelerator
sources.
Many years of
running.
Neutrino and antineutrino modes of
running.
Hundreds of km of
beam travel.
Matter effects being a
significant part of the
signal.
9/12/2012
Fermilab
9
The NOvA Experiment

Long Baseline Neutrino
Oscillation Experiment.
Designed to measure:

𝜈𝜇→𝜈e , 𝜈͞ 𝜇→𝜈͞ e , 𝜈𝜇→ 𝜈𝜇 , 𝜈͞ 𝜇→𝜈͞ 𝜇
Precision Measurement: of 𝜃13 , 𝜃23.



Goals:





Determination of the mass
hierarchy.
Observation of CP violation in
the lepton sector.
Resolution of 𝜃23 octant (𝜃23 <
or > 45o ).
Cross section of 𝜈 at 2 GeV.
The Collaboration:

9/12/2012
150+ scientists and engineers
from 27 institutions, 6
countries.
10
The NOvA detector design

32 cell fibers
The Detector Cell
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


9/12/2012
Extruded PVC walls.
Filled with liquid scintillator
Instrumented with wavelength-shifting fiber
Read out by avalanche photodiode (APD).
11
The NOvA detectors

Far detector:


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~14-kton, ~14,700 m2sr acceptance.
tracking calorimeter.
low-Z, highly-active.

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High segmentation.



960 planes x384 cells.
360,000 total channels.
Near detector:




64% active by mass.
X0=38cm (~6cells)
0.3-kton.
Functionally identical as Far.
18,000 channels.
High speed, dead-timeless,
continuous readout.
9/12/2012
12
NOvA prototype Near detector
Near Detector On the Surface (NDOS).
 Used for component production,
installation, and integration.
 Used for development of:

 DAQ
and Controls
 Calibration procedures,
 Validation of simulation,
 Reconstruction algorithms.
9/12/2012
13
NDOS runs


Installation completed in
May 2011.
Positioned


900 m from the NuMI target.
Between 2 beams



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To Far
detector
NDOS
NuMI: Parallel and 110mrad
off center.
Booster: 23o rotated and
inline.
100m above the beams.
Physics runs until May
2012.
Continuing engineering
runs.
9/12/2012
14
Asynchronous Triggering

Trigger info sent over the internet.
 Average
one way flight time is 11ms.
 Designed to tolerate at least 20s of latency.
 Real buffering can be much deeper (60+ minutes)

9/12/2012
Buffered data that has a time overlap with a trigger
window is saved to permanent storage
15
Dead--time
Dead
time--less readout

The electronics are always live, always
digitizing.
 Every
channel of the detector is being
continuously digitized.
The whole system is completely deadtimeless.
 The entire raw detector data stream (up to
4.3GB/s) is actively buffered in a large
computing farm.

9/12/2012
16
The Readout &
Digitization


32 pixel APD reads out
fibers from 32 cells.
FEB: front-end boards

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APD
Custom electronics
provides amplifier/ shaper.
Each pixel/cell
continuously digitized.
Detection threshold set
at ~1/2 MIP

9/12/2012
(6-8 MeV) for muon at far
end of cell.
To
DCM
17
Data Concentration Module
1 DCM=
64 FEB=
2048 cells
detector
9/12/2012
18
Hardware organization
Near detector
3 DCM per block
Far detector
12 DCM per diBlock
9/12/2012
19
Readout Buffering

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The data from DCMs are sent to
a farm of “buffer nodes”
Every 5ms the data stream from
ALL DCMs on the detector is
transmitted into a single buffer
node.
This gives a complete 5ms
snapshot of the detector in that
buffer node
The destination buffer node is
then rotated in a round-robin
pattern through the entire cluster
(1s return to start with nominal
200 buffer nodes)
Projected data rates allows us
to buffer up to 69min of raw, min
bias readout system wide
(baseline buffering 20s)
From A.Norman et.al. CHEP 2012 proceedings
9/12/2012
20
Custom timing system

ARM/PowerPC + FPGAs 56 bit timestamp at 64MHz

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

9/12/2012
Stable system clock (16/64MHz)
Timing Command Data
Synchronization pulses
Loopback calibration
21
Complete NOvA DAQ
9/12/2012
22
9/12/2012
23
Detector Control System (DCS):
NDOS--APD Cooling
NDOS
9/12/2012
NEAR
24
9/12/2012
25
Data Driven Triggers
9/12/2012
26
Neutrino events from the NuMI beam
beam
Cosmics within
the trigger
9/12/2012
27
Far detector Status
Overburden= 3m of
earth equivalent.
Beneficial occupancy of the
building since April 2011.
Construction started
Summer 2012.
Half of the 1st block
assembled
(1/56th of the
detector)
Detector cavern
Before installation
9/12/2012
28
First block
In place
Sept 2012
9/12/2012
29
NOvA construction plans
9/12/2012
30
Next at the Intensity Frontier
9/12/2012
31
…and beyond
NOvA era
9/12/2012
LBNE era
Muon era
32
Conclusions

The latest remarkable measurements in 𝜃13 open the road
for NOvA to address some of the most imposing questions.






NOvA may be able to resolve the mass hierarchy of neutrinos.
Define the 𝜃23 octant.
NOvA may see or at least constrain the extent of CP violation.
The NOvA Far detector is being assembled now and the
Near detector will be ready by 2014.
The prototype NDOS has been valuable in the preparation.
The next 20 years will be a very exciting time in neutrino
experiments at the Intensity Frontier of physics research.
UoM plastics factory.
9/12/2012
33
NOvA Collaboration
Argonne National Lab / Athens / Caltech / Institute of Physics ASCR / Charles University,
Prague / Cincinnati / FNAL / Harvard / India Universities Consortium / Indiana / Iowa State /
Lebedev / Michigan State / Minnesota, Crookston / Minnesota, Duluth / Minnesota, Twin
Cities / INR Moscow / South Carolina / Southern Methodist University / Stanford / Sussex /
Tennessee, Knoxville / Texas, Austin / Tufts / Virginia / Wichita State University / William &
Mary
9/12/2012
34
Extra slides
http://www.fnal.gov/pub/webcams/nova_webcam/
http://www.youtube.com/watch?v=Fe4veClYxkE&feature=youtu.be
9/12/2012
35
Basic building blocks
Neutrino interactions
Physics
9/12/2012
36
Neutrino interactions
9/12/2012
37
Neutrino sources
9/12/2012
38
Neutrino Oscillation
9/12/2012
39
Basic building blocks
The path forward

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



Physics goals

How do particles acquire mass?
Are there extra dimensions of space?
What is the nature of new particles and
new principles beyond the Standard
Model?
What is the dark matter?
What is the nature of the dark energy?
Do all the forces of nature become one
at high energies?
Why is the universe, as we know it,
made of matter with no antimatter
present?
What are the masses and properties of
neutrinos?
Is the building block of the stuff we are
made of, the proton, unstable?
How did the universe form?
http://projectx.fnal.gov/
9/12/2012
40
Since ’60s but most
importantly:


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More questions raised
Super-K (‘98)
KamLand (‘02)
SNO (‘02)
Borexino, SNO+ (presently).

Monitoring solar neutrino fluxes.
Opened the path in the last
century having proved neutrino
oscillations.
Continue with high precision
measurements using new
advanced detectors.




Why do neutrinos have
mass at all?
Why so small?
What are the masses?
Do we need a fourth
neutrino?
Are neutrinos and
antineutrinos the same?
Solar-neutrino oscillation
Solarexperiments
9/12/2012
41
Frontiers in Physics

Energy frontier.
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
Intensity frontier.


rare processes and small effects.
Cosmic frontier.


directly with colliders.
observations.
At the Intensity Frontier

Precision measurements

particle properties


New points of view into high
energies/short distances.

9/12/2012
(mass , couplings, mixing, etc).
Particularly now that new particles
are found at the Energy Frontier.
42
Neutrino
Oscillations
Principles
  
(23) Sector: Atmospheric +
Accelerator
L/E ~500 km/GeV
m232 (m2atm) = 2.3  10-3 eV2
sin2(223) >0.96
  e
(13) Sector
e  , 
(12) Sector: Reactor + Solar
L/E ~15000 km/GeV
2
m 21 (m2sol) = 7.5  10-5 eV2
tan212 = 0.45
Analogous to CKM Quark Mixing Matrix :
Mixing in lepton sector larger than in quark sector
23 maximal, 12 large, 13 very small, zero?
CP violation present in lepton sector? Large enough to explain
observed matter-antimatter asymmetry?
9/12/2012
43
Short baseline oscillations

Survival probability of anti-νe


No matter effects
No CP violation contribution.

Detection Signal:

Prompt signal from the positron


9/12/2012
0.7 < E < 12.2 MeV
Delayed signal from the neutron
capture.
44
Ranging
Short
Baselines
9/12/2012
45
Oscillations with long baseline

Accelerator driven.



Muon neutrino beam.
Matter effects present.
CP violation and mass hierarchy dependence.
9/12/2012
46
The latest measurements

Oscillation measurements:









From arXiv:1207.6632
3 mixing angles.
2 mass differences.
1 CP violating phase.
The mixing angles and the complex
phase are connected in the PMNS
matrix.
The θ13 went from the last unknown
angle to the best measured in a year.
K. Abe et al., Phys.Rev.Lett. “T2K” 107, 041801 (2011), 1106.2822.
P. Adamson et al., “MINOS” Phys. Rev. Lett. 107, 181802 (2011), hepex/1108.0015v1.
F. P. An et al, “Daya Bay” PRL 108,171803(2012), arXiv:1203.1669 [hep-ex].
Y. Abe et al, “Double Chooz ”arXiv:1207.6632v1[hep-ex] 27 A July 2012, DC
first indications arXiv:1112.6353[hep-ex] 13 March 2012.
9/12/2012
Error bars correspond to 1σ, except for T2K,
where the 90% CL interval is shown. For T2K and MINOS
the CP phase δ has been fixed (arbitrarily) to δ = 0.
47
The NuMI beam
(Neutrinos at the Main Injector).

Off-axis Neutrino energy spectrum


14 mrad off-axis yields a narrows band.



flattens out (tightens):
peaked at 2GeV
with Eν width ≈20%
The detector technology, geometry and
baseline are tuned to give:



L/E for 1st Oscillation Maximum.
Energy resolution for νμ CC events ≈4%
High efficiency EM shower reconstruction in
sub 2GeV region.
10s beam spill
(every 2.2 sec).
9/12/2012
48
Intensity Frontier:
Accelerator and NuMI upgrades

Shutdown May 2012 – April
2013.



Increase beam power to 700
kW.
The Recycler will be converted
to an accumulator.
Cycle time of the Main Injector
reduced to 1.33 s.


double the beam intensity for
NOvA
NuMI will be outfitted



New target and horns.
Shielding pile will be un-stacked
Move horn 2 to its location for
NOvA .

9/12/2012
10m downstream of its current
location.
49
The measurement principle

Independently measured
appearance probabilities:


The result depends on :



At 2 GeV neutrino energy.
for all 𝛿 and
both
hierarchies
ignoring
spectral
information
CP phase 𝛿
sign(m2) .
Allows for comparison of
rates to theory,
parameterized in the CPviolation parameter.
9/12/2012
50
NOvA measurement examples:
𝜃23 octant sensitivity
Expected NO𝜈A contours for one
example scenario at 3 yr + 3 yr
Simultaneous hierarchy,
CP phase, and
𝜃23 octant information
from NO𝜈A
9/12/2012
𝜈e
𝜈𝜏
𝜈3
𝜈e
?
𝜈𝜇
𝜈𝜏
𝜈𝜇
In “degenerate” cases, hierarchy and
𝛿 information is coupled. 𝜃23 octant
information is not.
51
The NOvA measurement
Example (for a maximal 𝜃 ) :
 Resolving Mass Hierarchy

Enhancement or
suppression of rates :
~ 30% from the baseline due
to matter effects.
Normal

Inverted
23

Potential for 2σ resolution

9/12/2012
3 year NOvA run on each mode
over 38% of the space in δCP
52
Topologies of the basic interactions
Efficiency 48% identifying ve CCQE and 1% fake NC rate
Proton recoil ~ few MeV.
1 meter
beam
𝜇+p
proton
Michel eGoal: large target mas & high granularity
e+p
𝜋0 + p
(simulated events with 2 GeV visible)
9/12/2012
53
Position dependence of cell
response (light attenuation)
Michel electrons
Calibration (NDOS)
9/12/2012
54
Neutrino events from the BNB beam
The reconstruction analysis can find the Booster neutrino directions at 23o from
the axis of the detector setup.
9/12/2012
55
Mass Hierarchy resolution
NOvA alone (left ) and with T2K predictions (right) based on numbers in
their 2011 publication and on 5.5E21 p.o.t., a number that comes from
projections for 2019,
9/12/2012
56

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