Changeset 8773


Ignore:
Timestamp:
Dec 3, 2007, 3:08:16 PM (13 years ago)
Author:
tbretz
Message:
*** empty log message ***
Location:
trunk/Dwarf/Documents/ApplicationDFG
Files:
2 edited

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Unmodified
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Removed
  • trunk/Dwarf/Documents/ApplicationDFG/application.bib

    r8772 r8773  
    28362836}
    28372837
    2838 @ARTICLE{Paneque:2004,
    2839    author = {{Paneque}, D. and {Gebauer}, H.~J. and {Lorenz}, E. and {Mirzoyan}, R.
    2840 },
    2841     title = "{A method to enhance the sensitivity of photomultipliers for Air Cherenkov Telescopes by applying a lacquer that scatters light}",
    2842   journal = {Nuclear Instruments and Methods in Physics Research A},
    2843      year = 2004,
    2844     month = feb,
    2845    volume = 518,
    2846     pages = {619-621},
    2847       doi = {10.1016/j.nima.2003.11.101},
    2848    adsurl = {http://cdsads.u-strasbg.fr/abs/2004NIMPA.518..619P},
    2849   adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}
    2850 }
    2851 
    28522838@ARTICLE{Milagro:2007,
    28532839   author = {{Abdo}, A.~A. and others},
     
    30433029
    30443030@ARTICLE{Albert:501,
    3045  author  = {{MAGIC Collaboration}},
    3046  title   = "{Variable VHE gamma-ray emission from Markarian 501}",
    3047  journal = {ArXiv Astrophysics e-prints},
    3048  eprint  = {astro-ph/0702008},
    3049  year    = 2007,
    3050  month   = feb,
    3051  adsurl  = {http://cdsads.u-strasbg.fr/abs/2007astro.ph..2008M},
    3052  adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}
     3031   author = {{Albert}, J. and others },
     3032    title = "{Variable Very High Energy {$\gamma$}-Ray Emission from Markarian 501}",
     3033  journal = {\apj},
     3034   eprint = {arXiv:astro-ph/0702008},
     3035     year = 2007,
     3036    month = nov,
     3037   volume = 669,
     3038    pages = {862-883},
     3039      doi = {10.1086/521382},
     3040   adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...669..862A},
     3041  adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}
    30533042}
    30543043
    30553044@INPROCEEDINGS{Muenich:Icrc,
    3056    author = {M"unich, K. and L"unemann, Jan},
     3045   author = {M\"{u}nich, K. and L\"{u}nemann, J.},
    30573046    title = {Measurement of the atmospheric lepton energy spectra with {AMANDA-II}},
    30583047booktitle = {$30^{th}$ International Cosmic Ray Conference},
     
    30623051@INPROCEEDINGS{Bretz:2005drive,
    30633052   author = {Bretz, T. and Dorner, D. and Wagner, R.M. and Riegel, B.},
    3064     title = { A Scalable Drive System Concept for Future Projects},
     3053    title = {A Scalable Drive System Concept for Future Projects},
    30653054booktitle = {Towards a network of atmospheric Cherenkov detectors VII},
    30663055     year = 2005,
     
    30773066
    30783067@ARTICLE{MAGICsensi,
    3079  author = {{MAGIC Collaboration}},
     3068 author = {{MAGIC website}},
    30803069 title = "{MAGIC sensitivity at \url{http://magic.mppmu.mpg.de/physics/results/}}",
    30813070 journal = {Official MAGIC website},
     
    31953184   editor = {{Medina}, J.},
    31963185}
     3186
     3187@ARTICLE{Meli,
     3188   author = {{Meli}, A. and {Becker}, J.~K. and {Quenby}, J.~J.},
     3189    title = "{Cosmic ray acceleration in subluminal and superluminal relativistic shock environments}",
     3190  journal = {ArXiv e-prints},
     3191   eprint = {0709.3031},
     3192     year = 2007,
     3193    month = sep,
     3194   volume = 709,
     3195   adsurl = {http://adsabs.harvard.edu/abs/2007arXiv0709.3031M},
     3196  adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}
     3197}
     3198
  • trunk/Dwarf/Documents/ApplicationDFG/application.tex

    r8772 r8773  
    55%\renewcommand{\familydefault}{\sfdefault}
    66%\usepackage{helvet}
     7
     8\originalTeX
    79
    810\setlength{\parindent}{0pt}
     
    3335%\topmargin=-1.5cm
    3436
    35 \title{Neuantrag auf Gew"ahrung einer Sachbeihilfe\\Proposal for a new research project}
     37\title{Neuantrag auf Gew\"{a}hrung einer Sachbeihilfe\\Proposal for a new research project}
    3638\author{Prof.\ Dr.\ Karl\ Mannheim\\Prof.\ Dr.\ Dr.\ Wolfgang Rhode}
    3739
     
    4042\maketitle
    4143
    42 %\noindent {\it Das Inhaltsverzeichnis dient nur zur "Ubersicht und ist im eigentlichen Antrag nicht enthalten. \\
    43 %
    44 %\
    45 %
    46 %{\underline{\bf to do Liste}}\\
    47 %\begin{itemize}
    48 %   \item [1.6] Es muss sich jemand einen der Texte (oder ein Konglomerat daraus) aussuchen.
    49 %   \item [2.1] ist inhaltlich (u.A.) um die (z.T. in deutsch) angegebenen Stichpunkte zu erg"anzen.
    50 %   \item [2.2] ist noch (von Wolfgang und Karl?) zu schreiben.
    51 %   \item [3.1] ist inhaltlich (u.A.) um die (z.T. in deutsch) angegebenen Stichpunkte zu erg"anzen.
    52 %   \item [3.2] ist w"ortlich aus dem LoI kopiert und bedarf wom"oglich einer "Uberarbeitung im Sinne der Kapitel"uberschrift.
    53 %   \item [4.x] sind sprachlich, inhaltlich und optisch zu "uberarbeiten.
    54 %   \item [5.1] ist sprachlich (in deutsch lassen?) und inhaltlich (v.A. W"urzburg) zu "uberarbeiten.
    55 %   \item [5.2] ist inhaltlich (u.A.) um die angegebenen Stichpunkte und Informationen aus W"urzburg zu erg"anzen.
    56 %   \item [--] Plots und Bilder sind noch zu erg"anzen.
    57 %   \item [--] Referenzen sind im ganzen Text noch zu erg"anzen.
    58 %   \item [{\bf alles}] muss nat"urlich noch auf Orthographie und "`sprachliche Eleganz"' hin gegengelesen werden.
    59 %\end{itemize}
    60 %\newpage
    61 %}
    6244%\tableofcontents
    63 %\newpage
    64 %%%
    65 
    66 %{\LARGE{\bf
    67 %\begin{center}
    68 %Neuantrag auf Gew"ahrung einer Sachbeihilfe\\Proposal for a research project
    69 %\end{center}
    70 %}}
    7145
    7246\section[1]{Allgemeine Angaben/General Information}
    73 %\anmerk{Die Gliederung ist von der DFG vorgegeben}
    74 
    75 %Neuantrag auf Gew"ahrung einer Sachbeihilfe.
    7647
    7748\subsection[1.1]{Antragsteller/Applicants}
    78 % IN CASE A PROJECT IS DISTRIBUTED BETWEEN SEVERAL INSTITUTES
    79 % PLEASE GIVE AT LEAST ONE APPLICANT FOR EACH INSTITUTE;
    80 % ALSO, IN THIS CASE, THE PROPOSAL MUST MAKE CLEAR WHICH
    81 % RESOURCES GO TO WHERE, HOW THE WORK IS SPLIT, HOW THE INTERACTION
    82 % SHALL PROCEED ETC.
    83 %\setlength{\tabcolsep}{5em}
    84 
     49\germanTeX
    8550\begin{tabular}{|p{0.44\textwidth}|p{0.22\textwidth}|p{0.22\textwidth}|}\hline
    8651{\bf Name}&\multicolumn{2}{l|}{\bf Akademischer Grad}\\
     
    11883\multicolumn{3}{|c|}{{\bf email}: mannhein@astro.uni-wuerzbueg.de}\\\hline
    11984\end{tabular}
    120 
     85\originalTeX
    12186\newpage
    12287
    123 \paragraph{1.2 Topic (Thema)}~\\
    124 %% MAXIMAL 140 Zeichen fuer den DFG Jahresbericht
    125 %% AUCH IN DEUTSCH BEIFšGEN
     88%\paragraph{1.2 Topic}~\\
     89\subsection[1.2]{Topic}
    12690Long-term VHE $\gamma$-ray monitoring of bright blazars with a dedicated Cherenkov telescope
    12791
     92%\paragraph{1.2 Thema}~\\
     93\subsection[1.2]{Thema}
    12894Langzeitbeobachtung von hellen VHE $\gamma$-Blazaren mit einem dedizierten Cherenkov Teleskop
    12995
    130 \paragraph{1.3 Discipline and field of work (Fachgebiet und Arbeitsrichtung)}~\\
     96%\paragraph{1.3 Discipline and field of work (Fachgebiet und Arbeitsrichtung)}~\\
     97\subsection[1.3]{Discipline and field of work (Fachgebiet und Arbeitsrichtung)}
    13198Astronomy and Astrophysics, Particle Astrophysics
    13299
    133 \paragraph{\bf 1.4 Scheduled duration in total (Voraussichtliche Gesamtdauer)}~\\
     100%\paragraph{\bf 1.4 Scheduled duration in total (Voraussichtliche Gesamtdauer)}~\\
     101\subsection[1.4]{Scheduled duration in total (Voraussichtliche Gesamtdauer)}
    134102After successful completion of the three-year work plan developed in
    135103this proposal, we will ask for an extension of the project for another
     
    137105of supermassive binary black holes.
    138106
    139 \paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\
     107%\paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\
     108\subsection[1.5]{Application period (Antragszeitraum)}
    1401093\,years. The work on the project will begin immediately after the
    141110funding.
    142111
    143 \paragraph{\bf 1.6 Summary (Zusammenfassung)}~\\
     112\newpage
     113%\paragraph{\bf 1.6 Summary}~\\
     114\subsection[1.6]{Summary}
    144115We propose to set up a robotic imaging air Cherenkov telescope with low
    145116cost, but high performance design for remote operation. The goal is to
     
    153124observations of flares with higher sensitivity telescopes such as
    154125MAGIC, VERITAS, and H.E.S.S.\ Joint observations with the Whipple
    155 monitoring telescope will start a future 24h-monitoring of selected
     126monitoring telescope will start a future 24\,h-monitoring of selected
    156127sources with a distributed network of robotic telescopes. The telescope
    157128design is based on a full technological upgrade of one of the former
     
    161132robotically, a much lower energy threshold below 350\,GeV will be
    162133achieved and the observation time required for gaining the same signal
    163 as with CT3 will be reduced by a factor of 6.
    164 
    165 Unser Vorhaben besteht darin, ein robotisches Luft-Cherenkov-Teleskop
     134as with CT3 will be reduced by a factor of six.
     135
     136\germanTeX
     137%\paragraph{\bf 1.6 Zusammenfassung}~\\
     138\subsection[1.6]{Zusammenfassung}
     139{\bf Unser Vorhaben besteht darin, ein robotisches Luft-Cherenkov-Teleskop
    166140mit geringen Kosten aber hoher Leistung fernsteuerbar in Betrieb zu
    167141nehmen. Das Ziel ist es, dieses gamma-ray Teleskop ganz der
     
    185159Energieschwelle von unter 350\,GeV aufweisen, w"ahrend gleichzeitig die
    186160notwendige Beobachtungszeit, um dasselbe Signal wie CT3 zu erhalten, um
    187 einen Faktor 6 verringert wird.
    188 
     161einen Faktor sechs verringert wird.}
     162\originalTeX
    189163\newpage
    190164
     
    205179
    206180The main class of extragalactic, very high energy gamma-rays sources
    207 detected with imaging air-Cherenkov telescopes are blazars, i.e.
     181detected with imaging air-Cherenkov telescopes are blazars, i.e.\
    208182accreting supermassive black holes exhibiting a relativistic jet that
    209183is closely aligned with the line of sight. The non-thermal blazar
     
    232206transport problem in gamma ray bursts, and is probably present in
    233207blazar jets as well, even if they originate as pair jets in a black
    234 hole ergosphere\citep{Meszaros}. Protons and ions accelerated in the
     208hole ergosphere \citep{Meszaros}. Protons and ions accelerated in the
    235209jets of blazars can reach extremely high energies before energy losses
    236210become important \citep{Mannheim:1993}. Escaping particles contribute
     
    371345
    372346Assuming conservatively the performance of a single HEGRA-type
    373 telescope, long-term monitoring of at least the following blazars is
    374 possible: Mrk\,421, Mrk\,501, 1ES\,2344+514, 1ES\,1959+650,
     347telescope, long-term monitoring of at least the following known blazars
     348is possible: Mrk\,421, Mrk\,501, 1ES\,2344+514, 1ES\,1959+650,
    375349H\,1426+428, PKS\,2155-304. We emphasize that DWARF will run as a
    376350facility dedicated to these targets only, providing a maximum
     
    380354improvement in sensitivity and a lower energy-threshold is reasonable.
    381355Current studies show that with a good timing resolution (2\,GHz) a
    382 further 50\% increase in sensitivity (compared to a 300\,MHz system) is
     356further 40\% increase in sensitivity (compared to a 300\,MHz system) is
    383357feasible. Together with an extended mirror area and a large camera, a
    384358sensitivity improvement compared to a single HEGRA telescope of a
     
    416390The ultra fast drive system of the MAGIC telscopes, suitable for fast
    417391repositioning in case of Gamma-Ray Bursts, has been developed,
    418 commissioned and programmed by the W"urzburg group
     392commissioned and programmed by the W\"{u}rzburg group
    419393\citep{Bretz:2003drive,Bretz:2005drive}. To correct for axis
    420394misalignments and possible deformations of the structure (e.g.\ bending
     
    429403Mirror structures made of plastic material have been developed as
    430404Winston Cones for balloon flight experiments previously by the group of
    431 Wolfgang Dr"oge. W"urzburg has also participated in the development of
    432 a HPD test bench, which has been setup in Munich and W"urzburg. With
     405Wolfgang Dr\"{o}ge. W\"{u}rzburg has also participated in the development of
     406a HPD test bench, which has been setup in Munich and W\"{u}rzburg. With
    433407this setup, HPDs for future improvement of the sensitivity of the MAGIC
    434408camera are investigated.
     
    436410\paragraph{Software}
    437411
    438 The W"urzburg group has developed a full MAGIC analysis package,
     412The W\"{u}rzburg group has developed a full MAGIC analysis package,
    439413flexible and modular enough to easily process DWARF data
    440414\citep{Bretz:2005paris,Riegel:2005icrc,Bretz:2005mars}. A method for
     
    449423years now. The datacenter is equipped with a professional multi-stage
    450424(hierarchical) storage system. Two operators are paid by the physics
    451 faculty. Currently efforts in W"urzburg and Dortmund are ongoing to
     425faculty. Currently efforts in W\"{u}rzburg and Dortmund are ongoing to
    452426turn the old inflexible Monte Carlo programs, used by the MAGIC
    453427collaboration, into modular packages which allows easy simulation of
     
    470444MAGIC and IceCube data is available in the Dortmund group. Research
    471445activities are also related with relativistic particle acceleration
    472 \citep{Meli} and gamma ray attenuation \citep{Kneiske}. The W"urzburg
     446\citep{Meli} and gamma ray attenuation \citep{Kneiske}. The W\"{u}rzburg
    473447group has organized and carried out multi-wavelength observations of
    474448bright blazars involving MAGIC, Suzaku, the IRAM telescopes, and the
     
    483457leading to predictions of correlated neutrino emission \citep{Rueger}.
    484458This includes simulations of particle acceleration due to the Weibel
    485 instability \citep{Burkart}. Much of this research at W"urzburg is
     459instability \citep{Burkart}. Much of this research at W\"{u}rzburg is
    486460carried out in the context of the research training school GRK\,1147
    487461{\em Theoretical Astrophysics and Particle Physics}.
    488462
    489 \section[3]{Ziele/Goals}
    490 
    491 \subsection[3.1]{Ziele/Goals}
     463\section[3]{Goals and Work Schedule (Ziele und Arbeitsprogramm)}
     464
     465\subsection[3.1]{Goals (Ziele)}
    492466
    493467The aim of the project is to put the former CT3 of the HEGRA
     
    496470efficiency, and new fast data acquisition system, under the name of
    497471DWARF. The energy threshold will be lowered, and  the sensitivity of
    498 DWARF will be greatly improved compared to HEGRA CT3 ({\bf see plot
    499 xxx/at the end}). Commissioning and the first year of data taking
     472DWARF will be greatly improved compared to HEGRA CT3 (see
     473figure~\ref{sensitivity}). Commissioning and the first year of data taking
    500474should be carried out within the three years of the requested funding
    501475period.
     
    521495(small number of experienced scientists) as optimal for achieving the
    522496project goals. The available automatic analysis package developed by
    523 the W"urzburg group for MAGIC is modular and flexible, and can thus be
     497the W\"{u}rzburg group for MAGIC is modular and flexible, and can thus be
    524498used with minor changes for the DWARF project.
    525499
    526500\begin{figure}[htb]
    527501\begin{center}
    528  \includegraphics*[width=0.8\textwidth,angle=0,clip]{visibility.eps}
    529  \caption{blablbaaaa}
     502 \includegraphics*[width=0.7\textwidth,angle=0,clip]{visibility.eps}
     503 \caption{Source visibility in hours per night versus month of the year
     504 for a maximum observation zenith angle of 65$^\circ$.
     505 Shown are all sources which we want to monitor including the CrabNebula
     506 necessary for calibration and quality assurance. }
    530507\label{visibility}
    531508\end{center}
    532509\end{figure}
    533510
    534 %[[Image:dwarf-source-visibility.png|thumb|300px|Source visibility ([[Media:dwarf-source-visibility.eps|eps]])]]
    535 
    536511The scientific focus of the project will be on the long-term monitoring
    537512of bright, nearby VHE emitting blazars.  At least one of the proposed
    538 targets will be visible any time of the year ({\bf see plot}). For
     513targets will be visible any time of the year (see figure~\ref{visibility}). For
    539514calibration purposes, some time will be scheduled for observations of
    540515the Crab nebula.  The blazar observations will allow
     
    551526extended bandwidth from below 100\,GeV to multi-TeV energies.
    552527\item to obtain multi-frequency observations together with the
    553 Mets"ahovi Radio Observatory and the optical Tuorla Observatory
    554 (Letters of support appendix). The measurements will be correlated with
    555 INTEGRAL and GLAST results, when available. x-ray monitoring using the
    556 SWIFT and Suzaku facilities will be proposed.
     528Mets\"{a}hovi Radio Observatory and the optical Tuorla Observatory. The
     529measurements will be correlated with INTEGRAL and GLAST results, when
     530available. x-ray monitoring using the SWIFT and Suzaku facilities will
     531be proposed.
    557532\end{itemize}
    558533
     
    562537jets. We plan to interpret the data with models currently developed in
    563538the context of the Research Training Group {\em Theoretical
    564 Astrophysics} in W"urzburg (Graduiertenkolleg, GK\,1147), including
     539Astrophysics} in W\"{u}rzburg (Graduiertenkolleg, GK\,1147), including
    565540particle-in-cell and hybrid MHD models.
    566541\item the black hole mass and accretion rate fitting the data with
     
    574549Constraints on the binary system will allow to compute most accurate
    575550templates of gravitational waves, which is a connected project at
    576 W"urzburg in the German LISA consortium funded by DLR.
     551W\"{u}rzburg in the German LISA consortium funded by DLR.
    577552\end{itemize}
    578553
    579 \subsection{Arbeitsprogramm/Work schedule}
     554\subsection[3.2]{Work schedule (Arbeitsprogramm)}
    580555
    581556To complete the mount to a functional Cherenkov telescope within a
     
    584559The work schedule assumes that the work will begin in January 2008,
    585560immediately after funding. Later funding would accordingly shift the
    586 schedule. Each year is divided into quarters ({\bf see figure xxx}).
     561schedule. Each year is divided into quarters (see figure~\ref{schedule}).
     562
     563\begin{figure}[htb]
     564\begin{center}
     565 \includegraphics*[angle=0,clip]{schedule.eps}
     566% \caption{Left: The old HEGRA CT3 telescope as operated within the
     567% HEGRA Sytem. Right: A photomontage how the revised CT3 telescope
     568% could look like with more and hexagonal mirrors.}
     569\label{schedule}
     570%\label{DWARF}
     571\end{center}
     572\end{figure}
    587573
    588574\paragraph{Software}
    589575\begin{itemize}
    590 \item MC adaption (Do/Wue): 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.
    591 \item Analysis adaption (Wue): 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.
    592 \item Adaption Drive software (Wue): 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.
     576\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.
     577\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.
     578\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.
    593579\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.
    594580\end{itemize}
    595581
    596 \paragraph{Mirrors (Wue)} 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.
    597 \paragraph{Drive (Wue)} 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.
    598 \paragraph{Auxiliary (Wue)} Before the final setup in 2009/1, all auxiliary systems (weather station, computers, etc.) will have been specified, ordered and shipped.
     582\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.
     583\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.
     584\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.
    599585\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.
    600 \paragraph{Full System (Do/Wue)} 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.
     586\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.
    601587
    602588Based on the experience with setting up the MAGIC telescope we estimate
    603589this workschedule as conservative.
    604590
    605 \subsubsection[3.3]{Experiments with humans (Untersuchungen am Menschen)}
     591\subsection[3.3]{Experiments with humans (Untersuchungen am Menschen)}
    606592none
    607 \subsubsection[3.4]{Experiments with animals (Tierversuche)}
     593\subsection[3.4]{Experiments with animals (Tierversuche)}
    608594none
    609 \subsubsection[3.5]{Experiments with recombinant DNA (Gentechnologische Experimente)}
     595\subsection[3.5]{Experiments with recombinant DNA (Gentechnologische Experimente)}
    610596none
    611597
    612 \section[4]{Beantragte Mittel/Funds requested}
     598\clearpage
     599
     600\section[4]{Funds requested (Beantragte Mittel)}
    613601
    614602We request funding for a total of three years. Summarizing, the
    615 expenses for the telescope ({\bf see section xxx}) are dominated by the
    616 camera and data acquisition. The financial volume for the complete
    617 hardware inclusive transport amounts to 372.985,-\,\euro.
    618 
    619 \subsection[4.1]{Required Staff (Personalbedarf)}
     603expenses for the telescope are dominated by the camera and data
     604acquisition.
     605%The financial volume for the complete hardware inclusive
     606%transport amounts to {\bf 372.985,-\,\euro}.
     607
     608\subsection[4.1]{Required Staff (Personalkosten)}
    620609
    621610For this period, we request funding for two postdocs and two PhD
    622 students, one in Dortmund and one in W"urzburg each.
    623 
    624 The staff members shall fulfill the tasks given in the work schedule
    625 above. To cover these tasks completely, one additional PhD student per
    626 group and a various number of Diploma students will complete the
    627 working group
     611students, one in Dortmund and one in W\"{u}rzburg each. The staff
     612members shall fulfill the tasks given in the work schedule above. To
     613cover these tasks completely, one additional PhD and a various number
     614of Diploma students will complete the working group.
    628615
    629616Suitable candidates interested in these positions are Dr.\ Thomas
    630 Bretz, Dr.\ dest.\ Daniela Dorner, Dr.\ dest.\ Kirsten M"unich, cand.\
    631 phys.\ Michael Backes, cand.\ phys.\ Daniela Hadasch and cand.\ phys.\
    632 Dominik Neise.
    633 
    634 \subsection[4.2]{Scientific equipment (Wissenschaftliche Ger"ate)}
    635 
    636 Support: At the Observatorio de los Muchachos (ORM), at the MAGIC site,
     617Bretz, Dr.\ dest.\ Daniela Dorner, Dr.\ dest.\ Kirsten M\"{u}nich,
     618cand.\ phys.\ Michael Backes, cand.\ phys.\ Daniela Hadasch and cand.\
     619phys.\ Dominik Neise.
     620
     621\subsection[4.2]{Scientific equipment (Wissenschaftliche Ger\"{a}te)}
     622
     623At the Observatorio Roque de los Muchachos (ORM), at the MAGIC site,
    637624the mount of the former HEGRA telescope CT3 now owned by the MAGIC
    638625collaboration is still operational. One hut for electronics close to
    639626the telescope is available. Additional space is available in the MAGIC
    640627counting house. The MAGIC Memorandum of Understanding allows for
    641 operating it as an auxiliary instrument (see appendix), and emergency
    642 support from the shift crew of MAGIC is guaranteed, although autonomous
    643 robotic operation is the primary goal.
    644 
    645 To achieve the planned sensitivity and threshold given in fig.\
    646 \ref{sensitivity} the following components have to be bought. To obtain
    647 reliable results as fast as possible well known components have been
    648 chosen.\\
    649 
     628operating DWARF as an auxiliary instrument (see appendix). Also
     629emergency support from the shift crew is guaranteed, although
     630autonomous robotic operation is the primary goal.
     631
     632To achieve the planned sensitivity and threshold
     633(figure~\ref{sensitivity}) the following components have to be bought.
     634To obtain reliable results as fast as possible well known components
     635have been chosen.
    650636\begin{figure}[hb]
    651637\centering{
    652 \includegraphics[width=0.8\textwidth]{sensitivity.eps}
    653 \caption{Integral flux sensitivity of current and former Cherenkov
    654 telescopes
    655 \citep{Moralejo:2004,Juan:2000,MAGICsensi,Magnussen:1998,Vassiliev:1999}
    656 as well as the expectations for DWARF, with both a
    657 PMT- and an APD-camera. These expectations are based on the sensitivity of
    658 the HEGRA CT1 telescope, scaled by the improvements mentioned in the text.
    659 }
    660 \label{sensitivity}
    661 }
     638\includegraphics[width=0.55\textwidth]{sensitivity.eps}
     639\caption{Integral flux sensitivity of current and former telescopes
     640\citep{Juan:2000,MAGICsensi,Vassiliev:1999}
     641as well as the expectations for DWARF, with both a PMT- and a
     642GAPD-camera. These expectations are based on the sensitivity of
     643HEGRA~CT1, scaled by the improvements mentioned in the text.
     644} \label{sensitivity} }
    662645\end{figure}
    663 
     646\clearpage
    664647{\bf Camera}\dotfill 207.550,-\,\euro\\[-3ex]
    665648\begin{quote}
     
    683666mode increases the sensitivity by a factor of $\sqrt{2}$,
    684667because spending observation time for dedicated background observations
    685 becomes obsolete, i.e. observation time for the source is doubled. This
     668becomes obsolete, i.e.\ observation time for the source is doubled. This
    686669ensures in addition a better time coverage of the observed sources.
    687670
     
    693676%}
    694677
    695 \begin{figure}[ht]
     678A camera completely containing shower images of events in the energy
     679region of 1\,TeV-10\,TeV should have a diameter in the order of
     6805$^\circ$. To decrease the dependence of the measurements on the camera
     681geometry, a camera layout as symmetric as possible will be chosen.
     682Consequently a camera allowing to fulfill these requirements should be
     683round and have a diameter of $4.5^\circ-5.0^\circ$.
     684\begin{figure}[th]
    696685\begin{center}
    697  \includegraphics*[width=0.4\textwidth,angle=0,clip]{cam271.eps}
    698  \includegraphics*[width=0.4\textwidth,angle=0,clip]{cam313.eps}
     686 \includegraphics*[width=0.495\textwidth,angle=0,clip]{cam271.eps}
     687 \includegraphics*[width=0.495\textwidth,angle=0,clip]{cam313.eps}
    699688 \caption{Left: Schematic picture of the 271 pixel CT-3 camera with a field of view of 4.6$^\circ$.
    700689 Right: Schematic picture of the 313 pixel camera for DWARF with a field of view of 5$^\circ$.}
     
    704693\end{figure}
    705694
    706 A camera completely containing shower images of events in the energy
    707 region of 1\,TeV-10\,TeV should have a diameter in the order of
    708 5$^\circ$. To decrease the dependence of the measurements on the camera
    709 geometry, a camera layout as symmetric as possible will be chosen.
    710 Consequently a camera allowing to fulfill these requirements should be
    711 round and have a diameter of $4.5^\circ-5.0^\circ$.
    712 
    713 Therefor a camera with 313 pixel camera (see figure \ref{camDWARF}) is
     695Therefor a camera with 313 pixel camera (see figure~\ref{camDWARF}) is
    714696chosen. The camera will be built based on the experience with HEGRA and
    715697MAGIC. 19\,mm diameter Photomultiplier Tubes (PM, EMI\,9083\,KFLA-UD)
    716698will be bought, similar to the HEGRA type (EMI\,9083\,KFLA). They have
    717 a 25\% improved quantum efficiency and ensure a granularity which is
    718 enough to guarantee good results even below the energy threshold (flux
    719 peak energy). Each individual pixel has to be equipped with a
    720 preamplifier, an active high-voltage supply and control. The total
    721 expense for a single pixel will be in the order of 650,-\,\euro.
     699a 25\% improved quantum efficiency (see figure~\ref{qe}) and ensure a
     700granularity which is enough to guarantee good results even below the
     701energy threshold (flux peak energy). Each individual pixel has to be
     702equipped with a preamplifier, an active high-voltage supply and
     703control. The total expense for a single pixel will be in the order of
     704650,-\,\euro.
    722705
    723706All possibilities of borrowing one of the old HEGRA cameras for a
     
    725708cameras.
    726709
    727 {\bf At ETH~Z"urich currently test measurements are ongoing to prove the
     710{\bf At ETH~Z\"{u}rich currently test measurements are ongoing to prove the
    728711ability, i.e.\ stability, aging, quantum efficiency, etc., of using
    729 Geiger-mode APDs (Advanced Photon Detector aka. Silicon PM) as photon
     712Geiger-mode APDs (GAPD) as photon
    730713detector in the camera of a Cherenkov telescope. The advantages are
    731 extremely high quantum efficiency (>50\%), easier gain stabilization and
     714extremely high quantum efficiency ($>$50\%), easier gain stabilization and
    732715simplified application compared to classical PMs. If these test
    733716measurements are successfully finished until 8/2008 we consider to use
    734 APDs in favor of classical PMs. The design of such a camera would take
     717GAPDs in favor of classical PMs. The design of such a camera would take
    735718place at University Dortmund in close collaboration with the experts
    736719from ETH. Construction would also take place at the electronics
     
    741724{\bf Camera support}\dotfill 204.000,-\,\euro\\[-3ex]
    742725\begin{quote}
    743 For this setup the camera holding has to be redesigned. (1500\,\euro)
     726For this setup the camera holding has to be redesigned. (1500,-\,\euro)
    744727The camera chassis must be water tight and will be equipped with an
    745728automatic lid protecting the PMs at day-time. For further protection, a
     
    755738planned.
    756739
    757 In total a gain of {\bf $\sim$ 15\%} in light-collection
     740In total a gain of {\bf $\sim$15\%} in light-collection
    758741efficiency compared to the old CT3 system can be acheived.
    759742\end{quote}\vspace{3ex}
     
    786769Current results obtained with the new 2\,GHz FADC system in the MAGIC
    787770data acquisition show that for a single telescope a sensitivity
    788 improvement 40$\%$ with a fast FADC system is achievable \citep{Tescaro:2007}.
    789 
    790 As for the HEGRA telescopes a simple multiplicity trigger is sufficient,
    791 but also a simple three-next-neighbors (closed package) could be
    792 programmed. (both cases $\sim$30.000,-\,\euro: $<$100,-\,\euro/channel).
    793 
    794 Additional data reduction and preprocessing in the readout hardware or
    795 the readout computer is provided. Assuming conservatively storage of
    796 raw-data at a readout rate of 30\,Hz the storage space needed is less
    797 than 250\,GB/month or 3\,TB/year. This amount of data can easily be
    798 stored and processed by the W"urzburg Datacenter (current online
    799 capacity $>$40\,TB, offline capacity $>$80\,TB, $>$40\,CPUs).
    800 %}\\[2ex]
     771improvement of 40\% with a fast FADC system is achievable \citep{Tescaro:2007}.
     772
     773As for the HEGRA telescopes a simple multiplicity trigger is
     774sufficient, but also a simple neighbor-logic could be programmed (both
     775cases $\sim$100,-\,\euro/channel).
     776
     777Additional data reduction and preprocessing within the readout chain is
     778provided. Assuming conservatively a readout rate of 30\,Hz the storage
     779space needed will be less than 250\,GB/month or 3\,TB/year. This amount
     780of data can easily be stored and processed by the W\"{u}rzburg
     781Datacenter (current capacity $>$80\,TB, $>$40\,CPUs).
    801782\end{quote}\vspace{3ex}
    802783
     
    805786\begin{quote}
    806787The existing mirrors are replaced by new plastic mirrors which are
    807 currently developed by Wolfgang Dr"oge's group. The cheap and
     788currently developed by Wolfgang Dr\"{o}ge's group. The cheap and
    808789light-weight material has been formerly used for Winston cones in
    809790balloon experiments. The mirrors are copied from a master coated with a
    810791reflecting and a protective material. Tests have given promising
    811792results. By a change of the mirror geometry, the mirror area can be
    812 increased from 8.5\,m$^2$ to 13\,m$^2$ (see picture \ref{CT3} and
    813 montage \ref{DWARF}); this includes an increase of $\sim$10$\%$ per
     793increased from 8.5\,m$^2$ to 13\,m$^2$ (see picture~\ref{CT3} and
     794montage~\ref{DWARF}); this includes an increase of $\sim$10$\%$ per
    814795mirror by using a hexagonal layout instead of a round one. A further
    815796increase of the mirror area would require a reconstruction of parts of
     
    824805aluminized Mylar mirror-foil, and a dialectical layer of SiO2 as for
    825806the Winston Cones. By this, a gain in reflectivity of $\sim10\%$ is
    826 achieved, {\bf see plot} \citep{Fraunhofer}.
    827 
    828 \begin{figure}[thb]
    829 \centering{
    830 \includegraphics[width=0.32\textwidth]{cherenkov.eps}
    831 \includegraphics[width=0.32\textwidth]{reflectivity.eps}
    832 \includegraphics[width=0.32\textwidth]{qe.eps}
    833 \caption{xxx yyy zzz }
    834 \label{reflectivity}
    835 }
    836 \end{figure}
    837 
     807achieved, see figure~\ref{reflectivity} \citep{Fraunhofer}.
    838808
    839809Both solutions would require the same expenses.
     
    842812individual mirrors and the point-spread function of the total mirror
    843813during long-term observations, the application of an automatic mirror
    844 adjustment system, as developed by ETH~Z"urich and successfully
     814adjustment system, as developed by ETH~Z\"{u}rich and successfully
    845815operated on the MAGIC telescope, is intended.
     816\begin{figure}[p]
     817\centering{
     818\includegraphics[width=0.57\textwidth]{cherenkov.eps}
     819\includegraphics[width=0.57\textwidth]{reflectivity.eps}
     820\includegraphics[width=0.57\textwidth]{qe.eps}
     821\caption{Top to bottom: The cherenkov spectrum as observed by a
     822telescope located at 2000\,m above sea level. The mirror's reflectivity
     823of a 300\,nm thick aluminum layer with a protection layer of 10\,nm and
     824100\,nm thickness respectively. For comparison the reflectivity of
     825HEGRA CT1's mirrors \citep{Kestel:2000} are shown. The bottom plot depicts
     826the quantum efficiency of the prefered PMs (EMI) together with the
     827predecessor used in CT1. A proper coating \citep{Paneque:2004} will
     828further enhance its effciency. An even better increase would be the
     829usage of Geiger-mode APDs.}
     830
     831\label{cherenkov}
     832\label{reflectivity}
     833\label{qe}
     834}
     835\end{figure}
     836
    846837%<grey>The system
    847838%will be provided by ETH Z"urich.</grey>
     
    870861produced.
    871862
    872 To ensure a homogeneous acceptance over the whole camera essential for
    873 wobble-mode observations the trigger rate of the individual pixels have
    874 to be measured. Therefore the slow control system will be equipped with
    875 a feedback on the individual pixel rate.
     863To ensure a homogeneous acceptance of the camera, essential for
     864wobble-mode observations, the trigger rate of the individual pixels
     865will be measured and controlled.
    876866
    877867To correct for axis misalignments and possible deformations of the
    878 structure (e.g. bending of camera holding masts), a pointing correction
     868structure (e.g.\ bending of camera holding masts), a pointing correction
    879869algorithm as used in the MAGIC tracking system will be applied. It is
    880870calibrated by measurements of the reflection of bright guide stars on
    881871the camera surface and ensures a pointing accuracy well below the pixel
    882 diameter. Therefore a high sensitive low-cost video camera, as already
    883 in operation for MAGIC\ I and~II, ({\bf 300,-\,\euro\ camera, 600,-\,\euro\
    884 optics, 300,-\,\euro\ housing, 250,-\,\euro\ Frame grabber}) will be
    885 installed.
     872diameter. Therefore a high sensitive low-cost video camera, as for
     873MAGIC\ I and~II, ({\bf 300,-\,\euro\ camera, 600,-\,\euro\ optics,
     874300,-\,\euro\ housing, 250,-\,\euro\ Frame grabber}) will be installed.
    886875
    887876A second identical CCD camera for online monitoring (starguider) will
     
    908897each will fulfill the requirement ($\sim$4.000,-\,\euro). The data will be
    909898transmitted as soon as possible after data taking via Internet to the
    910 W"urzburg Datacenter. Enough storage capacity and computing power
     899W\"{u}rzburg Datacenter. Enough storage capacity and computing power
    911900is available there and already reserved for this purpose.
    912901
     
    921910corrosion protection, cable ducts, etc. is needed (7.500,-\,\euro).
    922911
    923 For movement, motors, shaft encoders and control electronics in the
     912For the movement, motors, shaft encoders and control electronics in the
    924913order of 10.000,-\,\euro\ have to be bought. The costs have been estimated
    925914with the experience from building the MAGIC drive systems. The DWARF
     
    943932\begin{quote}
    944933   \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
    945    UPS\hfill 2.000,-\,\euro\\
     934   Uninterruptable power-supply (UPS)\hfill 2.000,-\,\euro\\
    946935   Security fence\hfill 2.000,-\,\euro\\
    947936   \end{minipage}\\[-0.5ex]
    948937%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
    949 An uninterruptable power-supply unit (UPS) with 5\,kW-10\,kW will be
     938A UPS with 5\,kW-10\,kW will be
    950939installed to protect the equipment against power cuts and ensure a safe
    951 telescope position at the time of sunrise. ($<$2.000,-\,\euro)
     940telescope position at the time of sunrise.
    952941
    953942A fence for protection in case of robotic movement will be
     
    957946{\bf Other expenses}\dotfill 7.500,-\,\euro\\[-3ex]
    958947\begin{quote}
    959 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
    960    Robotics\hfill 7.500,-\,\euro\\
    961    \end{minipage}\\[-0.5ex]
     948%\parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
     949%   Robotics\hfill 7.500,-\,\euro\\
     950%   \end{minipage}\\[-0.5ex]
    962951%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
    963 For remote operation a variety of remote controllable electronic
     952For remote, robotic operation a variety of remote controllable electronic
    964953components such as ethernet controlled sockets and switches will be
    965954bought. Monitoring equipment, for example different kind of sensors, is
    966955also mandatory.%}\\[2ex]
    967 \end{quote}\vspace{3ex}
    968 
    969 {\bf 4.2 Consumables (Verbrauchsmaterial)}\dotfill 10.750,-\,\euro\\[-3ex]
    970 \begin{quote}
    971    \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
    972    10 LTO\,4 tapes (8\,TB)\hfill 750,-\,\euro\\
    973    Consumables (overalls) tools and materials\hfill 10.000,-\,\euro\\
    974    \end{minipage}\\[-0.5ex]
    975 %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
    976 %For remote operation a variety of remote controllable electronic
    977 %components such as ethernet controlled sockets and switches will be
    978 %bought. Monitoring equipment, for example different kind of sensors, is
    979 %also mandatory.%}\\[2ex]
    980 \end{quote}\vspace{1ex}
    981 
     956\end{quote}
    982957\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
    983 \hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.1+4.2:\hfill{\bf
    984 352.985,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
     958\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.2:\hfill{\bf
     959342.235,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
    985960\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
    986961\hspace*{0.66\textwidth}\hrulefill\\
    987962
    988 
    989 \subsection[4.3]{Reisen/Travel expenses}
    990 
    991 In total, we apply for an amount of 72.200,-\,\euro\ for travelling. This
    992 large amount of travel funding is required due to the very close
    993 cooperation between Dortmund and W"urzburg and the work demands on the
    994 construction site.\\[-2ex]
     963\subsection[4.3]{Consumables (Verbrauchsmaterial)}
     964
     965\begin{quote}
     966%   \parbox[t]{1em}{~}\begin{minipage}[t]{0.9\textwidth}
     967   10 LTO\,4 tapes (8\,TB)\dotfill 750,-\,\euro\\
     968   Consumables (overalls) tools and materials\dotfill 10.000,-\,\euro
     969%   \end{minipage}\\[-0.5ex]
     970\end{quote}
     971
     972\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
     973\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.3:\hfill{\bf
     97410.750,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
     975\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
     976\hspace*{0.66\textwidth}\hrulefill\\
     977
     978\subsection[4.4]{Reisen (Travel expenses)}
     979The large amount of travel funding is required due to the very close
     980cooperation between Dortmund and W\"{u}rzburg and the work demands on
     981the construction site.\\[-2ex]
    995982
    996983\begin{quote}
    997984%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
    998 Per year one senior group member from Dortmund and W"urzburg should
    999 present the status of the work in progress on an international workshop
    1000 or conference:
    1001 
    1002 2 x 3 years x 1500\,\euro\dotfill 9.000,-\,\euro\\
    1003 
    1004 One participation on the biannual MAGIC collaboration meeting:
    1005 
    1006 2 x 3 years x 1000\,\euro\dotfill 6.000,-\,\euro\\
    1007 
    1008 PhD student exchange between W"urzburg and Dortmund
    1009 
    1010 1 student x 1 week x 24 (every six weeks) x 800\,\euro\dotfill
    1011 19.200,-\,\euro\\
     985Per year one senior group member from Dortmund and W\"{u}rzburg should
     986present the status of the work in progress at an international workshop
     987or conference:\\
     9882 x 3\,years x 1.500,-\,\euro\dotfill 9.000,-\,\euro\\[-2ex]
     989
     990One participation at the biannual MAGIC collaboration meeting:\\
     9912 x 3\,years x 1.000,-\,\euro\dotfill 6.000,-\,\euro\\[-2ex]
     992
     993PhD student exchange between W\"{u}rzburg and Dortmund:\\
     9941\,student x 1\,week x 24 (every six weeks) x 800,-\,\euro\dotfill
     99519.200,-\,\euro\\[-2ex]
    1012996
    1013997For setup of the telescope at La Palma the following travel expenses
    1014 are necessary:
    1015 
    1016 4 x 2 weeks at La Palma x 2 persons x 1800\,\euro\dotfill
    1017 28.800,-\,\euro\\
     998are necessary:\\
     9994 x 2\,weeks at La Palma x 2\,persons x 1.800,-\,\euro\dotfill
     100028.800,-\,\euro
    10181001%}
    10191002\end{quote}
    10201003
    1021 \subsection[4.5]{Publikationskosten/Publication costs}
     1004\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
     1005\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.4:\hfill{\bf
     100672.200,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
     1007\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
     1008\hspace*{0.66\textwidth}\hrulefill\\
     1009
     1010
     1011\subsection[4.5]{Publikationskosten (Publication costs)}
    10221012Will be covered by the proposing institutes.
    10231013
     1014
    10241015\subsection[4.6]{Other costs (Sonstige Kosten)}
    1025 
    1026 Storage container\dotfill 5.000,00\,\euro\\
    1027 dismantling (will be covered by proposing institutes)\dotfill n/a\\
    1028 Transport\dotfill 15.000,00\,\euro\\
    1029 
    1030 \section[5]{Voraussetzungen f"ur die Durchf"uhrung des Vorhabens\\Preconditions for carrying out the project}
     1016\begin{quote}
     1017Storage container (for shipment of the mirrors)\dotfill 5.000,-\,\euro\\
     1018Transport\dotfill 15.000,-\,\euro\\
     1019Dismantling (will be covered by proposing institutes)\dotfill n/a
     1020\end{quote}
     1021
     1022\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
     1023\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.6:\hfill{\bf
     102420.000,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
     1025\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
     1026\hspace*{0.66\textwidth}\hrulefill\\
     1027
     1028\newpage
     1029\germanTeX
     1030\section[5]{Preconditions for carrying out the project\\Voraussetzungen f"ur die Durchf"uhrung des Vorhabens}
    10311031none
    10321032
     
    10431043\item Dipl.-Phys.\ Jens Dreyer (Doktorand (IceCube), Grundausttattung)
    10441044\item M.Sc.\ Valentin Curtef (Doktorand (MAGIC), Grundausstattung)
    1045 \item cand.\ phys.\ Michael Backes (Diplomand (MAGIC), zum F\"orderbeginn diplomiert)
     1045\item cand.\ phys.\ Michael Backes (Diplomand (MAGIC), zum F"orderbeginn diplomiert)
    10461046\item cand.\ phys.\ Daniela Hadasch (Diplomand (MAGIC))
    10471047\item cand.\ phys.\ Anne Wiedemann (Diplomand (IceCube))
     
    10511051\end{itemize}
    10521052
    1053 \paragraph{W"urzburg}
     1053\paragraph{W\"{u}rzburg}
    10541054\begin{itemize}
    10551055\setlength{\itemsep}{0pt}
     
    10761076\item cand.\ phys.\ Tobias Viering
    10771077\end{itemize}
     1078\originalTeX
    10781079
    10791080\subsection[5.2]{Co-operation with other scientists (Zusammenarbeit mit
     
    10811082
    10821083Both applying groups co-operate with the international
    1083 MAGIC-Collaboration and the institutes represented therein. (W"urzburg
     1084MAGIC-Collaboration and the institutes represented therein. (W\"{u}rzburg
    10841085funded by the BMBF, Dortmund by means of appointment for the moment).
    10851086
    1086 W"urzburg is also in close scientific exchange with the group of
     1087W\"{u}rzburg is also in close scientific exchange with the group of
    10871088Prof.~Dr.~Victoria Fonseca, UCM Madrid and the University of Turku
    10881089(Finland) operating the KVA optical telescope at La Palma. Other
     
    10971098Moreover on the field of phenomenology there do exist good working
    10981099contacts to the groups of Prof.~Dr.~Reinhard Schlickeiser,
    1099 Ruhr-Universit"at Bochum and Prof.~Dr.~Peter Biermann, MPIfR Bonn.
     1100Ruhr-Universit\"{a}t Bochum and Prof.~Dr.~Peter Biermann, MPIfR Bonn.
    11001101There are furthermore intense contacts to Prof.~Dr.~Francis Halzen,
    11011102Madison, Wisconsin.
     
    11031104The telescope design will be worked out in close cooperation with the
    11041105group of Prof.~Dr.~Felicitas Pauss, Dr.~Adrian Biland and
    1105 Prof.~Dr.~Eckart Lorenz (ETH Z"urich). They will provide help in design
     1106Prof.~Dr.~Eckart Lorenz (ETH~Z\"{u}rich). They will provide help in design
    11061107studies, construction and software development. The DAQ design will be
    11071108contributed by the group of Prof.~Dr.~Riccardo Paoletti (Università di
    11081109Siena and INFN sez.\ di Pisa, Italy).
    11091110
    1110 The group of the newly appointed {\em Lehrstuhl f"ur Physik und Ihre
     1111The group of the newly appointed {\em Lehrstuhl f\"{u}r Physik und Ihre
    11111112Didaktik} (Prof.~Dr.~Thomas Trefzger) has expressed their interest to
    11121113join the project. They bring in a laboratory for photo-sensor testing,
     
    11231124\subsection[5.4]{Scientific equipment available (Apparative
    11241125Ausstattung)}
    1125 In Dortmund and W"urzburg extensive computer capacities for data
     1126In Dortmund and W\"{u}rzburg extensive computer capacities for data
    11261127storage as well as for data analysis are available.
    11271128
     
    11321133modern DAQ.
    11331134
    1134 The faculty of physics at the University of W"urzburg comes with a
     1135The faculty of physics at the University of W\"{u}rzburg comes with a
    11351136mechanical and an electronic workshop, as well as a special laboratory
    11361137of the chair for astronomy suitable for photosensor testing.
    11371138
    11381139\subsection[5.5]{The institution's general contribution (Laufende
    1139 Mittel f"ur Sachausgaben)}
     1140Mittel f\"{u}r Sachausgaben)}
    11401141Current total institute budget from the University Dortmund $\approx$
    1141114220.000\,\euro\ per year.\\
    11421143
    1143 Current total institute budget from the University W"urzburg $\approx$
     1144Current total institute budget from the University W\"{u}rzburg $\approx$
    1144114530.000\,\euro\ per year.\\
    11451146
    1146 %\paragraph{5.6 Conflicts of interest in economic activities\\Interessenskonflikte bei wirtschaftlichen Aktivit"aten}~\\
    1147 \subsection[5.6]{Conflicts of interest in economic activities\\Interessenskonflikte bei wirtschaftlichen Aktivit"aten}~\\
     1147%\paragraph{5.6 Conflicts of interest in economic activities\\Interessenskonflikte bei wirtschaftlichen Aktivit\"aten}~\\
     1148\subsection[5.6]{Conflicts of interest in economic activities\\Interessenskonflikte bei wirtschaftlichen Aktivit\"{a}ten}~\\
    11481149none
    11491150
     
    11541155\thispagestyle{empty}
    11551156
    1156 \paragraph{6 Declarations (Erkl"arungen)}
     1157\paragraph{6 Declarations (Erkl\"{a}rungen)}
    11571158
    11581159A request for funding this project has not been submitted to
     
    11611162
    11621163The corresponding persons (Vertrauensdozenten) at the
    1163 Universit"at Dortmund (Prof.\ Dr.\ Gather) and at the Universit"at
    1164 W"urzburg (Prof.\ Dr.\ G.\ Bringmann) have been informed about the
     1164Universit\"{a}t Dortmund (Prof.\ Dr.\ Gather) and at the Universit\"{a}t
     1165W\"{u}rzburg (Prof.\ Dr.\ G.\ Bringmann) have been informed about the
    11651166submission of this proposal.
    11661167
     
    11711172\hfill
    11721173\begin{minipage}[t]{6cm}
    1173 W"urzburg,\\[3.0cm]
     1174W\"{u}rzburg,\\[3.0cm]
    11741175\parbox[t]{6cm}{\hrulefill}\\
    11751176\parbox[t]{6cm}{~\hfill Prof.\ Dr.\ Karl Mannheim\hfill~}\\
     
    11831184
    11841185\newpage
    1185 \section[8]{Verzeichnis der Anlagen/List of appendices}
     1186\paragraph{8 List of appendices (Verzeichnis der Anlagen)}
    11861187
    11871188\begin{itemize}
     
    11891190%Schriftenverzeichnis der Antragsteller seit dem Jahr 2000
    11901191List of refereed publications of the applicants since 2000
    1191 \item
    1192 CV of Karl Mannheim
    1193 \item
    1194 CV of Wolfgang Rhode
     1192\item CV of Karl Mannheim
     1193\item CV of Wolfgang Rhode
     1194\item Letter of Support from the MAGIC collaboration
     1195\item Letter of Support from Mets\"{a}hovi Radio Observatory
     1196\item Letter of Support from the IceCube collaboration
     1197\item Letter of Support from KVA optical telescope
    11951198\end{itemize}
    11961199
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