----Distributed to --------
KEKVAX::NISHIKAW, KEKVAX::CHIKAMAT, kekux::"miyamoto@ieux01.ins.u-tokyo.ac.jp",
kekvax::kenzo, KEKVAX::SAKUDA, kekvax::kanzaki, KEKVAX::OYAMAY,
KEKVAX::SOSAMU, KEKVAX::MINORU, KEKPSA::ieiri,
KEKUX::"miyano@ngthep.hep.sc.niigata-u.ac.jp", kekvax::tamuran,
KEKUX::"SOBEL@MASTER.PS.UCI.EDU", kekvax::gajewski,
kekux::"chiaki@sbhep.physics.sunysb.edu", kekvax::suzukia,
kekux::"totsuka@jpnutins.bitnet", kekux::"suzuki@icrkm4.icrr.u-tokyo.ac.jp",
kekux::"koshio@icrr.u-tokyo.ac.jp", kekux::"masato@icrkm4.icrr.u-tokyo.ac.jp",
kekux::"itow@suketto.icrr.u-tokyo.ac.jp", kekux::"sakai@icrr.u-tokyo.ac.jp",
kekux::"kajita@icrr.u-tokyo.ac.jp", kekux::"nakahata@icrr.u-tokyo.ac.jp",
kekux::"koshio@icrr.u-tokyo.ac.jp", kekux::"inoue@icrkm4.icrr.u-tokyo.ac.jp",
kekux::"kaneyuki@phys.titech.ac.jp", kekux::"thara@kobe-u.ac.jp",
kekux::"aoki@kobe-u.ac.jp", KEKUX::"SUZUKI@PHYS01.PHYS.KOBE-U.AC.JP",
KEKVAX::NIWA, kekvax::asai, kekvax::miuram, kekvax::kohama, 
kekux::"kyosi@tkikam.sp.u-tokai.ac.jp",
kekux::"masayuki@tkikam.sp.u-tokai.ac.jp",
kekux::"alpinist@sbhep.physics.sunysb.edu", 
kekux::"jimhill@sksol1.physics.sunysb.edu"
 --------------------------

MINUTES OF E362 FRONT DETECTOR MEETING 
Date: 15:00-17:00, December 26, 1995
Place: ICRR 
Present: Nishikawa (Chairman), Ishii, Chikamatsu (INS), 
Nakamura, Ohyama, Sakuda(KEK), Nishijima, Etou(Toukai), 
on TV ( Y. Suzuki, Y. Itow (Kamioka) )

(1)  Nishikawa explains a figure of the target area for 50GeV neutrino
beam line (a figure by M. Takasaki).
  He also calculates the neutrino flux at L=300m wrt various radial positions
(r=0,1,2,3,4m) for10**20POT. eg. 4.7x10**12/cm**2 at r=0 and 3.0*10**12/cm**2
at r=3-4m.  
  Itow asks if we might have a similar pi/ki/mu monitor which MINOS proposes to
have after the Horn. No ideas at the moment. We welcome any ideas for monitors. 
  Nishikawa ordered a set of IIT+Inv-MCP+lenz+CCD to Hamamatsu according to 
Aoki (Kobe)'s proposal (Dec-6-95). 

(2) SCIFI 
Etou reports the offline analysis of SCIFI data taken on December 4.
He fits the pulse height distribution with a Poisson*Gaussian (convolution)
distribution and obtains the mean pe(photo-electrons) and attenuation length.
The quality of the fit is good except for the tail of the distribution, 
which is attributed to delta-rays (Landau tail). Using these data, he 
estimates the detection efficiency (1-exp(-pe)) for 2 layers of 0.5mmD 
and 0.7mmD fibers and 3 layers of 0.5 mmD fibers. 
                             L=1.5m from IIT    L=3.5m
(a) 0.5mmD, 2 layers             98+-0.5%       90+-1%  
(b) 0.5mmD, 3 layers             99%            96.5%
(c) 0.7mmD, 2 layers             99%            99%  
Note: L=1.5m and L=3.5m correspond to the edge of the fiducial volume.
He assumes the reflection (80%) at the other end of the fiber (L=4m). 
Although the result is preliminary, (c) looks better than others.
  Sakuda comments that even from a standpoint of the cost the option (c)
is cheeper by 20% than (b). 
 Etou will check the efficiency for an inclined beam instead of normal
incidence to the fiber plane.  

(3) Sakuda discusses the possibility of measuring Cherenkov light from 2-4
cm thick water using wavelength shifter bar and PMT. 5-10pe/cm of water
is expected. In fact, pi/proton separation is achieved at KEK-PS for 2.5cm
thick Lucite. This can be also used for a trigger of NC events which contain
showers. The feasibility can be tested using cosmic-rays.
 He shows two options for the mechanical design of water/SCIFI detector 
being considered (with Fujino, KEK mech-eng-center). 
  Sakuda introduces Chang Kee (Stony Brook)'s idea for water/SCIFI detector.
He sent us a triangle-shape scintillator (5mm thick, 1m long, readout via 
a wavelength shifter fiber). Merits:(a) more light yield, (b) less channels, 
thus lower cost. Demerits:(c) more material, (d) worse position resolution. 
Especially, the feature (b) is attractive. However, the performance must be 
demonstrated using MC.  
/(Memo by Sakuda)