% Sample file for encmacro
% use plain.tex
%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\input encmacro
\foroverseer         % more sparce output for overseers
%%\formyself         % more compact output for encoders
%
\headline={\tenrm 11/3/95 \hfil Encoded by Hikasa}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\R{AKERS 95R}{ZPC 67 203}{+Alexander, Allison, Ametewee, Anderson,  
Arcelli, Asai+}{OPAL\C}

\m{S030EE}{A}{<2\Em5}{95\%}{OPAL}{$Q=1$, $m=5$--45\GeV}

\m{S030EE}{A}{<1\Em5}{95\%}{OPAL}{$Q=2$, $m=5$--45\GeV}

\f{S030EE}{A}{AKERS 95R is a CERN-LEP experiment with $W_{cm}\sim m_Z$.  
The limit is for the production of a stable particle in multihadron 
events normalized to $\sigma(e^+e^-\to \rm hadrons)$.  Constant phase 
space distribution is assumed.}

\note Please change the sentence ``Ratio to $\sigma(e^+e^-\to\mu^+\mu^-)$'' 
in the section header to ``Ratio to $\sigma(e^+e^-\to\mu^+\mu^-)$ unless 
noted.''  (There is already one exception, ADACHI 90E, for this sentence.)

\m{S030Z}{B}{<5\Em6}{95\%}{OPAL}{$m=40.4$--45.6\GeV}

\f{S030Z}{B}{AKERS 95R give the 95\%CL limit 
$\sigma(X\bar X)/\sigma(\mu\mu) <1.8\Em4$ for the pair production of 
singly or doubly charged stable 
particle.  The limit applies for the mass range 40.4--45.6\GeV\ for 
$X^\pm$ and $<45.6\GeV$ for $X^{\pm\pm}$.}
\note I calculated the limit using $\B(Z\to\mu\mu)=3\%$.
\note This paper is basically for the quark search section (fractionally 
charged particle searches).  


%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\R{BALEST 95}{PRD 51 2053}{+Cho, Ford, Johnson, Lingel, Lohner+}{CLEO\C}

\m{S056ONI}{A}{<1.5\Em5}{90\%}{CLEO}{$\Upsilon\to\gamma X^0$, $m_{X^0}<5\GeV$}

\m{S056ONI}{B}{<3\Em5\endash 6\Em3}{90\%}{CLEO}{$\Upsilon\to
\gamma X^0\bar X^0$, $m_{X^0}<3.9\GeV$}

\f{S056ONI}{A}{BALEST 95 two-body limit is for pseudoscalar $X^0$.  
The limit becomes $<10^{-4}$ for $m_{X^0}<7.7\GeV$.}

\f{S056ONI}{B}{BALEST 95 three-body limit is for phase-space photon energy 
distribution and angular distribution same as for $\Upsilon\to gg\gamma$.}
\note The limits should be included in the Heavy Boson Section.  

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\NewSection{S030DM}{Cross Section Limits for Dark Matter Particles ($X^0$)
on Nuclei}%
{These limits are for weakly interacting stable particles which may 
consist the invisible mass in the Galaxy with a local mass density 
of 0.3\GeV/cm$^3$.  See each paper for assumptions on the velocity 
distribution.
\bigskip
\m{S030DMx}{}{\hbox{value (nb)}}{\hbox{CL\%}}{TECN}{COMMENT}}
\vfilneg
\note This section is to be subdivided into the following three:
\item{} S030DM1: For $m(X^0)=20\GeV$
\item{} S030DM2: For $m(X^0)=100\GeV$
\item{} S030DM3: For $m(X^0)=1\TeV$

\note I have chosen 20\GeV\ instead of 10\GeV\ because (1) some of the 
limits changes quite rapidly around 10\GeV\ and (2) the current neutralino 
mass limit is around 20\GeV\ (assuming gaugino mass unification).

\bye