\section{Introduction}
The Neutrino Factory will open up a regime of neutrino physics that is 
inaccessible at existing facilities. When combined with a
multi-kiloton detector located at a large distance, the proposed accelerator 
will allow the study of a number of unexplored neutrino oscillation 
parameters and a significant reduction in uncertainty of previously measured neutrino mass 
differences and mixing angles.
The Neutrino Factory, plus its long-baseline detector, will have a physics
program that is a logical continuation of current  and near-future neutrino 
oscillation experiments in the U.S., Japan and Europe~\cite{DET:industry}. The facility
will potentially enable physicists to determine values for all remaining 
unknown physical constants associated with current neutrino 
oscillation theory.


Features of the facility that allow these challenging
oscillation measurements are a high neutrino intensity, 
a well-collimated beam, precise 
understanding of beam composition and spectra, and optimized energy. 
In addition, detector facilities located in experimental areas near the
neutrino source will have access to integrated neutrino intensities 
$10^4$--$10^5$ times larger than previously available ($10^{20}$ 
neutrinos per year compared with $10^{15}$--$10^{16}$). Standard 
neutrino physics at this facility could include physics topics such as
precision ${\sin}^{2}\theta_{W}$, structure functions, 
high precision neutrino total charge current (CC) cross sections at low $\sqrt{s}$ (a few GeV),
nuclear effects (shadowing at low $x,$ 
anti-shadowing...), pQCD, and neutrino magnetic moments. These topics have
relevance for standard model physics, nuclear physics, astrophysics and
physics beyond the standard model. Finally, the Neutrino Factory will serve 
as a test accelerator for a high intensity muon collider and so is an R\&D 
facility that is a significant step toward a muon collider in the future.

\section{Beam Parameters}

Neutrino beams produced at  the Neutrino Factory are either
($\nu_{\mu}$,$\bar{\nu_{e}}$) or 
($\bar{\nu_{\mu}}$,$\nu_{e}$) depending on whether the 
machine is running $\mu^{-}$ or $\mu^{+}$. 
The characteristics of the machine design guarantee that the beam is pure,
 with no contamination from anti-particles of the same neutrino flavor. 
The design intensity is $10^{20}$ $\mu$
decays/year, where a year is defined as $1\times 10^{7}$~s. The angular 
dispersion of the $\nu$-beam is ${\Delta}{\theta}/\theta$ = 5.3~mrad with a 
momentum spread $\Delta{p}/p$ = 30\%.
The primary long-baseline
target site considered in this report is the Waste Isolation Pilot Plant 
(WIPP) located in Carlsbad, New Mexico~\cite{DET:wipp}. WIPP is located
2900~km from Brookhaven National Laboratory and requires a $13.1^{\circ}$ dip
angle in the muon storage ring. An alternative site with a smaller baseline, but with an already existing detector, Soudan, Minnesota, is discussed in the Appendix~\ref{Soudan-option}. Most recently, a new alternative site has been suggested, the Homestake Mine in Lead, SD, that has been recommended as the site for the National Deep Underground Laboratory~\cite{bhcomm}.

Based on design parameters in this report, the expected event rate at the 
WIPP site is given in Table~\ref{DET:ratesWIPP}.
%\bigskip
\begin{table}[!hbt]
\begin{center}
\caption{Event rates WIPP.}
\label{DET:ratesWIPP}
\begin{tabular}{|lccccc|}
\hline
$E_{\mu}$  & Baseline & ${E_{{\nu}_\mu}}$ & ${E_{{\nu}_e}}$ & 
$N({\nu_{\mu}}$ CC) & $N({\nu_{e}}$ CC) \\
(GeV) &(km) & & & (per kt-year) & (per kt-year) \\ \hline
%$10_{BNL-SOU}$ & 1700 & 7.5 & 6.5 & 260 & 120 \\ 
%$20_{BNL-SOU}$ & 1700 & 15 & 13 & 2150 & 960 \\ 
$20_{\textrm{BNL-WIPP}}$ & 2900 & 15 & 13 & 740 & 330 \\ \hline
\end{tabular}
\end{center}
\end{table}
\section{Physics Signals}
As discussed in detail in Section~\ref{physics-mot}, neutrino mixing can be described by the lepton CKM matrix:
\begin{equation}
U = U_{23}U_{13}U_{12}=\left( \begin{array}{ccc}
1&0&0 \\
0& c_{23} & s_{23} \\
0&-s_{23} & c_{23}
\end{array} \right)
\left( \begin{array}{ccc}
c_{13}&0&s_{13}\exp^{i\delta} \\
0& 1 & 0 \\
-s_{13}\exp^{-i\delta}& 0 & c_{13}
\end{array} \right)
\left( \begin{array}{ccc}
c_{12}&s_{12}&0\\
-s_{12}& c_{12} & 0 \\
0 & 0 & 1
\end{array} \right)\nonumber
\end{equation}
(The possibility of light sterile neutrinos is not considered here). 
Three-flavor neutrino oscillations can be described by 
seven parameters: three ${\Delta}{m_{ij}}^{2}$ terms; 
three mixing angles $\theta_{ij};$ and a CP violating term $\delta$. The
mass parameters are related by the simple identity 
$\Delta{\textrm{m}_{12}}^{2}+\Delta{\textrm{m}_{23}}^{2}+\Delta{\textrm{m}_{31}}^{2}=0.$
SuperKamiokande (SuperK)~\cite{DET:superK} has measured what appears to be non-zero values for 
${\Delta}{m_{23}}^{2}$ and $\theta_{23}$ in atmospheric neutrinos.
Over the next few years both K2K~\cite{DET:k2k} and MINOS~\cite{DET:minos}  will try to confirm the 
SuperK observation with accelerator-based experiments and obtain accurate
values for ${\Delta}{\textrm{m}_{23}}^{2}$ and $\theta_{23}$.
The $\nu$-oscillation parameters ${\Delta}{\textrm{m}_{12}}^{2}$ and $\theta_{12}$ 
are the province of solar and reactor-based experiments, either now running 
or planned for the next several years.
The values of these parameters, hopefully, will be measured over the next
 5--10~years. A long-baseline experiment 
at the Neutrino Factory will be able to measure $\theta_{13}$, the sign of
${\Delta}{m_{23}}^{2}$ and possibly the CP violation term $\delta$, 
providing $\theta_{13}$ is large enough. Depending on the values 
of the various neutrino parameters,  
it is conceivable that the Neutrino Factory will be in a position to measure 
all the remaining outstanding neutrino mixing parameters. Additionally,
a long-baseline neutrino detector should be  
able to make the first direct measurement of the neutrino-matter oscillation 
effect (MSW). It would study MSW and could make a model-independent
measurement of the matter parameter $A,$ where $A=\sqrt{2}G_{F}n_{e}$. 
Measurements of $A$ with 10\% accuracy 
are possible, and may even be of interest to geophysicists. 

\section{Long Baseline Oscillation Experiment}
The characteristics of a Neutrino Factory beam, $\nu_{\mu},{\bar{\nu_{e}}}$
with no ${\bar{\nu_{\mu}}},{\nu_{e}}$ contamination, naturally  
lend themselves to a neutrino appearance experiment. 
Since a $\mu^{-}$ beam at the Neutrino 
Factory  will not result in any initial production  of $\bar{\nu_{\mu}}$, a
$\bar{\nu_{\mu}}$ signal will be due to 
$\bar{\nu_{e}}\rightarrow\bar{\nu_{\mu}}$ oscillations. 
An experiment designed
to look for ${\bar{\nu_{\mu}}}$ CC events measures $P({\bar{\nu_{e}}}{\rightarrow}{\bar{\nu_{\mu}}}),$ where
\begin{center}
$P({\bar{\nu_{e}}}{\rightarrow}{\bar{\nu_{\mu}}}) = \sin^{2}
{2\theta_{13}}\sin^{2}{\theta_{23}}\sin^{2}({\Delta}m{^2}_{13}L/4E)$ 
\end{center}

A program to study both  $P({\bar{\nu_{e}}}{\rightarrow}{\bar{\nu_{\mu}}})$ 
and $P({\nu_{e}}{\rightarrow}{\nu_{\mu}})$ not only gives us access to
$\theta_{13}$ but also tells us the sign of the ${\Delta}{\textrm{m}_{23}}^{2}$ and
allows us to measure the matter parameter $A$ (Fig.~\ref{fg:cp}). 

\begin{figure}
\begin{center}
%\mbox{\epsfxsize 3.5in
\includegraphics*[width=15cm]{../template/report/ps-and-eps/neutrino_cp.ps}
%\end{center}
\caption[Measuring the ratio of $P({\bar{\nu_{e}}}{\rightarrow}{\bar{\nu_{\mu}}})$ to $P({\nu_{e}}{\rightarrow}{\nu_{\mu}})$  ]{Measuring the ratio of $P({\bar{\nu_{e}}}{\rightarrow}{\bar{\nu_{\mu}}})$ to $P({\nu_{e}}{\rightarrow}{\nu_{\mu}})$ enables measuring
the sign of ${\Delta}{m_{23}}^{2}$ and the value of the matter parameter $A.$}
\label{fg:cp}
\end{center}
\end{figure}

It is interesting to note that the matter parameter becomes accessible only 
when the beam has passed through a significant amount of material. Calculations 
show that the BNL-WIPP distance of 2900 km is far enough for the MSW effect
to be measurable.

As stated earlier, if both the CP violating term, 
$\delta,$ and $\theta_{13}$ 
are large enough, they may be disentangled in these measurements.
In addition, a spectral scan on the oscillation probabilities 
would potentially improve the precision of the ${\Delta}{m_{23}}^{2}$
and  $\theta_{23}$ measurements by nearly an order of magnitude~\cite{DET:golden}.

The experiment's concept is to start with the muon storage ring filled with
$\mu^{-},$ which produces a $\nu_{\mu}$,${\bar{\nu_{e}}}$ beam, and
look for a ${\bar\nu_{\mu}}$
appearance at the distant detector. The experiment would take sequential data sets with
both  $\mu^{-}$ and $\mu^{+}$ storage ring fills, enabling the study of both
the neutrino-matter oscillation effect and neutrino CP violations.
Measuring 
$P(\nu_{e}{\rightarrow}\nu_{\mu})$  and 
$P({\bar{\nu_{e}}}{\rightarrow}{\bar{\nu_{\mu}}})$/$P(\nu_{e}{\rightarrow}\nu_{\mu})$ gives  access to the oscillation parameters described above.

 $\bar{\nu_{\mu}}$  appearance experiment is typically done  by looking 
for the leading $\mu^{+}$  from the $\bar{\nu_{\mu}}$ CC
reaction in the detector. The challenges in a search for
 $\bar{\nu_{\mu}}$ events are threefold: i) distinguishing 
$\mu^{+}$ from  the $\mu^{-}$ coming from the non-oscillating ${\nu_{\mu}}$'s;
ii) separating $\mu^{+}$'s from $\pi^{+}$ punch-throughs; and iii) rejecting  $\mu^{+}$'s
coming from hadronic decays. Another potential background, which depends 
on the detector environment, is accidentals from either cosmics or some 
background radiation. 

There are a number of hadronic decay backgrounds for the $\mu^{+}$ signal.
They are:
\begin{itemize}
\item [\bf{-}] $\nu_{\mu}$ CC where the primary  $\mu^{-}$ is missed and  the
$\mu^{+}$ from hadronic decay of the $\pi^{+}$, $K^{+},$ or $D^{+}$ is observed
\item [\bf{-}] $\nu_{e}$ CC where the primary  $e^{+}$ is missed and the
$\mu^{+}$ from hadronic decay of the $\pi^{+}$ or $K^{+}$ is observed 
(The $D^{+}$ is not a significant concern here)
\item [\bf{-}] $\nu_{\mu}$,$\nu_{e}$ NC, where $\pi^{+}$ 
and  $K^{+}$ again cause problems
\end{itemize}


The requirement to both measure the signal and reject the background determines
a number of the detector's characteristics. Measurement of the sign of
the muon is critical to the experiment, which means the detector must contain
a magnetic field. Obtaining the muon spectrum is also important and
can be done either through bending in the spectrometer or by range,
using $\dfrac{dE}{dx}.$ Separation of $\mu$'s from $\pi$'s is accomplished through 
range-out in many interaction lengths of material. Rejection of hadronic
backgrounds requires a  combination of momentum, $p_{t},$ and isolation cuts.  
A detailed investigation of these backgrounds was carried out in 
Study-I~\cite{DET:study1}. 
It was determined that, to make the background manageable, 
a detector  requires both momentum resolution and transverse segmentation
(See Figs.~\ref{fg:mucut}, \ref{fg:muenergy}, \ref{fg:mubackground}). 
Rejection of accidental 
backgrounds can be handled
by a detector with moderate timing resolution. Timing resolutions on the 
order of 100~ns would allow the experiment to only take events in phase
with the machine time structure, and so reject accidentals by a factor of
200. A timing resolution of 10~ns gains an additional factor of two 
in background rejection by allowing a direction cut. 
Finally, the neutrino event rates seen in Table~\ref{DET:ratesWIPP} indicate the need
for the detector to be large, multiple ktons.

\begin{figure}
\begin{center}
\includegraphics*[width=15cm]{../template/report/ps-and-eps/mucut1.ps}
\caption[Fraction of neutrino events that produce a background signal ]{Fraction of neutrino events that produce a background signal as a 
function of minimum muon energy. Background sources include  $\pi$ and $K$ decays, $\pi$ punch-through, and charm decays.}
\label{fg:mucut}
\end{center}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics*[width=10cm]{../template/report/ps-and-eps/muenergy.ps}
\caption[Reconstructed neutrino energy distribution ]{Reconstructed neutrino energy distribution for several different
minimum muon energy cuts. Note that a minimum muon cut at 4 GeV reduces the
signal by 30--35\%.}
\label{fg:muenergy}
\end{center}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics*[width=10cm]{../template/report/ps-and-eps/mubackground.ps}
\caption[Distributions of the square of the muon momentum ]{Distributions of the square of the muon momentum component
transverse to the hadronic shower, $p_{t}^2,$ for $\nu_{\mu}$ CC 
events (solid line) and background muons (dashed line). The effectiveness
of a transverse cut can be seen.}
\label{fg:mubackground}
\end{center}
\end{figure}


\section{Detector Options}
Specifications for the long-baseline Neutrino Factory detector
are rather typical for an accelerator-based neutrino experiment. However,
because of the need to maintain a reasonable neutrino rate at these long
distances, the detectors considered here are between
3 and 10 times more massive than those in current neutrino experiments.

Large-mass detector designs are driven primarily by the cost of the absorbers.
Limiting the detector's cost drives us to two basic options:
steel-based and water-based designs. The
two detector options considered for the WIPP site in this study are a 50 kton 
Steel/Scintillator/Proportional Drift Tube (PDT) detector and a Water
Cerenkov Detector. The detector considered for the Soudan site, a 15 kton
PDT detector is discussed in Section~\ref{Soudan-option}.

The PDT detector would resemble MINOS, having steel absorber plates 
of 10--20~cm thickness, being magnetized with a toroidal field to 
1--1.5~T. A combination of PDT's and scintillator slats would be
interleaved with the absorber to provide longitudinal and transverse position
resolution and coarse timing. In addition, the scintillator layers provide 
the experiment with its trigger. The thickness of the steel absorber and the
ratio of PDT to scintillator slats would be optimized for momentum resolution 
and background rejection. The estimated electronics channel count
would be of the order $1-5\times 10^{5}.$ With a neutrino event rate
of a few mHz, the electronics could be highly multiplexed to reduce cost and
complexity. Phototube magnetic shielding in these detector geometries has
been solved by both MINOS and predecessor experiments, and so should not be an 
issue. Figure \ref{fg:steelwipp} shows a 50 kton detector with 
dimension $8~\textrm{m}\times 8~\textrm{m}\times 150$~m. This geometry would be convenient for access and services, though designs that maximize fiducial-volume-to-edge ratios are possible. A detector
of this size would record up to $4\times 10^{4}$ $\nu_{\mu}$ events/year. 

\begin{figure}
\begin{center}
\includegraphics*[width=10cm]{../template/report/ps-and-eps/steelwipp6.ps}
\caption[A possible 50 kton Steel/Scintillator/PDT detector at WIPP]{A possible 50~kton Steel/Scintillator/PDT detector at WIPP.}
\label{fg:steelwipp}
\end{center}
\end{figure}

A  large water Cerenkov counter would be similar
to SuperK but with either a magnetized water volume or toroids separating
smaller water tanks. The detector could be the large water-Cerenkov
UNO detector~\cite{DET:uno}, currently proposed  to study both proton decay and cosmic
neutrinos. UNO would be a 650~kton water-Cerenkov detector segmented into
a minimum of three tanks (Fig.~\ref{fg:unodet}). The gaps between the tanks 
may contain toroidal 
magnets, or perhaps large-gap dipoles to provide the $B$ field needed to
identify the charge of the leading muon (Fig.~\ref{fg:unodetmag}). 
The detector provides sufficient
muon/hadron separation  and muon containment up to 30 GeV/$c.$ A water-Cerenkov
detector would have background rejection of the same order as a steel/scintillator/PDT 
detector, though results from Study-I (Fig.~\ref{fg:mucut})
suggest muon $p_t$ cuts would 
need to be 1.0--1.5 GeV/$c$ higher in a water-Cerenkov counter to obtain the 
same  rejection levels. UNO would be read out with 70,000~phototubes,
a combination of the 20-inch SuperK tubes and 8-inch tubes. The timing provided
by the PMT's would allow UNO to gate events in time with the Neutrino 
Factory beam structure. This enables UNO to work simultaneously as
both a long-baseline neutrino experiment and a proton-decay experiment.
The multi-faceted nature  of the UNO physics program is an 
appealing aspect of this detector option.
However,  geometry of the water tanks does not provide a straightforward way to contain the spectrometer magnet fringe field, so magnetic shielding of the
PMT's could be a technical challenge.
UNO's active volume is large, $60~\textrm{m}\times 60~\textrm{m}\times 180~\textrm{m}$ $(\textrm{w}\times \textrm{h}\times \textrm{l}),$ which implies an 
experiment hall of substantial dimensions. To provide reasonable access,
the hall would need to be at least $100~\textrm{m}\times 80~\textrm{m}\times 300~\textrm{m},$ and perhaps more.  
The detector would
have an active fiducial mass of 440~ktons and would record up to
$3\,\times \,10^{5}$ $\nu_{\mu}$ events/year from the Neutrino Factory beam. 

\begin{figure}
\begin{center}
\includegraphics*[width=15cm]{../template/report/ps-and-eps/unodet1.ps}
\end{center}
\caption[Block schematic of the UNO detector]{Block schematic of the UNO detector, including initial design parameters.}
\label{fg:unodet}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics*[width=15cm]{../template/report/ps-and-eps/unodetmag1.ps}
\caption[Concept of multi-water tank Cerenkov counter]{Concept of multi-water tank Cerenkov counter with magnetic field 
included.}
\label{fg:unodetmag}
\end{center}
\end{figure}
\section{WIPP Site}

The WIPP facility is the U.S. Department of Energy's Waste Isolation Pilot Plant
located in Carlsbad, New Mexico. It is a large, underground depository
for the storage of low-level radioactive waste and has been in operation since
1999 (Fig.~\ref{fg:wipparea}). 

\begin{figure}
\begin{center}
\includegraphics*[width=15cm]{../template/report/ps-and-eps/wipparea1.ps}
\caption[The WIPP area]{The WIPP area.}
\label{fg:wipparea}
\end{center}
\end{figure}

The WIPP site is approximately 2900~km from Brookhaven 
National Laboratory. The active depository is located 650 m underground in a 
deep salt formation. Space is  potentially available for a large underground 
physics facility at depths of 740--1100~m and  discussions are under way between
DOE and the UNO project on the possible development of such a facility.
Infrastructure, such as elevator access and electricity, is currently 
available at the waste storage levels but new excavation and infrastructure
installation would need to
take place for the creation of an underground physics facility. The area
should be considered a green field, albeit a very salty one.

It is worth asking here whether these experiments need to be as deep underground as 
proposed, or even underground at all. The effort and expense to build an experiment 700+~m underground
adds significantly to the challenge of the experiment. Certainly for the 
UNO detector option, the experiment must be deep underground. A
proton decay experiment that is searching for events with maximum rates of a 
few per year can tolerate little cosmic ray background. The $\nu$ interaction
rate in a 50 kton steel-based detector is a few mHz at beam design intensity. 
At the surface, the cosmic ray interaction rate in the 50 kton
detector is a few 100~kHz.  These event rates would not provide 
significant data loading to the Data Acquisition System from either a
bandwidth or archiving perspective. The main issue is the signal-to-noise (S/N)  ratio of 
$10^{-7} - 10^{-8}$, which would be improved by gating with the 
Neutrino Factory beam structure, and
providing a veto array around the detector. These techniques should 
allow the S/N to be improved to  $10^{-3} - 10^{-2}$. Higher level software
triggers could further reduce backgrounds by making cuts on event topology.
A Monte Carlo study would be necessary to determine whether the remaining 
cosmic ray background events  could be removed through data analysis.
\section{The Near Detector}
Detector facilities located on-site at the Neutrino Factory
would have access to unprecedented luminosities of pure neutrino beams,
well focussed with narrow energy spectra.  A detector positioned 50~m
from the end of the muon storage ring straight-away  could expect
$\nu$-fluxes $10^{4}$--$10^{5}$ times higher than currently available from
accelerator sources. These luminosities would allow neutrino detectors
to be much more compact, with higher precision in particle momentum and energy
measurements. This in turn would enable standard neutrino physics
studies such as ${\sin}^{2}\theta_{W}$, structure functions, $\nu$ cross
sections, nuclear shadowing and pQCD to be performed with much
higher precision than previously obtainable. 

A compact Liquid Argon TPC (similar to the  ICARUS detector~\cite{ICARUS}),
cylindrically-shaped with a radius of 50~cm and a length of 1~m would
have an active volume of $10^{3}$ kg and a neutrino event rate O(10~Hz).
The detector provides tracking, an EM energy resolution of 
$3\%/\sqrt{E} + 1\%$ and hadronic energy resolution of $20\%/\sqrt{E} + 5\%$.
The TPC could be combined with a downstream magnetic spectrometer for
muon and hadron momentum measurements. At these $\nu$-luminosities it
is even possible to have an experiment with a relatively thin Pb target 
(1~$L_{rad}$) followed by a standard fixed target spectrometer
containing tracking chambers, time-of-flight and calorimetry with a
event rate O(1~Hz). Backgrounds from neutrino interactions in the upstream 
shield must be considered, but should be manageable with accurate tracking to 
the target.
\section{Summary}
The Neutrino Factory, combined with a long-baseline detector, will allow a
number of neutrino oscillation parameters to be measured 
($\theta_{13}$, sign of ${\Delta}{m_{23}}^{2}$, $\delta$, $A$),
some  for the first time. There is the potential that by the time the 
factory comes online, the long-baseline
experiment would be able to measure all the outstanding neutrino 
oscillation parameters. The experiment site  considered in this study, 
WIPP,  has space available 700+~m underground
with some associated infrastructure.  Detector options for the experiment include
a steel/scintillator/PDT detector similar to MINOS and its progenitors, and
weighing tens of ktons. The proposed 650 kton water-Cerenkov detector, UNO,
is also an option. Both choices are technically feasible, though the 
water-Cerenkov approach has a number of outstanding technical questions. Conventional
neutrino physics is also accessible at the Neutrino Factory with $\nu$ beam
intensities many orders of magnitude  higher than previously available
at accelerator facilities.

\begin{thebibliography}{99}
\bibitem{DET:industry}An index of experiments and related subjects having to do with neutrino mass and oscillations,\\
\textsl{http://www.hep.anl.gov/ndk/hypertext/nuindustry.html} 

\bibitem{DET:wipp}The WIPP Home Web Page,\\
\textsl{http://www.wipp.carlsbad.nm.us/wipp.htm}

\bibitem{bhcomm}For the recommendations by the Bahcall-Haxton committee, see 
http://www.sns.ias.edu/~jnb. 

\bibitem{DET:superK}Official Home Page,\\
\textsl{ http://www-sk.icrr.u-tokyo.ac.jp/doc/sk/index.html}

\bibitem{DET:k2k}Long Baseline Neutrino Oscillation Experiment,\\
 \textsl{http://superk.physics.sunysb.edu/k2k/}

\bibitem{DET:minos}The MINOS Experiment and the NuMI beam line,\\
\textsl{http://www-numi.fnal.gov:8875/}

\bibitem{DET:golden}  A. Cervera et al., \textsl{Golden measurements at a Neutrino Factory}, CERN-TH/2000-40
\bibitem{DET:study1} C. Albright et al., \textsl{Physics at the Neutrino Factory}, Fermilab-FN-692, 2000

\bibitem{DET:uno}Official Home Page,\\
\textsl{http://superk.physics.sunysb.edu/uno/}

\bibitem{ICARUS} F. Arneodo {\it et al.}, \textsl{Study of Solar Neutrinos with the 600-T Liquid Argon ICARUS Detector}, NIMA 455 (2000) 376-389.

\end{thebibliography}









