1. Giles Barr Cosener’s House 19 Feb 2005
Neutrino Production in the Atmosphere and Accelerator Hadron Yield Measurements
Giles Barr
Cosener’s House
19 Feb 2005

2. Synopsis Section 1: Production of Neutrinos by Cosmic Rays
Neutrino Oscillations (brief)
Fluxes and their calculations
Key uncertainties
Section 2: Hadron production
Experiments: HARP/NA49/MIPP
Section 3: Outlook
Errors on fluxes
Further measurement possibilities with atmospheric neutrinos

3. Neutrinos produced from a shower
Primary cosmic ray
Neutrinos produced from a shower π π N
Primary cosmic ray: proton or heavier nucleus
Interacts in ~90g/cm2
Atmosphere depth 1050 g/cm2
Cascade
Most hadrons don’t reach ground. N π K ν μ

4. SuperKamiokande results (1)
hep-ex/

5. SuperKamiokande results (2)
From hep-ex/ : PRL 93 (2004)

6. Soudan2 e e μ μ 5.9 kton・yr exposure
Partially contained events included.
L/E analysis with the “high resolution” sample
Reconstructed Lν/ Eν dist.
Zenith angle
Phys.Rev. D68 (2003) e e μ μ
Up-going
Down-going
No osc.
nm  nt osc.

7. Contained
Partially C
Through Going ν induced μ
Eν (GeV)

8. Eν (GeV) Contained Partially C Through Going ν induced μ Osc Max Down
Horizontal Up
Δm2=2.5 x 10-3 eV2

9. Eν (GeV) Pions Interact Vertical μ reach Earth’s surface
Kaons Interact
Contained
Partially C
Through Going ν induced μ
Eν (GeV)
3D effects
Osc Max
Down
Horizontal Up

10. Summary of Atmospheric Neutrino Calculations
Zatsepin, Kuz’min
SP JETP 14:1294(1961) 1D
E. V. Bugaev and V. A. Naumov,
PL B232:391 (1989)
Agrawal, Gaisser, Lipari, Stanev
PRD 53:1314 (1996)
Target
D. Perkins
Asp.Phys. 2:249 (1994) Mu
Honda, Kajita, Kasahara, Midorikawa
PRD 52:4985 (1995)
FRITIOF
Battistoni et al
Asp.Phys 12:315 (2000)
Asp.Phys 19:269 (2003) 3D
FLUKA
P. Lipari
Asp.Phys 14:171 (2000)
V. Plyaskin
PL B516:213 (2001)
hep-ph/
GHEISHA
Tserkovnyak et al
Asp.Phys 18:449 (2003)
CALOR-FRITIOF
GFLUKA/GHEISHA
Wentz et al
PRD (2003)
Corsika: DPMJET VENUS, UrQMD
Liu, Derome, Buénerd
PRD (2003)
Favier, Kossalsowski, Vialle
PRD (2003)
GFLUKA
Barr, Gaisser, Lipari, Robbins, Stanev
PRD (July 2004)
PRD (2001)
PRD submitted (2004)
DPMJET

11. Key uncertainties Hadron production Primary Fluxes (Geomagnetic Field)
3D effects
Atmosphere

12. dφ/d ln(E) (m-2s-1sr-1)

13. Azimuth angle distribution East-West effect
Eν>315 MeV
Eν>315 MeV

14. Return to 3D: Is it important?
bigger 3D
>30%
10%-30%
3%-10%
<3%
1D bigger
SuperKamiokande Collaboration
hep-ex/

15. Flux of primaries at top of atmosphere
Primary fluxes
dN/dEK /m2/s/sr/n
Protons α K b c H
2.74
14900
2.15
0.21 He
2.64
600
1.25
0.14
CNO 14
2.70
62.4
1.78
0.02
Ne-Si 24
21.4
Fe(56)
5.1
Helium
Protons = 75% of all nucleon fluxes
Helium = 15% of all nucleons = 60% of all nuclei.
Primary Kinetic Energy (GeV/n)

16. Residuals: Newest measurements
(Data-Fit)/Fit
100%

17. Helium Fluxes
(Data-Fit)/Fit
100%

18. Section 2: Hadron production Measurements at Accelerators

19. Summary of measurements available10
Boxes show importance of phase space region for contained atmospheric neutrino events.
Daughter energy
1 TeV
100 10
1 GeV
1 GeV 10
100
1 TeV 10
Parent energy

20. PT range covered 1 GeV 10 100 1 TeV Daughter energy
Boxes show importance of phase space region for contained atmospheric neutrino events.
SPY
Atherton et. al.
Barton et. al.
Serpukov
Allaby et. al.
Eichten et. al.
Cho et. al.
Abbott et. al.
Measurements.
1-2 pT points
3-5 pT points
>5 pT points
1 GeV 10
100
1 TeV
Parent energy

21. pT range coverage
This energy is best situation

22. New measurements 1 GeV 10 100 1 TeV Daughter energy
Boxes show importance of phase space region for contained atmospheric neutrino events.
MIPP
NA49
HARP
New measurements.
1 GeV 10
100
1 TeV
Parent energy

23. Plot courtesy of M. Messier
Another view (MINOS)...
Atherton
400 GeV Be
Barton
100 GeV C
Spy
450 GeV Be
Plot courtesy of M. Messier

24. NA20 (Atherton et al.), CERN-SPS (1980)
H2 beam line in the SPS north-area
Secondary energy scan: 60,120,200,300 GeV
Overall quoted errors
Absolute rates: ~15%
Ratios: ~5%

25. Needs... Pion and kaon production Projectile: p, He, π, K etc.
Very large range of primary energies [2 GeV,>1 TeV]
Target: Air nuclei (nearby isoscalar nuclei acceptable)
Full phase space coverage
pT distribution not interesting
Full coverage of pT important
Importance of kaons at high energy
(Thanks to S. Robbins for plot)

26. NA49

27. NA49 experimental layout
Vertex TPCs
Main TPCs
Target
S4 counter
Gap TPC

28. NA49 originally designed for Lead-Lead collisions.
Also used for pp and pA collision physics

29. NA49 Proton-Carbon run
‘P322 group’ consisting of some atmospheric neutrino flux calculators, HARP experimentalists and MINOS experimentalists formed collaboration with NA49 and proposed a series of measurements.
Received a 1 week test run with a carbon target.
It took place in June 2002.
158 GeV run, 500k triggers.
100 GeV run, 160k triggers.
1% interaction length carbon target.
Immediately preceeding run was an NA49 proton-proton run, using a liquid hydrogen target.

30. Main TPC
Left
Vertex TPC 1
B=1.7T
Vertex TPC 2
B=1.7T
Gap
TPC
Main TPC
Right

31. Particle ID
NA49 dE/dx plots
dE/dx plot for positives
P (GeV)

32. Particle ID
NA49 dE/dx fits

33. Bins Technique: Follow closely the analysis of p-p data xF and pT bins
Some corrections are identical
Pion analysis

34. Pion extraction straightforward
Analysis:
Get pion yields for proton-proton,
followed by pion yields for proton-carbon
Later, do kaons, antiprotons.
Pion extraction straightforward
shifts and resolution easy to determine
Above xF = 0.5, dE/dx information not available near gap. We do have the track distributions.
Particular region at low xF where π and p dE/dx curves overlap. Use reflection in p-p.
Almost no information at negative xF

35. Corrections and errors on pion yields
Binning correction
~1%
Target re-interaction
<1%
Detector material interaction
<1%→few %
S4 trigger correction
5-15%
Feed down correction
K0, Λ0, Σ decays
In progress
Pion→Muon decay
small
K→pion decay

36. HARP

37. The Harp detector: Large Acceptance, PID Capabilities , Redundancy
Threshold gas
Cherenkov:
p identification
at large Pl
TOF:
p identification
in the low Pl
and low Pt
region
Drift Chambers:
Tracking and low
Pt spectrometer
EM filter (beam
muon ID and
normalization)
Target-Trigger
0.7T solenoidal coil
Drift Chambers:
Tracking
TPC, momentum
and PID (dE/dX)
at large Pt
1.5 T dipole spectrometer

38. HARP Experiment Targets: LH2, LD2, LO2 LN2 Be, C, Al, Cu, Tn, Sn, Pb
Beam 3-15 GeV secondaries from CERN PS
Collected data 2001, 2002
Close to full acceptance
Targets:
LH2, LD2, LO2 LN2
Be, C, Al, Cu, Tn, Sn, Pb
O(106) events per setting
2% accuracy non è molto chiaro
pi+/pi- ratio
a che energie le cross section?
all phase space
spezzata in due

39. Beam Particle Identification
Beam Time Of Flight (TOF):
separate p/K/p at low energy
over 21m flight distance
time resolution 170 ps after TDC and ADC equalization
proton selection purity >98.7% p
3.0 GeV/c beam K d
12.9 GeV/c (K2K) Beam
p/d p
Beam Cherenkov:
Identify electrons at low energy, p
at high energy, K above 12 GeV
~100% eff. in e-p tagging K
Cherenkov ADC

40. Forward PID: TOF Wall Separate p/p (K/p) at low momenta (0–4.5 GeV/c)
42 slabs of fast scintillator read at both ends by PMTs
3 GeV beam particles
PMT
data p
Scintillator p
TOF time resolution ~160 ps
3s separation: p/p up to 4.5 GeV/c
K/p up to 2.4 GeV/c
 7s separation of p/p at 3 GeV/c

41. Pion yield: K2K thin target
5%l Al target (20mm)
Use K2K thin target (5%l)
To study primary p-Al interaction
To avoid absorption / secondary interactions
K2K replica (650mm)
p > 0.2 GeV/c
|y | < 50 mrad
25 < |x| < 200 mrad
Raw data 2 4 6 8 10
-200
-100
100
200
P(GeV/c)
qx(mrad)
p-e/p misidentification
background

42. Brookhaven National Laboratory R. Winston EFI, University of Chicago
Y. Fisyak
Brookhaven National Laboratory
R. Winston
EFI, University of Chicago
M.Austin,R.J.Peterson
University of Colorado, Boulder,
E.Swallow
Elmhurst College and EFI
W.Baker,D.Carey,J.Hylen, C.Johnstone,M.Kostin, H.Meyer, N.Mokhov, A.Para, R.Raja,S. Striganov
Fermi National Accelerator Laboratory
G. Feldman, A.Lebedev, S.Seun
Harvard University
P.Hanlet, O.Kamaev,D.Kaplan, H.Rubin,N.Solomey, C.White
Illinois Institute of Technology
U.Akgun,G.Aydin,F.Duru,Y.Gunyadin,Y.Onel, A.Penzo
University of Iowa
N.Graf, M. Messier,J.Paley
Indiana University
P.D.BarnesJr.,E.Hartouni,M.Heffner,D.Lange,R.Soltz, D.Wright
Lawrence Livermore Laboratory
R.L.Abrams,H.R.Gustafson,M.Longo, H-K.Park, D.Rajaram
University of Michigan
A.Bujak, L.Gutay,D.E.Miller
Purdue University
T.Bergfeld,A.Godley,S.R.Mishra,C.Rosenfeld,K.Wu
University of South Carolina
C.Dukes, H.Lane,L.C.Lu,C.Maternick,K.Nelson,A.Norman
University of Virginia
~50 people, 11 graduates students, 11 postdocs.

43. MIPP :Physics Program Netrinos related Measurements
Particle Physics-To acquire unbiased high statistics data with complete particle id coverage for hadron interactions.
Study non-perturbative QCD hadron dynamics, scaling laws of particle production
Investigate light meson spectroscopy, pentaquarks, glueballs
Nuclear Physics
Investigate strangeness production in nuclei- RHIC connection
Nuclear scaling
Propagation of flavor through nuclei
Netrinos related Measurements
Atmospheric neutrinos – Cross sections of protons and pions on Nitrogen from 5 GeV- 120 GeV (5,15,25,5070,90) GeV
Improve shower models in MARS, Geant4
Make measurements of production of pions for neutrino factory/muon collider targets
MINOS target measurements – pion production measurements to control the near/far systematics
Complementary with HARP at CERN

44. Brookhaven Experiment 910
E910 used a spectrometer with good acceptance and particle ID over the momentum and angular range of interest to MiniBooNE.
Particle ID from dE/dx in the TPC, threshold Čerenkov, and Time of Flight.

45. The Results
The π+ production cross section for a beam momentum of 17.6 GeV/c.
Preliminary

46. Sanford-Wang Fit Results
6.4 GeV/c
12.3 GeV/c
Preliminary
Preliminary

47. Section 3: Outlook Estimating impact of Hadron production New measurements with atmospheric neutrinos.

48. Estimating Hadron production errors on Cosmic Ray fluxes

49. π production at 20 GeV

50. Lower energy

51. Proposed total errors Pions Kaons xLAB (low edge) .0 .1 .2 .3 .4 .5 .6.7 .8 .9
<8 GeV
10%
30%
40%
8-15 GeV
15-30 GeV 30 10 5% 20
GeV
15% 40
>500 GeV
15%+Energy dep.
30%+Energy dep.

52. More sophisticated combination
(1)
Pions
Kaons
xLAB (low edge) .0 .1 .2 .3 .4 .5 .6 .7 .8 .9
<8 GeV
10%
40%
8-15 GeV
15-30 GeV 5%
GeV
15%
30%
>500 GeV
Pions
Kaons
xLAB (low edge) .0 .1 .2 .3 .4 .5 .6 .7 .8 .9
<8 GeV
10%
30%
40%
8-15 GeV
15-30 GeV 30 10 5% 20
GeV
15% 40
>500 GeV
15%+Energy dep.
30%+Energy dep.
Flaws: No difference pi+pi-, or K+K-

53. νμ/anti-νμ Flux syst errors Flux & syst errors Flux ratio syst errors

54. Possible future atmospheric n detectors
Very large water Cherenkov detector
UNO
Hyper-K (1Mton)
Mton class detector at Frejus
Magnetized large tracking detector
MONOLITH,　
INO (India-based Neutrino Observatory, …

55. 1+multi-ring, e-like, 2.5 - 5 GeV
Search for non-zero q13
(Dm122=0 assumed)
MC, SK 20yrs
En(GeV)
cosQ
Matter effect
1+multi-ring, e-like, GeV
Electron appearance
s213=0.05
s213=0.00
null oscillation
cosQ
Electron appearance in the 5 – 10GeV upward going events.
From: Talk by T. Kajita, NuFact 04 (Osaka U. Aug 2004)

56. Quick glance of oscillation effects
s22q12=0.825
s2q23=0.4
s2q13=0.04
dcp=45o
Dm212=8.3e-5
Dm223=2.5e-3
From: Talk by M. Shiozawa
Workshop on Sub Dominant
Oscillation Effects, Kashiwa
Dec 2004
Y(ne)/Y0(ne)
s2q13=0.0

57. effect of dCP dCP= 45o dCP=225o s22q12=0.825 s2q23=0.5 s2q13=0.04
dcp=45o or 225o
Dm212=8.3e-5
Dm223=2.5e-3

58. effect of dCP after n interactions
s22q12=0.825
s2q23=0.5
s2q13=0.04
dcp=0o~360o
Dm212=8.3e-5
Dm223=2.5e-3
no osc. with 80yrs stat.error
dCP= 45o
135o
225o
315o
slightly enhance the effect by taking ratio of Ne/Nm (not shown here)

60. Shower graphic from ICRC
80km altitude
Detector
No energy threshold
Earth’s surface

61. Shower graphic from ICRC
80km altitude
Detector
No energy threshold
Earth’s surface

62. Also, other detectors: Soudan/Macro
Soudan-2 Preliminary
The main effect happens near horizon, just where the L changes *VERY* rapidly with energy.
Soudan-2 Preliminary