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

\begin{document}

\maketitle

%\tableofcontents

\section[1]{General Information (Allgemeine Angaben)}

\subsection[1.1]{Applicants (Antragsteller)}
\germanTeX
\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 1963&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}
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\newpage

%\paragraph{1.2 Topic}~\\
\subsection[1.2]{Topic}
Long-term VHE $\gamma$-ray monitoring of bright blazars with a dedicated Cherenkov telescope

%\paragraph{1.2 Thema}~\\
\subsection[1.2]{Thema}
Langzeitbeobachtung von hellen VHE $\gamma$-Blazaren mit einem dedizierten Cherenkov Teleskop

%\paragraph{1.3 Discipline and field of work (Fachgebiet und Arbeitsrichtung)}~\\
\subsection[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)}~\\
\subsection[1.4]{Scheduled duration in total (Voraussichtliche Gesamtdauer)}
After successful completion of the three-year work plan developed in
this proposal, we will ask for an extension of the project for another
two years to carry out an observation program centered on the signatures
of supermassive binary black holes.

%\paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\
\subsection[1.5]{Application period (Antragszeitraum)}
3\,years. The work on the project will begin immediately after the
funding. 

\newpage
%\paragraph{\bf 1.6 Summary}~\\
\subsection[1.6]{Summary}
We propose to set up a robotic imaging air Cherenkov telescope with low
cost, but high performance design for remote operation. The goal is to
dedicate this gamma-ray telescope to long-term monitoring observations
of nearby, bright blazars at very high energies. We will (i) search for
orbital modulation of the blazar emission due to supermassive black
hole binaries, (ii) study the statistics of flares and their physical
origin, and (iii) correlate the data with corresponding data from the
neutrino observatory IceCube to search for evidence of hadronic
emission processes. The observations will also trigger follow-up
observations of flares with higher sensitivity telescopes such as
MAGIC, VERITAS, and H.E.S.S.\ Joint observations with the Whipple
monitoring telescope will start a future 24\,h-monitoring of selected
sources with a distributed network of robotic telescopes. The telescope
design is based on a full technological upgrade of one of the former
telescopes of the HEGRA collaboration (CT3) still located at the
Observatorio Roque de los Muchachos on the Canarian Island La Palma
(Spain). After this upgrade, the telescope will be operated
robotically, a much lower energy threshold below 350\,GeV will be
achieved and the observation time required for gaining the same signal
as with CT3 will be reduced by a factor of six.

\germanTeX
%\paragraph{\bf 1.6 Zusammenfassung}~\\
\subsection[1.6]{Zusammenfassung}
{\bf Unser Vorhaben besteht darin, ein robotisches Luft-Cherenkov-Teleskop
mit geringen Kosten aber hoher Leistung fernsteuerbar in Betrieb zu
nehmen. Das Ziel ist es, dieses gamma-ray Teleskop ganz der
Langzeitbeobachtung von nahen, hellen Blazaren bei sehr hohen Energien
zu widmen. Wir werden (i) nach Modulationen der Blazar-Emission durch
Bin"arsysteme von supermassiven Schwarzen L"ochern suchen, (ii) die
Statistik von gamma-Ausbr"uchen und deren physikalischen Ursprung
untersuchen und (iii) die Daten mit entsprechenden Daten von dem
Neutrino-Telskop IceCube korrelieren, um Nachweise f"ur hadronische
Emissionsprozesse zu finden. Die Beobachtungen werden zus"atzlich
Nachfolgebeobachtungen von gamma-Ausbr"uchen mit h"ohersensitiven
Teleskopen wie MAGIC, VERITAS und H.E.S.S.\ triggern. Auf einander
abgestimmte Beobachtungen zusammen mit dem Whipple Teleskop werden der
Auftakt zu einer zuk"unftigen 24-Stunden-Beobachtung von selektierten
Quellen mit einem verteilten Netzwerk robotischer Cherenkov-Teleskope
sein. Das Teleskop-Design basiert auf einem kompletten technologischen
Upgrade eines der Teleskope der fr"uheren HEGRA-Kollaboration, welches
noch immer am Observatorio Roque de los Muchachos auf der kanarischen
Insel La Palma (Spanien) gelegen ist. Nach diesem Upgrade wird das
Teleskop robotisch betrieben werden und eine wesentlich geringere
Energieschwelle von unter 350\,GeV aufweisen, w"ahrend gleichzeitig die
notwendige Beobachtungszeit, um dasselbe Signal wie CT3 zu erhalten, um
einen Faktor sechs verringert wird.}
\originalTeX
\newpage

\section[2]{Stand der Forschung, eigene Vorarbeiten\\(Science case, preliminary work by proposer)}

\subsection[2.1]{Science case (Stand der Forschung)}

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 astronomy detecting tens of formerly unknown gamma
ray sources and analyzing their energy spectra, morphology, 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. A diversity of astrophysical
source types such as pulsar wind nebulae, supernova remnants,
microquasars, pulsars, radio galaxies, clusters of galaxies, gamma ray
bursts and blazars have been studied with these telescopes.

The main class of extragalactic, very high energy gamma-rays sources
detected with imaging air-Cherenkov telescopes are blazars, i.e.\
accreting supermassive black holes exhibiting a relativistic jet that
is closely aligned with the line of sight. The non-thermal blazar
spectrum covers up to 20 orders of magnitude in energy, from
long-wavelength radio waves to multi-TeV gamma-rays. In addition,
blazars are characterized by rapid variability, high degrees of
polarization, and super-luminal motion of knots in their
high-resolution radio images. The observed behavior can readily be
explained assuming relativistic bulk motion and in situ particle
acceleration, e.g. at shock waves, leading to synchrotron
(radio-to-x-ray) and self-Compton (gamma-ray) emission \citep{Blandford}.
Additionally, inverse Compton scattering of external photons may play a
role in producing the observed gamma rays \citep{Dermer,Begelman}.
Variability may hold the key to understanding the details of the
emission processes and the source geometry, and the development of
time-dependent models is currently on the agenda of model builders
worldwide.

Although particle acceleration inevitably affects electrons and protons
(ions), the electrons are commonly believed to be responsible for
producing the observed emission owing to their lower mass and thus much
stronger energy losses (at the same energy). The relativistic protons,
which could either originate from the accretion flow or from entrained
ambient matter, will quickly dominate the momentum flow of the jet.
This {\em baryon pollution} has been suggested to solve the energy
transport problem in gamma ray bursts, and is probably present in
blazar jets as well, even if they originate as pair jets in a black
hole ergosphere \citep{Meszaros}. Protons and ions accelerated in the
jets of blazars can reach extremely high energies before energy losses
become important \citep{Mannheim:1993}. Escaping particles contribute
to the observed flux of ultrahigh energy cosmic rays in a major way.
Blazars and their unbeamed hosts, the radio galaxies, are thus the
prime candidates for origin of ultrahigh energy cosmic rays
\citep{Rachen}, and this can be investigated with the IceCube and AUGER
experiments. Recent results of the AUGER experiment show a significant
anisotropy of the highest energy cosmic rays and point at either nearby
AGN or sources with a similar spacial distribution as their origin
\citep{AUGER-AGN}.

In some flares, a large ratio of the gamma-ray to optical luminosity is
observed. This is difficult to reconcile with the primary leptonic
origin of the emission, since the accelerated electron pressure would
largely exceed the magnetic field pressure. For shock acceleration to
work efficiently, particles must be confined by the magnetic field for
a time longer than the cooling time. The problem vanishes in the
following model: Photo-hadronic interactions of accelerated protons and
synchrotron photons induce electromagnetic cascades, which in turn
produce secondary electrons causing high energy synchrotron
gamma-radiation. This demands much stronger magnetic fields in line
with magnetic confinement \citep{Mannheim:1995}. Short variability time
scales can result from dynamical changes of the emission zone, running
e.g. through an inhomogeneous environment.

The contemporaneous spectral energy distributions for hadronic and
leptonic models bear many similarities, but also marked differences,
such as multiple bumps which are possible even in a one-zone hadronic
model \citep{Mannheim:1999}. These properties allow conclusions
about the accelerated particles. Noteworthy, even for nearby blazars
the spectrum must be corrected for attenuation of the gamma rays due to
pair production in collisions with low-energy photons from the
extragalactic background radiation field \citep{Kneiske}.
Ultimately, the hadronic origin of the emission must be probed with
correlated gamma-ray and neutrino observations, since the pion decay
initiating the cascades involves a fixed ratio of electron-positron
pairs, gamma-rays, and neutrinos. A dedicated monitoring campaign
jointly with IceCube has the best chance for success. Pilot studies
done with MAGIC and IceCube indicate that the investigation of neutrino
event triggered gamma-ray observations are statistically
inconclusive \citep{Leier:2006}.

The variability time scale of blazars ranges from minutes to months,
generally showing the largest amplitudes and the shortest time scales
at the highest energies. Recently, a doubling time scale of two minutes
has been observed in a flare of Mrk\,501 with the MAGIC
telescope \citep{Albert:501}. A giant flare of PKS\,2155-304 discovered by
H.E.S.S.\ \citep{Aharonian:2007pks} has shown similarly short
doubling time scales and a flux of up to 16 times the flux of the Crab
Nebula. Indications for TeV flares without evidence for an accompanying
x-ray flare, coined orphan flares, have been observed, questioning the
synchrotron-self-Compton mechanism being responsible for the
gamma-rays. Model ramifications involving several emission components,
external seed photons, or hadronically induced emission may solve the
problem \citep{Blazejowski}. Certainly, the database for contemporaneous
multi-wavelength observations is still far from proving the
synchrotron-self-Compton model.

Generally, observations of flares are prompted by optical or x-ray
alerts, leading to a strong selection bias. The variability presumably
reflects the non-steady feeding of the jets and the changing interplay
between particle acceleration and cooling. In this situation,
perturbations of the electron density or the bulk plasma velocity are
traveling down the jet. The variability could also reflect the changing
conditions of the external medium to which the jet flow adapts during
its passage through it. In fact, a clumpy, highly inhomogeneous
external medium is typical for active galactic nuclei, as indicated by
their clumpy emission line regions, if visible against the
Doppler-enhanced blazar emission. Often the jets bend with a large
angle indicating shocks resulting from reflections off intervening
high-density clouds. Changes in the direction of the jet flow lead to
large flux variations due to differential Doppler boosting.

Helical trajectories, as seen in high-resolution radio maps resulting
from the orbital modulation of the jet base in supermassive black hole
binaries, would lead to periodic variability on time scales of months
to years \citep{Rieger:2007}. Binaries are expected to be the most
common outcome of the repeated mergers of galaxies which have
originally built up the blazar host galaxy. Each progenitor galaxy
brings its own supermassive black hole as expected from the
Magorrian-Kormendy relations. It is subject to stellar dynamical
evolution in the core of the merger galaxy, of which only one pair of
black holes is expected to survive near the center of gravity.
Supermassive black hole binaries close to coalescence are thus expected
to be generic in blazars. Angular momentum transport by collective
stellar dynamical processes is efficient to bring them to distances
close to where the emission of gravitational waves begins to dominate
their further evolution until coalescence. Their expected gravitational
wave luminosity is spectacularly high, even long before final
coalescence and the frequencies are favorable for the detectors under
consideration (LISA). Detection of gravitational waves relies on exact
templates to filter out the signals and the templates can be computed
from astrophysical constraints on the orbits and masses of the black
holes. TeV gamma-rays, showing the shortest variability time scales,
probe deepest into the jet and are thus the most sensitive probe of the
orbital modulation at the jet base. Relativistic aberration is helpful
in bringing down the observed periods to below the time scale of years.
A tentative hint for a 23-day periodicity of the TeV emission from
Mrk\,501 during a phase of high activity in 1997 was reported by
HEGRA \citep{Kranich}, and was later confirmed including x-ray and
Teleacope Array data \citep{Osone}. The observations can be explained in
a supermassive black hole binary scenario \citep{Rieger:2000}.
Indications for helical trajectories and periodic modulation of optical
and radio lightcurves on time scales of tens of years have also been
described in the literature (e.g. \cite{Hong,Merrit}).

To overcome the limitations of biased sampling, a complete monitoring
database for a few representative bright sources needs to be obtained.
Space missions with all-sky observations at lower photon energies, such
as GLAST, GRIPS, or eROSITA, will provide significant multi-wavelength
exposure simultaneous to the VHE observations, and this is a new
qualitative step for blazar research. For the same reasons, the VERITAS
Collaboration keeps the former Whipple telescope alive, albeit its
performance seems to have strongly degraded. It is obvious that the
large Cherenkov telescopes such as MAGIC, H.E.S.S.\ or VERITAS are mainly
used to discover new sources at the sensitivity limit. Thus they will
not perform monitoring observations of bright sources with complete
sampling during their visibility. However, these telescopes will be
triggered by monitoring telescopes and thus improve the described
investigations. In turn, operating a smaller but robotic telescope is
an essential and cost-effective contribution to the plans for
next-generation instruments in ground-based gamma-ray astronomy.
Know-how for the operation of future networks of robotic Cherenkov
telescopes, e.g. a monitoring array around the globe or a single-place
array like CTA, is certainly needed given the high operating shift
demands of the current installations.

In summary, 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). Its robotic design will keep
the demands on personal and infrastructure on the low side, rendering
it compatible with the resources of University groups. The approach is
also optimal to educate students in the strongly expanding field of
astroparticle physics.

Assuming conservatively the performance of a single HEGRA-type
telescope, long-term monitoring of at least the following known blazars
is possible: Mrk\,421, Mrk\,501, 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. Utilizing recent developments, such
as improvements of the light collection efficiency due to an improved
mirror reflectivity and a better PM quantum efficiency, a 30\%
improvement in sensitivity and a lower energy-threshold is reasonable.
Current studies show that with a good timing resolution (2\,GHz) a
further 40\% increase in sensitivity (compared to a 300\,MHz system) is
feasible. Together with an extended mirror area and a large camera, a
sensitivity improvement compared to a single HEGRA telescope of a
factor of 2.5 and an energy threshold below 350\,GeV is possible.

\subsection[2.2]{Preliminary work by proposers (Eigene Vorarbeiten)}

From the experience with the construction, operation and data analysis
of Amanda, IceCube, HEGRA and MAGIC the proposing groups contribute the
necessary knowledge and experience to build and operate a small imaging
air Cherenkov telescope.

\paragraph{Hardware}

The Dortmund group is working on experimental and phenomenological
astroparticle physics. In the past, the following hardware components
were successfully developed: a Flash-ADC based DAQ (TWR, transient
waveform recorder), currently in operation for data acquisition in the
AMANDA subdetector within the IceCube telescope \citep{Wagner:PhD}, an
online software Trigger for the TWR-DAQ system \citep{Messarius:PhD},
online data compression mechanisms (TWR DAQ) \citep{Refflinghaus:Dipl},
monitoring software for the TWR-DAQ-data \citep{Dreyer:Dipl} and
in-ice-HV-power-supply for IceCube. This development was done with the
companies CAEN, Pisa, Italy and Iseg, Rossendorf, Germany. The HV
modules were long time tested under different temperature conditions
connected to operating photomultipliers \citep{Bartelt:Dipl}. Prototypes
for the scintillator counters of the planned Air Shower Array {\em
SkyView} were developed and operated for two years \citep{Deeg:Dipl}.
Members of the group (engineers) were involved in the fast trigger
development for H1 and are involved in the FPGA-programming for the
LHCb data read out. The group may further use the well equipped
mechanical and electronic workshops in Dortmund and the electronic
development departure of the faculty.

The ultra fast drive system of the MAGIC telscopes, suitable for fast
repositioning in case of Gamma-Ray Bursts, has been developed,
commissioned and programmed by the W\"{u}rzburg group
\citep{Bretz:2003drive,Bretz:2005drive}. To correct for axis
misalignments and possible deformations of the structure (e.g.\ bending
of camera holding masts), a pointing correction algorithm was developed
\citep{Dorner:Diploma}. Its calibration is done by measurement of the
reflection of bright guide stars on the camera surface and ensures a
pointing accuracy well below the pixel diameter. Hardware and software
(CCD readout, image processing and pointing correction algorithms) have
also been developed and are in operation successfully since more than
three years \citep{Riegel:2005icrc2}.

Mirror structures made of plastic material have been developed as
Winston Cones for balloon flight experiments previously by the group of
Wolfgang Dr\"{o}ge. W\"{u}rzburg has also participated in the development of
a HPD test bench, which has been setup in Munich and W\"{u}rzburg. With
this setup, HPDs for future improvement of the sensitivity of the MAGIC
camera are investigated.

\paragraph{Software}

The W\"{u}rzburg group has developed a full MAGIC analysis package,
flexible and modular enough to easily process DWARF data
\citep{Bretz:2005paris,Riegel:2005icrc,Bretz:2005mars}. A method for
absolute light calibration of the PMs based on Muon images has been
adapted and further improved for the MAGIC telescope
\citep{Meyer:Diploma,Goebel:2005}. Both, data analysis and Monte Carlo
production, have been fully automatized, such that both can run with
sparse user interaction \citep{Dorner:2005icrc}. The analysis was
developed to be powerful and as robust as possible to be best suited
for automatic processing \citep{Dorner:2005paris}. Experience with
large amount of data (up to 15\,TB/month) has been gained over five
years now. The datacenter is equipped with a professional multi-stage
(hierarchical) storage system. Two operators are paid by the physics
faculty. Currently efforts in W\"{u}rzburg and Dortmund are ongoing to
turn the old inflexible Monte Carlo programs, used by the MAGIC
collaboration, into modular packages which allows easy simulation of
other setups. Experience with Monte Carlo simulations, especially
CORSIKA, is contributed by the Dortmund group, which has actively
implemented changes into the CORSIKA program, such as an extension to
large zenith angles, prompt meson production and a new atmospheric
model \citep{Haffke:Dipl,Schroeder:PhD} for the local atmosphere of La
Palma. Furthermore the group has developed high precision Monte Carlos
for Lepton propagation in different media \citep{hepph0407075}. An
energy unfolding method and program has been adapted for IceCube and
MAGIC data analysis \citep{Curtef:CM,Muenich:ICRC}.

\paragraph{Phenomenology}

Both groups further have experience with source models and theoretical
computations of gamma ray and neutrino spectra expected from blazars.
The relation between the two messengers is a prime focus of interest.
Experience with corresponding multi-messenger data analyses involving
MAGIC and IceCube data is available in the Dortmund group. Research
activities are also related with relativistic particle acceleration
\citep{Meli} and gamma ray attenuation \citep{Kneiske}. The W\"{u}rzburg
group has organized and carried out multi-wavelength observations of
bright blazars involving MAGIC, Suzaku, the IRAM telescopes, and the
optical KVA telescope \citep{Ruegamer}. Signatures of supermassive
black hole binaries, which are most relevant also for gravitational
wave detectors, are investigated jointly with the German LISA
consortium (Burkart, Elbracht ongoing research, funded by DLR).
Secondary gamma rays due to dark matter annihilation events are
investigated both from their particle physics and astrophysics aspects.
Another main focus of research is on models of radiation and particle
acceleration processes in blazar jets (hadronic and leptonic models),
leading to predictions of correlated neutrino emission \citep{Rueger}.
This includes simulations of particle acceleration due to the Weibel
instability \citep{Burkart}. Much of this research at W\"{u}rzburg is
carried out in the context of the research training school GRK\,1147
{\em Theoretical Astrophysics and Particle Physics}.

\section[3]{Goals and Work Schedule (Ziele und Arbeitsprogramm)}

\subsection[3.1]{Goals (Ziele)}

The aim of the project is to put the former CT3 of the HEGRA
collaboration on the Roque de los Muchachos back into operation - with
an enlarged mirror surface, a new camera with higher quantum
efficiency, and new fast data acquisition system, under the name of
DWARF. The energy threshold will be lowered, and  the sensitivity of
DWARF will be greatly improved compared to HEGRA CT3 (see 
figure~\ref{sensitivity}). Commissioning and the first year of data taking
should be carried out within the three years of the requested funding
period.

\begin{figure}[ht]
\begin{center}
 \includegraphics*[width=0.495\textwidth,angle=0,clip]{CT3.eps}
 \includegraphics*[width=0.495\textwidth,angle=0,clip]{DWARF.eps}
 \caption{Left: The old HEGRA CT3 telescope as operated within the
 HEGRA Sytem. Right: A photomontage how the revised CT3 telescope
 could look like with more and hexagonal mirrors.}
\label{CT3}
\label{DWARF}
\end{center}
\end{figure}

The telescope will be operated robotically to reduce costs and man
power demands.  Furthermore, we seek to obtain know-how for the
operation of future networks of robotic 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, 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\"{u}rzburg group for MAGIC is modular and flexible, and can thus be
used with minor changes for the DWARF project. 

\begin{figure}[htb]
\begin{center}
 \includegraphics*[width=0.7\textwidth,angle=0,clip]{visibility.eps}
 \caption{Source visibility in hours per night versus month of the year
 for a maximum observation zenith angle of 65$^\circ$.
 Shown are all sources which we want to monitor including the CrabNebula
 necessary for calibration and quality assurance. }
\label{visibility}
\end{center}
\end{figure}

The scientific focus of the project will be on the long-term monitoring
of bright, nearby VHE emitting blazars.  At least one of the proposed
targets will be visible any time of the year (see figure~\ref{visibility}). For
calibration purposes, some time will be scheduled for observations of
the Crab nebula.  The blazar observations will allow 
\begin{itemize}
\item to determine the duty cycle, the baseline emission, and the power
spectrum of flux variations.
\item to cooperate with the Whipple monitoring telescope for an
extended time coverage.
\item to prompt Target-of-Opportunity (ToO) observations with MAGIC in
the case of flares increasing time resolution. Corresponding
ToO proposals to H.E.S.S.\ and Veritas are in
preparation.
\item to observe simultaneously with MAGIC which will provide an
extended bandwidth from below 100\,GeV to multi-TeV energies.
\item to obtain multi-frequency observations together with the
Mets\"{a}hovi Radio Observatory and the optical Tuorla Observatory. The
measurements will be correlated with INTEGRAL and GLAST results, when
available. x-ray monitoring using the SWIFT and Suzaku facilities will
be proposed.
\end{itemize}

Interpretation of the data will yield crucial information about
\begin{itemize}
\item the nature of the emission processes going on in relativistic
jets. We plan to interpret the data with models currently developed in
the context of the Research Training Group {\em Theoretical
Astrophysics} in W\"{u}rzburg (Graduiertenkolleg, GK\,1147), including 
particle-in-cell and hybrid MHD models.
\item the black hole mass and accretion rate fitting the data with
emission models.  Results will be compared with estimates of the black
hole mass from  the Magorrian relation.
\item the flux of relativistic protons (ions) by correlating the rate
of neutrinos detected with the neutrino telescope IceCube and the rate
of gamma ray photons detected with DWARF, and thus the rate of escaping
cosmic rays.
\item the orbital modulation owing to a supermassive binary black hole.
Constraints on the binary system will allow to compute most accurate
templates of gravitational waves, which is a connected project at
W\"{u}rzburg in the German LISA consortium funded by DLR.
\end{itemize}

\subsection[3.2]{Work schedule (Arbeitsprogramm)}

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

The work schedule assumes that the work will begin in January 2008,
immediately after funding. Later funding would accordingly shift the
schedule. Each year is divided into quarters (see figure~\ref{schedule}).

\begin{figure}[htb]
\begin{center}
 \includegraphics*[angle=0,clip]{schedule.eps}
% \caption{Left: The old HEGRA CT3 telescope as operated within the
% HEGRA Sytem. Right: A photomontage how the revised CT3 telescope
% could look like with more and hexagonal mirrors.}
\label{schedule}
%\label{DWARF}
\end{center}
\end{figure}

\paragraph{Software}
\begin{itemize}
\item MC adaption (Do/W\"{u}): Due to the large similarities with the MAGIC telescope, within half a year new Monte Carlo code can be programmed using parts of the existing MAGIC Monte Carlo code. For tests and cross-checks another period of six months is necessary.
\item Analysis adaption (W\"{u}): The modular concept of the Magic Analysis and Reconstruction Software (MARS) allows a very fast adaption of the telescope setup, camera and data acquisition properties within half a year.
\item Adaption Drive software (W\"{u}): Since the new drive electronics will be based on the design of the MAGIC II drive system the control software can be reused unchanged. The integration into the new slow control system will take about half a year. It has to be finished at the time of arrival of the drive system components in 2009/1.
\item Slow control/DAQ (Do): A new data acquisition and slow control system for camera and auxiliary systems has to be developed. Based on experiences with the AMANDA DAQ, the Domino DAQ developed for MAGIC II will be adapted and the slow control integrated within three quarters of a year. Commissioning will take place with the full system in 2009/3.
\end{itemize}

\paragraph{Mirrors (W\"{u})} First prototypes for the mirrors are already available. After testing (six months), the production will start in summer 2008 and shipment will be finished before the full system assembly 2009/2.
\paragraph{Drive (W\"{u})} After a planning phase of half a year to simplify the MAGIC II drive system for a smaller telescope (together with the delivering company), ordering, production and shipment should be finished in 2009/1. The MAGIC I and II drive systems have been planned and implemented successfully by the Wuerzburg group.
\paragraph{Auxiliary (W\"{u})} Before the final setup in 2009/1, all auxiliary systems (weather station, computers, etc.) will have been specified, ordered and shipped.
\paragraph{Camera (Do)} The camera has to be ready six month after the shipment of the other mechanical parts of the telescope. For this purpose camera tests have to take place in 2009/2, which requires the assembly of the camera within six months before. By now, a PM test bench which allows to finish planning and ordering of the camera parts and PMs until summer 2008, before the construction begins, is set up in Dortmund. In addition to the manpower permanently provided by Dortmund for production and commissioning, two engineers will participate in the construction phase.
\paragraph{Full System (Do/W\"{u})} The full system will be assembled after delivering of all parts in the beginning of spring 2009. Start of the commissioning is planned four months later. First light is expected in autumn 2009. This would allow an immediate full system test with a well measured, strong and steady source (CrabNebula). After the commissioning phase will have been finished in spring 2010, full robotic operation will be provided.

Based on the experience with setting up the MAGIC telescope we estimate
this workschedule as conservative.

\subsection[3.3]{Experiments with humans (Untersuchungen am Menschen)}
none
\subsection[3.4]{Experiments with animals (Tierversuche)}
none
\subsection[3.5]{Experiments with recombinant DNA (Gentechnologische Experimente)}
none

\clearpage

\section[4]{Funds requested (Beantragte Mittel)}

We request funding for a total of three years. Summarizing, the
expenses for the telescope are dominated by the camera and data
acquisition. 
%The financial volume for the complete hardware inclusive
%transport amounts to {\bf 372.985,-\,\euro}.

\subsection[4.1]{Required Staff (Personalkosten)}

For this period, we request funding for two postdocs and two PhD
students, one in Dortmund and one in W\"{u}rzburg each. The staff
members shall fulfill the tasks given in the work schedule above. To
cover these tasks completely, one additional PhD and a various number
of Diploma students will complete the working group.

Suitable candidates interested in these positions are Dr.\ Thomas
Bretz, Dr.\ dest.\ Daniela Dorner, Dr.\ dest.\ Kirsten M\"{u}nich,
cand.\ phys.\ Michael Backes, cand.\ phys.\ Daniela Hadasch and cand.\
phys.\ Dominik Neise. 

\subsection[4.2]{Scientific equipment (Wissenschaftliche Ger\"{a}te)}

At the Observatorio Roque 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 DWARF as an auxiliary instrument (see appendix). Also
emergency support from the shift crew is guaranteed, although
autonomous robotic operation is the primary goal.

To achieve the planned sensitivity and threshold
(figure~\ref{sensitivity}) the following components have to be bought.
To obtain reliable results as fast as possible well known components
have been chosen.
\begin{figure}[hb]
\centering{
\includegraphics[width=0.605\textwidth]{sensitivity.eps}
\caption{Integral flux sensitivity of several telescopes
\citep{Juan:2000,MAGICsensi,Vassiliev:1999} 
and the expectation for DWARF, with both a PMT- and a
GAPD-camera. It is based on the sensitivity of
HEGRA~CT1, scaled by the improvements mentioned in the text.
} \label{sensitivity} } 
\end{figure}
\clearpage
{\bf Camera}\dotfill 207.550,-\,\euro\\[-3ex]
\begin{quote}
   To setup a camera with 313 pixels the following components are needed:\\
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Photomultiplier Tube EMI\,9083B\hfill 220,-\,\euro\\
   Active voltage divider ({\bf !!!!})\hfill 80,-\,\euro\\
   High voltage support and control\hfill {\bf 300,-}\,\euro\\
   Preamplifier\hfill 50,-\,\euro\\
   Spare parts (overall)\hfill 3000,-\,\euro\\
   \end{minipage}\\[-0.5ex]
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
For long-term observations, the stability of the camera is a major
criterion. To keep the systematic errors small, a 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 $\sqrt{2}$,
because spending observation time for dedicated background observations
becomes obsolete, i.e.\ observation time for the source is doubled. This
ensures in addition a better time coverage of the observed sources.

A further increase in sensitivity can be achieved by better background
statistics from not only one but several independent positions for the
background estimation in the camera \citep{Lessard:2001}. For wobble mode
observations allowing for this, the source position should be shifted
$0.6^\circ-0.7^\circ$ out of the camera center. 
%}

A camera completely containing shower images of events in the energy
region of 1\,TeV-10\,TeV should have a diameter in the order of
5$^\circ$. To decrease the dependence of the measurements on the camera
geometry, a camera layout as symmetric as possible will be chosen.
Consequently a camera allowing to fulfill these requirements should be
round and have a diameter of $4.5^\circ-5.0^\circ$.
\begin{figure}[th]
\begin{center}
 \includegraphics*[width=0.495\textwidth,angle=0,clip]{cam271.eps}
 \includegraphics*[width=0.495\textwidth,angle=0,clip]{cam313.eps}
 \caption{Left: Schematic picture of the 271 pixel CT-3 camera with a field of view of 4.6$^\circ$.
 Right: Schematic picture of the 313 pixel camera for DWARF with a field of view of 5$^\circ$.}
\label{camCT3}
\label{camDWARF}
\end{center}
\end{figure}

Therefor a camera with 313 pixel camera (see figure~\ref{camDWARF}) is
chosen. The camera will be built based on the experience with HEGRA and
MAGIC. 19\,mm diameter Photomultiplier Tubes (PM, EMI\,9083\,KFLA-UD)
will be bought, similar to the HEGRA type (EMI\,9083\,KFLA). They have
a 25\% improved quantum efficiency (see figure~\ref{qe}) and 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
650,-\,\euro.

All possibilities of borrowing one of the old HEGRA cameras for a
transition time have been probed and refused by the owners of the
cameras.

{\bf At ETH~Z\"{u}rich currently test measurements are ongoing to prove the
ability, i.e.\ stability, aging, quantum efficiency, etc., of using
Geiger-mode APDs (GAPD) as photon
detector in the camera of a Cherenkov telescope. The advantages are
extremely high quantum efficiency ($>$50\%), easier gain stabilization and
simplified application compared to classical PMs. If these test
measurements are successfully finished until 8/2008 we consider to use
GAPDs in favor of classical PMs. The design of such a camera would take
place at University Dortmund in close collaboration with the experts
from ETH. Construction would also take place at the electronics
workshop of Dortmund.}

\end{quote}\vspace{3ex}

{\bf Camera support}\dotfill 204.000,-\,\euro\\[-3ex]
\begin{quote}
For this setup the camera holding has to be redesigned. (1500,-\,\euro)
The camera chassis must be water tight and will be equipped with an
automatic lid protecting the PMs at day-time. For further protection, a
plexi-glass window will be installed in front of the camera. By coating
this window with an anti-reflex layer of magnesium-fluoride, a gain in
transmission of {\bf 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\ for all winston cones). The
current design will be improved by using a high reflectivity aluminized
Mylar mirror-foil, coated with a dialectical layer ($Si\,O_2$
alternated with Niobium Oxide), to reach a reflectivity in the order of
98\%. An electric and optical shielding of the individual PMs is
planned.

In total a gain of {\bf $\sim$15\%} in light-collection
efficiency compared to the old CT3 system can be acheived.
\end{quote}\vspace{3ex}

{\bf Data acquisition}\dotfill 61.035,-\,\euro\\[-3ex]
\begin{quote}
313 pixels a\\
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Readout\hfill 95,-\,\euro\\
   Trigger\hfill 100,-\,\euro\\
   \end{minipage}\\[-0.5ex]
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
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 \citep{Barcelo}. This technology allows to sample
the pulses with high frequencies and readout several channels with a
single Flash-ADC resulting in low costs. The low power consumption will
allow to include the digitization near the signal source which makes
the transfer of the analog signal obsolete. The advantage is less
pick-up noise and less signal dispersion. By high sampling rates
(1.2\,GHz), additional information about the pulse shape can be
obtained. This increases 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.

%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
Current results obtained with the new 2\,GHz FADC system in the MAGIC
data acquisition show that for a single telescope a sensitivity
improvement of 40\% with a fast FADC system is achievable \citep{Tescaro:2007}.

As for the HEGRA telescopes a simple multiplicity trigger is
sufficient, but also a simple neighbor-logic could be programmed (both
cases $\sim$100,-\,\euro/channel).

Additional data reduction and preprocessing within the readout chain is
provided. Assuming conservatively a readout rate of 30\,Hz the storage
space needed will be less than 250\,GB/month or 3\,TB/year. This amount
of data can easily be stored and processed by the W\"{u}rzburg
Datacenter (current capacity $>$80\,TB, $>$40\,CPUs). 
\end{quote}\vspace{3ex}

{\bf Mirrors}\dotfill 15.000,-\,\euro\\[-3ex]
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
\begin{quote}
The existing mirrors are replaced by new plastic mirrors which are
currently developed by Wolfgang Dr\"{o}ge's group. The cheap and
light-weight material has been formerly used for Winston cones in
balloon experiments. The mirrors are copied from a master coated with a
reflecting and a protective material. 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 instead of a round one. A further
increase of the mirror area would require a reconstruction of parts of
the mount and will therefore be considered only in a later phase of the
experiment.

If the current development of the plastic mirrors 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. 

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. By this, a gain in reflectivity of $\sim10\%$ is
achieved, see figure~\ref{reflectivity} \citep{Fraunhofer}.

Both solutions would require the same expenses.

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\"{u}rich and successfully
operated on the MAGIC telescope, is intended.
\begin{figure}[p]
\centering{
\includegraphics[width=0.57\textwidth]{cherenkov.eps}
\includegraphics[width=0.57\textwidth]{reflectivity.eps}
\includegraphics[width=0.57\textwidth]{qe.eps}
\caption{Top to bottom: The cherenkov spectrum as observed by a
telescope located at 2000\,m above sea level. The mirror's reflectivity
of a 300\,nm thick aluminum layer with a protection layer of 10\,nm and
100\,nm thickness respectively. For comparison the reflectivity of
HEGRA CT1's mirrors \citep{Kestel:2000} are shown. The bottom plot depicts
the quantum efficiency of the prefered PMs (EMI) together with the
predecessor used in CT1. A proper coating \citep{Paneque:2004} will
further enhance its effciency. An even better increase would be the
usage of Geiger-mode APDs.}

\label{cherenkov}
\label{reflectivity}
\label{qe}
}
\end{figure}

%<grey>The system
%will be provided by ETH Z"urich.</grey>

%{\bf For a diameter mirror of less than 2.4\,m, the delay between an
%parabolic (isochronus) and a spherical mirror shape at the edge is well
%below 1ns (see figure). Thus for a sampling rate of 1.2\,GHz parabolic
%individual mirrors are not needed. Due to their small size the
%individual mirrors can have a spherical shape.}
%}\\[2ex]
\end{quote}\vspace{3ex}

{\bf Calibration System}\dotfill 6.650,-\,\euro+IPR?\\[-3ex]
\begin{quote}
Components\\
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Absolute light calibration\hfill 2.000,-\,\euro\\
   Individual pixel rate control\hfill ???,-\,\euro\\
   Weather station\hfill 500,-\,\euro\\
   GPS clock\hfill 1.500,-\,\euro\\
   CCD cameras with readout\hfill 2.650,-\,\euro\\
   \end{minipage}\\[-0.5ex]
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
For the absolute light calibration (gain-calibration) of the PMs a
calibration box as successfully used in the MAGIC telescope will be
produced.

To ensure a homogeneous acceptance of the camera, essential for
wobble-mode observations, the trigger rate of the individual pixels
will be measured and controlled.

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 measurements 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 for
MAGIC\ I and~II, ({\bf 300,-\,\euro\ camera, 600,-\,\euro\ optics,
300,-\,\euro\ housing, 250,-\,\euro\ Frame grabber}) will be installed.

A second identical CCD camera for online monitoring (starguider) will
be bought.

A GPS clock is necessary for an accurate tracking. The weather station
helps judging the data quality.
%}\\[2ex]
\end{quote}\vspace{3ex}


{\bf Computing}\dotfill 12.000,-\,\euro\\[-3ex]
\begin{quote}
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   On-site\hfill 12.000,-\,\euro\\
   Three PCs\hfill 8.000,-\,\euro\\
   SATA RAID 3TB\hfill 4.000,-\,\euro\\
   \end{minipage}\\[-0.5ex]
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
For on-site computing three standard PCs are needed ($\sim$8.000,-\,\euro).
This includes readout and storage, preprocessing and telescope control.
For safety reasons, a firewall is mandatory. For local cache-storage
and backup, two RAID\,5 SATA disk arrays with one Terabyte capacity
each will fulfill the requirement ($\sim$4.000,-\,\euro). The data will be
transmitted as soon as possible after data taking via Internet to the
W\"{u}rzburg Datacenter. Enough storage capacity and computing power
is available there and already reserved for this purpose.

Monte Carlo production and storage will take place at University
Dortmund.%}\\[2ex]
\end{quote}\vspace{3ex}

{\bf Mount and Drive}\dotfill 17.500,-\,\euro\\[-3ex]
\begin{quote}
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
The present mount is used. Only a smaller investment for safety,
corrosion protection, cable ducts, etc. is needed (7.500,-\,\euro). 

For the movement, motors, shaft encoders and control electronics in the
order of 10.000,-\,\euro\ have to be bought. The costs have been estimated
with the experience from building the MAGIC drive systems. The DWARF
drive system should allow for relatively fast repositioning for three
reasons: (i)~Fast movement might be mandatory for future ToO
observations. (ii)~Wobble-mode observations will be done changing the
wobble-position continuously (each 20\,min) for symmetry reasons. (iii)~To
ensure good time coverage of more than one source visible at the same
time, the observed source will be changed in constant time intervals
($\sim$20\,min). 

Therefore three 150\,Watt servo motors are intended to be bought. A
micro-controller based motion control unit (Siemens SPS L\,20) 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 will be setup.
%}\\[2ex]
\end{quote}\vspace{3ex}

{\bf Security}\dotfill 4.000,-\,\euro\\[-3ex]
\begin{quote}
   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
   Uninterruptable power-supply (UPS)\hfill 2.000,-\,\euro\\
   Security fence\hfill 2.000,-\,\euro\\
   \end{minipage}\\[-0.5ex]
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
A UPS with 5\,kW-10\,kW will be
installed to protect the equipment against power cuts and ensure a safe
telescope position at the time of sunrise.

A fence for protection in case of robotic movement will be
installed.%}\\[2ex]
\end{quote}\vspace{3ex}

{\bf Other expenses}\dotfill 7.500,-\,\euro\\[-3ex]
\begin{quote}
%\parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
%   Robotics\hfill 7.500,-\,\euro\\
%   \end{minipage}\\[-0.5ex]
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
For remote, robotic operation a variety of remote controllable electronic
components such as ethernet controlled sockets and switches will be
bought. Monitoring equipment, for example different kind of sensors, is
also mandatory.%}\\[2ex]
\end{quote}
\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.2:\hfill{\bf
342.235,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
\hspace*{0.66\textwidth}\hrulefill\\

\subsection[4.3]{Consumables (Verbrauchsmaterial)}

\begin{quote}
%   \parbox[t]{1em}{~}\begin{minipage}[t]{0.9\textwidth}
   10 LTO\,4 tapes (8\,TB)\dotfill 750,-\,\euro\\
   Consumables (overalls) tools and materials\dotfill 10.000,-\,\euro
%   \end{minipage}\\[-0.5ex]
\end{quote}

\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.3:\hfill{\bf
10.750,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
\hspace*{0.66\textwidth}\hrulefill\\

\subsection[4.4]{Reisen (Travel expenses)}
The large amount of travel funding is required due to the very close
cooperation between Dortmund and W\"{u}rzburg and the work demands on
the construction site.\\[-2ex]

\begin{quote}
%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
Per year one senior group member from Dortmund and W\"{u}rzburg should
present the status of the work in progress at an international workshop
or conference:\\
2 x 3\,years x 1.500,-\,\euro\dotfill 9.000,-\,\euro\\[-2ex]

One participation at the biannual MAGIC collaboration meeting:\\
2 x 3\,years x 1.000,-\,\euro\dotfill 6.000,-\,\euro\\[-2ex]

PhD student exchange between W\"{u}rzburg and Dortmund:\\
1\,student x 1\,week x 24 (every six weeks) x 800,-\,\euro\dotfill
19.200,-\,\euro\\[-2ex]

For setup of the telescope at La Palma the following travel expenses
are necessary:\\
4 x 2\,weeks at La Palma x 2\,persons x 1.800,-\,\euro\dotfill
28.800,-\,\euro
%}
\end{quote}

\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.4:\hfill{\bf
72.200,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
\hspace*{0.66\textwidth}\hrulefill\\


\subsection[4.5]{Publikationskosten (Publication costs)}
Will be covered by the proposing institutes.


\subsection[4.6]{Other costs (Sonstige Kosten)}
\begin{quote}
Storage container (for shipment of the mirrors)\dotfill 5.000,-\,\euro\\
Transport\dotfill 15.000,-\,\euro\\
Dismantling (will be covered by proposing institutes)\dotfill n/a
\end{quote}

\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.6:\hfill{\bf
20.000,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
\hspace*{0.66\textwidth}\hrulefill\\

\newpage
\germanTeX
\section[5]{Preconditions for carrying out the project\\(Voraussetzungen f"ur die Durchf"uhrung des Vorhabens)}
none

\subsection[5.1]{The research team (Zusammensetzung der Arbeitsgruppe)}

\paragraph{Dortmund}
\begin{itemize}
\setlength{\itemsep}{0pt}
\setlength{\parsep}{0pt}
\item Prof.\ Dr.\ Dr.\ Wolfgang Rhode (Grundausttattung)
\item Dr.\ Tanja Kneiske (Postdoc (Ph"anomenologie), DFG-Forschungsstipendium)
\item Dr.\ Julia Becker (Postdoc (Ph"anomenologie), Drittmittel)
\item Dipl.-Phys.\ Kirsten M"unich (Doktorand (IceCube), Drittmittel)
\item Dipl.-Phys.\ Jens Dreyer (Doktorand (IceCube), Grundausttattung)
\item M.Sc.\ Valentin Curtef (Doktorand (MAGIC), Grundausstattung)
\item cand.\ phys.\ Michael Backes (Diplomand (MAGIC), zum F"orderbeginn diplomiert)
\item cand.\ phys.\ Daniela Hadasch (Diplomand (MAGIC))
\item cand.\ phys.\ Anne Wiedemann (Diplomand (IceCube))
\item cand.\ phys.\ Dominik Neise (Diplomand (MAGIC))
\item Dipl.-Ing.\ Kai Warda (Elektronik)
\item PTA Matthias Domke (Systemadministration) 
\end{itemize}

\paragraph{W\"{u}rzburg}
\begin{itemize}
\setlength{\itemsep}{0pt}
\setlength{\parsep}{0pt}
\item Prof.\ Dr.\ Karl Mannheim (Landesmittel)
\item Prof.\ Dr.\ Thomas Trefzger (Landesmittel)
\item Prof.\ Dr.\ Wolfgang Dr"oge (Landesmittel)
\item Dr.\ Thomas Bretz (Postdoc (MAGIC), BMBF)
\item Dr.\ Felix Spanier (Postdoc, Landesmittel)
\item Dipl.-Phys.\ Jordi Albert (Doktorand, DFG-GRK1147)
\item Dipl.-Phys.\ Karsten Berger (Doktorand (MAGIC), Landesmittel)
\item Dipl.-Phys.\ Thomas Burkart (Doktorand (LISA), DLR)
\item Dipl.-Phys.\ Oliver Elbracht (Doktorand, Elitenetzwerk Bayern)
\item Dipl.-Phys.\ Dominik Els"asser (Doktorand, Elitenetzwerk Bayern)
\item Dipl.-Phys.\ Daniela Dorner (Doktorand (MAGIC), BMBF)
\item Dipl.-Phys.\ Daniel H"ohne (Doktorand (MAGIC), Landesmittel)
\item Dipl.-Phys.\ Markus Meyer (Doktorand, DFG-GRK1147)
\item M.Sc.\ Surajit Paul (Doktorand, DFG-GRK1147)
\item Dipl.-Phys.\ Stefan R"ugamer (Doktorand (MAGIC), Landesmittel)
\item Dipl.-Phys.\ Michael R"uger (Doktorand, Elitenetzwerk Bayern)
\item Dipl.-Phys.\ Martina Wei"s (Doktorand, Elitenetzwerk Bayern)
\item cand.\ phys.\ Sebastian Huber
\item cand.\ phys.\ Tobias Hein
\item cand.\ phys.\ Tobias Viering
\end{itemize}
\originalTeX

\subsection[5.2]{Co-operation with other scientists\\(Zusammenarbeit mit
anderen Wissenschaftlern)}

Both applying groups co-operate with the international
MAGIC-Collaboration and the institutes represented therein. (W\"{u}rzburg
funded by the BMBF, Dortmund by means of appointment for the moment).

W\"{u}rzburg is also in close scientific exchange with the group of
Prof.~Dr.~Victoria Fonseca, UCM Madrid and the University of Turku
(Finland) operating the KVA optical telescope at La Palma. Other
cooperations refer to the projects JEM-EUSO (science case), GRIPS
(simulation), LISA (astrophysical input for templates), STEREO (data
analysis), and SOLAR ORBITER (electron-proton telescope). A cooperation
with GLAST science team members (Dr.~Anita and Dr.~Olaf Reimer,
Stanford) is also relevant for the proposed project.

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\"{a}t Bochum and Prof.~Dr.~Peter Biermann, MPIfR Bonn.
There are furthermore intense contacts to Prof.~Dr.~Francis Halzen,
Madison, Wisconsin.

The telescope design will be worked out in close cooperation with the
group of Prof.~Dr.~Felicitas Pauss, Dr.~Adrian Biland and
Prof.~Dr.~Eckart Lorenz (ETH~Z\"{u}rich). They will provide help in design
studies, construction and software development. The DAQ design will be
contributed by the group of Prof.~Dr.~Riccardo Paoletti (Università di
Siena and INFN sez.\ di Pisa, Italy).

The group of the newly appointed {\em Lehrstuhl f\"{u}r Physik und Ihre
Didaktik} (Prof.~Dr.~Thomas Trefzger) has expressed their interest to
join the project. They bring in a laboratory for photo-sensor testing,
know-how from former contributions to ATLAS and a joint interest in
operating a data pipeline using GRID technologies.

\subsection[5.3]{Work outside Germany, Cooperation with foreign
partners\\(Arbeiten im Ausland, Kooperation mit Partnern im Ausland)}

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[5.4]{Scientific equipment available (Apparative
Ausstattung)}
In Dortmund and W\"{u}rzburg extensive computer capacities for data
storage as well as for data analysis are available.

The faculty of physics at the University of Dortmund has modern
equipped mechanical and electrical workshops including a department for
development of electronics at its command. The chair of astroparticle
physics possesses common technical equipment required for constructing
modern DAQ.

The faculty of physics at the University of W\"{u}rzburg comes with a
mechanical and an electronic workshop, as well as a special laboratory
of the chair for astronomy suitable for photosensor testing.

\subsection[5.5]{The institution's general contribution\\(Laufende
Mittel f\"{u}r Sachausgaben)}

Current total institute budget from the University Dortmund
$\sim$20.000,-\,\euro\ per year.

Current total institute budget from the University W\"{u}rzburg
$\sim$30.000,-\,\euro\ per year.

%\paragraph{5.6 Conflicts of interest in economic activities\\Interessenskonflikte bei wirtschaftlichen Aktivit\"aten}~\\
\subsection[5.6]{Conflicts of interest in economic activities\\(Interessenskonflikte bei wirtschaftlichen Aktivit\"{a}ten)}~\\
none

\subsection[5.7]{Other requirements (Sonstige Voraussetzungen)}~\\
none

\newpage
\thispagestyle{empty}

\paragraph{6 Declarations (Erkl\"{a}rungen)}

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\"{a}t Dortmund (Prof.\ Dr.\ Gather) and at the Universit\"{a}t
W\"{u}rzburg (Prof.\ Dr.\ G.\ Bringmann) have been informed about the
submission of this proposal.

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

\vspace{2.5 cm}

\hfill
\begin{minipage}[t]{6cm}
W\"{u}rzburg,\\[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
\paragraph{8 List of appendices (Verzeichnis der Anlagen)}

\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
\item Letter of Support from the MAGIC collaboration
\item Letter of Support from Mets\"{a}hovi Radio Observatory
\item Letter of Support from the IceCube collaboration
\item Letter of Support from KVA optical telescope
\end{itemize}

\newpage
%\section{References}

(References of our groups are marked by an asterix *)
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\bibliographystyle{plainnat}
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\end{document}