1. Neutrino Physics & Astrophysics : Overview
Neutrino Physics: WHY & HOW
Highlights : solar neutrinos (+ atm. n)
Highlights : Future Projects
TEXONO research program in Taiwan
Experimentalists
Theorist
Henry T. Wong / 王子敬
Academia Sinica / 中央研究院
@ NTHU / 國立清華大學
October 2002

2. Nobel Prize in Physics (2002) 50% for n astrophys. :
Ray. Davis Jr. (U. Penn) :
“Classic” Chlorine Expt.
Masatoshi Koshiba (U. Tokyo) :
Kamiokande & SuperK
Citations leave room for future prizes on n physics !!!
50% to Riccardo Giacconi, in X-Ray Astronomy

4. Neutrino Physics Road-Map
Grand Unified Theories (GUT)
L(n-mass)0
Structures & Compositions of Universe
mn’s;Uij’s 0
n-Oscil.
mn’s
n-decays
0nbb
b-spect.dist.
anomal. int.
……….
Particle Physics
Cosmology
Nuclear Physics
Astrophysics
n’s as Probe

5. Neutrino Physicist :

6. Neutrino History 1914: continuous b-spectra (Chadwick)
1930: postulation of neutrinos (Pauli)
1934: theory of b-decay (Fermi)
calculation of s(np) (Bethe,Peierls)
1956: observartion reactor ne (Reines,Cowan)
1957: measurement of n helicity (Goldhaber)
1962: discovery of accelerator nm (BNL)
1968: observation of solar neutrinos (Davis)
1974: discovery of weak neutral currents (CERN)
1987: observation of supernova SN1987a n’s (IMB,Kamiokande)
1989: three families of light neutrinos (CERN)
1998: evidence of atmospheric neutrino oscillation (Super-Kam., …)
2000: observation of nt (Fermilab)
2001: evidence solar neutrino oscillation (SNO+SK+GALLEX ……)

7. Neutrino Sources n‘s everywhere: 300 per c.c.
Observed window
n‘s everywhere:
300 per c.c.
from sun, supernovae, cosmic rays, reactors, accelerators, astrophysical sources, & relic Big Bang …

8. Cross Sections Challenges of Neutrino Experiments :
Strong
Electro-magnetic
Weak
 l(H2O)  250 light years !
Challenges of Neutrino Experiments :
“How to Beat the Small Cross-Section?”
i.e. By building Massive Detectors
 while keeping cost/background Low !

9. Super-Kamionkande
※ Water Cerenkov detector: 5k tons, viewed by 11,000+ =50 cm PMTs
in 1000 m underground site in central Japan
※ Physics: solar n, atmospheric n , long baseline accelerator n, proton decays ..
※ Accidents (PMTs imploded) Nov 01, 50% PMT data again end of 02 !!!

10. Atmospheric Neutrinos
nm disappearing, ne OK,
Strong evidence : > 15s
Better fits for nt appearing e n n

11. Solar Neutrinos

12. Measurement of Eccentricity of Earth’s Orbit !!!
The Sun IS Burning !!

13. Sudbury Neutrino Observatory (SNO)
※ Heavy Water Cerenkov detector: 1k ton, shielded
by 7k ton of water viewed by 9456 PMTs located
2000 m underground in Canada.
※ Physics: Solar n …

14. Actual measurements : only detect e- (a burst of light) : deconvolute the channels

15. (also Cl, Ga, diff. E)
(also SK)
( 5s effect )

16. Three Families of Neutrino Mixing
The Maki-Nakagawa-Sakata (MNS) matrix :
atmospheric
solar
Possible CP Violation in n Sector:

18. Dm2 –  : Summary
PDG 2000:
2002

19. KEK-SuperK (K2K) Accelerator n Flight path 250 km
Goals : confirm SK atm. n results, measure 23
First results consistent with SK
2006+ , evolve to JHFSK

20. KamLAND
Long Baseline Reactor n (sensitive to 20% of world’s reactors !)
ave. flight path of 160 km
1 kton liquid scintillator in old Kamiokande site
probe “LMA” for solar n
first results “any time” (only 5 years from approved !!!!)

21. Fermilab: NuMI to MINOS (2004+)
CERN: CNGS to Gran Sasso (2006+)
Both with 750 km baseline accelerator n beams
Precision measurement of atm. n’s q23
Explicit observation of nt

22. IceCube – km3 n Telescope
※ To detect high
energy n’s
South Pole
AMANDA
IceCube

23. Neutrino Factory with Muon Storage Ring
ne & nm + anti-n’s, control & selectable
intense source
known spectra
precision measurements of Dm2 and ij
search of CP violation
need O(1000 km) baseline
BIG projects !!!

24. TEXONO* Collaboration
W.C. Chang¶, C.P. Chen, K.C. Cheng, H.C. Hsu, F.S. Lee, S.C. Lee, S.T. Lin,
D.S. Su, P.K. Teng, W.S. Tse¶, H.T.K. Wong†, C.S. Wu, S.C. Wu
Academia Sinica, Taipei, Taiwan
W.P. Lai
Chung Kuo Institute of Technology, Taipei, Taiwan
C.H. Hu, J.M. Huang, W.S. Kuo, T.R. Yeh
Institute of Nuclear Energy Research, Lungtan, Taiwan
H.B. Li, M.Z. Wang¶
National Taiwan University, Taipei, Taiwan
J.H. Chao, J.H. Liang
National Tsing Hua University, Hsinchu, Taiwan
Z.M. Fang, R.F. Su
Nuclear Power Station II, Kuosheng, Taiwan
M. He, S. Jiang, L. Hou, H.Q. Tang, B. Xin, Z.Y. Zhou¶
Institute of Atomic Energy, Beijing, China
J. Li†, Y. Liu, Z.P. Mao, J. Nie, J.F. Qiu, H.Y. Sheng, P.L. Wang, X.W. Wang,
Q. Yue, D.X. Zhao, J.W. Zhao, P.P. Zhao, S.Q. Zhao, B.A. Zhuang
Institute of High Energy Physics, Beijing, China
Z.S. Liu, Z.Y. Zhang
Institute of Radiation Protection, Taiyuan, China
T.Y. Chen
Nanjing University, Nanjing, China
J.P. Cheng, D.Z. Liu
Tsing Hua University, Beijing, China
C.Y. Chang, G.C.C. Chang†
University of Maryland, Maryland, U.S.A.
† Co-Prinicipal Investigators
¶ Project Leaders
Ph.D. Students
*Taiwan EXperiement On NeutrinO
Home
HISTORY
Initiate : Chang Chung-Yung 1996
First Collab. Meeting/Official Start : October 1997
First Paper : October 1998
KS Reactor Experiment Installation : June 2000
First Ph.D. : Liu Yan , July 2000
First Physics Data Taking : June 2001.

25. TEXONO Overview Goals : Program: Neutrino and Astroparticle Physics
 Starting phase: 1st particle physics expt in Taiwan
Build up a Qualified Group
 1st big research Coll. % Taiwan & China
Kuo-Sheng Reactor Neutrino Lab.
※ reactor : high flux of low energy electron anti-neutrinos
※ mn0  anomalous n properties & interactions
※ n’s strange & full of surprises
 study/constraint new regime wherever possible experimentally
R&D Projects
 diversified program ※ reactor program as base
※ explore various future scenarios
Program:

26. Kuo-Sheng Nuclear Power Plant
KS NPS-II :
2 cores X 2.9 GW
KS n Lab:
28 m from
core#1

27. Kuo-Sheng Neutrino Laboratory
High flux of ne (also ….. ne )
Modular Design : independent detector, electronics, shielding
high-Z target, large re
Improved detector performance:
 good energy & spatial resolution,
 low threshold, a/g separation
Elaborate electronics+DAQ+control sys.
 complete record of pulse shape + timing info.
Elaborate Shieldings
 radon purge & 4p cosmic veto
Configuration:
Modest yet Unique
Flexible Design:
Allows different detectors
conf. for different physics

28. Kuo Sheng Reactor Neutrino Laboratory
Front Gate
Front View
(cosmic vetos, shieldings,
control room …..)
Inner Target Volume

29. ULB-HPGe + Anti-Comptons
KS Expt. : Period I Configuration
Period I : June 01 – April 02 (60 days OFF)
Shielding & Veto [one side]
ULB-HPGe + Anti-Comptons
CsI(Tl) Array (46 kg)

30. KS Expt: Period I Detectors
ULB-HPGe [1 kg]
CsI(Tl) [46 kg]
FADC Readout
[16 ch., 20 MHz, 8 bit]
Multi-Disks Array [600 Gb]

31. mn with Reactor ne mn Experimental Probe:
 parametrize possible niL njR + g vertices
  both i = j “diagonal” & i  j “transition” moments
Experimental Probe:
 Study ne + e-  nX + e-
 Focus on low recoil energy
※ sm  T–1
※ decouples SM “background”
[ ……… LE reactor f(ne) not accurately known]
 Look for Excess in Reactor ON/OFF
Neutrino Radiative Decay (Gn):
 sm & Gn related:
 same vertices – real g for Gn
Electron Recoil Spectra

32. Reactor mn(ne) Sensitivities
Gn Sensitivities

33. KS/P1 Analysis HPGe : exploit the low threshold data
Established Problem:
mn and Gn for ne via : ne + e  nx + e
Speculative Analysis:
※ study ne flux from reactor
 due to neutron excitation producing
e.g. 51Cr, 55Fe [distinct energy & timing …..]
 study mn & Gn for ne
※ anomalous Neutrino Interactions in Matter
e.g. anomalous energy deposition X (>eV)
ne + N  nx + N + X
[similar analysis as accelerator nm]
※ study possible nuclear transitions
e.g. 73Ge* decays by 2g’s separated by t1/2=4.6 ms
CsI(Tl) : Technical Run
Event Reconstruction
Background Studies
Optimize for P2

34. CsI(Tl) Array : Highlights
40 cm length (longest commercial prod.)
Energy+3D info:  10% FWHM at 660 keV
 s(z) <2 cm @ E>250 keV
Detector Threshold ~ 20 keV
PSD for g/a : > 99%
Intrinsic Purity :  238U/232Th < g/g (equil.)
 40K < g/g
cosmic muon events 46 kg target
Goals:
Commission 180+ kg target on-site
for Period-II
DAQ with large dynamic range

35. KS Expt.: Future Thoughts
Existing configurations:
 push mn/Gn sensitivities
 s(ne–e) scatterings
 analysis opened up by low threshold
Push threshold lower ( X 1/10 )
 coherent nN scattering [ observe SM + test exotic processes….]
Insert passive targets for s(nucl.) e.g. 6Li, 7Li, 10B, 11B,2H ..
 s(NC) related to axial isoscalar &
strange quark structure in nucleon
As base to launch other projects
 explored by R&D program

36. R&D Projects Upgrading FADCs
Explore New Detectors Scenarios
 loaded crystal scintillator
 ultra low energy HPGe
CsI(Tl) for Dark Matter Searches
Upgrading FADCs
Trace Radio-purity with AMS ( Accelerator Mass Spectrometry)
Sono-Luminescence Project
Close Contact with :  CsI(Tl) CDM Korea
 JHFBeijing LBL n IHEP
 Ultra HE (1015 eV) n NTU

37. Status: TEXONO Collaboration: Kuo-Sheng Neutrino Lab.:
 Built-Up and Growing
Kuo-Sheng Neutrino Lab.:
 Established & Operational
※Modular & Flexible Design
 Physics Data Taking since June 01
※Unique HPGe Low Energy Data
※ Bkg Level ~ Underground CDM Expt.
Expect Results on mn (Gn) soon
※ Other speculative analyses under way
Preparation of Period-II DAQ
 Improved HPGe Conf.
 Commissioning 150+ kg CsI(Tl) [+ s(ne) …]
Diversified R&D Program in parallel

38. Summary & Outlook Neutrinos are important but strange objects
history of n physics full of surprises !
Strong evidenceS of massive n’s & finite mixings
Physics Beyond the Standard Model !
More experiments & projects coming up
EVEN MORE EXCITEMENT !
TEXONO is also a (modest) part of it