\documentclass[12pt,openbib]{article} \usepackage{german,graphicx,eurosym,amssymb,amsmath,wasysym,stmaryrd,times,a4wide,wrapfig,exscale,xspace,url,fancyhdr} \usepackage[round]{natbib} %\renewcommand{\familydefault}{\sfdefault} %\usepackage{helvet} \originalTeX \setlength{\parindent}{0pt} %\label{dummy} %cleardoubleplain,liststotoc,bibtotoc,idxtotoc, %\documentclass[a4paper,12pt,oneside,german]{article} %\usepackage[ansinew]{inputenc} \input library.def %\frenchspacing \newcommand{\loi}{\large \textbf{LoI:}\normalsize} \newcommand{\anmerk}[1]{ \marginpar [{\parbox[t]{19.mm}{\footnotesize\sf {#1}} \parbox[t]{2.mm}{\rule[-14.4mm]{1.mm}{17.mm}}}] {\parbox[t]{2.mm}{\rule[-14.4mm]{1.mm}{17.mm}}\parbox[t]{17.mm}{ \footnotesize \sf {#1} } } } %\textwidth17cm %\oddsidemargin-0.5cm %\oddsidemargin-1.cm %\textheight25cm %\topmargin=-1.5cm \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 \thispagestyle{empty} %\begin{figure}[ht] \vspace{2.7cm} \begin{center} \includegraphics*[width=0.496\textwidth,angle=0,clip]{DWARF.eps} \end{center} %\end{figure} \newpage \mbox{} \thispagestyle{empty} \cleardoublepage \newpage \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\,(173)\,284\,79\,10}\\ {\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: +49\,(931)\,404\,81\,90} }\\ {\parbox[t]{1.5cm}{Fax:}+49\,(931)\,888-4603}&\multicolumn{2}{l|}{~}\\\hline\hline \multicolumn{3}{|c|}{{\bf email}: mannheim@astro.uni-wuerzbueg.de}\\\hline \end{tabular} \originalTeX \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 a high performance design for remote operation. The goal is the 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 furthermore trigger follow-up observations of flares with higher sensitivity telescopes such as MAGIC, \mbox{VERITAS} and H.E.S.S. Joint observations with the Whipple monitoring telescope will start a future \mbox{24\,h-monitoring} of selected sources with a distributed network of robotic telescopes. The telescope design is based on a complete technological upgrade of one of the former telescopes of the HEGRA collaboration (CT3) still located at the Observatorio del Roque de los Muchachos on the Canary 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} Das Ziel unseres Vorhabens ist es, ein abbildendes Luft-Cherenkov-Teleskop mit geringen Kosten, aber hoher Leistung f"ur den ferngesteuerten Betrieb aufzubauen. Die Motivation ist die kontinuierliche Langzeitbeobachtung von hellen, nahen Blazaren bei sehr hohen Energien. Mit diesen Beobachtungen werden wir nach bahndynamischen Modulationen suchen, welche von Bin"arsystemen supermassiver schwarzer L"ocher in der emittierten Strahlung hervorgerufen werden. Au"serdem werden die gewonnenen Daten mit den entsprechenden Daten des Neutrinoteleskops IceCube korreliert, um nach Hinweisen f"ur hadroninduzierte Emissionsprozesse zu suchen. Die kontinuierliche "Uberwachung ausgew"ahlter Quellen wird zudem besser aufgel"oste Beobachtungen und Nachbeobachtungen von Strahlungsausbr"uchen durch Teleskope h"oherer Sensitivit"at, wie z.B.\ MAGIC, VERITAS und H.E.S.S., erlauben. Die zeitversetzten, gemeinsamen Beobachtungen zusammen mit dem Whipple-Teleskop stellen den Beginn ununterbrochener Beobachtungen mit einem weltweiten Netzwerk robotischer Teleskope dar. Unser Teleskopdesign basiert auf einer technischen Runderneuerung eines Teleskops der fr"uheren HEGRA-Kollaboration (CT3), welches noch immer am Observatorio del Roque de los Muchachos auf der Kanarischen Insel La Palma (Spanien) steht. Nach dieser Aufr"ustung wird das Teleskop vollst"andig ferngesteuert betrieben werden, eine viel niedrigere Energieschwelle von unter 350\,GeV erreichen und die Beobachtungszeit, um ein gleichstarkes Signal wie mit CT3 zu erhalten, wird um einen Faktor sechs k"urzer sein. \originalTeX \newpage \section[2]{Science case, preliminary work by proposer\\(Stand der Forschung, eigene Vorarbeiten)} \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, micro-quasars, 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 superluminal 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. The development of time-dependent models is currently under investigation 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}. 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). The 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 Telescope 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 Whipple telescope alive. 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 monitor\-ing 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 telescopes, 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, especially important for long-term monitoring, 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 8\,TB/month) has been gained since 2004. 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 allowing for 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{Chirkin:2004}. An energy unfolding method and program has been adapted for IceCube and MAGIC data analysis \citep{Curtef:CM,Muenich:ICRC}. \paragraph{Phenomenology} Both groups 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 KVA optical 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). \mbox{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. It will be setup, under the name DWARF, with an enlarged mirror surface (fig.~\ref{DWARF}), a new camera with higher quantum efficiency and new fast data acquisition system. The energy threshold will be lowered, and the sensitivity of DWARF will be greatly improved compared to HEGRA CT3 (see fig.~\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=0.496\textwidth,angle=0,clip]{CT3.eps} \includegraphics*[width=0.496\textwidth,angle=0,clip]{DWARF.eps} \caption{The old CT3 telescope as operated within the HEGRA System (left) and a photomontage of the revised CT3 telescope with more and hexagonal mirrors (right).} \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 sited difficult to access. 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 considering a maximum observation zenith angle of 65$^\circ$ for all sources which we want to monitor including the Crab Nebula, 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 fig.~\ref{visibility}). For calibration purposes, some time will be scheduled for observations of the Crab \mbox{Nebula}.\\ The blazar observations will allow \begin{itemize} \item to determine the baseline emission, the duty cycle 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 telescopes of the 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 fig.~\ref{schedule}). \begin{figure}[htb] \begin{center} \includegraphics*[width=\textwidth,angle=0,clip]{schedule.eps} \caption{Work schedule for the expected funding period of three years. More details about the work distribution is given in the text.} \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 the 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 W\"{u}rzburg 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 is set up in Dortmund, which allows to finish planning and ordering of parts of the camera, including the PMs, until summer 2008, before the construction begins. 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 the delivery 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 (Crab Nebula). After the commissioning phase will have been finished in spring 2010, complete 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)} Summarizing, the expenses for the telescope are dominated by the camera and data acquisition. We request funding for a total of three years. %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 (3\,x\,TV-L13).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 del 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 serviceable. 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. \begin{figure}[hb] \centering{ %\includegraphics[width=0.605\textwidth]{sensitivity.eps} \includegraphics[width=0.70\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, scaled from the sensitivity of HEGRA~CT1 by the improvements mentioned in the text. } \label{sensitivity} } \end{figure} To achieve the planned sensitivity and threshold (fig.~\ref{sensitivity}), the following components have to be bought. To obtain reliable results as fast as possible well known components have been chosen.\\ {\bf Camera}\dotfill 206.450,-\,\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 (EMI)\hfill 80,-\,\euro\\ High voltage support and control\hfill 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 measurement 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}. To allow for this the source position in Wobble mode should be shifted $0.6^\circ-0.7^\circ$ out of the camera center. A camera completely containing the 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 CT3 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} Therefore a camera with 313 pixel camera (see fig.~\ref{camDWARF}) is chosen. The camera will be built based on the experience with HEGRA and MAGIC. 19\,mm diameter Photomultiplier Tubes (PM, EMI\,9083B/KFLA-UD) will be bought, similar to the HEGRA type (EMI\,9083\,KFLA). They have a quantum efficiency improved by 25\% (see fig.~\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. 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 detectors in the camera of a Cherenkov telescope. The advantages are an extremely high quantum efficiency ($>$50\%), easier gain stabilization and simplified application compared to classical PMs. If these test measurements are successfully finished until 8/2008, we consider to use GAPDs in favor of classical PMs. The design of such a camera would take place at University Dortmund in close collaboration with the experts from ETH. The construction would also take place at the electronics workshop of Dortmund. \end{quote}\vspace{3ex} {\bf Camera support}\dotfill 7.500,-\,\euro\\[-3ex] \begin{quote} For this setup the camera holding has to be redesigned. (1500,-\,\euro) The camera chassis must be water tight and will be equipped with an automatic lid, protecting the PMs at daytime. For further protection, a plexi-glass window will be installed in front of the camera. By coating this window with an anti-reflex layer of magnesium-fluoride, a gain in transmission of 5\% is expected. Each PM will be equipped with a light-guide (Winston cone) as developed by UC Davis and successfully in operation in the MAGIC camera. (3000,-\,\euro\ for all Winston cones). The current design will be improved by using a high reflectivity aluminized Mylar mirror-foil, coated with a dialectical layer ($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 $\sim$15\% in light-collection efficiency compared to the old CT3 system can be achieved. \end{quote}\vspace{3ex} \newpage {\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/IV), 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 making the transfer of the analog signal obsolete. This results in less pick-up noise and reduces the 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-, i.e.\ 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}. Like 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, $>$40\,CPUs). \end{quote}\vspace{3ex} {\bf Mirrors}\dotfill 15.000,-\,\euro\\[-3ex] %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ \begin{quote} The existing mirrors will be replaced by new plastic mirrors currently developed by Wolfgang Dr\"{o}ge's group. The cheap and light-weight material has been formerly used for Winston cones in balloon experiments. The mirrors are copied from a master and coated with a reflecting and a protective material. Tests have given promising results. By a change of the mirror geometry, the mirror area can be increased from 8.5\,m$^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 $SiO_2$ as for the Winston cones. By this, a gain in reflectivity of $\sim10\%$ is achieved, see fig.~\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. %The system %will be provided by ETH Z"urich. %{\bf For a diameter mirror of less than 2.4\,m, the delay between an %parabolic (isochronous) 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 9.650,-\,\euro\\[-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 3.000,-\,\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. For a correction of axis misalignments and possible deformations of the structure (e.g.\ bending of camera holding masts) a pointing correction algorithm will be applied, as used in the MAGIC tracking system. 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, (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. For an accurate tracking a GPS clock is necessary. 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} 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} %%%%%%%%%%%%%% PLOTS HERE???? %%%%%%%%%%%%%%%%%%%%%%%%%% {\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). 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. For the drive system 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. For protection in case of robotic movement a fence 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 341.135,-\,\euro}\hfill\hspace*{0pt}\\[-1ex] \hspace*{0.66\textwidth}\hrulefill\\[-1.9ex] \hspace*{0.66\textwidth}\hrulefill\\ \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 preferred PMs (EMI) together with the predecessor used in CT1. A proper coating \citep{Paneque:2004} will further enhance its efficiency. An even better increase would be the usage of Geiger-mode APDs.} \label{cherenkov} \label{reflectivity} \label{qe} } \end{figure} \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]{Travel expenses (Reisen)} 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 63.000,-\,\euro}\hfill\hspace*{0pt}\\[-1ex] \hspace*{0.66\textwidth}\hrulefill\\[-1.9ex] \hspace*{0.66\textwidth}\hrulefill\\ \subsection[4.5]{Publication costs (Publikationskosten)} 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 (Grundauststattung) \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), Grundauststattung) \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]{Cooperation with other scientists\\(Zusammenarbeit mit anderen Wissenschaftlern)} Both applying groups cooperate 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 good working contacts exist 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 (Universit\`{a} 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 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~ \thispagestyle{empty} \newpage \mbox{} \thispagestyle{empty} \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 Appendix A: Chapter 4 in German \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 \item Email with offer from EMI for the PMs \end{itemize} \newpage \mbox{} \thispagestyle{empty} \newpage \appendix \germanTeX \section[4]{Beantragte Mittel} Die beantragten Mittel werden durch die Ausgaben f"ur die Kamera und die Datennahme dominiert. Wir beantragen eine F"orderung von drei Jahren. \subsection[4.1]{Personalkosten} F"ur diesen Zeitraum beantragen wir die Finanzierung von zwei Postdocs und zwei Doktoranden, jeweils einer in Dortmund und einer in W"urzburg (3\,x\,TV-L13). Mit den besetzten Stellen sollen die erw"ahnten Arbeiten zur Planung und zum Bau des Teleskops durchgef"uhrt werden. Zus"atzlich wird noch eine schwankende Zahl an Doktoranden und Diplomanden zur Verf"ugung stehen. Interessierte Kandidaten sind Dr.\ Thomas Bretz, Dr.\ dest.\ Daniela Dorner, Dr.\ dest.\ Kirsten M\"{u}nich, cand.\ phys.\ Michael Backes, cand.\ phys.\ Daniela Hadasch und cand.\ phys.\ Dominik Neise. \subsection[4.2]{Wissenschaftliche Ger\"{a}te} Am Observatorio del Roque de los Muchachos (ORM), nahe dem MAGIC Teleskop, steht noch das ehemalige HEGRA-Teleskop (CT3) zur Verf"ugung. Es ist noch immer nutzbar und geh"ort jetzt der MAGIC Kollaboration. Au"serdem ist noch ein Container zur Unterbringung von Elektronik, sowie weiterer Platz im MAGIC-eignenen Haus vorhanden. Der Memorandum of Understanding der MAGIC-Kollaboration erlaubt uns den Betrieb des Teleskops als DWARF (siehe Anlage). F"ur Notfallsituationen steht die MAGIC Schichtmannschaft zur Verf"ugung. Um die angestrebte Sensitivit"at und Energieschwelle (Abb.~\ref{sensitivity}) in m"oglichgst kurzer Zeit zu erreichen, wurden die folgenden Komponenten ausgew"ahlt. Einzelheiten zu den Auswahlkriterien k"onnen im Kapitel~4 nachgelesen werden.\\ {\bf Kamera}\dotfill 206.450,-\,\euro\\[-3ex] \begin{quote} F"ur eine Kamera mit 313 Pixel werden folgende Komponenten ben"otigt:\\ \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth} Photomultiplier R"ohre EMI\,9083B\hfill 220,-\,\euro\\ Aktiver Spannungsteiler (EMI)\hfill 80,-\,\euro\\ Hochspannungsversorgung und -kontrolle\hfill 300,-\,\euro\\ Vorverst"arker\hfill 50,-\,\euro\\ Ersatzteile (pauschal)\hfill 3000,-\,\euro\\ \end{minipage}\\[-0.5ex] %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 measurement 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}. To allow for %this the source position in Wobble mode should be shifted %$0.6^\circ-0.7^\circ$ out of the camera center. % %A camera completely containing the 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 $4.5^\circ-5.0^\circ$. % %Therefore a camera with 313 pixel camera (see fig.~\ref{camDWARF}) is %chosen. The camera will be built based on the experience with HEGRA and %MAGIC. 19\,mm diameter Photomultiplier Tubes (PM, EMI\,9083B/KFLA-UD) %will be bought, similar to the HEGRA type (EMI\,9083\,KFLA). They have %a quantum efficiency improved by 25\% (see fig.~\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. % %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 detectors in the camera of a %Cherenkov telescope. The advantages are an extremely high quantum %efficiency ($>$50\%), easier gain stabilization and simplified %application compared to classical PMs. If these test measurements are %successfully finished until 8/2008, we consider to use GAPDs in favor %of classical PMs. The design of such a camera would take place at %University Dortmund in close collaboration with the experts from ETH. %The construction would also take place at the electronics workshop of %Dortmund. \end{quote}\vspace{3ex} \newpage {\bf Kameraaufh"angung und -geh"ause}\dotfill 7.500,-\,\euro\\[-3ex] \begin{quote} %For this setup the camera holding has to be redesigned. (1500,-\,\euro) %The camera chassis must be water tight and will be equipped with an %automatic lid, protecting the PMs at daytime. For further protection, a %plexi-glass window will be installed in front of the camera. By coating %this window with an anti-reflex layer of magnesium-fluoride, a gain in %transmission of 5\% is expected. Each PM will be equipped with a %light-guide (Winston cone) as developed by UC Davis and successfully in %operation in the MAGIC camera. (3000,-\,\euro\ for all Winston cones). The %current design will be improved by using a high reflectivity aluminized %Mylar mirror-foil, coated with a dialectical layer ($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 $\sim$15\% in light-collection %efficiency compared to the old CT3 system can be achieved. \end{quote}%\vspace{1ex} {\bf Datennahme}\dotfill 61.035,-\,\euro\\[-3ex] \begin{quote} 313 Pixel\\ \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth} Auslese\hfill 95,-\,\euro\\ Triggerelektronik\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/IV), 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 making %the transfer of the analog signal obsolete. This results in less %pick-up noise and reduces the 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-, i.e.\ %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. % %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}. % %Like 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, $>$40\,CPUs). \end{quote}\vspace{3ex} {\bf Spiegel}\dotfill 15.000,-\,\euro\\[-3ex] %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ \begin{quote} %The existing mirrors will be replaced by new plastic mirrors currently %developed by Wolfgang Dr\"{o}ge's group. The cheap and light-weight %material has been formerly used for Winston cones in balloon %experiments. The mirrors are copied from a master and coated with a %reflecting and a protective material. Tests have given promising %results. By a change of the mirror geometry, the mirror area can be %increased from 8.5\,m$^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 $SiO_2$ as for %the Winston cones. By this, a gain in reflectivity of $\sim10\%$ is %achieved, see fig.~\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. \end{quote}%\vspace{3ex} {\bf Kalibrationssystem}\dotfill 9.650,-\,\euro\\[-3ex] \begin{quote} Einzelkomponenten\\ \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth} Absolute Lichtkalibration\hfill 2.000,-\,\euro\\ Messung der Triggerrate einzelner Pixel\hfill 3.000,-\,\euro\\ Wetterstation\hfill 500,-\,\euro\\ GPS gesteuerte Uhr\hfill 1.500,-\,\euro\\ CCD Kameras mit Auslese\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. % %For a correction of axis misalignments and possible deformations of the %structure (e.g.\ bending of camera holding masts) a pointing correction %algorithm will be applied, as used in the MAGIC tracking system. 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, (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. % %For an accurate tracking a GPS clock is necessary. 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} Drei 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 Antrieb und Positionsauslese}\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). % %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. % %For the drive system 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 Sicherheit}\dotfill 4.000,-\,\euro\\[-3ex] \begin{quote} \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth} Unterbrechungsfreie Stromversorgung (UPS)\hfill 2.000,-\,\euro\\ Sicherheitszaun\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. % %For protection in case of robotic movement a fence will be %installed.%}\\[2ex] \end{quote}\vspace{3ex} {\bf Andere Ausgaben}\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}{ F"ur den Betrieb in Fernsteuerung werden verschiedene fernbedienbare Komponenten, wie z.B.\ Ethernet steuerbare Steckdosen und "Uberwachungselektronik, gekauft. \end{quote} \hspace*{0.66\textwidth}\hrulefill\\[0.5ex] \hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.2:\hfill{\bf 341.135,-\,\euro}\hfill\hspace*{0pt}\\[-1ex] \hspace*{0.66\textwidth}\hrulefill\\[-1.9ex] \hspace*{0.66\textwidth}\hrulefill\\ \subsection[4.3]{Verbrauchsmaterial} \begin{quote} % \parbox[t]{1em}{~}\begin{minipage}[t]{0.9\textwidth} 10 LTO\,4 B"ander (8\,TB)\dotfill 750,-\,\euro\\ Verbrauchsgegenst"ande (pauschal): Werkzeug und Materialien\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} Die hohen Reisekosten sind in der engen Zusammenarbeit zwischen Dortmund und W"urzburg, sowie den notwendigen Aufenthalten in La Palma begr"undet.\\[-2ex] \begin{quote} %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ Jedes Jahr sollte ein erfahrenes Gruppenmitglied aus Dortmund und W"urzburg den Status des Projektes bei einer internationalen Konferenz vorstellen:\\ 2 x 3\,Jahre x 1.500,-\,\euro\dotfill 9.000,-\,\euro\\[-2ex] Teilnahme am MAGIC Kollaborationstreffen (zweimal j"ahrlich):\\ 2 x 3\,Jahre x 1.000,-\,\euro\dotfill 6.000,-\,\euro\\[-2ex] Austausch von Doktoranden zwischen W\"{u}rzburg and Dortmund:\\ 1\,Student x 1\,Woche x 24 (alle sechs Wochen) x 800,-\,\euro\dotfill 19.200,-\,\euro\\[-2ex] Zum Aufbau des Teleskops vor Ort sind folgende Reisekosten n"otig:\\ 4 x 2\,Wochen auf La Palma x 2\,Personen 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 63.000,-\,\euro}\hfill\hspace*{0pt}\\[-1ex] \hspace*{0.66\textwidth}\hrulefill\\[-1.9ex] \hspace*{0.66\textwidth}\hrulefill\\ \subsection[4.5]{Publikationskosten} Werden von den beantragenden Universit"aten "ubernommen. \subsection[4.6]{Sonstige Kosten} \begin{quote} Euro-Container (zum Versand der Spiegel)\dotfill 5.000,-\,\euro\\ Transport\dotfill 15.000,-\,\euro\\ Abbau (wird von den Antragstellern "ubernommen)\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 \thispagestyle{empty} \mbox{} \newpage \originalTeX %(References of our groups are marked by an asterix *) \bibliography{application} \bibliographystyle{plainnat} %\bibliographystyle{alpha} %\bibliographystyle{plain} \end{document}