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\title{Neuantrag auf Gew"ahrung einer Sachbeihilfe\\Proposal for a new research project}
\author{Prof.\ Dr.\ Karl\ Mannheim\\Prof.\ Dr.\ Dr.\ Wolfgang Rhode}

\begin{document}

\maketitle

%\noindent {\it Das Inhaltsverzeichnis dient nur zur "Ubersicht und ist im eigentlichen Antrag nicht enthalten. \\
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%{\LARGE{\bf
%\begin{center}
%Neuantrag auf Gew"ahrung einer Sachbeihilfe\\Proposal for a research project
%\end{center}
%}}

\section[1]{Allgemeine Angaben/General Information}
%\anmerk{Die Gliederung ist von der DFG vorgegeben}

%Neuantrag auf Gew"ahrung einer Sachbeihilfe.

\subsection[1.1]{Antragsteller/Applicants}
% IN CASE A PROJECT IS DISTRIBUTED BETWEEN SEVERAL INSTITUTES
% PLEASE GIVE AT LEAST ONE APPLICANT FOR EACH INSTITUTE;
% ALSO, IN THIS CASE, THE PROPOSAL MUST MAKE CLEAR WHICH 
% RESOURCES GO TO WHERE, HOW THE WORK IS SPLIT, HOW THE INTERACTION
% SHALL PROCEED ETC.
%\setlength{\tabcolsep}{5em}

\begin{tabular}{|p{0.44\textwidth}|p{0.22\textwidth}|p{0.22\textwidth}|}\hline
{\bf Name}&\multicolumn{2}{l|}{\bf Akademischer Grad}\\
{\sc Rhode, Wolfgang, Prof.~Dr.~Dr.}&\multicolumn{2}{l|}{Universit"atsprofessor (C3)}\\\hline\hline
{\ }&{\bf Birthday}&{\bf Nationality}\\
{\ }&Oct 17 1961&German\\\hline
\multicolumn{3}{|l|}{\bf Institut, Lehrstuhl}\\
\multicolumn{3}{|l|}{Institut f"ur Physik}\\
\multicolumn{3}{|l|}{Experimentelle Physik V (Astroteilchenphysik)}\\\hline
{\bf Address at work        }&\multicolumn{2}{l|}{\bf Home address}\\[0.5ex]
{Universit"at Dortmund      }&\multicolumn{2}{l|}{                }\\
{                           }&\multicolumn{2}{l|}{Am Schilken 28  }\\
{44221 Dortmund             }&\multicolumn{2}{l|}{58285 Gevelsberg}\\
{Germany                    }&\multicolumn{2}{l|}{Germany         }\\[0.5ex]
{\parbox[t]{1.5cm}{Phone:}+49\,(231)\,755-3550}&\multicolumn{2}{l|}{\parbox[t]{1.5cm}{Phone:}+49\,(931)\, }\\
{\parbox[t]{1.5cm}{Fax:}+49\,(231)\,755-4547}&\multicolumn{2}{l|}{~}\\\hline\hline
\multicolumn{3}{|c|}{{\bf email}: wolfgang.rhode@udo.edu}\\\hline

\multicolumn{3}{c}{~}\\[1ex]\hline

{\bf Name}&\multicolumn{2}{l|}{\bf Akademischer Grad}\\
{\sc Mannheim, Karl, Prof.~Dr.}&\multicolumn{2}{l|}{Universit"atsprofessor (C4)}\\\hline\hline
{\ }&{\bf Birthday}&{\bf Nationality}\\
{\ }&Jan 4 1960&German\\\hline
\multicolumn{3}{|l|}{\bf Institut, Lehrstuhl}\\
\multicolumn{3}{|l|}{Institut f"ur Theoretische Physik und Astrophysik}\\
\multicolumn{3}{|l|}{Lehrstuhl f"ur Astronomie}\\\hline
{\bf Address at work        }&\multicolumn{2}{l|}{\bf Home address}\\[0.5ex]
{Julius-Maximilians-Universit"at}&\multicolumn{2}{l|}{                }\\
{                           }&\multicolumn{2}{l|}{Oswald-Kunzemann-Str. 12}\\
{97074 W"urzburg            }&\multicolumn{2}{l|}{97299 Zell am Main      }\\
{Germany                    }&\multicolumn{2}{l|}{Germany                 }\\[0.5ex]
{\parbox[t]{1.5cm}{Phone:}+49\,(931)\,888-5031}&\multicolumn{2}{l|}{\parbox[t]{1.5cm}{Phone:} }\\
{\parbox[t]{1.5cm}{Fax:}+49\,(931)\,888-4603}&\multicolumn{2}{l|}{~}\\\hline\hline
\multicolumn{3}{|c|}{{\bf email}: mannhein@astro.uni-wuerzbueg.de}\\\hline
\end{tabular}

\newpage

\paragraph{1.2 Topic (Thema)}~\\
%% MAXIMAL 140 Zeichen fuer den DFG Jahresbericht
%% AUCH IN DEUTSCH BEIFGEN
Long-term VHE $\gamma$-ray monitoring of bright blazars with a dedicated Cherenkov telescope

\paragraph{1.3 Discipline and field of work (Fachgebiet und Arbeitsrichtung)}~\\
Astronomy and Astrophysics, Particle Astrophysics

\paragraph{\bf 1.4 Scheduled duration in total (Voraussichtliche Gesamtdauer)}~\\
3\,years (+ seit wann das Vorhaben l"auft, seit wann es von der DFG gef"ordert wird)
(evtl. gr"o"ser als der Antragszeitraum?)

\paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\
3\,years. Work on the project may and will begin immediately after the
funding.

\paragraph{\bf 1.6 Summary (Zusammenfassung)}~\\
% AUCH IN DEUTSCH BEIFGEN
We propose to set up an imaging air Cherenkov telescope with low-cost
but high performance design for robotic and remote operation. The goal
is to achieve long-term monitoring of bright blazars which will unravel
the origin and nature of their variability (und den zugrunde liegen
Beschleunigungsmachanismen der kosmischen Strahlung). The telescope
design is based on a technological upgrade of one of the former
telescopes of the HEGRA collaboration still located at the Observatorio
Roque de los Muchachos on the Canarian Island La Palma (Spain). With
the upgrade an improvement in senitivity by 25\%{\bf (?)} and a lower
energy threshold in the order of 350\,GeV{\bf (?)} will be achieved.

{\bf IceCube erw"ahnen?}
{\em Nicht gescheduled von anderen IACTs?}

{\em
\begin{itemize}
\item Kerziele des Antrags f"ur die bewilligenden Gremien
\item Bei Bewilligung: Internet Datenbank 
\item Verwendung von themenrelevanten Schl"uselbegriffe
\item M"oglichst keine Abk"urzungen
\item Verst"andlichkeit auch f"ur nicht Fachleute (gegeben?)
\item nicht mehr als 15 Zeilen oder max. 1600 Zeichen.
\end{itemize}
}

\newpage

\section[2]{Stand der Forschung, eigene Vorarbeiten\\State of the art, preliminary work by proposer}

\subsection[2.1]{State of the art (Stand der Forschung)}

{\em
\begin{itemize}
\item Knapp und pr"azise in der unmittelbaren Beziehung zum Vorhaben
\item Als Begr"undung f"ur eigene Arbeit
\item inkl. einschl"agiger Arbeiten anderer Wissenschaftler
\item $\to$ Einordnung eigener Arbeit, welcher Beitrag zu welchen Fragen
\end{itemize}
}

{\bf Hier gibt es glaub ich drei Punkte: Physik, IACTs und gAPD}

\paragraph{Introduction:} Since the termination of the HEGRA
observations, the succeeding experiments MAGIC and H.E.S.S.\ have
impressively extended the physical scope of gamma ray observations by
detecting tens of formerly unknown gamma ray sources and analyzing
their energy spectra and temporal behavior. This became possible by
lowering the energy threshold from 700\,GeV to less than 100\,GeV and
increasing at the same time the sensitivity by a factor of five.

To fully exploit the discovery potential of the improved sensitivity,
the discovery of new, faint objects has become the major task for the
new telescopes. A diversity of astrophysical source types such as
pulsar wind nebulae, supernova remnants, microquasars, pulsars, radio
galaxies, clusters of galaxies, gamma ray bursts, and blazers can be
studied with these telescopes and limits their availability for
monitoring purposes of well-known bright sources.

There are strong reasons to make an effort for the continuous
monitoring of the few exceptionally bright blazars. This can be
achieved by operating a dedicated monitoring telescope of the
HEGRA-type, referred to in the following as DWARF (Dedicated
multiWavelength Agn Research Facility). The reasons are outlined in
detail below.

\textbf{The science case:} The variability of blazars, seen across the
entire electromagnetic spectrum, arises from the dynamics of
relativistic jets and the particle acceleration going on in them. The
jets are launched from the vicinity of accreting supermassive black
holes, and theoretical models predict variability arising from the
interplay between jet expansion, particle injection, acceleration and
cooling.\\

Long-term monitor observations of bright blazars are the key to obtain
a solid and complete data base for variability investigations. 

{\bf Hier sollte ganz klar rauskommen was der aktuelle Stand der
Forschung ist und wieso man um weiter zu kommen unbedingt ein 
long-term monitoring IACT braucht}

{\bf Geigermode APDs?}

\subsubsection{High energy gamma and neutrino sources}

{\bf Aus den folgenden beiden Abschnitten kann man vielleicht einen 
(k"urzeren) machen?}

The TeV photon astronomy succeeded in discovering {\bf 14}
extragalactic and {\bf ???} galactic objects at the sky during the past
decades. Additionally there are two diffuse regions within our galaxy
which have been detected by H.E.S.S.\cite{Aharonian:2006} and Milagro
\cite{Milagro:2007}.
%The first source was discovered in the
%year 19{\bf??} by the {\bf HEGRA} collaboration {\it (War das nicht wer
%anders, die zu allererst den Crab sahen?...ZITAT?)}.
In comparison to
x-ray measurments, which are able to scan the entire sky for sources
and thus have cataloged more than {\bf 1000 ???} sources, this number
appears to be quite small. One reason for this is the small field of
view of imaging air cherenkov telesopes (IACTs), another reason the
absorption of the TeV photon signal of distant ($z>0.2$) sources due to
extragalactic background light (EBL). Due to this small statistic at
the moment it is of particular importance that instruments with high
sensitivity concentrate on the observation of new objects in the TeV sky
and not on the quantitative, permanent observation of already known
sources. 
% BRAUCHT MAN DEN FOLGENDEN ABSATZ WIRKLICH
%Even when a source was observed over a longer period of time
%this does mean {\bf  less than three month ???? {\it Viel l"anger sind
%die Quellen am St"uck doch gar nicht sichtbar, oder? Sinnvoller w"are
%es wom"oglich die wenigen Beobachtungsstunden in diesen X Monaten
%hervorzuheben.}} But one has to take into account that during this time
%also periods of bad weather and times with strong moon light can
%significantly reduce  observation time. Furthermore one has to consider
%that the sources are visible in the sky only for a few hours each night.

%{\bf Ist die Aufz"ahlung nich total "ubertrieben? Ist es f"ur unseren
%Antrag wirklich interessant welchem Typ die detektierten AGN angeh"oren
%und  wie sie hei"sen?}

The so far observed galactic objects are microqasars and supernova
remnands (SNR). The identified extragalactic sources are active
galactic nuclei (AGN). 
%NOETIG??? The objects are listed in table~\ref{dummy} {\bf
%TESHIMAS VORTRAG IN MADISON}. 
The AGN are 13 BLLacs and one FR-I
galaxy, M87. So High-peaked BL Lacertae objects are the prime source
population for studies with Cherenkov telescopes. It is obvious that
monitoring observations of strong blazars are orthogonal to the mission
of the larger Cherenkov telescopes with their discovery potential for
new sources (luminosity function, redshift distribution).
{\bf Das hatten wir oben eigtnlich schonmal}

In case of hadronic particle acceleration within the TeV emitters, the
signal may arise from $\pi^0$-decays. These neutral pions are decay
products of delta resonances, which are formed in proton-photon
interactions. Another decay channel of the delta resonance leads to the
production of charged pions and thus to neutrino production, coincident
with the TeV photons. Therefrom TeV sources are always
interesting objects for investigations with high energy neutrino
telescopes.

The strong variability in the temporal evolution of the AGN TeV photon
spectra cannot be explained conclusively yet, {\it warum braucht man
f"ur die Untersuchung Langzeitbeobachtungen?}

{\bf SENSITIVIT\"ATSPLOT, Was hat der hier zu suchen?, Aber irgendwo muessen
wir noch glaubhaft machen dass unsere Sensitivit"at ausreicht}\\
{\bf TABELLE QUELLEN, Was bringt das f"ur den Antrag oder den Referee?}\\
{\bf AGN Physik kann man nicht ohne die unteren Paragraphen erkl"aren,
Muss man die hier erkl"aren? Wir m"ussen nur deutlich machen warum wir 
Langzeitbeobachtungen brauchen, nicht, dass wir die Physik verstehen}\\
{\it Die Frage ist, ob man galaktische Quellen mit in die
Langzeit-Beobachtung nehmen will, dann mu"s man das einzeln
durchgehen. Ich bau die Argumentation gerade nur auf AGN auf,
keine galaktischen Quellen!}

\begin{itemize}
\item Welche Quellen wurden oberhalb von 1 TeV bislang beobachtet?
\item Welche Sensitivit"at braucht man?
\item $\to$ Hier muesste doch der Abschnitt aus Ziele und ein Verweis
darauf reichen, das HEGRA die Quellen detektiert hat und wir besser
sein werden, oder?
\end{itemize}

\paragraph{Physikalische Modelle}
Erkl"are die verschiedenen Szenarien:
{\bf Ist das wirklich n"otig. Da sollten doch referenzen reichen...
das ist ja wirklich nichts aktuelles!}
\begin{itemize}
\item Inverse Compton
\item Proton Synchrotron
\item Pion decay
\end{itemize}

Unterschiede darstellen: Pion bump ist nicht so Spitz; Inverse Compton:
wenn man den 2. bump erh"oht, erh"oht sich automatisch auch der
erste; oft widerspruch zu den Daten. Ich glaube, Proton Synchrotron hat
das Problem nicht so, und auch Pion Zerfall nat"urlich nicht. 

Au"serdem: Stand der Dinge, um die Variabilit"at zu erkl"aren
{\bf (Wichtig?) }

\paragraph{Ergebnisse von Multiwavelangth-Kampangen}
{\it hier m"ussen die verschiedenen Szenarien - inverse Compton von
elektronen/ proton Synchrotron und Pion-Zerf"alle an Einzelf"allen
diskutiert werden. Es gibt Bsp., bei denen Inverse Compton sehr gut
klappt; dann gibt's welche, wo das gar nicht hinhaut. Einen Fall
gibt's, wo Integral-Daten "uberhaupt nicht ins Bild passen. Da gibts
z.B. ein Papier von Aharonian zu auf astro-ph - irgendwann aus den
letzten 3 Monaten.}

Experimente erw"ahnen: EGRET, COMPTEL, Integral, H.E.S.S., MAGIC, wer
noch???  f"ur bisherige Spektren; GLAST zum F"ullen der L"ucke!!!

Auch hier: Diskussion der Variabilit"at; ``Orphan Flares''...

\paragraph{Die Photon-Neutrino-Verbindung}
{\bf Steht das nicht oben schon {\em AGNs are interstng
Targets for Neutrino Teleskops}?}

\subsection{Eigene Vorarbeiten/Preliminary work by proposer}

{\em
\begin{itemize}
\item Vollst"andige und konkrete Darstellung der eigenen Vorarbeiten
\item Fremde/eigene Literatur kennzeichenen (ggf. \"im Druck\")
\item Relevante wissenschaftl. Ver"offentlichung der letzen f"unf Jahre
\item Relavante Vor"offentlichung beif"ugen
\end{itemize}
}

Hie sollte was stehen zu (Ich denke der Abschnitt ist wichtig um zu
zeigen, dass man auch leisten kann was man verspricht)
\begin{itemize}
\item Aufbau von Drive und Starguider (W"urzburg)
\item Erfahrungen mit Spiegeln (Dr"oge, W"urzburg)
\item Erfahrungen mit PMTs/HV (Dortmund)
\item Erfahrungen mit HPDs (W"urzburg)
\item Die modulare und powerfull Analyse Software (W"urzburg)
\item Das bestreben die MCs modular umzuschreiben (W"urzburg, Dortmund?)
\item Erfahrungen mit MCs: Unfolding, Athmosphaere, Corsika? (Dortmund)
\item Die Automatisierung der Analyse und MCs, wichtig! (W"urzburg)
\item Neutrino Studien, um zu zeigen, dass die angestrebten 
Korrelationen auch wirklich von jemandem ausgewertet werden k"onnen 
(Dortmund)
\item Multi-Wellenl"angen Kampagnen (Suzaku, Swift), W"urzburg/Dortmund?
\item Bestehende Monitoring Proposal (MAGIC)
\item Die SSC Modellrechnungen aus W"urzburg
\item LISA? (W"urzburg)
\end{itemize}


\subsubsection{Beteiligung an Experimenten}

\paragraph{MAGIC}

\paragraph{IceCube}

The Dortmund group is IceCube member and working since years on
phenomenological calculations and data analysis of possible
coincidences between VHE-gamma and neutrino-emission. \\

The available automatic analysis package developed by the W"urzburg
group for MAGIC is modular and flexible, and can thus be used with
minor changes for the DWARF project.\\

Monte Carlo production and storage will take place at Universit"at
Dortmund Monte-Carlo-Erfahrung Dortmund $\to$ Marijkes Diplomarbeit

A microcontroller based motion control unit (SPS) similar to the one of
the current MAGIC II drive system will be used.\\
$\to$DriveSystem-Erfahrung W"urzburg

To correct for axis misalignments and possible deformations of the
structure (e.g. bending of camera holding masts) a pointing correction
algorithm as used in the MAGIC tracking system will be applied. It is
calibrated by measurement of the reflection of bright guide stars on
the camera surface and ensures a pointing accuracy well below the pixel
diameter. \\ $\to$ Diplomarbeit Benjamin Riegel (W"urzburg)

\section[3.1]{Ziele/Goals}

\subsection{Ziele/Goals}

{\em 
\begin{itemize}
\item Gestraffte Darstellung des wissenschaftlichen Programs und Zielsetzung
\item Ich denke das ist eine Art Abstract des Arbeitsprogramms.
\end{itemize}
}

The present application aims at putting the former CT3 of the HEGRA
collaboration on the Roque de los Muchachos back into operation - with
an enlarged mirror surface and a new camera and data taking, under the
name of DWARF. The sensitivity above  500\,GeV of this new instrument
will thus correspond with the one of the also disused  Whipple
telescope. \textbf{WHIPPLE wird aber noch benutzt!!!}

The layout of the telescope shall be carried out modular in such a
sense that components of future telescopes (mirror, camera, DAQ) can be
tested and optimized at this bodywork.

%Wissenschaftlich sollen folgende Punkte realisiert werden:
With the upgraded instrument the following scientific aims shall be
realized:

\begin{enumerate}
\item Long-term observations of temporal variations of TeV gamma
ray sources.\\
An understanding of this variability will deepen our knowledge about

  \begin{itemize}
  \item the composition and generation of the jets, intimately connected
to the physics of the ergosphere of rapidly spinning black holes
embedded into the hot plasma from the accretion flow.
  \item the plasma physics responsible for highly efficient particle
acceleration, bearing similarities to plasma physics of the interaction
between	extremely intense laser beams and matter.
  \item {the orbital modulation of jets due to binary black holes
expected from galaxy merger models.\\ \textbf{the search for signatures of
binary black hole systems from orbital modulation of VHE gamma ray
emission} \cite{Rieger:2000, Rieger:2001}\\
\item {\bf Wird das nicht ein bisschen viel Rieger?
\item Rieger; Periodic variability and binary black hole systems in blazars
\item Rieger; Supermassive binary black holes among cosmic gamma-ray sources
\item Rieger; On the geometric origin of periodicity in blazar-type sources
}}
  \end{itemize}

Long-term monitor observations of bright blazars are the key to obtain
a solid data base for variability investigations. Assuming
conservatively the performance of a single HEGRA-type telescope,
long-term monitoring of at least the following blazars is possible:
Mrk421, Mrk501, 1ES 2344+514, 1ES 1959+650, H 1426+428, PKS 2155-304.
We emphasize that DWARF will run as a facility dedicated to these
targets only, providing a maximum observation time for the program.
\textbf{\textit{oder ist dieser Abschnitt doch besser in 3.2.
aufgehoben?!}} 

\item Coincident observations with gamma telescopes in different
energy ranges:\\ Flux variations will be determined and compared with
variability properties in other wavelength ranges. 

\item Coincident observations with the neutrino telescope
IceCube:\\ Hadronic emission processes and possible coincidences
between VHE-gamma and neutrino-emission will be studied. 

\item Furthermore, we seek to obtain know-how for the operation
of future networks of Cherenkov telescopes (e.g. a monitoring array
around the globe or CTA) or telescopes at inaccessible sites. 
\end {enumerate}

\subsection{Arbeitsprogramm/Work schedule}

{\em
\begin{itemize}
\item Detaillierte Angaben "uber Vorgehen w"ahrend der Laufzeit
\item Hauptkriterium f"ur die Genehmigung
\item Halber Antrag
\item Warum welche Mittel f"ur was beantragt werden
\item Welche Methoden stehen zur Verf"ugung
\item Welche Methoden m"ussen entwickelt werden
\item Welche Hilfe von au"serhalb der eigenen Arbeitsgruppe ist notwendig
\end{itemize}
}

At least one of the proposed targets will be visible any time of the
year (see plot/appendix). For calibration purposes, some time will be
scheduled for observations of the Crab nebula, which is the brightest
known VHE emitter with constant flux.\\

In detail the following investigations are planned:
\begin{itemize}
\item As direct result of the measurements, the duty cycle, the
baseline emission, and the power spectrum of flux variations will be
determined and compared with variability properties in other wavelength
ranges.

\item The lightcurves will be interpreted using models for the
nonthermal emission from relativistically expanding plasma jets. In
particular models currently developed in the context of the Research
Training Group "Theoretical Astrophysics" in W"urzburg
(Graduiertenkolleg, GK1147) shall be used. Particle acceleration is
studied with hybrid MHD and particle-in-cell methods.

\item The black hole mass and accretion rate will be determined from
the emission models. Estimates of the black hole mass from emission
models, a possible orbital modulation, and the Magorrian relation
(relating the black hole mass with the stellar bulge mass of the host
galaxy) will be compared. \cite{Rieger:2003} {\bf eigentlich ist das
nicht mehr die Stelle mit Zitaten sondern die wo wir sagen, dass
wir das Know-how - in Form von Frank - haben.}

\item \textbf{To achieve a maximal database for these studies the
observation  schedule will be arranged together with the one for
Whipple. (Letter of  support?) ($\rightarrow$ collaboration with
Veritas)}

\item When flaring states will be discovered during the monitor
program, MAGIC will issue a Target of Opportunity observation to obtain
better time resolution (Letters of support?). Corresponding
Target-of-Opportunity (ToO) proposals to H.E.S.S.\ and Veritas are in
preparation.

\item DWARF observations will be combined with simultaneous MAGIC
observations. By this kind of observation the energy range of the MAGIC
telescope can be stretched to higher energies. This in turn leads to
the so far unique possibility to cover an energy range of tens of GeV
to several tens of TeV at the same time allowing the study of the
inverse compton peaks as well as absorption due to EBL simultaneously.
By a software coincidence trigger the sensitivity in the overlapping
energy region might be improved further.

\item Correlating the arrival times of neutrinos detected by the
neutrino telescope IceCube with simultaneous measurements of DWARF will
allow to test the hypothesis that flares in blazar jets are connected
to hadronic emission processes and thus to neutrino emission from these
sources. The investigation proposed here is complete for both, neutrino
and gamma observations, and can therefore lead to conclusive results.

\item The diffusive fluxes of escaping UHE cosmic rays obtained from
AUGER or flux limits of neutrinos from IceCube, respectively, will be
used to constrain models of UHE cosmic ray origin and large-scale
magnetic fields.

\item Multi-frequency observations together with the Mets"ahovi Radio
Observatory and the optical Tuorla Observatory are planned (Letters of
support appendix). The measurements will be correlated with INTEGRAL
and GLAST results, when available. X-ray monitoring using the SWIFT and
Suzaku facilities will be proposed.

\item The most ambitious scientific goal of this proposal is the search
for signatures of binary black hole systems from orbital modulation of
VHE gamma ray emission. In case of a confirmation of the present hints
in the temporal behaviour of Mrk501, gravitational wave templates could
be computed with high accuracy to establish their discovery with LISA
(PhD project at W"urzburg funded by the German LISA consortium).
\end{itemize}

\textbf{The technical setup:} At the Observatorio de los Muchachos
(ORM), at the MAGIC site, the mount of the former HEGRA telescope CT3
now owned by the MAGIC collaboration is still operational. One hut for
electronics close to the telescope is available. Additional space is
available in the MAGIC counting house.  The MAGIC Memorandum of
Understanding allows for operating it as an auxiliary instrument, and
basic support from the shift crew of MAGIC is guaranteed, although
robotic operation is the primary goal. Robotic operation is necessary
to reduce costs and man power demands. \textbf{Besides it reduces air 
pollution by significantly reducing traveling.} Furthermore, we seek to obtain
know-how for the operation of future networks of Cherenkov telescopes
(e.g. a monitoring array around the globe or CTA) or telescopes at
inaccessible sites. From the experience with the construction and
operation of MAGIC or HEGRA, respectively, the proposing groups
consider the planned focused approach (small number of experienced
scientists) as optimal for achieving the project goals. The available
automatic analysis package developed by the W"urzburg group for MAGIC
is modular and flexible, and can thus be used with minor changes for
the DWARF project. Therefore construction, commissioning and operation
of a small scale Cherenkov telescope are best suitable for education
and training of students by experienced scientists. 

To complete the mount to a functional Cherenkov telescope within a
period of one year, the following steps are necessary:

\paragraph{Camera:}
For long-term observations stability of the camera is a major
criterion. To keep the systematic errors small good background
estimation is mandatory. The only possibility for a synchronous
determination of the background is the determination from the night-sky
observed in the same field-of-view with the same instrument. To achieve
this the observed position is moved out of the camera center which
allows the estimation of the background from positions symmetric with
respect to the camera center (so called wobble-mode). This observation
mode increases the sensitivity by a factor of two \textbf{$\sqrt{2}$?} because spending
observation for dedicated background observations becomes obsolete,
which also ensures a better time coverage of the observed sources.
Having a camera large enough allowing more than one independent
position for background estimation increases sensitivity further by
better background statistics. This is the case if the source can be
shifted 0.6deg-0.7deg out of the camera center. A camera completely
containing shower images of events in the energy region of 1TeV-10TeV
should have a diameter in the order of 5 deg. To decrease the
dependence of the background measurement on the camera geometry, a
camera layout as symmetric as possible will be chosen. Consequently a
camera allowing for wobble-mode observations should be round and have a
diameter of 4.5deg-5.0deg.

To achieve this requirements a 313 Pixel camera (see figure
\ref{camDWARF}) will been build based on the experience with HEGRA and
MAGIC. 19 mm diameter Photomultiplier Tubes (PM, EMI 4035) will be
bought, similar to the HEGRA type (EMI\,9083\,KFLA). With a 20$\%$
improved quantum efficiency they ensure a granularity which is enough
to guarantee good results even below the energy threshold (flux peak
energy). Each individual pixel has to be equipped with a preamplifier,
an active high-voltage supply and control. The total expense for a
single pixel will be in the order of 600 EURO.

If development of geigermode APDs (QE$\ge$50$\%$) will be fast enough,
respectively the price low enough, and their long term stability is
proven well in time, their usage will be considered.

For a transition time one of the old HEGRA cameras might be borrowed
(see figure \ref{camCT3}). With a special coating (wavelength shifter)
its quantum efficiency might be improved by ~8$\%$\cite{Paneque:2004}.
\textbf{8\% sind f"ur flat-window-pmts angegeben... nach den Zeichnungen 
in z.B. German Hermanns Diss. sind sie aber nicht v"ollig flach...demnach 
k"onnten wir wohl 19\% zitieren.}
\textbf{Figure?}

\paragraph{Camera support:}
The camera chassis must be water tight. An automatic lid protecting the
PMs at day-time will be installed. For further protection a plexi-glass
window will be installed in the front of the camera. By over-coating
the window with an anti-reflex layer of magnesium-fluoride a gain in
transmission of 5$\%$ is expected. Each PM will be equipped with a
light-guide (Winston Cone) as developed by UC Davis and successfully in
operation in the MAGIC camera. (3000 EURO). The current design will be
improved by using a high reflectivity aluminized Mylar mirror-foil,
overcoated with a dialectical layer (SiO2 alternated with Niobium
Oxide), to reach a reflectivity in the order of 98$\%$. In total this
will gain ~15$\%$ in light-collection efficiency compared to the old
CT3 system.

For this setup the camera holding has to be redesigned. (1500\,Eur?)

An electric and optical shielding of the individual PMs is planned.

The mechanical work is done at Universit"at Dortmund.

\paragraph{Data acquisition:}
For the data acquisition system a hardware readout based on an analog
ring buffer (Domino II/III), currently developed for the MAGIC II
readout, will be used. This technology allows sampling the pulses with
high frequencies and allows to readout several channels with a single
Flash-ADC resulting in low-costs. The low power consumption will allow
including the digitization near the signal source which makes an analog
signal transfer obsolete. The advantage is less pick-up noise and less
signal dispersion. By high sampling rates (0.5\,GHz-1.2\,GHz) additional
information about the pulse shape can be obtained. This increasing the
over-all sensitivity further, because the short integration time allows
for almost perfect suppression of noise due to night-sky background
photons. The estimated trigger- (readout-) rate of the telescope is
below 100\,Hz (HEGRA: $<$10\,Hz) which allows to use a low-cost industrial
solution for readout of the system like USB\,2.0. (30.000-45.000:
95-145/channel). 

{\bf Current result obtained with the new 2\,GHz FADC system
in the MAGIC dat aacquisition show that for a single telescope
a sensitivity improvement with a fast FADC system is achievable.}

As for the HEGRA telescopes a simple multiplicity trigger is enough,
but also a simple three-next-neighbors (closed package) could be
programmed. ($<$30.000: $<$100/channel).

To guarantee a homogenous trigger setup over the whole camera the
individual pixel rates, dominated by night-sky noise, will be monitored
and kept constant.

Additional data reduction and preprocessing in the readout hardware or
the readout computer is provided. Assuming conservatively storage of
raw-data at a readout rate of 30\,Hz the storage space needed is less
than 250\,GB/month or 3\,TB/year. This amount of data can easily be stored
and processed by the W"urzburg Datacenter (current online capacity
$>$20\,TB, offline capacity $>$30\,TB, $>$16\,CPUs). To archive the data
safely 25 tapes (LTO3 with 400\,GB each, $\sim$1000\,Eur) and a SATA
disk-array ($\sim$4000\,Eur) will be bought.

\paragraph{On-site computing:}
For on-site computing less than three standard PCs are needed
($\sim$8.000\,Eur). This includes readout and storage, preprocessing,
and telescope control. For safety reasons a firewall is mandatory. For
local storage and backup two RAID\,5 SATA disk arrays with less than one
Terabyte capacity each will fulfill the requirement ($\sim$4.000\,Eur).
The data will be transmitted as soon as possible after data taking via
Internet to the W"urzburg Datacenter.

Monte Carlo production and storage will take place at Universit"at
Dortmund

For the absolute time necessary for an accurate source tracking a GPS
clock will be bought.

\paragraph{Mount and Drive:}
The present mount is used. Only a smaller investment for safety,
corrosion protection, cable ducts, etc. is needed (7.500). 

For movement motors, shaft encoders and control electronics in the
order of 10.000 EURO have to be bought. The drive system should allow
for relatively fast repositioning for three reasons: 1) Fast movement
might be mandatory for future ToO observations. 2) Wobble-mode
observations will be done changing the wobble-position continuously
(each 20\,min) for symmetry reasons. 3) To ensure good time coverage  of
more than one source visible at the same the observed source will be
changed in constant time intervals ($\sim$20\,min). Therefore three 150
Watt servo motors are intended. A microcontroller based motion control
unit (SPS) similar to the one of the current MAGIC II drive system will
be used. For communication with the readout-system a standard Ethernet
connection based on the TCP/IP- and UDP-protocol is applied.

\paragraph{Security:}
An uninterruptible power-supply unit (UPS) with 5-10\,kW will be
installed to protect the equipment against power cuts and ensure a safe
telescope position at the time of sun-rise. ($<$2000\,Eur)

\paragraph{Mirrors:}
The existing mirrors are replaced by new plastic mirrors which are
currently developed by the group of Wolfgang Dr"oge. The cheap and
light-weight material has been formerly used for Winston cones flown in
balloon experiments. The mirrors are copied from a master, coated with
a reflecting and a protective material. Previous tests have given
promising results. By a change of the mirror geometry the mirror area
can be increased from 8.5\,m$^2$ to 13\,m$^2$ (see picture \ref{CT3} and
montage \ref{DWARF}); this includes an increase of $\sim$10$\%$ per
mirror by using a hexagonal layout. A further increase of the mirror
area would require a reconstruction of parts of the mount and will
therefore be considered only in later phase of the experiment. 

If the current development cannot be finished in time a re-machining of
the old glass mirrors (8.5\,m$^2$) is possible with high purity aluminum
and quartz coating. (Both cases: 30 mirrors, 10k, offer by L-Tec
$\lesssim$500\,Eur/mirror * 30\,mirrors = 15.000\,Eur without transfer)

\textbf{In both cases the mirrors can be coated with the same high 
reflectivity aluminized Mylar mirror-foil, and a dialectical layer of SiO2
as for the Winston Cones (ref: Fraunhofer, private communication?). By this a
gain in reflectivity of ~10\% is achieved.}

To keep track of the alignment, reflectivity and optical
quality of the individual mirrors, and the point-spread function of the
total mirror, during long-term observations the application of an
automatic mirror adjustment system, as developed by ETH Z"urich and
successfully operated on the MAGIC telescope, is intended. The system
will be provided by ETH Z"urich. (1.000 EURO/pannel)

For a 3.5\,m \textbf{4\,m} diameter mirror the delay between an isochronous parabolic
mirror and a spherical mirror at the edge is in the order of\textbf{well below} 1ns (see
figure/appendix). For a sampling rate in the order of 2\,GHz a mirror
mounting with a parabolic shape is not needed. Since their small size the
individual mirrors can have a spherical shape.

\paragraph{Telescope calibration:}

Tracking: To correct for axis misalignments and possible deformations
of the structure (e.g. bending of camera holding masts) a pointing
correction algorithm as used in the MAGIC tracking system will be
applied. It is calibrated by measurement of the reflection of bright
guide stars on the camera surface and ensures a pointing accuracy well
below the pixel diameter. Therefore a high sensitive low-cost video
camera, as already in operation for MAGIC I and II, (300\,Eur camera,
300\,Eur optics, 300\,Eur housing) will be installed.

PM Gain: For the calibration of the PM gain a calibration system as
used for the MAGIC telescope is build. (2.000\,Eur)

Summarizing, the expenses for the telescope are dominated by the camera
and DAQ. The financial volume for the complete hardware inclusive
transport amounts roughly 400.000\,Eur.

\textbf{Future extensions:} The known duty cycle of 10\%
($\sim$1000\,h/year) for a Cherenkov telescope operated at La Palma
limits the time-coverage of the observations. Therefore we propose a
worldwide network of ($<$10) small scale Cherenkov telescopes to be
build in the future allowing 24\,h monitoring of the bright AGNs. Such a
system is so far completely unique in this energy range. In a first
stage of the project mounts of other former HEGRA telescopes could be
used operated at locations in Croatia, the United States and Mexico.
For an increased sensitivity and improved energy threshold the use of a
low-cost mount build by the company MERO for solar power generation is
proposed. The mount is based on the experiences with the MAGIC
telescope, also builds by MERO, and has a diameter in the order of
eight meters. Including support (concrete foundation, railways, etc)
the costs are below 100.000\,Eur.
\textbf{The intended future use of a camera built of G-APDs will by their 
highly improved QE (50\% instead of 20\%) increase the sensitivity by a factor 
of $\sim$2 and additionally lower the threshold by an equal amount.\\
MAGIC PMTs?}

\begin{figure}[ht]
\centering{
\includegraphics[width=12cm]{cam271.eps}
\caption{Schematic picture of the 313 pixel camera for DWARF with a field of view of 5$^\circ$.}
\label{camDWARF}
}
\end{figure}

\begin{figure}[ht]
\centering{
\includegraphics[height=0.4\textheight]{cam313.eps}
\caption{Schematic picture of the 271 pixel CT-3 camera with a field of view of 4.6$^\circ$.}
\label{camCT3}
}
\end{figure}

\begin{figure}[ht]
\centering{
\includegraphics[height=0.4\textheight]{cam313.eps}
\caption{Picture of the HEGRA CT-3 taken at a time when it was still in operation.}
\label{CT3}
}
\end{figure}

\begin{figure}[ht]
\centering{
\includegraphics[height=0.4\textheight]{cam313.eps}
\caption{Photo montage of DWARF as it will look alike after the mirror replacement.}
\label{DWARF}
}
\end{figure}

\clearpage
\newpage
\paragraph{3.3 ???? Untersuchungen}~\\
n/a

\paragraph{3.4 ???? Untersuchungen}~\\
n/a

\paragraph{3.5 ???? Untersuchungen}~\\
n/a

\newpage


\section[4]{Beantragte Mittel/Funds requested}

We request funding for a total of three years.

\subsection[4.1]{Personalbedarf/Required staff}
%Wir beantragen die F"orderung von je einem Postdoc und Doktoranden in
%W"urzburg und Dortmund.
We request funding for two postdocs (BATIIa, 3y) and two Ph.D. students
(BATIIa/2, 3y), one in Dortmund and one in W"urzburg each.

(im Antrag ist der qualifizierte Einsatz der studentischen Hilfskraefte
darzulegen, KEINE Betr"age angeben!)

(Bezahlung ab wann?, Kurzer Abriss der Aufgaben, ggf. Namen)

\anmerk{2 Institute x 3 Jahre x (1
PD = 60.000 + 1 PhD = 30.000) = 2 x 250.000 = 500.000}

%Von den Mitarbeitern sollen folgende Aufgaben erf"ullt werden:
The staff members shall fulfill the following tasks:

\begin{itemize}

\item Postdoc W"urzburg

\item Doktorand W"urzbug

\item Postdoc Dortmund

\item Doktorand Dortmund

\end{itemize}

%Geeignete und ggf. interessierte Kandidaten f"ur Postdocstellen sind...
Suitable candidates interested in these positions are Dr. xxx, Dr. yyy,
Dipl.-Phys. zzz and Dipl.-Phys. www.

\subsection[4.2]{Wissenschaftliche Ger"ate/Scientific equipment}

{\em 
\begin{itemize}
\item Alle Ger"ate "uber 10kEur, so spezifizieren, dass nach Bewilligung von der DFG beschafft werden k"onnen
\item Alle Ger"ate unter 10kEur, "Ubersicht mit Modellen, Begr"undung der Notwendigkeit
\end{itemize}
}


{\bf Camera} (self-made)\dotfill 204.000,00\,Eur\\[1ex]
   313\,pixels \'a\\
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Photomultiplier Tube EMI 4051\hfill 350,00\,Eur\\
   High voltage support and control (EMI)\hfill 250,00\,Eur\\
   Preamplifier\hfill 50,00\,Eur\\
   \end{minipage}\\[-0.5ex]
\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{The chosen PMT is the
successor of the PMT type formerly used in  the HEGRA cameras. It has
an 25\% enhances quantum efficiency and will be delivered with the HV
support and control, including the control electronics such as the high
voltage power supply.}\\[2ex]

{\bf Data acquisition}(self-made)\dotfill 77.000\,Eur\\[1ex]
   313\,pixels \'a\\
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Readout/channel\hfill 145,00\,Eur\\
   Trigger/channel\hfill 100,00\,Eur\\
   \end{minipage}\\[-0.5ex]
\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{Wie schreiben wir das auf?
Wenn ich es richtig verstehe k"onnen wir nicht schreiben wir w"urden
f"ur Riccardo die Elektronik bezahlen, denn sagt die DFG das m"u"ste
Riccardo selber beantragen. Es ist ja nicht  ausgeschlossen, da"s er es
tut.}\\[2ex]

{\bf Calibration System}\dotfill 9.000\,Eur\\[1ex]
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Absolute light calibration\hfill 2.000\,Eur\\
   Individual pixel rate control\hfill ?.???\,Eur\\
   Weather station\hfill 500\,Eur\\
   GPS clock\hfill 1.500\,Eur\\
   CCD camera with readout\hfill 5.000\,Eur\\
   \end{minipage}\\[-0.5ex]
\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{The GPs clock is necessary
for an accurate tracking. The light calibration box (was ist das?) will
be baught from the institute which produced the MAGIC calibration box.
The weather station helps judging the data  quality and the CCD cameras
are necessary for calibration of the tracking system (misalignment of
the telescope) and mispointing correction, e.g. due to wind gusts.}\\[2ex]

{\bf Mirrors} (total expense)\dotfill 15.000\,Eur\\

{\bf On-site computing}\dotfill 12.000\,Eur\\
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Three PCs\hfill 8.000\,Eur\\
   SATA RAID 3\,TB\hfill 4.000\,Eur\\
   \end{minipage}\\[-0.5ex]

{\bf Computing}\dotfill 4.000\,Eur\\
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   3\,TB disk extension\hfill 4.000\,Eur\\
   \end{minipage}\\[-0.5ex]

\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Summe 4.1:\hfill{\bf 500.000\,Eur}\hfill\hspace*{0pt}\\[-1ex]
\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
\hspace*{0.66\textwidth}\hrulefill\\


%@{\extracolsep{1em} \vfill
%\begin{tabular*}{\textwidth}{@{}l@{\extracolsep\fill}r@{}}
%\begin{tabular*}{\textwidth}{l@{\extracolsep\fill}|r|r}
%{\bf Ger"at A} (Typ)&& 1.000,75\,Eur\\
%Angebor der Firma xyz vom&&\\[1ex]
%{\bf Ger"at B} (Typ)&& 1.000,75\,Eur\\
%Angebot der Firma... vom&&\\[1ex]

%{\bf Camera} (Eigenbau)&& 204.000\,Eur\\[0.1ex]
%313\,Pixel*650\,Euro/Pixel&&\\

%\multicolumn{2}{p{0.5\textwidth}}
%{
%  \begin{tabular}{@{\hspace{1.5em}}l@{\extracolsep\fill}r}
%  313 Pixel a 650,00\,Eur&xxx,yy Eur\\
%  \multicolumn{2}{p{1.0\textwidth}}
%  {
%      \end{tabular}
%  }\\[0.1ex]
%  Winston Cones&3.000,00\,Eur\\
%  Holding and chassis&3.000,00\,Eur\\
%  \end{tabular}
  
  %begin{list}{-}{\topsep 0pt\parskip 0pt }
  %\begin{itemize}
  %\item Pixel: 650EURO/Pixel
  %   \begin{itemize}
  %   %\begin{itemize}
  %   \item 300-350Euro Photomultiplier (EMI 4051)
  %   \item 50EURO Preamplifier
  %   \item 200-250EURO HV control and support (EMI)
  %   \end{itemize}
  %\item Winston Cones: 3000Eur (?)
  %\item Camera holding and chassis: 3000EURO(?)
  %\end{itemize}
%}\\

%Linie nur rechts&&\\ \cline{3-3}\\[-1.5ex]
%&Summe 4.2&{\bf 250.000 Eur}\\ \cline{3-3}\\[-1.9ex]\cline{3-3}
%\end{tabular*}


\begin{itemize}

%\item Data acquisition: 313channel*245EURO/channel ~ 77.000EURO
%  \begin{itemize}
%  \item 145 (95) EURO/channel Readout
%  \item 100EURO/channel Trigger
%  \end{itemize}

%\item Calibration System: 9.000EURO
%  \begin{itemize}
%  \item 2000EURO Absolute light calibration?
%  \item IPR control?
%  \item Weather station 500EURO
%  \item 1500EURO GPS clock 
%  \item 5.000EURO CD Cameras + readout
%  \end{itemize}


%\item On-site computing: 12.000EURO
%  \begin{itemize}
%  \item 3xPC: 8000EURO
%  \item SATA RAID 3TB: 4000EURO
%  \end{itemize}	
%
%\item Computing: 4.000EURO
%  \begin{itemize}
%  \item 3TB SATA Disk space: 4000EURO(?)
%  \end{itemize}

\item AMC: 1000EURO/pannel
\item UPS: 2000EURO
\item 7.500EURO Robotics 

\end{itemize}

\subsection{Verbrauchsmaterial/Consumables}
{\em 
\begin{itemize}
\item Chemikalien, Glaswaren, etc. (Werkzeug?)
\item Stromrechnung La Palma (IAC Beitrag?), wie hoch pro Jahr?
\end{itemize}
}

\begin{itemize}
  \item operation costs: 5000EURO/3years
  \item 25 LTO3 Tapes: 1000EURO
  \item 10.000EURO Consumables
\end{itemize}

\subsection{Reisen/Travel expenses}

{\em
\begin{itemize}
\item Alle Reisen begr"unden
\item Zusammenarbeit mit anderen Wissenschaftlern
\item Einladung von G"asten (Zahl und Dauer)
\item Workshops
\item Kongressreisen (KEIN weiterer Antrag bei der DFG m"oglich)
\item Telskop Aufbau
\end{itemize}
}

\begin{itemize}
  \item 35.000EURO Travel and construction
\end{itemize}

\subsection{Publikationskosten/Publication costs}
%keine
none

\subsection {Sonstige Kosten}
%keine\\
\begin{itemize}
   \item 5.000EURO transport and storage container
   \item Dismantling (0, will be covered by proposing institutes)
   \item 15.000EURO Transport
   \item \textbf{2.000EURO security fence}
	 \item \textbf{150.000EURO Kick-off Meeting Lapland}
\end{itemize}

\section[5]{Voraussetzungen f"ur die Durchf"uhrung des Vorhabens\\Preconditions for carrying out the project}
%Vor Durchf"uhrung ist die Zustimmung der Magic-Kollaboration und des
%IAC einzuholen. Nach Vorgespr"achen ist von der Erteilung dieser
%Zustimmung auszugehen.

Before realization the consent of the Magic collaboration and the IAC
is required. According to preliminary talks this consent is expected to
be given.

\subsection{Zusammensetzung der Arbeitsgruppe/The research team}

{\em 
\begin{itemize}
\item Name, akademischer Grad, Dienststellung aller die am geplanten Vorhaben mitarbeiten sollen
\item technisches Personal, Hilfskr"afte: Anzahl reicht
\item Trenning nach Drittmitteln (Stipendien) und Istitutsmitteln
\end {itemize}
}




\noindent {\bf Dortmund}:

\begin{itemize}
\item Prof. Dr. Dr. Wolfgang Rhode (Grundausttattung)
\item Dr. Tanja Kneiske (Postdoc (Ph"anomenologie), Forschungsstipendium)
\item Dr. Julia Becker (Postdoc (Ph"anomenologie), Grundausttattung)
\item Dipl.-Phys. Jens Dreyer (Doktorand (IceCube), Grundausttattung)
\item Dipl.-Phys Kirsten M"unich (Doktorandin (IceCube), Projekt-finanziert)
\item M.Sc. Valentin Curtef (Doktorand (MAGIC), Projekt-finanziert)
\item cand. phys. Jan L"unemann (Diplomand (IceCube), zum F\"orderbeginn diplomiert)
\item cand. phys. Dominik Leier (Diplomand (Ph"anomenologie), zum F\"orderbeginn diplomiert)
\item cand. phys. Michael Backes (Diplomand (MAGIC), zum F\"orderbeginn diplomiert)
\item cand. phys. Daniela Hadasch (Diplomandin (MAGIC))
\item Dipl.-Ing. Kai Warda (Elektronik)
\item PTA Matthias Domke (Systemadministration)
\end{itemize}

\noindent{\bf W"urzburg}:

\begin{itemize}
\item Prof. Dr. Karl Mannheim (Grundausttattung)
\item Prof. Dr. Wolfgang Dr"oge (Grundausttattung???)
\item Dipl.-Phys. nn (Grundausstattung)
\item Dipl.-Phys. nn (Fremdfinanziert)
\end{itemize}

\subsection{Zusammenarbeit mit anderen Wissenschaftlern\\Co-operation with other scientists}

{\em Nennung der Wissenschaftler mit denen eine konkrete(!) Zusammenarbeit oder Abstimmung besteht}

Both applying groups co-operate with the international MAGIC-Collaboration
and the institutes represented therein. (W"urzburg funded by the BMBF, Dortmund
by means of appointment for the moment.)\\
{\bf Dr.~Adrian Biland, Prof.~Dr.~Eckart Lorenz (both ETH Z"urich)}\\
{\bf Prof.~Riccardo Paoletti (Universitā di Siena and INFN sez. di Pisa, Italy)}\\

\noindent The group in Dortmund is involved in the IceCube experiment
(BMBF funding) and maintains close contacts to the collaboration
partners. Moreover on the field  of phenomenology there do exist good
working contacts to the groups of  Prof.~Dr.~Reinhard~Schlickeiser,
Ruhr-Universit"at Bochum and Prof.~Dr.~Peter~Biermann,  MPIfR Bonn.
There are furthermore contacts to Dr.~Anita Reimer, Stanford (USA) and 
Prof.~Dr.~Ray~Protheroe, Adelaide (Australien).\\ {\bf Francis Halzen,
evtl. John Quenby}\\

\noindent W"urzburg is involved in ... maintains contacts to ...\\
Prof.~Dr.~Wolfgang Dr\"oge\\

\subsection{Arbeiten im Ausland, Kooperation mit Partnern im Ausland\\Work outside Germany, Cooperation with foreign partners}

{\em 
\begin{itemize}
\item Wird das Vorhaben ganz oder teilw. im Ausland durchgef"uhrt
\item Findet konkrete Kooperation (Kolaboration!) statt (welche L"ander)
\item Art und Umfang der Zusammenhang darlegen (Name, Adresse, Stellung)
\end{itemize}
}

The work on DWARF will take place at the ORM on the Spanish island La
Palma. It will be performed in close collaboration with the
MAGIC-collaboration.

\subsection{Apparative Ausstattung/Scientific equipment available}

{\em 
\begin{itemize}
\item Am Ort vorhandene gr"o"sere Ger"ate
\end{itemize}
}


Both in Dortmund and in W"urzburg there are extensive computer
capacities available for data storing as well as for data analysis.

%Dortmund: Der Fachbereich Physik der Universit"at Dortmund verf"ugt "uber
%modern ausgestattete mechanische und elektronische Werkst"atten
%einschlie"slich einer Elektronik-Entwicklung. Der Lehrstuhlbereich
%Astroteilchenphysik verf"ugt "uber g"angige zur Erstellung moderner
%DAQ erforderliche apparative Ausstattung.\\
Dortmund: The Fachbereich Physik at the Universit"at Dortmund has
modern equipped mechanical and electrical workshops including a
department for development of electronics at its command. The
Lehrstuhlbereich Astroteilchenphysik possesses common technical
equipment required for constructing modern DAQ.

W"urzburg:...

\subsection{Laufende Mittel f"ur Sachausgaben\\The institution's general contribution}

{\em 
\begin{itemize}
\item Angaben "uber Instituts-/Drittmittel (trennen) die f"ur das Projekt(!) j"arhrlich zur Verf"ugung stehen
\end{itemize}
}

%Das gegenw"artige Budget des Lehrstuhls f"ur Astronomie der Universit"at
%W"urzburg betr"agt $\approx $ 12345 EURO pro Jahr.\\ 
%Das gegenw"artige Budget des Lehrstuhlbereiches Astroteilchnphysik der
%Universit"at Dortmund betr"agt $\approx $ 20000 EURO pro Jahr.
Current total institute budget from the Universit"at Dortmund $\approx$
20000 EURO per year.\\

Current total institute budget from the Universit"at W"urzburg
$\approx$ xxxxx EURO per year.\\

\newpage
\paragraph{5.6 Conflicts of interest in economic activities\\Interessenskonflikte bei wirtschaftlichen Aktivit"aten}~\\
none

\paragraph{5.7 Other requirements (Sonstige Voraussetzungen)}~\\
none

\paragraph{6 Declarations (Erkl"arungen)}

A request for funding this project has not been submitted to
any other addressee. In case we submit such a request we will inform
the Deutsche Forschungsgemeinschaft immediately. \\

The corresponding persons (Vertrauensdozenten) at the
Universit"at Dortmund (Prof. Dr. Gather) and at the Universit"at
W"urzburg (Prof. XXXXX) have been informed about the submission of this
proposal.

\paragraph{7 Signatures (Unterschriften)}~\\

\vspace{2.5 cm}

\hfill
\begin{minipage}[t]{6cm}
W"urzburg,\\[3.0cm]
\parbox[t]{6cm}{\hrulefill}\\
\parbox[t]{6cm}{~\hfill Prof.\ Dr.\ Karl Mannheim\hfill~}\\
\end{minipage}
\hfill
\begin{minipage}[t]{6cm}
Dortmund,\\[3.0cm]
\parbox[t]{6cm}{\hrulefill}\\
\parbox[t]{6cm}{~\hfill Prof.\ Dr.\ Dr.\ Wolfgang Rhode\hfill~}\\
\end{minipage}\hfill~

\newpage
\section[8]{Verzeichnis der Anlagen/List of appendages}

\begin{itemize}
\item
%Schriftenverzeichnis der Antragsteller seit dem Jahr 2000
List of refereed publications of the applicants since 2000
\item
CV of Karl Mannheim
\item
CV of Wolfgang Rhode
\end{itemize}

\newpage
%\section{References}

\newpage
%(Referenzen aus unseren Gruppen sind mit einem Stern gekennzeichnet *)
(References of our groups are marked by an asterix *)
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\end{document}
