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					Oto Cosmo Observatory
    Present and Future
       Hiro Ejiri
       RCNP Osaka Univ., & JASRI Spring 8
       For the ELEGANT Collaboration




                    1. Oto Cosmo Observatory
                    2. Detectors and Physics Results
                    3. Future Plans

                    4. Progress of Oto Lab.
                      Ring Cycrotron lab.
                      0.4-0.5 GeV p, & light ions
     RCNP
Research Center
      for
Nuclear Physics

National Nuclear                                    National and
                   RCNP laboratory complex          International users
  Physics Lab.

Nucleon, Meson,
    and
Quark Lepton

Nuclear Physics.
             RCNP & Physics Osaka Univ.
           Neutrinos and DM research programs
                                 .

 I. Oto Cosmo Observatory Underground Lab.
 n masses and natures by bb with ELEGANT V & VI
     DM WIMPs search by nuclear scattering .
 II. Cyclotron Lab. Charge exchange spin flip reactions to study
     nuclear responses for charged weak currents.
 III. Laser Electron Photon Lab. at Spring 8.
     Nuclear responses for neutral weak currenta.
Oto Lab. is close to
Osaka Univ. 100 km
Kansai/Osaka Airport 40 km
                         SK




       Osaka Univ.

   Air port




                         Oto
                    Oto Cosmo Observatory
Unused 5 km                60 km south of Osaka, near Int. Airport
  railway tunnel.
    1400 m we
                         Nishiyoshino                               Oto
                                        Lab.II   Lab.I, III
Lab.I, lab.II, lab.III
                                                                     To
                                                                    Osaka
 New labs can be set
 in the center region
 of the 5 km tunnel.
   H. Ohsumi
Proc. XI RCNP. Symp.,
  World Scientific,
 (1996) 274-279
                           Lab. II. 45 m2                 Lab.I. 33 m2
 http://www.rcnp.        ELEGANT V, bb of                ELEGANT VI
 Osaka-u.ac.jp/             100Mo and                  bb of 48Ca and DM
    Divisions/
 np1-c/index.html
                           DM with NaI                     with CaF2
Experimental Roon I
 Muon flux
       at
underground labs.     Oto Cosmo Observatory 1400 m w.e
     in the
      world

         m
   4 10-3 /m2/s

    Neutron
   4 10-1/m2/s

   Rn 10 Bq/m3
(Detector container
   10 m Bq /m3)
         III. ELEGANT V
   ELEctron GAmma-ray Neutrino Telescope
ELEGANT V                H. Ejiri et al. NIM A302 1991 304
 bb of 100Mo,116Cd bb-ray E&T PL g-ray by NaI
           DM –nucleus recoil E by NaI




                                                    .   
         100Mo        0nbb by ELEGANT V
 100M0   95% enriched. 0.17 kg.

   Most stringent limit by
    exclusive(bb tracking)

   T0n > 1.0 (0.55) 1023y
                 68(90)%CL


   <mn> < 1.5 (2.1) eV
   <gB> < 9 (11) 10-5

H.Ejiri, N.Kudomi, et al.,
Phys. Rev. C 63 ’01, 65501
Present
         ELEGANT VI
CaF2 for 48Ca bb and 19F Spin Coupled DM
                         ELEGANT IV
         CaF2 for 48Ca bb and 19F Spin Coupled DM
CaF2(pure) as light guide &
active shield against PMT
CaF2(Eu) is not transparent
for U.V. light.
bb & DM signals selected by
role off ratio
            Measurement of 48Ca bb at Oto
Isotope                            48Ca    76Ge    82Se   100Mo    116Cd   136Xe   150Nd

Q-value (MeV)                       4.27    2.04   3.00   3.03      2.80    2.48   3.37
G0v×10-25 (year-1eV- 2.44 0.244 1.08 1.75
 48Ca double beta decay                                             1.89    1.81   8.00
2)

                          10 3
          counts/20 keV


                                     BG (sim)
                                                                                      no even
                               2
                          10


                                                           0nbb window
                          10
                                     2nbb (sim)
                                                                                      T1/2 > 1.
                           1



                      10 -1
                       2000                3000            4000              5000
                                                                  Energy (keV)


    T0n > 1.8 1022 y 90 % CL                         I. Ogawa et al., PANIC02, Nucl.Phys.2003
                      ELEGANT VI CaF2
 19F    light mass and simple large spin matrix element




I. Ogawa, et al. Nucl. Phys. 663(2000) 869c   R. Hazama, NIM A482 (2002) 297
                 Results of ELEGANT’s
Double beta decays
    EL III . Ge with NaI for bb of 76Ge : Limit of 1.9 eV (68% CL) on
            mn and 1st stringent limit on 0nbb to 2+ state.
    EL IV. 100Mo with Si detector array and Nal.
    EL V. Drift chamber for bb tracks , plastic scintillators for bb
            and NaI for g.
             1st 2nbb lives for 100Mo and 116Cd.
            Most stringent limits on onbb 100Mo mn < 1.5 eV(68% CL).
     EL VI. Ca(F)2 Crystals with CsI. Limit on 0nbb of 48Ca: 7 eV
     Dark matter
     EL V. NaI 760 kg , annular modulation of WIMPS .
           Most stringent limits at the low mass region.
     EL VI. Ca(F)2 Spin-coupled WIMPS.
    http://www.rcnp.osak-u.ac.jp/~ejiri/PUB.html
        V. Future Experiments

   A. MOON
   Molybdenum Observatory Of Neutrinos for
   bb and low energy solar n’s.
   MOON 1 Proto - type MOON and R&D.


   B. CANDLES
    CA lcium fluoride for studies of Neutrinos and
    Dark Matters by Low Energy Spectrometers
          V. Future Experiments I
                  MOON.
    Molybdenum Observatory Of Neutrinos for
              http://ewi.npl.washington.edu.
 . bb-n, and low energy solar and supernova n’s.

   MOON collaboration : Interenational collaboration
 RCNP/ Physics, Osaka Univ. General Arts Tokushima Univ.
 Phys. ICU. Tokyo,
 Phys. CENPA, Univ. Washington,    LANL
 Univ. North Carolina.             FNAL
 Phys. Charles Univ.               CERN
 High Energy Physics, Protvino.
 JINR                              VNIIEF
 Contact persons Hiro Ejiri and Hamish Robertson
                  MOON Objectives                          .
    n studies in 100Mo : large responses for bb-n & low E ne’s .

   Double beta (bb) decays
   with mn~0.03 eV.
   Low E solar and SN ne .

   Two charged particle (b,b)
    spectroscopy with high
   localization in time & space.

   MOON, a super module of
   ~1 ton 100Mo & scintillators with modest volume and realistic purity

            H.Ejiri,, Phys, Rev. Lett.,85 (2000) 2917
               MOON Hybrid Detector
Super modules of fiber-plate scintillators with 100Mo films.


1. Position read-out
    Fibers (x-y) 2m - 2 mm - 0.4 mm                    Fiber x
2. Energy read-out
   Plate scintillator with DE ~ s ~ 2 % Mo film
3. Modest volume with enriched Mo
4. Enriched Mo 85 % in 100Mo
   Centrifuges MoF6 gas
   Laser

MOON 1. Proto type 100Mo 1 kg. Mn ~0.3 eV

MOON 2. 1 unit : 100Mo 0.25 ton 2m – 2m – 1.7 m,   Mn ~0.05 eV
MOON 3. 4 units: 100Mo 1 ton. 2m – 2m -- 7 m,      Mn ~0.02eV
    Future Experiments II         CANDLES


EL VI  ---CANDLES
48Ca for bb large Q =
                    bb
  4.27 MeV, small 0.19%

48Ca  7.7 g (EL VI) to
 O(10kg) & Enrichment
1K of 1 l crystals of
 CaF2 in iiquid scintillator
3.1 kg of 48Ca in 3.2 ton nCaF2
  Goal 0.1 eV sensitivity.

 R & D Osaka Univ.Physics.
           VII. Progress & Grants
   I. ELEGANTs at Kamoka 1982--1994
 1981        Start bb and n project at Osaka
 1981-1982 ELEGANT I, II, Ge with NaI at Osaka
 1982 –1984 ELEGANT III. Ge wih NaI        Grant A. B
 1982 – 1985 ELEGANT IV. Mo with Si.       Toray Science Award
 1984        EL III Starts at Kamioka       Grant A.
 1986 – 1990 ELEGANT V Mo Cd
             Drift Chamber & NaI            Grant Special Project
 1990 – EL V Starts run.
 1993 – 1995 EL VI CaF2 with CsI
            Construction                    Grant Basic Research

           Oto Underground Lab.
 1994 New underground lab. n & DM project start.
 1994 – 1995 survey of new underground lab.
 1995 Select Oto and proposal.
 1996 Start construction                  Grant COE lab.
 1997 Commencement of Oto Lab.
       Improve EL V and set at Oto.
 1998 EL V starts run at Oto
 1999 EL IV starts run at Oto


 MOON
   2000 MOON project, MOON R&D Yamada award 2001,
   2003 MOON 1 Proto-type     Government Grant A.
 CANDLES 2002 R&D and          Government Grant A.
                            References
Nuclear responses for neutrinos.
Review                        H.Ejiri, Phys. Rep. 338 (2000) 265.
GR and bb, solar & sn n’s H.Ejiri, Nucl. Phys. A 687 (2001) 350c
LI reactions. 3He              H.Ejiri, et al. PLB 433 (1998) 257.
11B,11Li                  H. Ejiri, K. Takahisa, et al., 1997, 2001.

Double beta decays and neutrinos.
bb EL V        H.Ejiri, N.Kudomi, et al., Phys. Rev. C 63 (2001) 65501
Review                H.Ejiri, Nucl. Phys.B 91 (2001) 255, v2000 proc

MOON
bb and solar n      H.Ejiri, J.Engel, G.Hazama, P.Krastev, N.Kudomi,
                    R.G.H.Robertson, Phys, Rev. Lett.,85 (2000) 2917
Supernova n         H.Ejiri, J.Engel, N.Kudomi, PL B530 (2002) 27
http://www.rcnp.osak-u.ac.jp/~ejiri/PUB.html
 We      would express our cordial thanks to
 Oto & Nishiyoshino villages & the chiefs,
   Mr T. Kitamura & Mr S.Nakagaki,
    for the great and timely support for
    construction of the new lab.
National   Railway Corporation for transfer of
the   tunnel to the two villages to be used for our
   underground lab.
Japanese    people for their great contributions.
Toray, Takeda,    and Yamada S.F.for their timely
    awards/suports.
   .




        Thank you for attension
 Here we would like to express our cordial thanks t
The distinguished chief of Oto,
                    Mr. Toshihiro. Kitamura




for great, timely , & crucial supports for our science proje

				
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posted:9/22/2011
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