GENIUS - A New Facility of Non-Accelerator Particle Physics
H.V. Klapdor--Kleingrothaus \address{Max--Planck--Institut f\"ur Kernphysik, P.O.Box 10 39 80, D--69029 Heidelberg, Germany
Spokesman of HEIDELBERG-MOSCOW and GENIUS Collaborations
The GENIUS (\underline {Ge}rmanium in Liquid \underline {Ni}trogen \underline {U}nderground \underline {S}etup) project has been proposed in 1997 \cite{KK-BEY97} as first third generation double beta decay project, with a sensitivity aiming down to a level of an effective neutrino mass of $<m>\sim$ 0.01 - 0.001 eV. Such sensitivity has been shown to be indispensable to solve the question of the structure of the neutrino mass matrix which cannot be solved by neutrino oscillation experiments alone \cite{KKPS}. It will allow broad access also to many other topics of physics beyond the Standard Model of particle physics at the multi-TeV scale. For search of cold dark matter GENIUS will cover almost the full range of the parameter space of predictions of SUSY for neutralinos as dark matter \cite{KK-Ram,Bed-KK2}. Finally, GENIUS has the potential to be the first real-time detector for low-energy (pp and $^7{Be}$) solar neutrinos \cite{Bau-KK,KKPropos99}. A GENIUS-Test Facility has just been funded and will come into operation by end of 2001. \vspace{1pc}
Genius-art1.tex
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\hyphenation{author another created financial paper re-commend-ed Post-Script}

\title{GENIUS - A New Facility of Non-Accelerator Particle Physics}


\author{H.V. Klapdor--Kleingrothaus
\address{Max--Planck--Institut f\"ur Kernphysik, 
P.O.Box 10 39 80, D--69029 Heidelberg, Germany\\
Spokesman of HEIDELBERG-MOSCOW and GENIUS Collaborations\\
e-mail:klapdor@gustav.mpi-hd.mpg.de, home page: http://mpi-hd.mpg.de.non-acc/}
}

\begin{document}

\begin{abstract}
	The GENIUS (\underline {Ge}rmanium in Liquid 
	\underline {Ni}trogen \underline {U}nderground \underline {S}etup) 
	project has been proposed in 1997 
\cite{KK-BEY97} 
	as first third generation double beta decay project, with 
	a sensitivity aiming down to a level of an effective neutrino 
	mass of 
$<m>\sim$ 0.01 - 0.001 eV. 
	Such sensitivity has been shown 
	to be indispensable to solve the question of the structure of the 
	neutrino mass matrix which cannot be solved by neutrino oscillation 
	experiments alone 
\cite{KKPS}. 
	It will allow broad access also to many other topics of 
	physics beyond the Standard Model of particle physics at the 
	multi-TeV scale. For search of cold dark matter GENIUS will cover 
	almost the full range of the parameter space of predictions of SUSY 
	for neutralinos as dark matter 
\cite{KK-Ram,Bed-KK2}. 
	Finally, GENIUS has the potential to be the first real-time detector 
	for low-energy (pp and $^7{Be}$) solar neutrinos 
\cite{Bau-KK,KKPropos99}. 
	A GENIUS-Test Facility has just been funded and will come into 
	operation by end of 2001.
\vspace{1pc}
\end{abstract}

\maketitle

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%Introduction%%%%%%%%%%%%%%%%%%%
\section{Introduction}

	Underground physics can complement in many ways the search for 
	New Physics at future colliders such as LHC and NLC and can serve 
	as important bridge between the physics that will be gleaned from 
	future high energy accelerators on the one hand, and satellite 
	experiments such as MAP and PLANCK on the other 
\cite{KK60Y}. 
	The first indication for beyond SM physics indeed has come from 
	underground experiments (neutrino oscillations from SK), and this 
	type of physics will play an even large role in the future.

	Concerning neutrino physics, without double beta decay there will be 
	no solution of the nature of the neutrino (Dirac or Majorana 
	particle) and of the structure of the neutrino mass matrix. Only 
	investigation of $\nu$ oscillations {\it and} double beta decay 
	together can lead to an absolute mass scale.

	Concerning the search for cold dark matter, even a discovery of 
	SUSY by LHC will not have proven that neutralinos form 
	indeed the cold dark matter in the Universe. Direct detection 
	of the latter by underground detectors remains indispensable. 
	Concerning solar neutrino physics, present information on possible 
$\nu$ 
	oscillations relies on 
0.2$\%$ 
	of the solar neutrino flux. The total pp neutrino flux has not 
	been measured and also no real-time information is available for 
	the latter.

	The GENIUS project proposed in 1997 (see 
%\cite {KK97,KH97,KK99nu98,KK99WEIN98,KKHH98,KKet99} 
\cite{KK-BEY97,KK60Y})
	as the first third generation $\beta\beta$ detector, could attack 
	all of these problems with an unpredented sensitivity.

%%%%%%%%%%%%%%%%%%%%%%%%%%%%% Section 2 %%%%%%%%%%%%%%%%%%%%%%%%%%%%

\section{GENIUS, Double Beta Decay and the Light Majorana Neutrino Mass}

	Present double beta experiments are not able to reach a limit 
	for the (effective) neutrino mass below 
$\sim$ 0.1 eV. 
	The most sensitive experiment is {\it since eight years} the 
	HEIDELBERG-MOSCOW experiment using the world's largest source 
	strength of 11 kg of 86$\%$ enriched $^{76}{Ge}$ 
	in form of 5 high-purity Ge detectors, run in the Gran Sasso 
	Underground laboratory. The limits reached after 37.24 kg y 
	of measurement\\ 
	$T^{0\nu}_{1/2}$ $>3.5(2.1)\cdot{10}^{25}y$ and 
	$<m_{\nu}><0.26 (0.34) eV$, 68$\%$ and 90$\%$ c.l., respectively.

	The status and potential of other experiments are shown in 
Fig. 1.

%%%%%%%%%Fig1%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{figure}[htb]
\vspace{9pt}
\centering{
\includegraphics*[width=50mm, height=75mm, angle=-90]{Now4-gist-mass.ps}}
%\includegraphics*[width=75mm, height=50mm]{LIM-Engl.ps}}
\caption{Present situation, 2000, and expectation for the future, of the 
	most promising $\beta\beta$ experiments. Light parts of the bars: 
	present status; dark parts: expectation for running experiments; 
	solid and dashed lines: experiments under construction  
	or proposed experiments. For references see \cite{LowNu2}.}
\end{figure}

	With the era of the HEIDELBERG-MOSCOW experiment which will 
	remain the most sensitive experiment for the next years, the time 
	of the small smart experiments is over.

%%%%%%%%%Fig2%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{figure}[htb]
\vspace{9pt}
\centering{
\includegraphics*[width=50mm, height=75mm, angle=-90]
{Jahr00-Sum-difSchemNeutr.ps}}
%\includegraphics*[width=75mm, height=50mm]{cstatessum.eps}}
\caption{Values expected from $\nu$ oscillation experiments for 
	$m_{ee}\equiv(<m_\nu >)$ 
	in different schemes. The expectations are compared with the 
	present neutrino mass limits {\it obtained} from the 
	HEIDELBERG-MOSCOW experiment as well as the {\it expected}  
	sensitivities for the CUORE, MOON, EXO proposals and the 1 ton 
	and 10 ton proposal of GENIUS \cite{KKP}. For references  and more 
	details about the different experiments see 
\cite{KK60Y,LowNu2}.}
\end{figure}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%end fig.2 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

The requirements in sensitivity for future experiments to play 
	a decisive role in the solution of the structure of the neutrino 
	mass matrix are shown in 
Fig.2.
	Shown are the expectations for the effective neutrino mass (the 
	observable in $\beta\beta$ decay) from the present experimental 
	status of all existing neutrino oscillation experiments in the 
	different presently experimentally favored neutrino mass models 
\cite{KKPS,KKP}.

	It can be seen that a sensitivity down to\\ 
$<m_{\nu}>\approx$ 0.001 eV as it may be reached {\it only} by the GENIUS 
	project will be able to test {\it all} neutrino scenarios 
	allowed by the oscillation experiments, except for one, the not 
	favoured hierarchical LOW solution. For details see
\cite{KKPS,KKP,KKPcomm}. 

	To reach this level of sensitivity $\beta\beta$ experiments have 
	to become large. A source strength of up to 10 tons of enriched 
	material touches the world production limits. At the same time the 
	background has to be reduced by a factor of 1000 and more compared 
	to that of the HEIDELBERG-MOSCOW experiment. 

Table 1 
	lists some key numbers for GENIUS, and of the main other proposals 
	made after the GENIUS proposal. Their potential is shown also 
in Fig.2. 
	It is seen that not all of these proposals fully cover the region 
	to be probed. Among them is also the recently presented MAJORANA 
	project. 
	
%	e.g., the CUORE proposal will not be able to 
%	seriously contribute to the field, simply because increase of source 
%	strength alone without simultaneous sufficient improvement of the 
%	background is not enough.
%	The same serious limitation is true for the recently 
%	presented MAJORANA project.

	In the GENIUS project a reduction by a factor of more than 1000 down 
	to a background level of 0.1 events/tonne y keV in the range of 
$0\nu\beta\beta$ is reached by removing all material close to the detectors, 
	and by using naked Germanium detectors in a large 
	tank of liquid nitrogen. It has been shown that the detectors show 
	excellent performance under such conditions
\cite{KKPropos99}.
	
	For technical questions and extensive Monte Carlo simulations of the 
	GENIUS project for its application in double beta decay we refer to 
%\cite{KKHH98,Bau99,KKet99}. 
\cite{KKPropos99}.

%%%%%%%%%Fig3%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\vspace{190pt}
\begin{figure}[t!]
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%\vspace{-190pt}
\centering{
\put(0,-120){\special{PSfile=Bedn-Wp2000.ps hscale=40 vscale=40}}}
%\includegraphics*[width=75mm, height=50mm]{AAAA1.ps}}
\end{picture}

\vspace{30pt}
\caption{WIMP-nucleon cross section limits in pb for scalar
	interactions as function of the WIMP mass in GeV.
	Shown are contour lines of present experimental limits (solid lines) 
	and of projected experiments (dashed lines). Also shown is the 
	region of evidence published by DAMA. The theoretical expectations 
	are shown by a scatter plot (from \cite{Bed-KK2}) and by the grey 
	region (from \cite{Ell}).} 
\end{figure}
%%%%%%%%%%%%%%%% end Fig. 3 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

  %%%%%%%%%%%%%%%%%%%%%%%%%%%%% Section 3 %%%%%%%%%%%%%%%%%%%%%%%%%%%%

\section{GENIUS and Other Beyond Standard Model Physics}

	GENIUS will allow besides the major step in neutrino physics 
	described in section 2 the access to a broad range of other beyond 
	SM physics topics in the multi-TeV range. Already now 
	$\beta\beta$ decay probes the TeV scale on 
	which new physics should manifest itself (see, e.g. 
\cite{KK-BEY97,KK-TR98}). 
	Basing to a large extent on the theoretical work of the Heidelberg 
	group in the last four years, the HEIDELBERG-MOSCOW experiment yields 
	results for SUSY models (R-parity breaking, sneutrino mass), 
	leptoquarks (leptoquarks-Higgs coupling), compositeness, 
	right-handed W mass, nonconservation of Lorentz invariance and 
	equivalence 
	principle, mass of a heavy left or righthanded neutrino, 
	competitive to corresponding results from high-energy accelerators 
	like TEVATRON and HERA. The potential of GENIUS extends into the 
	multi-TeV region for these fields and its sensitivity would 
	correspond to that of LHC or NLC and beyond (for details see 
%\cite{C, KK??}. 
\cite{KK60Y,KK-TR98}).

%%%%%%%%%%%%%%%%%%%%%%%%%%%%% Section 4 %%%%%%%%%%%%%%%%%%%%%%%%%%%%

\section{GENIUS and Cold Dark Matter Search}

	Already now the HEIDELBERG-MOSCOW experiment is the most sensitive 
	Dark Matter experiment worldwide concerning the raw data. GENIUS 
	would already in a first step, with 100 kg of {\it natural} Ge 
	detectors, cover a significant part of the MSSM parameter space 
	for prediction of neutralinos as cold dark matter 
(Fig. 3). For this purpose the background 
	in the energy range $<$ 100 keV has to be reduced to 
	${10}^{-2}$ events/kg y keV, which is possible if the detectors 
	are produced and handled on Earth surface under heavy shielding, 
	to reduce the cosmogenic background produced by spallation through 
	cosmic radiation (critical products are tritium, 
$^{68}{Ge}$, $^{63}{Ni}$, ...) 
	to a minimum. For details we refer to 
\cite{KKPropos99}. 
Fig. 3 shows together with the expected sensitivity of GENIUS predictions 
	for neutralinos as dark matter by two models, one basing on 
	supergravity
\cite{Ell}, 
	another starting from more relaxed unification conditions  
\cite{Bed-KK2}.
 
	The sensitivity of GENIUS for Dark Matter corresponds to that 
	obtainable with a 1 ${km}^3$ AMANDA detector for 
	{\it indirect} detection (neutrinos 
	from neutralino annihilation at the Sun). Interestingly both 
	experiments would probe different neutralino 
	compositions: GENIUS mainly gaugino-dominated neutralinos, 
	AMANDA mainly neutralinos with comparable 
	gaugino and Higgsino components. 
	It should be stressed that, together with DAMA, GENIUS will be the 
	only future Dark Matter experiment, which would be able to positively 
	identify a dark matter signal by the seasonal modulation signature. 
	This {\it cannot} be achieved, for example, by the CDMS experiment.

%%%%%%%%%%%%%%%%%%%%%%%%%TABLE 1 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{table*}[h]
\caption{Some key numbers of future double beta decay experiments (and of 
	the {\sf HEIDELBERG-MOSCOW} experiment). Explanations: 
	${\nabla}$ - assuming the background of the present pilot project. 
	$\ast\ast$ - with matrix element from [Sta90*-II], [Tom91**-I], 
	[Hax84**-I], [Wu91*-II], [Wu92*-II] (see Table II in [HM99*-III]). 
	${\triangle}$ - this case shown 
	to demonstrate {\bf the ultimate limit} of such experiments. 
	For details see \cite{KK60Y}.}
\label{table:1}
\newcommand{\m}{\hphantom{$-$}}
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{\footnotesize
%{\normalsize
{  
\begin{tabular}[!h]{|c|c|c|c|c|c|c|c|}
%[!h]{|c|c|c|c|c|c|c|c|}
\hline
\hline
 &  &  &  & Assumed &  &  & \\
 &  &  &  & backgr. & Run- & Results & \\
$\beta\beta$-- & & & Mass & $\dag$ events/ & $ning$ & limit for & 
${<}m_{\nu}{>}$ \\
$Isoto-$ & $Name$ & $Status$ & $(ton-$ & kg y keV, & Time  
& $0\nu\beta\beta$ & \\
pe & & & nes) & $\ddag$ events/kg & (tonn. & half-life & ( eV )\\ 
& & & & y FWHM,  & years) & (years) & \\
& & & & $\ast$ events &  &  & \\
& & &  & /yFWHM &  &  & \\
\hline
\hline
 &  &  &  &  &  &  & \\
~${\bf ^{76}{Ge}}$ & {\bf HEIDEL-} & {\bf run-}  & 0.011 & $\dag$ 0.06 
& {\bf 35.5} & ${\bf 1.9\cdot{10}^{25}}$ & {\bf $<$ 0.34} $\ast\ast$\\
 & {\bf BERG}  &  &  (enri-  &  &  {\bf kg y} &  {\bf 90$\%$ c.l.} 
& {\bf 90$\%$ c.l.} \\
& {\bf MOSCOW} & {\bf ning} & ched) & $\ddag$ 0.24  &  
& ${\bf 3.1\cdot{10}^{25}}$ & {\bf $<$ 0.26} $\ast\ast$\\
& {\bf [Kla99e**]} &  &  & $\ast$ 2 & & 
{\bf 68$\%$ c.l.} & {\bf 68$\%$ c.l.}\\
& {\bf [HM2000*]} &  &  &  &  & {\bf NOW !!}  & {\bf NOW !!}\\
& {\bf [-III]} &  &  &  &  &  &\\
\hline
\hline
\hline
 &  &  &  &  &  &  & \\
${\bf ^{100}{Mo}}$ & {\sf NEMO III} & {\it under} & $\sim$0.01 & $\dag$ 
{\bf 0.0005} &  &  &\\
 & {\tt [NEM2000]}& {\it constr.} & (enri- & $\ddag$ 0.2  & 50 & 
${10}^{24-25}$ & 0.3-0.7\\
 &  &  & -ched) &  $\ast$ 2 &kg y  &  &\\
\hline
\hline
&  &  &  &  &  &  & \\
${\bf ^{130}{Te}}$ & ${\sf CUORE}^{\nabla}$ & Pro- & 0.75 & $\dag$ 0.5 & 5 & 
$9\cdot{10}^{24}$ & 0.2-0.5\\
 & {\tt [Gui99a*}& posal &(natu-  & $\ddag$ 4.5  &  & & \\ 
 &{\tt  -VI]} &  & ral)& $\ast$ 1000  &  &  & \\
\hline
&  &  &  &  &  &  &  \\
${\bf ^{130}{Te}}$ & {\sf CUORE}  &  Pro- & 0.75   & $\dag$ 0.005 & 5 
& $9\cdot{10}^{25}$ & 0.07-0.2\\
&  &  posal  & (natu-  &  $\ddag$ 0.045&  & &\\
&  & &  ral) &  $\ast$ 45 &  &  & \\
\hline
&  &  &  &  &  &  & \\
${\bf ^{100}{Mo}}$ & {\sf MOON} & idea & 10 (en-& ? & 30 & ? & \\
 & {\tt [Eji99b*} &  & rich.) & & & &0.03 \\
 & {\tt -VI]} &  & 100 &  & 300 &  & \\
 &  &  & (nat.) &  &  &  & \\
\hline
&  &  &  &  &  &  & \\
${\bf ^{136}{Xe}}$ & {\sf EXO} & Pro-& 1 & $\ast$ 0.4 & 5 & 
$8.3\cdot{10}^{26}$ & 0.05-0.14\\
&  & &  &  &  &  & \\
${\bf ^{136}{Xe}}$ & {\tt [Dan2000a]} & posal  & 10 & $\ast$ 0.6 & 10 & 
$1.3\cdot{10}^{28}$ & 0.01-0.04\\
&  &  &  &  &  &  & \\ 
\hline 
\hline
\hline
\hline
&  &  &  &  &  &  &  \\
~${\bf ^{76}{Ge}}$ & {\bf GENIUS} & Pro- & 1  & $\dag$ 
${\bf 0.04\cdot{10}^{-3}}$ & 1 & ${\bf 5.8\cdot{10}^{27}}$ & 
{\bf 0.02-0.05} \\
 & {\tt [Kla97**}  & posal &(enrich.)  
& $\ddag$ ${\bf 0.15\cdot{10}^{-3}}$ & & & \\
& {\tt -VI]} &  &  & $\ast$ {\bf 0.15} &  &  &  \\
&  &  & 1 & ${\bf \ast~ 1.5}$ & 10 & ${\bf 2\cdot{10}^{28}}$  & 
{\bf 0.01-0.028} \\
\hline
&  &  &  &  &  &  &  \\
~${\bf ^{76}{Ge}}$ & {\bf GENIUS} & Pro- & 10 
& $\ddag$ ${\bf 0.15\cdot{10}^{-3}}$ & 10 &
${\bf 6\cdot{10}^{28}}$ & {\bf 0.006 -}\\
&  {\tt [Kla97**-} &  &  &  &  &  &  {\bf 0.016}\\
 &  {\tt -VI]} &  posal &(enrich.) & ${\bf 0^{\triangle}}$ & 10 & 
${\bf 5.7\cdot{10}^{29}}$ & {\bf 0.002 -}\\
&  &  &  &  &  &  &  {\bf 0.0056}\\ 
\hline 
\hline
\end{tabular}\\[2pt]
}}
%\vspace{0.3cm}
\end{table*}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%end TABLE 1 %%%%%%%%%%%%%%%%%%%%%%%%


%%%%%%%%%%%%%%%% Fig.4 %%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{figure}[htb]
\vspace{9pt}
\centering{
%\includegraphics*[scale=0.4, angle=-90]{LLL.ps}} %which I bild
\includegraphics*[width=60mm, height=80mm, angle=-90]{Cosmo-1d-3y.ps}} 
%\includegraphics*[width=80mm, height=55mm]{cosmo_1d_3y_nonsat.eps}} %orig.file
\caption{Simulated cosmogenic background during detector production. 
	Assumptions: 30 days exposure of material before processing, 
	1 d activation after zone refining, 3 y deactivation underground 
	(see \cite{LowNu2}).}
\end{figure}

%%%%%%%%%%%%%%%% end Fig. 4 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

%%%%%%%%%%%%%%%%%%%%%%%%%%%%% Section 5 %%%%%%%%%%%%%%%%%%%%%%%%%%%%

\section{GENIUS and Low-Energy Solar Neutrinos}

	Gallex and Sage 
	measure pp + $^7{Be}$ + $^{8}B$ neutrinos (60 + 30 + 10$\%$) down 
	to 0.24 MeV, the Chlorine experiment measured $^7{Be}$ + $^8{B}$ 
	neutrinos (80$\%$ $^8{B}$) above $E_\nu$= 0.817 MeV, all without 
	spectral, time and detection information. No experiment has 
	separately measured the pp and $^7{Be}$ neutrinos and no experiment 
	has measured the {\it full} pp $\nu$ flux. BOREXINO plans to 
	measure $^7{Be}$ neutrinos, the access to pp neutrinos 
	being limited by $^{14}C$ contamination (the usual problem of 
	organic scintillators). GENIUS could be the first detector measuring 
	the {\it full} pp ( and $^7{Be}$) neutrino flux in real time.

%%%%%%%%%%%%%%%% Fig.5 %%%%%%%%%%%%%%%%%%%%%%%%%%
\begin{figure}[htb]
\vspace{9pt}
\centering{
\includegraphics*[width=80mm, height=55mm]{pp_7be.eps}}
\caption{Simulated spectrum of low-energy solar neutrinos (according to SSM) 
	for the GENIUS detector (1 tonne natural or enriched Ge) 
(from \cite{Bau-KK}).}
\end{figure}
%%%%%%%%%%%%%%%% end Fig. 5 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

	Extending the radius of GENIUS to 13 m and improving some of the 
	shielding parameters as described in 
\cite{KKPropos99,Bau-KK} 
	the background can be reduced to a level of 
${10}^{-3}$ events/ kg y keV (Fig. 4) (see also 
\cite{LowNu2}). 
	This will allow to look for the pp and $^7{Be}$ solar neutrinos by 
	elastic neutrino-electron scattering with a threshold of 11 keV or at 
	most 19 keV (limit of possible tritium background) (Fig. 5) which 
	would be the 
	lowest threshold among other proposals to detect pp 
	neutrinos, such as HERON, HELLAZ, NEON, LENS, MOON, XMASS.

	The counting rate of GENIUS (10 ton) would be 6 events per day 
	for pp and 18 per day for $^7{Be}$ neutrinos, i.e. similar to 
	BOREXINO, but by a factor of 30 to 60 larger than a 20 ton LENS 
	detector and a factor of 10 larger than the MOON detector.

%%%%%%%%%%%%%%%%%%%%%%%%%%%%% Section 6 %%%%%%%%%%%%%%%%%%%%%%%%%%%%

\section{GENIUS - Test Facility}

	Construction of a test facility for GENIUS - GENIUS-TF - 
	consisting of $\sim$ 40 kg of HP Ge detectors suspended in a 
	liquid nitrogen box has been started. Up to end of 2000, three 
	detectors each of $\sim$ 2.5 kg and with a threshold of as low as 
	$\sim$ 500 eV have been produced.

	Besides test of various parameters of the GENIUS project, the test 
	facility would allow, with the projected background of 
	4 events/kg y keV in the low-energy range, to probe the DAMA evidence 
	for dark matter by the seasonal modulation signature within about 
	one year of measurement  
	with 95 $\%$ c.l.. Even for an initial lower mass of 20 kg the 
	time scale would be not larger than three years (for details see 
\cite{KK2000,Bau2000}. 
	If using the enriched $^{76}{Ge}$ detectors of the HEIDELBERG-MOSCOW 
	experiment in the GENIUS-TF setup, a background in the 
	$0\nu\beta\beta$ region a factor 30 smaller than in the 
	HEIDELBERG-MOSCOW experiment could be obtained, 
	which would allow to test the effective Majorana neutrino mass down 
	to 0.15 eV (90$\%$ c.l.) in 6 years of measurement. This limit is 
	similar to what much larger experiments aim at, at much larger 
	time scale (see Table 1.).

%%%%%%%%%%%%%%%%%%%%%%%%%%%%% Section 7 %%%%%%%%%%%%%%%%%%%%%%%%%%%%

\section{Conclusion}

	The GENIUS project is - among the projected or discussed other third 
	generation double beta detectors - the one which exploits this method 
	to obtain information on the neutrino mass to the ultimate limit. 
	Nature is extremely generous to us, that with an increase of the 
	sensitivity by two orders of magnitude compared to the present 
	limit, down to $<m_\nu>\sim {10}^{-3}$ eV, indeed essentially all 
	neutrino scenarios allowed by present neutrino oscillation 
	experiments can be probed.

	GENIUS is the only of the new projects which 
	simultaneously has a huge potential for cold dark matter search, 
	{\it and} for real-time detection of low-energy neutrinos. 

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%THE BIBLIOGR>%%%%%%%%%%%%%%%%%

\begin{thebibliography}{9}

\bibitem{KK-BEY97} \KK ~in Proceedings of the First International 
	Conference on 
	Particle Physics Beyond the Standard Model, Castle Ringberg, 
	Germany, 8-14 June 1997, edited by  H.V. Klapdor-Kleingrothaus 
	and H.P\"as, {\it IOP Bristol} (1998) 485-531 and
	{\it Int. J. Mod. Phys.} {\bf A 13} (1998) 3953, and
	{\it J. Phys.} {\bf G 24} (1998) 483 - 516. 

\bibitem{KKPS} H.V. Klapdor-Kleingrothaus, H. P\"as and A.Yu. Smirnov,
	Preprint: {\it hep-ph/}{\bf 0003219}, (2000) and in press  
	in {\it Phys. Rev.} {\bf D} (2000).

\bibitem{KK-Ram} \KK ~and Y. Ramachers, {\it Eur. Phys. J} {\bf A 3} (1998)
	85 - 92.

\bibitem{Bed-KK2}  
	V.A. Bednyakov and H.V. Klapdor-Kleingrothaus, \PRD {\bf 62} (2000)
	043524/1-9; V.A. Bednyakov and H.V. Klapdor-Kleingrothaus, 
	Preprint: {\it hep-ph/}{\bf 0011233} (2000).

\bibitem{KKPropos99} H.V. Klapdor-Kleingrothaus, L. Baudis, G.~Heusser,
  	B.~Majorovits and H.~P\"as, GENIUS - a Supersensitive Germanium
  	Detector System for Rare Events, Proposal, {\it MPI-Report} 
	{\bf MPI-H-V26-1999} 
	and Preprint: {\it hep-ph/}{\bf 9910205} and in Proceedings of the 
	Second International Conference on Particle Physics Beyond the 
	Standard Model ``BEYOND'99'', Castle Ringberg, Germany, 6-12 June 
	1999, edited by \KK~ and I.V. Krivosheina, {\it IOP Bristol}, 
	(2000) 915 - 1014. 

\bibitem{Bau-KK} L. Baudis and H.V. Klapdor-Kleingrothaus, 
	{\it Eur. Phys. J.} {\bf A 5} (1999) 441-443. 
%\and Preprint: {\it hep-ex/}{\bf 9906044}

\bibitem{KK60Y} \KK, {\sf "60 Years of Double Beta Decay"},
	{\it World Scientific, Singapore} (2001) 1253p.

%\bibitem{KK97} ??????????????????
%
%\bibitem{KH97} ???????????????????????/
%
%\bibitem{KK99nu98} \KK, ~in Proc. of 18th International Conference on
%	Neutrino Physics and Astrophysics (NEUTRINO 98), Takayama, Japan, 
%	4-9 Jun 1998, (eds) Y. Suzuki et al. 
%	{\it Nucl. Phys. Proc. Suppl.} {\bf 77} (1999) 357 - 368.
%
%\bibitem{KK99WEIN98} \KK, ~in Proc. of WEIN'98, "Physics Beyond the 
%	Standard Model", Proceedings of the Fifth International WEIN 
%	Conference, P. Herczeg, C.M. Hoffman and \KK (Editors),  
%	{\it World Scientific, Singapore} (1999) 275 -- 311.
%
%\bibitem{KKHH98} \KK ~, J.~Hellmig and M.~Hirsch, 
%	{\it J. Phys.} {\bf G 24} (1998) 483.
%
%\bibitem{KKet99} ?????????????????? 
%
%\bibitem{KK2000Bucharest} \KK, ~in Proc. of the International Symposium on
%	Advances in Nuclear Physics, eds.: D. Poenaru and S. Stoica, 
%	{\it World Scientific, Singapore} (2000) 123 - 129 pp.
%
\bibitem{KKP} H.V. Klapdor-Kleingrothaus, H. P\"as and A.Yu. Smirnov, 
	to be publ. (2001)

\bibitem{KKPcomm} \KK ~and H. P\"as, Preprint: {\it physics/}{\bf 0006024} 
	and {\it Comm. in Nucl. and Part. Phys.} (2000).


%\bibitem{Bau99} HEIDELBERG-MOSCOW Coll.: L. Baudis, A. Dietz, G. Heusser, 
%	\KK, I.V. Krivosheina, St. Kolb, B. Majorovits, V.F. Melnikov, 
%	H. P\"as, F. Schwamm, H. Strecker, V. Alexeev, A. Balysh, 
%	A. Bakalyarov, S.T. Belyaev, V.I. Lebedev and S. Zhukov, 
%	{\it Phys. Rev. Lett.} {\bf 83} (1999) 41-44 
%	and {\it hep-ex/}{\bf 9902014}.
%
%\bibitem{KKet99} ??????????????????????

\bibitem{KK-TR98} H.V. Klapdor-Kleingrothaus, in Proc of International 
	Symposium on Lepton and Baryon Number Violation, Trento, Italy, 
	20-25 April, 1998, ed H.V. Klapdor-Kleingrothaus and 
	I.V. Krivosheina, {\it IOP, Bristol}, (1999) 251-301 and 
	Preprint: {\it hep-ex/}{\bf 9901021} and \KK ~, {\it Springer Tracts 
	in Modern Physics}, {\bf 163} (2000) 69 - 104.
%	Eds.: A. Faessler, Kosmas and Leontaris, {\it Springer-Verlag}, 
%	Heidelberg, Germany (2000) 69 - 104.
 
%	{\it Int. J. Mod. Phys.} {\bf A13} (1998) 3953 - 3992.

\bibitem{Ell} J. Ellis, A. Ferstl and K.A. Olive, {\it Phys. Lett.} 
	{\bf B 481} (2000) 304 - 314 and Preprint: {\it hep-ph/}{\bf 0001005} 
	and  Preprint: {\it hep-ph/}{\bf 0007113}.

\bibitem{LowNu2} \KK~, in Proc. Int. Workshop on Low Energy Solar 
	Neutrinos, LowNu2, Dec. 4-5; and in Proc. of NOON2000 Conf., 
	Dec. 6-8 (2000) Tokyo, Japan, 
	ed: Y. Suzuki et al. {\it World Scientific, Singapore} (2001).

\bibitem{KK2000} \KK, ~L. Baudis, A. Dietz, G. Heusser, I. Krivosheina, 
	B. Majorovits, H. Strecker , S.T. Belyaev, V.I. Lebedev and 
	coworkers, {\bf MPI-H-V32-2000}. 

\bibitem{Bau2000} L. Baudis, A. Dietz, G. Heusser, B. Majorovits, 
	H. Strecker, H.V. Klapdor-Kleingrothaus, 
	hep-ex/0012022, submitted for publication.

\end{thebibliography}

\end{document}


espcrc2.tex
%%%%%%%%%% espcrc2.tex %%%%%%%%%%
%
% $Id: espcrc2.tex 1.1 1999/07/26 10:28:22 Simon Exp spepping $
%
\documentclass[twoside]{article}
\usepackage{fleqn,espcrc2}

% change this to the following line for use with LaTeX2.09
% \documentstyle[twoside,fleqn,espcrc2]{article}

% if you want to include PostScript figures
\usepackage{graphicx}
% if you have landscape tables
\usepackage[figuresright]{rotating}

% put your own definitions here:
%   \newcommand{\cZ}{\cal{Z}}
%   \newtheorem{def}{Definition}[section]
%   ...
\newcommand{\ttbs}{\char'134}
\newcommand{\AmS}{{\protect\the\textfont2
  A\kern-.1667em\lower.5ex\hbox{M}\kern-.125emS}}

% add words to TeX's hyphenation exception list
\hyphenation{author another created financial paper re-commend-ed Post-Script}

% declarations for front matter
\title{Elsevier instructions for the preparation of a
       2-column format camera-ready paper in \LaTeX}

\author{P. de Groot\address{Mathematics and Computer Science Division, 
        Elsevier Science Publishers B.V., \\ 
        P.O. Box 103, 1000 AC Amsterdam, The Netherlands}%
        \thanks{Footnotes should appear on the first page only to
                indicate your present address (if different from your
                normal address), research grant, sponsoring agency, etc.
                These are obtained with the {\tt\ttbs thanks} command.}
        and 
        X.-Y. Wang\address{Economics Department, University of Winchester, \\
        2 Finch Road, Winchester, Hampshire P3L T19, United Kingdom}}
       
\begin{document}

\begin{abstract}
These pages provide you with an example of the layout and style for
100\% reproduction which we wish you to adopt during the preparation of
your paper. This is the output from the \LaTeX{} document class you
requested.
\vspace{1pc}
\end{abstract}

% typeset front matter (including abstract)
\maketitle

\section{FORMAT}

Text should be produced within the dimensions shown on these pages:
each column 7.5 cm wide with 1 cm middle margin, total width of 16 cm
and a maximum length of 20.2 cm on first pages and 21 cm on second and
following pages. The \LaTeX{} document class uses the maximal stipulated
length apart from the following two exceptions (i) \LaTeX{} does not
begin a new section directly at the bottom of a page, but transfers the
heading to the top of the next page; (ii) \LaTeX{} never (well, hardly
ever) exceeds the length of the text area in order to complete a
section of text or a paragraph. Here are some references:
\cite{Scho70,Mazu84}.

\subsection{Spacing}

We normally recommend the use of 1.0 (single) line spacing. However,
when typing complicated mathematical text \LaTeX{} automatically
increases the space between text lines in order to prevent sub- and
superscript fonts overlapping one another and making your printed
matter illegible.

\subsection{Fonts}

These instructions have been produced using a 10 point Computer Modern
Roman. Other recommended fonts are 10 point Times Roman, New Century
Schoolbook, Bookman Light and Palatino.

\section{PRINTOUT}

The most suitable printer is a laser printer. A dot matrix printer
should only be used if it possesses an 18 or 24 pin printhead
(``letter-quality'').

The printout submitted should be an original; a photocopy is not
acceptable. Please make use of good quality plain white A4 (or US
Letter) paper size. {\em The dimensions shown here should be strictly
adhered to: do not make changes to these dimensions, which are
determined by the document class}. The document class leaves at least
3~cm at the top of the page before the head, which contains the page
number.

Printers sometimes produce text which contains light and dark streaks,
or has considerable lighting variation either between left-hand and
right-hand margins or between text heads and bottoms. To achieve
optimal reproduction quality, the contrast of text lettering must be
uniform, sharp and dark over the whole page and throughout the article.

If corrections are made to the text, print completely new replacement
pages. The contrast on these pages should be consistent with the rest
of the paper as should text dimensions and font sizes.

\section{TABLES AND ILLUSTRATIONS}

Tables should be made with \LaTeX; illustrations should be originals or
sharp prints. They should be arranged throughout the text and
preferably be included {\em on the same page as they are first
discussed}. They should have a self-contained caption and be positioned
in flush-left alignment with the text margin within the column. If they
do not fit into one column they may be placed across both columns
(using \verb-\begin{table*}- or \verb-\begin{figure*}- so that they
appear at the top of a page).

\subsection{Tables}

Tables should be presented in the form shown in
Table~\ref{table:1}.  Their layout should be consistent
throughout.

\begin{table*}[htb]
\caption{The next-to-leading order (NLO) results
{\em without} the pion field.}
\label{table:1}
\newcommand{\m}{\hphantom{$-$}}
\newcommand{\cc}[1]{\multicolumn{1}{c}{#1}}
\renewcommand{\tabcolsep}{2pc} % enlarge column spacing
\renewcommand{\arraystretch}{1.2} % enlarge line spacing
\begin{tabular}{@{}lllll}
\hline
$\Lambda$ (MeV)           & \cc{$140$} & \cc{$150$} & \cc{$175$} & \cc{$200$} \\
\hline
$r_d$ (fm)                & \m1.973 & \m1.972 & \m1.974 & \m1.978 \\
$Q_d$ ($\mbox{fm}^2$)     & \m0.259 & \m0.268 & \m0.287 & \m0.302 \\
$P_D$ (\%)                & \m2.32  & \m2.83  & \m4.34  & \m6.14  \\
$\mu_d$                   & \m0.867 & \m0.864 & \m0.855 & \m0.845 \\
$\mathcal{M}_{\mathrm{M1}}$ (fm)   & \m3.995 & \m3.989 & \m3.973 & \m3.955 \\
$\mathcal{M}_{\mathrm{GT}}$ (fm)   & \m4.887 & \m4.881 & \m4.864 & \m4.846 \\
$\delta_{\mathrm{1B}}^{\mathrm{VP}}$ (\%)   
                          & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ \\
$\delta_{\mathrm{1B}}^{\mathrm{C2:C}}$ (\%) 
                          & \m0.03  & \m0.03  & \m0.03  & \m0.03  \\
$\delta_{\mathrm{1B}}^{\mathrm{C2:N}}$ (\%) 
                          & $-0.19$ & $-0.19$ & $-0.18$ & $-0.15$ \\
\hline
\end{tabular}\\[2pt]
The experimental values are given in ref. \cite{Eato75}.
\end{table*}

\begin{sidewaystable}
\caption{The next-to-leading order (NLO) results
{\em without} the pion field.}
\label{table:2}
\newcommand{\m}{\hphantom{$-$}}
\newcommand{\cc}[1]{\multicolumn{1}{c}{#1}}
\renewcommand{\arraystretch}{1.2} % enlarge line spacing
\begin{tabular*}{\textheight}{@{\extracolsep{\fill}}lllllllllllll}
\hline
& $\Lambda$ (MeV) & \cc{$140$} & \cc{$150$} & \cc{$175$} & \cc{$200$} & \cc{$225$} & \cc{$250$} &
\cc{Exp.} & \cc{$v_{18}$~\cite{v18}} &  \\
\hline
%b
 & $r_d$ (fm)                        & \m1.973 & \m1.972 & \m1.974 & \m1.978 & \m1.983 & \m1.987 & 1.966(7) & \m1.967 & \\[2pt]
 & $Q_d$ ($\mbox{fm}^2$)             & \m0.259 & \m0.268 & \m0.287 & \m0.302 & \m0.312 & \m0.319 & 0.286    & \m0.270 & \\[2pt]
 & $P_D$ (\%)                        & \m2.32  & \m2.83  & \m4.34  & \m6.14  & \m8.09  & \m9.90  & $-$      & \m5.76  & \\[2pt]
 & $\mu_d$                           & \m0.867 & \m0.864 & \m0.855 & \m0.845 & \m0.834 & \m0.823 & 0.8574   & \m0.847 & \\[5pt]
 & $\mathcal{M}_{\mathrm{M1}}$ (fm)             & \m3.995 & \m3.989 & \m3.973 & \m3.955 & \m3.936 & \m3.918 & $-$      & \m3.979 & \\[5pt]
 & $\mathcal{M}_{\mathrm{GT}}$ (fm)             & \m4.887 & \m4.881 & \m4.864 & \m4.846 & \m4.827 & \m4.810 & $-$      & \m4.859 & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{VP}}$ (\%)   & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ & $-0.44$ & $-$      & $-0.45$ & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{C2:C}}$ (\%) & \m0.03  & \m0.03  & \m0.03  & \m0.03  & \m0.03  & \m0.03  & $-$      & \m0.03  & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{C2:N}}$ (\%) & $-0.19$ & $-0.19$ & $-0.18$ & $-0.15$ & $-0.12$ & $-0.10$ & $-$      & $-0.21$ & \\
\hline
\end{tabular*}\\[2pt]
The experimental values are given in ref. \cite{Eato75}.
\end{sidewaystable}

Horizontal lines should be placed above and below table headings, above
the subheadings and at the end of the table above any notes. Vertical
lines should be avoided.

If a table is too long to fit onto one page, the table number and
headings should be repeated above the continuation of the table. For
this you have to reset the table counter with
\verb|\addtocounter{table}{-1}|. Alternatively, the table can be turned
by $90^\circ$ (`landscape mode') and spread over two consecutive pages
(first an even-numbered, then an odd-numbered one) created by means of
\verb|\begin{table}[h]| without a caption. To do this, you prepare the
table as a separate \LaTeX{} document and attach the tables to the
empty pages with a few spots of suitable glue.

\subsection{Useful table packages}

Modern \LaTeX{} comes with several packages for tables that
provide additional functionality. Below we mention a few. See
the documentation of the individual packages for more details. The
packages can be found in \LaTeX's \texttt{tools} directory.

\begin{description}
  
\item[\texttt{array}] Various extensions to \LaTeX's \texttt{array}
  and \texttt{tabular} environments.
  
\item[\texttt{longtable}] Automatically break tables over several
  pages. Put the table in the \texttt{longtable} environment instead
  of the \texttt{table} environment.
  
\item [\texttt{dcolumn}] Define your own type of column. Among others,
  this is one way to obtain alignment on the decimal point.

\item[\texttt{tabularx}] Smart column width calculation within a
  specified table width.
  
\item[\texttt{rotating}] Print a page with a wide table or figure in
  landscape orientation using the \texttt{sidewaystable} or
  \texttt{sidewaysfigure} environments, and many other rotating
  tricks. Use the package with the \texttt{figuresright} option to
  make all tables and figures rotate in clockwise. Use the starred
  form of the \texttt{sideways} environments to obtain full-width
  tables or figures in a two-column article.

\end{description}

\subsection{Line drawings}

Line drawings should be drawn in India ink on tracing paper with the
aid of a stencil or should be glossy prints of the same; computer
prepared drawings are also acceptable. They should be attached to your
manuscript page, correctly aligned, using suitable glue and {\em not
transparent tape}. When placing a figure at the top of a page, the top
of the figure should be at the same level as the bottom of the first
text line.

All notations and lettering should be no less than 2\,mm high. The use
of heavy black, bold lettering should be avoided as this will look
unpleasantly dark when printed.

\subsection{PostScript figures}

Instead of providing separate drawings or prints of the figures you
may also use PostScript files which are included into your \LaTeX{}
file and printed together with the text. Use one of the packages from
\LaTeX's \texttt{graphics} directory: \texttt{graphics},
\texttt{graphicx} or \texttt{epsfig}, with the \verb|\usepackage|
command, and then use the appropriate commands
(\verb|\includegraphics| or \verb|\epsfig|) to include your PostScript
file.

The simplest command is: \newline
\verb|\includegraphics{file}|, which inserts the
PostScript file \texttt{file} at its own size. The starred version of
this command: \newline
\verb|\includegraphics*{file}|, does the same, but clips
the figure to its bounding box.

With the \texttt{graphicx} package one may specify a series of options
as a key--value list, e.g.:
\begin{tabular}{@{}l}
\verb|\includegraphics[width=15pc]{file}|\\
\verb|\includegraphics[height=5pc]{file}|\\
\verb|\includegraphics[scale=0.6]{file}|\\
\verb|\includegraphics[angle=90,width=20pc]{file}|
\end{tabular}

See the file \texttt{grfguide}, section ``Including Graphics Files'',
of the \texttt{graphics} distribution for all options and a detailed
description.

The \texttt{epsfig} package mimicks the commands familiar from the
package with the same name in \LaTeX2.09. A PostScript file
\texttt{file} is included with the command
\verb|\psfig{file=file}|.

Grey-scale and colour photographs cannot be included in this way,
since reproduction from the printed CRC article would give
insufficient typographical quality. See the following subsections.

\begin{figure}[htb]
\vspace{9pt}
\framebox[55mm]{\rule[-21mm]{0mm}{43mm}}
\caption{Good sharp prints should be used and not (distorted) photocopies.}
\label{fig:largenenough}
\end{figure}
%
\begin{figure}[htb]
\framebox[55mm]{\rule[-21mm]{0mm}{43mm}}
\caption{Remember to keep details clear and large enough.}
\label{fig:toosmall}
\end{figure}

\subsection{Black and white photographs}

Photographs must always be sharp originals ({\em not screened
versions\/}) and rich in contrast. They will undergo the same reduction
as the text and should be pasted on your page in the same way as line
drawings.

\subsection{Colour photographs}

Sharp originals ({\em not transparencies or slides\/}) should be
submitted close to the size expected in publication. Charges for the
processing and printing of colour will be passed on to the author(s) of
the paper. As costs involved are per page, care should be taken in the
selection of size and shape so that two or more illustrations may be
fitted together on one page. Please contact the Technical Editor in the
Camera-Ready Publications Department at Elsevier for a price quotation
and layout instructions before producing your paper in its final form.

\section{EQUATIONS}

Equations should be flush-left with the text margin; \LaTeX{} ensures
that the equation is preceded and followed by one line of white space.
\LaTeX{} provides the package {\tt fleqn} to get the flush-left
effect.

\begin{equation}
H_{\alpha\beta}(\omega) = E_\alpha^{(0)}(\omega) \delta_{\alpha\beta} +
                          \langle \alpha | W_\pi | \beta \rangle 
\end{equation}

You need not put in equation numbers, since this is taken care of
automatically. The equation numbers are always consecutive and are
printed in parentheses flush with the right-hand margin of the text and
level with the last line of the equation. For multi-line equations, use
the {\tt eqnarray} environment. For complex mathematics, use the
\AmS-\LaTeX{} package.

\begin{thebibliography}{9}
\bibitem{Scho70} S. Scholes, Discuss. Faraday Soc. No. 50 (1970) 222.
\bibitem{Mazu84} O.V. Mazurin and E.A. Porai-Koshits (eds.),
                 Phase Separation in Glass, North-Holland, Amsterdam, 1984.
\bibitem{Dimi75} Y. Dimitriev and E. Kashchieva, 
                 J. Mater. Sci. 10 (1975) 1419.
\bibitem{Eato75} D.L. Eaton, Porous Glass Support Material,
                 US Patent No. 3 904 422 (1975).
\end{thebibliography}

References should be collected at the end of your paper. Do not begin
them on a new page unless this is absolutely necessary. They should be
prepared according to the sequential numeric system making sure that
all material mentioned is generally available to the reader. Use
\verb+\cite+ to refer to the entries in the bibliography so that your
accumulated list corresponds to the citations made in the text body. 

Above we have listed some references according to the
sequential numeric system \cite{Scho70,Mazu84,Dimi75,Eato75}.
\end{document}

hep-ph0102277.extracted_bib
\begin{thebibliography}{9}

\bibitem{KK-BEY97} \KK ~in Proceedings of the First International 
	Conference on 
	Particle Physics Beyond the Standard Model, Castle Ringberg, 
	Germany, 8-14 June 1997, edited by  H.V. Klapdor-Kleingrothaus 
	and H.P\"as, {\it IOP Bristol} (1998) 485-531 and
	{\it Int. J. Mod. Phys.} {\bf A 13} (1998) 3953, and
	{\it J. Phys.} {\bf G 24} (1998) 483 - 516. 

\bibitem{KKPS} H.V. Klapdor-Kleingrothaus, H. P\"as and A.Yu. Smirnov,
	Preprint: {\it hep-ph/}{\bf 0003219}, (2000) and in press  
	in {\it Phys. Rev.} {\bf D} (2000).

\bibitem{KK-Ram} \KK ~and Y. Ramachers, {\it Eur. Phys. J} {\bf A 3} (1998)
	85 - 92.

\bibitem{Bed-KK2}  
	V.A. Bednyakov and H.V. Klapdor-Kleingrothaus, \PRD {\bf 62} (2000)
	043524/1-9; V.A. Bednyakov and H.V. Klapdor-Kleingrothaus, 
	Preprint: {\it hep-ph/}{\bf 0011233} (2000).

\bibitem{KKPropos99} H.V. Klapdor-Kleingrothaus, L. Baudis, G.~Heusser,
  	B.~Majorovits and H.~P\"as, GENIUS - a Supersensitive Germanium
  	Detector System for Rare Events, Proposal, {\it MPI-Report} 
	{\bf MPI-H-V26-1999} 
	and Preprint: {\it hep-ph/}{\bf 9910205} and in Proceedings of the 
	Second International Conference on Particle Physics Beyond the 
	Standard Model ``BEYOND'99'', Castle Ringberg, Germany, 6-12 June 
	1999, edited by \KK~ and I.V. Krivosheina, {\it IOP Bristol}, 
	(2000) 915 - 1014. 

\bibitem{Bau-KK} L. Baudis and H.V. Klapdor-Kleingrothaus, 
	{\it Eur. Phys. J.} {\bf A 5} (1999) 441-443. 
%\and Preprint: {\it hep-ex/}{\bf 9906044}

\bibitem{KK60Y} \KK, {\sf "60 Years of Double Beta Decay"},
	{\it World Scientific, Singapore} (2001) 1253p.

%\bibitem{KK97} ??????????????????
%
%\bibitem{KH97} ???????????????????????/
%
%\bibitem{KK99nu98} \KK, ~in Proc. of 18th International Conference on
%	Neutrino Physics and Astrophysics (NEUTRINO 98), Takayama, Japan, 
%	4-9 Jun 1998, (eds) Y. Suzuki et al. 
%	{\it Nucl. Phys. Proc. Suppl.} {\bf 77} (1999) 357 - 368.
%
%\bibitem{KK99WEIN98} \KK, ~in Proc. of WEIN'98, "Physics Beyond the 
%	Standard Model", Proceedings of the Fifth International WEIN 
%	Conference, P. Herczeg, C.M. Hoffman and \KK (Editors),  
%	{\it World Scientific, Singapore} (1999) 275 -- 311.
%
%\bibitem{KKHH98} \KK ~, J.~Hellmig and M.~Hirsch, 
%	{\it J. Phys.} {\bf G 24} (1998) 483.
%
%\bibitem{KKet99} ?????????????????? 
%
%\bibitem{KK2000Bucharest} \KK, ~in Proc. of the International Symposium on
%	Advances in Nuclear Physics, eds.: D. Poenaru and S. Stoica, 
%	{\it World Scientific, Singapore} (2000) 123 - 129 pp.
%
\bibitem{KKP} H.V. Klapdor-Kleingrothaus, H. P\"as and A.Yu. Smirnov, 
	to be publ. (2001)

\bibitem{KKPcomm} \KK ~and H. P\"as, Preprint: {\it physics/}{\bf 0006024} 
	and {\it Comm. in Nucl. and Part. Phys.} (2000).


%\bibitem{Bau99} HEIDELBERG-MOSCOW Coll.: L. Baudis, A. Dietz, G. Heusser, 
%	\KK, I.V. Krivosheina, St. Kolb, B. Majorovits, V.F. Melnikov, 
%	H. P\"as, F. Schwamm, H. Strecker, V. Alexeev, A. Balysh, 
%	A. Bakalyarov, S.T. Belyaev, V.I. Lebedev and S. Zhukov, 
%	{\it Phys. Rev. Lett.} {\bf 83} (1999) 41-44 
%	and {\it hep-ex/}{\bf 9902014}.
%
%\bibitem{KKet99} ??????????????????????

\bibitem{KK-TR98} H.V. Klapdor-Kleingrothaus, in Proc of International 
	Symposium on Lepton and Baryon Number Violation, Trento, Italy, 
	20-25 April, 1998, ed H.V. Klapdor-Kleingrothaus and 
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%	Eds.: A. Faessler, Kosmas and Leontaris, {\it Springer-Verlag}, 
%	Heidelberg, Germany (2000) 69 - 104.
 
%	{\it Int. J. Mod. Phys.} {\bf A13} (1998) 3953 - 3992.

\bibitem{Ell} J. Ellis, A. Ferstl and K.A. Olive, {\it Phys. Lett.} 
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	and  Preprint: {\it hep-ph/}{\bf 0007113}.

\bibitem{LowNu2} \KK~, in Proc. Int. Workshop on Low Energy Solar 
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\bibitem{KK2000} \KK, ~L. Baudis, A. Dietz, G. Heusser, I. Krivosheina, 
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\bibitem{Bau2000} L. Baudis, A. Dietz, G. Heusser, B. Majorovits, 
	H. Strecker, H.V. Klapdor-Kleingrothaus, 
	hep-ex/0012022, submitted for publication.

\end{thebibliography}