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\title{Mini-LANNDD:
A Very Sensitive Neutrino Detector To Measure $\sin ^2(2 \theta
_{13})* $ }

\author{
   David B. Cline, 
   Stanislaw Otwinowski\dag\
   and Franco Sergiampietri\ddag\
}

\address{
\dag\ Center for Advanced Accelerators
Department of Physics and Astronomy University of California, Los
Angeles Los Angeles, California 90095-1547
}

\address{
\ddag\ , INFN-Pisa, Istituto Nazionale di Fisica Nucleare, Via Livornese,
129156010 San Piero a Grado (PI), Italy
}

\begin{abstract}
The ICARUS Detector at the LGNS will carry out a sensitive search
for a $\sin ^2(2 \theta _{13}$). We describe a small version for
the LANNDD proton decay detector (70kT Liquid Argon) to measure
$\nu _{\mu}\rightarrow \nu_{e} $ in a low energy or off-axis
neutrino beam. We find an optimal detector size is 5 kT and at a
distance of about 700 km from a high-energy neutrino source. This
detector uses the ICARUS method.
\end{abstract}

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\section{Introduction}
The ICARUS detector concept is now well tested and plans for a 3
KT detector at the LGNS are in place by 2005-2006 [1]. This
detector with the CNGS neutrino beam will provide the most
sensitive search for $\nu _{\mu}\rightarrow \nu_{e} $ that is
currently planned. To go beyond this sensitivity, a new detector
will be required in a different (lower energy or off-axis) beam.
In this note we discuss a possible 5 kT detector based on the
ICARUS method, and a smaller version of the proposed LANNDD
detector. LANNDD (Liquid Argon and Neutrino and Nuclear Decay
Detector) is a 70 kT magnetized detector for the WIPP Site at
Carlsbad, New Mexico. Figure 1 shows a schematic of LANNDD and
Figure 2 shows a schematic of the detector located at the WIPP
Site[2].

In this note we provide a brief discussion of Mini-LANNDD, a 5kT
detector based on the LANNDD concept. We emphasize here the use to
search for In this note we provide a brief discussion of
Mini-LANNDD, a 5kT detector based on the LANNDD concept. We
emphasize here the use to search for $\nu _{\mu}\rightarrow
\nu_{e} $ beyond the ICARUS [3] range to the level of $\sin ^2(2
\theta _{13} $ of 0.005.

\section{Reach of ICARUS T3000}
The ICARUS T600 will be installed soon in the LNGS - most likely
in Hall B. A proposal has been submitted to INFN and the USA DOE
to construct on additional 2400 tons of ICARUS [4]. In this
proposal on analysis of the limit on $\sin ^2(2 \theta _{13} $
that could be reached after 8 years of operating with the CNGS
beam - Table 1, lists the events rate for different channels as
well as the expected ne background. A detailed analysis by Andre
Rubbia [5] and his group indicates that 0.02 could be reached to
90\% C.L. A schematic of the limit that one can reach compared to
the background is given Table 2. We see that a value of 0.01 is
optimal and with a great deal of effort (or a very good
detector)(Table 3 and 4) like mini LANNDD; 0.005 might be reached.

%table 1 here
%table 2 here

\section{Mini-LANNDD}

We have made a very preliminary design of a 5 kt LANNDD like
detector to use in a NuMi like beam (or off axis CNGS beam). Fig.
3 shows one design including the Cryostat whereas Fig.4 shows a
cut through of the detector. We assume 5 m drift length. In Table
5 we give some preliminary parameters of the detector.

\section{The reach of Mini-LANNDD}

Using some value given to us by Adam Para [6] [7] we show the
signal and background for Mini-LANNDD with 20 kty exposure - Table
3 and Table 4. Neutral current will be unimportant. Mini-LANNDD
can reach ultimate limit possible in the NuMi beam (or off axis
CNGS) of 0.005.

%table 3 here
%table 4 here
%table 5 here

We wish to thank Adam Para and Debbie Harris for requesting this
study

\begin{table}
\caption{} \lineup
\begin{tabular}{@{}ll}
\br
CoM energy (TeV)&{\rm 0.4}\\
\mr
P energy (GeV)&16\\
P/bunch&$2.5 x 10^{13} $\\
Bunches/fill&4\\
Rep. rate (Hz)&15\\
1/$\tau _{\mu} $&240\\
$P$ power (MW)&4\\
$\mu $/bunch&$2 x 10^{12} $\\
$\mu $ power (MW)&4\\
Wall power (MW)&120\\
Collider cirumference (m)&1000\\
$<B> (T)$ &4.7\\
$\delta p$ (\%) &0.14\\
6-D $\eta _{6,N} (\pi m ^3 )$ &$1.7 x 10^{-10} $\\
Rms $\eta _{n} $ ($\pi $ mm-mrad)&50\\
$\beta $ * (cm)&2.6\\
$\sigma _{z}$ (cm)&26\\
$\sigma _{r}$ spot ($\mu m $)&1.0\\
$\sigma _{\theta} $ IP (mrad)&0.044\\
Tune shift&\\
$n^{effective}_{turns} $&700\\
\mr
Luminosity $(cm^{-2}s^{-1}) $&$10^{33} $\\
Higgs/year&\\
\br
\end{tabular}
\end{table}

\smallskip

\section{References}
\begin{thebibliography}{5}

\item ICARUS Team, private communication \item Cline, D et al,
ASTRO-PH/0105442. \item The first study of $\nu _{\mu} \rightarrow
\nu _{e}$ was carried out by D.B. Cline and S. Otwinowski,
ICARUS-TM/2001-09. \item ICARUS Collaboration, ICARUS TM/2001-09,
proposal submitted to INFN 2001 and to the USA DOE 2002. \item
Andre Rubbia, private communication. \item Szleper, M and Para, A,
NuMi-B-786, HEP-PH/0110032. \item Adam Para, private
communication.

\end{thebibliography}


\end{document}
