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1\documentclass[12pt,openbib]{article}
2\usepackage{german,graphicx,eurosym,amssymb,amsmath,wasysym,stmaryrd,times,a4wide,wrapfig,exscale,xspace,url,fancyhdr}
3\usepackage[round]{natbib}
4
5%\renewcommand{\familydefault}{\sfdefault}
6%\usepackage{helvet}
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8\originalTeX
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12\label{dummy}
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36
37\title{Neuantrag auf Gew\"{a}hrung einer Sachbeihilfe\\Proposal for a new research project}
38\author{Prof.\ Dr.\ Karl\ Mannheim\\Prof.\ Dr.\ Dr.\ Wolfgang Rhode}
39
40\begin{document}
41
42\maketitle
43
44%\tableofcontents
45
46\section[1]{Allgemeine Angaben/General Information}
47
48\subsection[1.1]{Antragsteller/Applicants}
49\germanTeX
50\begin{tabular}{|p{0.44\textwidth}|p{0.22\textwidth}|p{0.22\textwidth}|}\hline
51{\bf Name}&\multicolumn{2}{l|}{\bf Akademischer Grad}\\
52{\sc Rhode, Wolfgang, Prof.~Dr.~Dr.}&\multicolumn{2}{l|}{Universit"atsprofessor (C3)}\\\hline\hline
53{\ }&{\bf Birthday}&{\bf Nationality}\\
54{\ }&Oct 17 1961&German\\\hline
55\multicolumn{3}{|l|}{\bf Institut, Lehrstuhl}\\
56\multicolumn{3}{|l|}{Institut f"ur Physik}\\
57\multicolumn{3}{|l|}{Experimentelle Physik V (Astroteilchenphysik)}\\\hline
58{\bf Address at work }&\multicolumn{2}{l|}{\bf Home address}\\[0.5ex]
59{Universit"at Dortmund }&\multicolumn{2}{l|}{ }\\
60{ }&\multicolumn{2}{l|}{Am Schilken 28 }\\
61{44221 Dortmund }&\multicolumn{2}{l|}{58285 Gevelsberg}\\
62{Germany }&\multicolumn{2}{l|}{Germany }\\[0.5ex]
63{\parbox[t]{1.5cm}{Phone:}+49\,(231)\,755-3550}&\multicolumn{2}{l|}{\parbox[t]{1.5cm}{Phone:}+49\,(931)\, }\\
64{\parbox[t]{1.5cm}{Fax:}+49\,(231)\,755-4547}&\multicolumn{2}{l|}{~}\\\hline\hline
65\multicolumn{3}{|c|}{{\bf email}: wolfgang.rhode@udo.edu}\\\hline
66
67\multicolumn{3}{c}{~}\\[1ex]\hline
68
69{\bf Name}&\multicolumn{2}{l|}{\bf Akademischer Grad}\\
70{\sc Mannheim, Karl, Prof.~Dr.}&\multicolumn{2}{l|}{Universit"atsprofessor (C4)}\\\hline\hline
71{\ }&{\bf Birthday}&{\bf Nationality}\\
72{\ }&Jan 4 1963&German\\\hline
73\multicolumn{3}{|l|}{\bf Institut, Lehrstuhl}\\
74\multicolumn{3}{|l|}{Institut f"ur Theoretische Physik und Astrophysik}\\
75\multicolumn{3}{|l|}{Lehrstuhl f"ur Astronomie}\\\hline
76{\bf Address at work }&\multicolumn{2}{l|}{\bf Home address}\\[0.5ex]
77{Julius-Maximilians-Universit"at}&\multicolumn{2}{l|}{ }\\
78{ }&\multicolumn{2}{l|}{Oswald-Kunzemann-Str. 12}\\
79{97074 W"urzburg }&\multicolumn{2}{l|}{97299 Zell am Main }\\
80{Germany }&\multicolumn{2}{l|}{Germany }\\[0.5ex]
81{\parbox[t]{1.5cm}{Phone:}+49\,(931)\,888-5031}&\multicolumn{2}{l|}{\parbox[t]{1.5cm}{Phone:} }\\
82{\parbox[t]{1.5cm}{Fax:}+49\,(931)\,888-4603}&\multicolumn{2}{l|}{~}\\\hline\hline
83\multicolumn{3}{|c|}{{\bf email}: mannhein@astro.uni-wuerzbueg.de}\\\hline
84\end{tabular}
85\originalTeX
86\newpage
87
88%\paragraph{1.2 Topic}~\\
89\subsection[1.2]{Topic}
90Long-term VHE $\gamma$-ray monitoring of bright blazars with a dedicated Cherenkov telescope
91
92%\paragraph{1.2 Thema}~\\
93\subsection[1.2]{Thema}
94Langzeitbeobachtung von hellen VHE $\gamma$-Blazaren mit einem dedizierten Cherenkov Teleskop
95
96%\paragraph{1.3 Discipline and field of work (Fachgebiet und Arbeitsrichtung)}~\\
97\subsection[1.3]{Discipline and field of work (Fachgebiet und Arbeitsrichtung)}
98Astronomy and Astrophysics, Particle Astrophysics
99
100%\paragraph{\bf 1.4 Scheduled duration in total (Voraussichtliche Gesamtdauer)}~\\
101\subsection[1.4]{Scheduled duration in total (Voraussichtliche Gesamtdauer)}
102After successful completion of the three-year work plan developed in
103this proposal, we will ask for an extension of the project for another
104two years to carry out an observation program centered on the signatures
105of supermassive binary black holes.
106
107%\paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\
108\subsection[1.5]{Application period (Antragszeitraum)}
1093\,years. The work on the project will begin immediately after the
110funding.
111
112\newpage
113%\paragraph{\bf 1.6 Summary}~\\
114\subsection[1.6]{Summary}
115We propose to set up a robotic imaging air Cherenkov telescope with low
116cost, but high performance design for remote operation. The goal is to
117dedicate this gamma-ray telescope to long-term monitoring observations
118of nearby, bright blazars at very high energies. We will (i) search for
119orbital modulation of the blazar emission due to supermassive black
120hole binaries, (ii) study the statistics of flares and their physical
121origin, and (iii) correlate the data with corresponding data from the
122neutrino observatory IceCube to search for evidence of hadronic
123emission processes. The observations will also trigger follow-up
124observations of flares with higher sensitivity telescopes such as
125MAGIC, VERITAS, and H.E.S.S.\ Joint observations with the Whipple
126monitoring telescope will start a future 24\,h-monitoring of selected
127sources with a distributed network of robotic telescopes. The telescope
128design is based on a full technological upgrade of one of the former
129telescopes of the HEGRA collaboration (CT3) still located at the
130Observatorio Roque de los Muchachos on the Canarian Island La Palma
131(Spain). After this upgrade, the telescope will be operated
132robotically, a much lower energy threshold below 350\,GeV will be
133achieved and the observation time required for gaining the same signal
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
140mit geringen Kosten aber hoher Leistung fernsteuerbar in Betrieb zu
141nehmen. Das Ziel ist es, dieses gamma-ray Teleskop ganz der
142Langzeitbeobachtung von nahen, hellen Blazaren bei sehr hohen Energien
143zu widmen. Wir werden (i) nach Modulationen der Blazar-Emission durch
144Bin"arsysteme von supermassiven Schwarzen L"ochern suchen, (ii) die
145Statistik von gamma-Ausbr"uchen und deren physikalischen Ursprung
146untersuchen und (iii) die Daten mit entsprechenden Daten von dem
147Neutrino-Telskop IceCube korrelieren, um Nachweise f"ur hadronische
148Emissionsprozesse zu finden. Die Beobachtungen werden zus"atzlich
149Nachfolgebeobachtungen von gamma-Ausbr"uchen mit h"ohersensitiven
150Teleskopen wie MAGIC, VERITAS und H.E.S.S.\ triggern. Auf einander
151abgestimmte Beobachtungen zusammen mit dem Whipple Teleskop werden der
152Auftakt zu einer zuk"unftigen 24-Stunden-Beobachtung von selektierten
153Quellen mit einem verteilten Netzwerk robotischer Cherenkov-Teleskope
154sein. Das Teleskop-Design basiert auf einem kompletten technologischen
155Upgrade eines der Teleskope der fr"uheren HEGRA-Kollaboration, welches
156noch immer am Observatorio Roque de los Muchachos auf der kanarischen
157Insel La Palma (Spanien) gelegen ist. Nach diesem Upgrade wird das
158Teleskop robotisch betrieben werden und eine wesentlich geringere
159Energieschwelle von unter 350\,GeV aufweisen, w"ahrend gleichzeitig die
160notwendige Beobachtungszeit, um dasselbe Signal wie CT3 zu erhalten, um
161einen Faktor sechs verringert wird.}
162\originalTeX
163\newpage
164
165\section[2]{Stand der Forschung, eigene Vorarbeiten\\Science case, preliminary work by proposer}
166
167\subsection[2.1]{Science case (Stand der Forschung)}
168
169Since the termination of the HEGRA observations, the succeeding
170experiments MAGIC and H.E.S.S. have impressively extended the physical
171scope of gamma ray astronomy detecting tens of formerly unknown gamma
172ray sources and analyzing their energy spectra, morphology, and
173temporal behavior. This became possible by lowering the energy
174threshold from 700\,GeV to less than 100\,GeV and increasing at the same
175time the sensitivity by a factor of five. A diversity of astrophysical
176source types such as pulsar wind nebulae, supernova remnants,
177microquasars, pulsars, radio galaxies, clusters of galaxies, gamma ray
178bursts and blazars have been studied with these telescopes.
179
180The main class of extragalactic, very high energy gamma-rays sources
181detected with imaging air-Cherenkov telescopes are blazars, i.e.\
182accreting supermassive black holes exhibiting a relativistic jet that
183is closely aligned with the line of sight. The non-thermal blazar
184spectrum covers up to 20 orders of magnitude in energy, from
185long-wavelength radio waves to multi-TeV gamma-rays. In addition,
186blazars are characterized by rapid variability, high degrees of
187polarization, and super-luminal motion of knots in their
188high-resolution radio images. The observed behavior can readily be
189explained assuming relativistic bulk motion and in situ particle
190acceleration, e.g. at shock waves, leading to synchrotron
191(radio-to-x-ray) and self-Compton (gamma-ray) emission \citep{Blandford}.
192Additionally, inverse Compton scattering of external photons may play a
193role in producing the observed gamma rays \citep{Dermer,Begelman}.
194Variability may hold the key to understanding the details of the
195emission processes and the source geometry, and the development of
196time-dependent models is currently on the agenda of model builders
197worldwide.
198
199Although particle acceleration inevitably affects electrons and protons
200(ions), the electrons are commonly believed to be responsible for
201producing the observed emission owing to their lower mass and thus much
202stronger energy losses (at the same energy). The relativistic protons,
203which could either originate from the accretion flow or from entrained
204ambient matter, will quickly dominate the momentum flow of the jet.
205This {\em baryon pollution} has been suggested to solve the energy
206transport problem in gamma ray bursts, and is probably present in
207blazar jets as well, even if they originate as pair jets in a black
208hole ergosphere \citep{Meszaros}. Protons and ions accelerated in the
209jets of blazars can reach extremely high energies before energy losses
210become important \citep{Mannheim:1993}. Escaping particles contribute
211to the observed flux of ultrahigh energy cosmic rays in a major way.
212Blazars and their unbeamed hosts, the radio galaxies, are thus the
213prime candidates for origin of ultrahigh energy cosmic rays
214\citep{Rachen}, and this can be investigated with the IceCube and AUGER
215experiments. Recent results of the AUGER experiment show a significant
216anisotropy of the highest energy cosmic rays and point at either nearby
217AGN or sources with a similar spacial distribution as their origin
218\citep{AUGER-AGN}.
219
220In some flares, a large ratio of the gamma-ray to optical luminosity is
221observed. This is difficult to reconcile with the primary leptonic
222origin of the emission, since the accelerated electron pressure would
223largely exceed the magnetic field pressure. For shock acceleration to
224work efficiently, particles must be confined by the magnetic field for
225a time longer than the cooling time. The problem vanishes in the
226following model: Photo-hadronic interactions of accelerated protons and
227synchrotron photons induce electromagnetic cascades, which in turn
228produce secondary electrons causing high energy synchrotron
229gamma-radiation. This demands much stronger magnetic fields in line
230with magnetic confinement \citep{Mannheim:1995}. Short variability time
231scales can result from dynamical changes of the emission zone, running
232e.g. through an inhomogeneous environment.
233
234The contemporaneous spectral energy distributions for hadronic and
235leptonic models bear many similarities, but also marked differences,
236such as multiple bumps which are possible even in a one-zone hadronic
237model \citep{Mannheim:1999}. These properties allow conclusions
238about the accelerated particles. Noteworthy, even for nearby blazars
239the spectrum must be corrected for attenuation of the gamma rays due to
240pair production in collisions with low-energy photons from the
241extragalactic background radiation field \citep{Kneiske}.
242Ultimately, the hadronic origin of the emission must be probed with
243correlated gamma-ray and neutrino observations, since the pion decay
244initiating the cascades involves a fixed ratio of electron-positron
245pairs, gamma-rays, and neutrinos. A dedicated monitoring campaign
246jointly with IceCube has the best chance for success. Pilot studies
247done with MAGIC and IceCube indicate that the investigation of neutrino
248event triggered gamma-ray observations are statistically
249inconclusive \citep{Leier:2006}.
250
251The variability time scale of blazars ranges from minutes to months,
252generally showing the largest amplitudes and the shortest time scales
253at the highest energies. Recently, a doubling time scale of two minutes
254has been observed in a flare of Mrk\,501 with the MAGIC
255telescope \citep{Albert:501}. A giant flare of PKS\,2155-304 discovered by
256H.E.S.S.\ \citep{Aharonian:2007pks} has shown similarly short
257doubling time scales and a flux of up to 16 times the flux of the Crab
258Nebula. Indications for TeV flares without evidence for an accompanying
259x-ray flare, coined orphan flares, have been observed, questioning the
260synchrotron-self-Compton mechanism being responsible for the
261gamma-rays. Model ramifications involving several emission components,
262external seed photons, or hadronically induced emission may solve the
263problem \citep{Blazejowski}. Certainly, the database for contemporaneous
264multi-wavelength observations is still far from proving the
265synchrotron-self-Compton model.
266
267Generally, observations of flares are prompted by optical or x-ray
268alerts, leading to a strong selection bias. The variability presumably
269reflects the non-steady feeding of the jets and the changing interplay
270between particle acceleration and cooling. In this situation,
271perturbations of the electron density or the bulk plasma velocity are
272traveling down the jet. The variability could also reflect the changing
273conditions of the external medium to which the jet flow adapts during
274its passage through it. In fact, a clumpy, highly inhomogeneous
275external medium is typical for active galactic nuclei, as indicated by
276their clumpy emission line regions, if visible against the
277Doppler-enhanced blazar emission. Often the jets bend with a large
278angle indicating shocks resulting from reflections off intervening
279high-density clouds. Changes in the direction of the jet flow lead to
280large flux variations due to differential Doppler boosting.
281
282Helical trajectories, as seen in high-resolution radio maps resulting
283from the orbital modulation of the jet base in supermassive black hole
284binaries, would lead to periodic variability on time scales of months
285to years \citep{Rieger:2007}. Binaries are expected to be the most
286common outcome of the repeated mergers of galaxies which have
287originally built up the blazar host galaxy. Each progenitor galaxy
288brings its own supermassive black hole as expected from the
289Magorrian-Kormendy relations. It is subject to stellar dynamical
290evolution in the core of the merger galaxy, of which only one pair of
291black holes is expected to survive near the center of gravity.
292Supermassive black hole binaries close to coalescence are thus expected
293to be generic in blazars. Angular momentum transport by collective
294stellar dynamical processes is efficient to bring them to distances
295close to where the emission of gravitational waves begins to dominate
296their further evolution until coalescence. Their expected gravitational
297wave luminosity is spectacularly high, even long before final
298coalescence and the frequencies are favorable for the detectors under
299consideration (LISA). Detection of gravitational waves relies on exact
300templates to filter out the signals and the templates can be computed
301from astrophysical constraints on the orbits and masses of the black
302holes. TeV gamma-rays, showing the shortest variability time scales,
303probe deepest into the jet and are thus the most sensitive probe of the
304orbital modulation at the jet base. Relativistic aberration is helpful
305in bringing down the observed periods to below the time scale of years.
306A tentative hint for a 23-day periodicity of the TeV emission from
307Mrk\,501 during a phase of high activity in 1997 was reported by
308HEGRA \citep{Kranich}, and was later confirmed including x-ray and
309Teleacope Array data \citep{Osone}. The observations can be explained in
310a supermassive black hole binary scenario \citep{Rieger:2000}.
311Indications for helical trajectories and periodic modulation of optical
312and radio lightcurves on time scales of tens of years have also been
313described in the literature (e.g. \cite{Hong,Merrit}).
314
315To overcome the limitations of biased sampling, a complete monitoring
316database for a few representative bright sources needs to be obtained.
317Space missions with all-sky observations at lower photon energies, such
318as GLAST, GRIPS, or eROSITA, will provide significant multi-wavelength
319exposure simultaneous to the VHE observations, and this is a new
320qualitative step for blazar research. For the same reasons, the VERITAS
321Collaboration keeps the former Whipple telescope alive, albeit its
322performance seems to have strongly degraded. It is obvious that the
323large Cherenkov telescopes such as MAGIC, H.E.S.S.\ or VERITAS are mainly
324used to discover new sources at the sensitivity limit. Thus they will
325not perform monitoring observations of bright sources with complete
326sampling during their visibility. However, these telescopes will be
327triggered by monitoring telescopes and thus improve the described
328investigations. In turn, operating a smaller but robotic telescope is
329an essential and cost-effective contribution to the plans for
330next-generation instruments in ground-based gamma-ray astronomy.
331Know-how for the operation of future networks of robotic Cherenkov
332telescopes, e.g. a monitoring array around the globe or a single-place
333array like CTA, is certainly needed given the high operating shift
334demands of the current installations.
335
336In summary, there are strong reasons to make an effort for the
337continuous monitoring of the few exceptionally bright blazars. This can
338be achieved by operating a dedicated monitoring telescope of the
339HEGRA-type, referred to in the following as DWARF (Dedicated
340multiWavelength Agn Research Facility). Its robotic design will keep
341the demands on personal and infrastructure on the low side, rendering
342it compatible with the resources of University groups. The approach is
343also optimal to educate students in the strongly expanding field of
344astroparticle physics.
345
346Assuming conservatively the performance of a single HEGRA-type
347telescope, long-term monitoring of at least the following known blazars
348is possible: Mrk\,421, Mrk\,501, 1ES\,2344+514, 1ES\,1959+650,
349H\,1426+428, PKS\,2155-304. We emphasize that DWARF will run as a
350facility dedicated to these targets only, providing a maximum
351observation time for the program. Utilizing recent developments, such
352as improvements of the light collection efficiency due to an improved
353mirror reflectivity and a better PM quantum efficiency, a 30\%
354improvement in sensitivity and a lower energy-threshold is reasonable.
355Current studies show that with a good timing resolution (2\,GHz) a
356further 40\% increase in sensitivity (compared to a 300\,MHz system) is
357feasible. Together with an extended mirror area and a large camera, a
358sensitivity improvement compared to a single HEGRA telescope of a
359factor of 2.5 and an energy threshold below 350\,GeV is possible.
360
361\subsection[2.2]{Preliminary work by proposers (Eigene Vorarbeiten)}
362
363From the experience with the construction, operation and data analysis
364of Amanda, IceCube, HEGRA and MAGIC the proposing groups contribute the
365necessary knowledge and experience to build and operate a small imaging
366air Cherenkov telescope.
367
368\paragraph{Hardware}
369
370The Dortmund group is working on experimental and phenomenological
371astroparticle physics. In the past, the following hardware components
372were successfully developed: a Flash-ADC based DAQ (TWR, transient
373waveform recorder), currently in operation for data acquisition in the
374AMANDA subdetector within the IceCube telescope \citep{Wagner:PhD}, an
375online software Trigger for the TWR-DAQ system \citep{Messarius:PhD},
376online data compression mechanisms (TWR DAQ) \citep{Refflinghaus:Dipl},
377monitoring software for the TWR-DAQ-data \citep{Dreyer:Dipl} and
378in-ice-HV-power-supply for IceCube. This development was done with the
379companies CAEN, Pisa, Italy and Iseg, Rossendorf, Germany. The HV
380modules were long time tested under different temperature conditions
381connected to operating photomultipliers \citep{Bartelt:Dipl}. Prototypes
382for the scintillator counters of the planned Air Shower Array {\em
383SkyView} were developed and operated for two years \citep{Deeg:Dipl}.
384Members of the group (engineers) were involved in the fast trigger
385development for H1 and are involved in the FPGA-programming for the
386LHCb data read out. The group may further use the well equipped
387mechanical and electronic workshops in Dortmund and the electronic
388development departure of the faculty.
389
390The ultra fast drive system of the MAGIC telscopes, suitable for fast
391repositioning in case of Gamma-Ray Bursts, has been developed,
392commissioned and programmed by the W\"{u}rzburg group
393\citep{Bretz:2003drive,Bretz:2005drive}. To correct for axis
394misalignments and possible deformations of the structure (e.g.\ bending
395of camera holding masts), a pointing correction algorithm was developed
396\citep{Dorner:Diploma}. Its calibration is done by measurement of the
397reflection of bright guide stars on the camera surface and ensures a
398pointing accuracy well below the pixel diameter. Hardware and software
399(CCD readout, image processing and pointing correction algorithms) have
400also been developed and are in operation successfully since more than
401three years \citep{Riegel:2005icrc2}.
402
403Mirror structures made of plastic material have been developed as
404Winston Cones for balloon flight experiments previously by the group of
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
407this setup, HPDs for future improvement of the sensitivity of the MAGIC
408camera are investigated.
409
410\paragraph{Software}
411
412The W\"{u}rzburg group has developed a full MAGIC analysis package,
413flexible and modular enough to easily process DWARF data
414\citep{Bretz:2005paris,Riegel:2005icrc,Bretz:2005mars}. A method for
415absolute light calibration of the PMs based on Muon images has been
416adapted and further improved for the MAGIC telescope
417\citep{Meyer:Diploma,Goebel:2005}. Both, data analysis and Monte Carlo
418production, have been fully automatized, such that both can run with
419sparse user interaction \citep{Dorner:2005icrc}. The analysis was
420developed to be powerful and as robust as possible to be best suited
421for automatic processing \citep{Dorner:2005paris}. Experience with
422large amount of data (up to 15\,TB/month) has been gained over five
423years now. The datacenter is equipped with a professional multi-stage
424(hierarchical) storage system. Two operators are paid by the physics
425faculty. Currently efforts in W\"{u}rzburg and Dortmund are ongoing to
426turn the old inflexible Monte Carlo programs, used by the MAGIC
427collaboration, into modular packages which allows easy simulation of
428other setups. Experience with Monte Carlo simulations, especially
429CORSIKA, is contributed by the Dortmund group, which has actively
430implemented changes into the CORSIKA program, such as an extension to
431large zenith angles, prompt meson production and a new atmospheric
432model \citep{Haffke:Dipl,Schroeder:PhD} for the local atmosphere of La
433Palma. Furthermore the group has developed high precision Monte Carlos
434for Lepton propagation in different media \citep{hepph0407075}. An
435energy unfolding method and program has been adapted for IceCube and
436MAGIC data analysis \citep{Curtef:CM,Muenich:ICRC}.
437
438\paragraph{Phenomenology}
439
440Both groups further have experience with source models and theoretical
441computations of gamma ray and neutrino spectra expected from blazars.
442The relation between the two messengers is a prime focus of interest.
443Experience with corresponding multi-messenger data analyses involving
444MAGIC and IceCube data is available in the Dortmund group. Research
445activities are also related with relativistic particle acceleration
446\citep{Meli} and gamma ray attenuation \citep{Kneiske}. The W\"{u}rzburg
447group has organized and carried out multi-wavelength observations of
448bright blazars involving MAGIC, Suzaku, the IRAM telescopes, and the
449optical KVA telescope \citep{Ruegamer}. Signatures of supermassive
450black hole binaries, which are most relevant also for gravitational
451wave detectors, are investigated jointly with the German LISA
452consortium (Burkart, Elbracht ongoing research, funded by DLR).
453Secondary gamma rays due to dark matter annihilation events are
454investigated both from their particle physics and astrophysics aspects.
455Another main focus of research is on models of radiation and particle
456acceleration processes in blazar jets (hadronic and leptonic models),
457leading to predictions of correlated neutrino emission \citep{Rueger}.
458This includes simulations of particle acceleration due to the Weibel
459instability \citep{Burkart}. Much of this research at W\"{u}rzburg is
460carried out in the context of the research training school GRK\,1147
461{\em Theoretical Astrophysics and Particle Physics}.
462
463\section[3]{Goals and Work Schedule (Ziele und Arbeitsprogramm)}
464
465\subsection[3.1]{Goals (Ziele)}
466
467The aim of the project is to put the former CT3 of the HEGRA
468collaboration on the Roque de los Muchachos back into operation - with
469an enlarged mirror surface, a new camera with higher quantum
470efficiency, and new fast data acquisition system, under the name of
471DWARF. The energy threshold will be lowered, and the sensitivity of
472DWARF will be greatly improved compared to HEGRA CT3 (see
473figure~\ref{sensitivity}). Commissioning and the first year of data taking
474should be carried out within the three years of the requested funding
475period.
476
477\begin{figure}[ht]
478\begin{center}
479 \includegraphics*[width=0.495\textwidth,angle=0,clip]{CT3.eps}
480 \includegraphics*[width=0.495\textwidth,angle=0,clip]{DWARF.eps}
481 \caption{Left: The old HEGRA CT3 telescope as operated within the
482 HEGRA Sytem. Right: A photomontage how the revised CT3 telescope
483 could look like with more and hexagonal mirrors.}
484\label{CT3}
485\label{DWARF}
486\end{center}
487\end{figure}
488
489The telescope will be operated robotically to reduce costs and man
490power demands. Furthermore, we seek to obtain know-how for the
491operation of future networks of robotic Cherenkov telescopes (e.g. a
492monitoring array around the globe or CTA) or telescopes at inaccessible
493sites. From the experience with the construction and operation of MAGIC
494or HEGRA, the proposing groups consider the planned focused approach
495(small number of experienced scientists) as optimal for achieving the
496project goals. The available automatic analysis package developed by
497the W\"{u}rzburg group for MAGIC is modular and flexible, and can thus be
498used with minor changes for the DWARF project.
499
500\begin{figure}[htb]
501\begin{center}
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. }
507\label{visibility}
508\end{center}
509\end{figure}
510
511The scientific focus of the project will be on the long-term monitoring
512of bright, nearby VHE emitting blazars. At least one of the proposed
513targets will be visible any time of the year (see figure~\ref{visibility}). For
514calibration purposes, some time will be scheduled for observations of
515the Crab nebula. The blazar observations will allow
516\begin{itemize}
517\item to determine the duty cycle, the baseline emission, and the power
518spectrum of flux variations.
519\item to cooperate with the Whipple monitoring telescope for an
520extended time coverage.
521\item to prompt Target-of-Opportunity (ToO) observations with MAGIC in
522the case of flares increasing time resolution. Corresponding
523ToO proposals to H.E.S.S.\ and Veritas are in
524preparation.
525\item to observe simultaneously with MAGIC which will provide an
526extended bandwidth from below 100\,GeV to multi-TeV energies.
527\item to obtain multi-frequency observations together with the
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.
532\end{itemize}
533
534Interpretation of the data will yield crucial information about
535\begin{itemize}
536\item the nature of the emission processes going on in relativistic
537jets. We plan to interpret the data with models currently developed in
538the context of the Research Training Group {\em Theoretical
539Astrophysics} in W\"{u}rzburg (Graduiertenkolleg, GK\,1147), including
540particle-in-cell and hybrid MHD models.
541\item the black hole mass and accretion rate fitting the data with
542emission models. Results will be compared with estimates of the black
543hole mass from the Magorrian relation.
544\item the flux of relativistic protons (ions) by correlating the rate
545of neutrinos detected with the neutrino telescope IceCube and the rate
546of gamma ray photons detected with DWARF, and thus the rate of escaping
547cosmic rays.
548\item the orbital modulation owing to a supermassive binary black hole.
549Constraints on the binary system will allow to compute most accurate
550templates of gravitational waves, which is a connected project at
551W\"{u}rzburg in the German LISA consortium funded by DLR.
552\end{itemize}
553
554\subsection[3.2]{Work schedule (Arbeitsprogramm)}
555
556To complete the mount to a functional Cherenkov telescope within a
557period of one year, the following steps are necessary:
558
559The work schedule assumes that the work will begin in January 2008,
560immediately after funding. Later funding would accordingly shift the
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}
573
574\paragraph{Software}
575\begin{itemize}
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.
579\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.
580\end{itemize}
581
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.
585\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.
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.
587
588Based on the experience with setting up the MAGIC telescope we estimate
589this workschedule as conservative.
590
591\subsection[3.3]{Experiments with humans (Untersuchungen am Menschen)}
592none
593\subsection[3.4]{Experiments with animals (Tierversuche)}
594none
595\subsection[3.5]{Experiments with recombinant DNA (Gentechnologische Experimente)}
596none
597
598\clearpage
599
600\section[4]{Funds requested (Beantragte Mittel)}
601
602We request funding for a total of three years. Summarizing, the
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)}
609
610For this period, we request funding for two postdocs and two PhD
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.
615
616Suitable candidates interested in these positions are Dr.\ Thomas
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,
624the mount of the former HEGRA telescope CT3 now owned by the MAGIC
625collaboration is still operational. One hut for electronics close to
626the telescope is available. Additional space is available in the MAGIC
627counting house. The MAGIC Memorandum of Understanding allows for
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.
636\begin{figure}[hb]
637\centering{
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} }
645\end{figure}
646\clearpage
647{\bf Camera}\dotfill 207.550,-\,\euro\\[-3ex]
648\begin{quote}
649 To setup a camera with 313 pixels the following components are needed:\\
650 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
651 Photomultiplier Tube EMI\,9083 KFLA-UD\hfill 220,-\,\euro\\
652 Active voltage divider ({\bf !!!!})\hfill 80,-\,\euro\\
653 High voltage support and control\hfill {\bf 300,-}\,\euro\\
654 Preamplifier\hfill 50,-\,\euro\\
655 Spare parts (overall)\hfill 3000,-\,\euro\\
656 \end{minipage}\\[-0.5ex]
657%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
658For long-term observations, the stability of the camera is a major
659criterion. To keep the systematic errors small, a good background
660estimation is mandatory. The only possibility for a synchronous
661determination of the background is the determination from the night-sky
662observed in the same field-of-view with the same instrument. To achieve
663this, the observed position is moved out of the camera center which
664allows the estimation of the background from positions symmetric with
665respect to the camera center (so called wobble-mode). This observation
666mode increases the sensitivity by a factor of $\sqrt{2}$,
667because spending observation time for dedicated background observations
668becomes obsolete, i.e.\ observation time for the source is doubled. This
669ensures in addition a better time coverage of the observed sources.
670
671A further increase in sensitivity can be achieved by better background
672statistics from not only one but several independent positions for the
673background estimation in the camera \citep{Lessard:2001}. For wobble mode
674observations allowing for this, the source position should be shifted
675$0.6^\circ-0.7^\circ$ out of the camera center.
676%}
677
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]
685\begin{center}
686 \includegraphics*[width=0.495\textwidth,angle=0,clip]{cam271.eps}
687 \includegraphics*[width=0.495\textwidth,angle=0,clip]{cam313.eps}
688 \caption{Left: Schematic picture of the 271 pixel CT-3 camera with a field of view of 4.6$^\circ$.
689 Right: Schematic picture of the 313 pixel camera for DWARF with a field of view of 5$^\circ$.}
690\label{camCT3}
691\label{camDWARF}
692\end{center}
693\end{figure}
694
695Therefor a camera with 313 pixel camera (see figure~\ref{camDWARF}) is
696chosen. The camera will be built based on the experience with HEGRA and
697MAGIC. 19\,mm diameter Photomultiplier Tubes (PM, EMI\,9083\,KFLA-UD)
698will be bought, similar to the HEGRA type (EMI\,9083\,KFLA). They have
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.
705
706All possibilities of borrowing one of the old HEGRA cameras for a
707transition time have been probed and refused by the owners of the
708cameras.
709
710{\bf At ETH~Z\"{u}rich currently test measurements are ongoing to prove the
711ability, i.e.\ stability, aging, quantum efficiency, etc., of using
712Geiger-mode APDs (GAPD) as photon
713detector in the camera of a Cherenkov telescope. The advantages are
714extremely high quantum efficiency ($>$50\%), easier gain stabilization and
715simplified application compared to classical PMs. If these test
716measurements are successfully finished until 8/2008 we consider to use
717GAPDs in favor of classical PMs. The design of such a camera would take
718place at University Dortmund in close collaboration with the experts
719from ETH. Construction would also take place at the electronics
720workshop of Dortmund.}
721
722\end{quote}\vspace{3ex}
723
724{\bf Camera support}\dotfill 204.000,-\,\euro\\[-3ex]
725\begin{quote}
726For this setup the camera holding has to be redesigned. (1500,-\,\euro)
727The camera chassis must be water tight and will be equipped with an
728automatic lid protecting the PMs at day-time. For further protection, a
729plexi-glass window will be installed in front of the camera. By coating
730this window with an anti-reflex layer of magnesium-fluoride, a gain in
731transmission of {\bf 5\%} is expected. Each PM will be equipped with a
732light-guide (Winston Cone) as developed by UC Davis and successfully in
733operation in the MAGIC camera. (3000,-\,\euro\ for all winston cones). The
734current design will be improved by using a high reflectivity aluminized
735Mylar mirror-foil, coated with a dialectical layer ($Si\,O_2$
736alternated with Niobium Oxide), to reach a reflectivity in the order of
737{\bf 98\%}. An electric and optical shielding of the individual PMs is
738planned.
739
740In total a gain of {\bf $\sim$15\%} in light-collection
741efficiency compared to the old CT3 system can be acheived.
742\end{quote}\vspace{3ex}
743
744{\bf Data acquisition}\dotfill 61.035,-\,\euro\\[-3ex]
745\begin{quote}
746313 pixels a\\
747 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
748 Readout\hfill 95,-\,\euro\\
749 Trigger\hfill 100,-\,\euro\\
750 \end{minipage}\\[-0.5ex]
751%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
752For the data acquisition system a hardware readout based on an analog
753ring buffer (Domino\ II/III), currently developed for the MAGIC\ II
754readout, will be used \citep{Barcelo}. This technology allows to sample
755the pulses with high frequencies and readout several channels with a
756single Flash-ADC resulting in low costs. The low power consumption will
757allow to include the digitization near the signal source which makes
758the transfer of the analog signal obsolete. The advantage is less
759pick-up noise and less signal dispersion. By high sampling rates
760(1.2\,GHz), additional information about the pulse shape can be
761obtained. This increases the over-all sensitivity further, because the
762short integration time allows for almost perfect suppression of noise
763due to night-sky background photons. The estimated trigger- (readout-)
764rate of the telescope is below 100\,Hz (HEGRA: $<$10\,Hz) which allows
765to use a low-cost industrial solution for readout of the system like
766USB\,2.0.
767
768%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
769Current results obtained with the new 2\,GHz FADC system in the MAGIC
770data acquisition show that for a single telescope a sensitivity
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, $>$40\,CPUs).
782\end{quote}\vspace{3ex}
783
784{\bf Mirrors}\dotfill 15.000,-\,\euro\\[-3ex]
785%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
786\begin{quote}
787The existing mirrors are replaced by new plastic mirrors which are
788currently developed by Wolfgang Dr\"{o}ge's group. The cheap and
789light-weight material has been formerly used for Winston cones in
790balloon experiments. The mirrors are copied from a master coated with a
791reflecting and a protective material. Tests have given promising
792results. By a change of the mirror geometry, the mirror area can be
793increased from 8.5\,m$^2$ to 13\,m$^2$ (see picture~\ref{CT3} and
794montage~\ref{DWARF}); this includes an increase of $\sim$10$\%$ per
795mirror by using a hexagonal layout instead of a round one. A further
796increase of the mirror area would require a reconstruction of parts of
797the mount and will therefore be considered only in a later phase of the
798experiment.
799
800If the current development of the plastic mirrors cannot be finished in
801time, a re-machining of the old glass mirrors (8.5\,m$^2$) is possible
802with high purity aluminum and quartz coating.
803
804In both cases the mirrors can be coated with the same high reflectivity
805aluminized Mylar mirror-foil, and a dialectical layer of SiO2 as for
806the Winston Cones. By this, a gain in reflectivity of $\sim10\%$ is
807achieved, see figure~\ref{reflectivity} \citep{Fraunhofer}.
808
809Both solutions would require the same expenses.
810
811To keep track of the alignment, reflectivity and optical quality of the
812individual mirrors and the point-spread function of the total mirror
813during long-term observations, the application of an automatic mirror
814adjustment system, as developed by ETH~Z\"{u}rich and successfully
815operated 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
837%<grey>The system
838%will be provided by ETH Z"urich.</grey>
839
840%{\bf For a diameter mirror of less than 2.4\,m, the delay between an
841%parabolic (isochronus) and a spherical mirror shape at the edge is well
842%below 1ns (see figure). Thus for a sampling rate of 1.2\,GHz parabolic
843%individual mirrors are not needed. Due to their small size the
844%individual mirrors can have a spherical shape.}
845%}\\[2ex]
846\end{quote}\vspace{3ex}
847
848{\bf Calibration System}\dotfill 6.650,-\,\euro+IPR?\\[-3ex]
849\begin{quote}
850Components\\
851 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
852 Absolute light calibration\hfill 2.000,-\,\euro\\
853 Individual pixel rate control\hfill ???,-\,\euro\\
854 Weather station\hfill 500,-\,\euro\\
855 GPS clock\hfill 1.500,-\,\euro\\
856 CCD cameras with readout\hfill 2.650,-\,\euro\\
857 \end{minipage}\\[-0.5ex]
858%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
859For the absolute light calibration (gain-calibration) of the PMs a
860calibration box as successfully used in the MAGIC telescope will be
861produced.
862
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.
866
867To correct for axis misalignments and possible deformations of the
868structure (e.g.\ bending of camera holding masts), a pointing correction
869algorithm as used in the MAGIC tracking system will be applied. It is
870calibrated by measurements of the reflection of bright guide stars on
871the camera surface and ensures a pointing accuracy well below the pixel
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.
875
876A second identical CCD camera for online monitoring (starguider) will
877be bought.
878
879A GPS clock is necessary for an accurate tracking. The weather station
880helps judging the data quality.
881%}\\[2ex]
882\end{quote}\vspace{3ex}
883
884
885{\bf Computing}\dotfill 12.000,-\,\euro\\[-3ex]
886\begin{quote}
887 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
888 On-site\hfill 12.000,-\,\euro\\
889 Three PCs\hfill 8.000,-\,\euro\\
890 SATA RAID 3TB\hfill 4.000,-\,\euro\\
891 \end{minipage}\\[-0.5ex]
892%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
893For on-site computing three standard PCs are needed ($\sim$8.000,-\,\euro).
894This includes readout and storage, preprocessing and telescope control.
895For safety reasons, a firewall is mandatory. For local cache-storage
896and backup, two RAID\,5 SATA disk arrays with one Terabyte capacity
897each will fulfill the requirement ($\sim$4.000,-\,\euro). The data will be
898transmitted as soon as possible after data taking via Internet to the
899W\"{u}rzburg Datacenter. Enough storage capacity and computing power
900is available there and already reserved for this purpose.
901
902Monte Carlo production and storage will take place at University
903Dortmund.%}\\[2ex]
904\end{quote}\vspace{3ex}
905
906{\bf Mount and Drive}\dotfill 17.500,-\,\euro\\[-3ex]
907\begin{quote}
908%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
909The present mount is used. Only a smaller investment for safety,
910corrosion protection, cable ducts, etc. is needed (7.500,-\,\euro).
911
912For the movement, motors, shaft encoders and control electronics in the
913order of 10.000,-\,\euro\ have to be bought. The costs have been estimated
914with the experience from building the MAGIC drive systems. The DWARF
915drive system should allow for relatively fast repositioning for three
916reasons: (i)~Fast movement might be mandatory for future ToO
917observations. (ii)~Wobble-mode observations will be done changing the
918wobble-position continuously (each 20\,min) for symmetry reasons. (iii)~To
919ensure good time coverage of more than one source visible at the same
920time, the observed source will be changed in constant time intervals
921($\sim$20\,min).
922
923Therefore three 150\,Watt servo motors are intended to be bought. A
924micro-controller based motion control unit (Siemens SPS L\,20) similar to
925the one of the current MAGIC~II drive system will be used. For
926communication with the readout-system, a standard ethernet connection
927based on the TCP/IP- and UDP-protocol will be setup.
928%}\\[2ex]
929\end{quote}\vspace{3ex}
930
931{\bf Security}\dotfill 4.000,-\,\euro\\[-3ex]
932\begin{quote}
933 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
934 Uninterruptable power-supply (UPS)\hfill 2.000,-\,\euro\\
935 Security fence\hfill 2.000,-\,\euro\\
936 \end{minipage}\\[-0.5ex]
937%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
938A UPS with 5\,kW-10\,kW will be
939installed to protect the equipment against power cuts and ensure a safe
940telescope position at the time of sunrise.
941
942A fence for protection in case of robotic movement will be
943installed.%}\\[2ex]
944\end{quote}\vspace{3ex}
945
946{\bf Other expenses}\dotfill 7.500,-\,\euro\\[-3ex]
947\begin{quote}
948%\parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth}
949% Robotics\hfill 7.500,-\,\euro\\
950% \end{minipage}\\[-0.5ex]
951%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
952For remote, robotic operation a variety of remote controllable electronic
953components such as ethernet controlled sockets and switches will be
954bought. Monitoring equipment, for example different kind of sensors, is
955also mandatory.%}\\[2ex]
956\end{quote}
957\hspace*{0.66\textwidth}\hrulefill\\[0.5ex]
958\hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.2:\hfill{\bf
959342.235,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]
960\hspace*{0.66\textwidth}\hrulefill\\[-1.9ex]
961\hspace*{0.66\textwidth}\hrulefill\\
962
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]
982
983\begin{quote}
984%\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
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]
996
997For setup of the telescope at La Palma the following travel expenses
998are necessary:\\
9994 x 2\,weeks at La Palma x 2\,persons x 1.800,-\,\euro\dotfill
100028.800,-\,\euro
1001%}
1002\end{quote}
1003
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)}
1012Will be covered by the proposing institutes.
1013
1014
1015\subsection[4.6]{Other costs (Sonstige Kosten)}
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}
1031none
1032
1033\subsection[5.1]{The research team (Zusammensetzung der Arbeitsgruppe)}
1034
1035\paragraph{Dortmund}
1036\begin{itemize}
1037\setlength{\itemsep}{0pt}
1038\setlength{\parsep}{0pt}
1039\item Prof.\ Dr.\ Dr.\ Wolfgang Rhode (Grundausttattung)
1040\item Dr.\ Tanja Kneiske (Postdoc (Ph"anomenologie), DFG-Forschungsstipendium)
1041\item Dr.\ Julia Becker (Postdoc (Ph"anomenologie), Drittmittel)
1042\item Dipl.-Phys.\ Kirsten M"unich (Doktorand (IceCube), Drittmittel)
1043\item Dipl.-Phys.\ Jens Dreyer (Doktorand (IceCube), Grundausttattung)
1044\item M.Sc.\ Valentin Curtef (Doktorand (MAGIC), Grundausstattung)
1045\item cand.\ phys.\ Michael Backes (Diplomand (MAGIC), zum F"orderbeginn diplomiert)
1046\item cand.\ phys.\ Daniela Hadasch (Diplomand (MAGIC))
1047\item cand.\ phys.\ Anne Wiedemann (Diplomand (IceCube))
1048\item cand.\ phys.\ Dominik Neise (Diplomand (MAGIC))
1049\item Dipl.-Ing.\ Kai Warda (Elektronik)
1050\item PTA Matthias Domke (Systemadministration)
1051\end{itemize}
1052
1053\paragraph{W\"{u}rzburg}
1054\begin{itemize}
1055\setlength{\itemsep}{0pt}
1056\setlength{\parsep}{0pt}
1057\item Prof.\ Dr.\ Karl Mannheim (Landesmittel)
1058\item Prof.\ Dr.\ Thomas Trefzger (Landesmittel)
1059\item Prof.\ Dr.\ Wolfgang Dr"oge (Landesmittel)
1060\item Dr.\ Thomas Bretz (Postdoc (MAGIC), BMBF)
1061\item Dr.\ Felix Spanier (Postdoc, Landesmittel)
1062\item Dipl.-Phys.\ Jordi Albert (Doktorand, DFG-GRK1147)
1063\item Dipl.-Phys.\ Karsten Berger (Doktorand (MAGIC), Landesmittel)
1064\item Dipl.-Phys.\ Thomas Burkart (Doktorand (LISA), DLR)
1065\item Dipl.-Phys.\ Oliver Elbracht (Doktorand, Elitenetzwerk Bayern)
1066\item Dipl.-Phys.\ Dominik Els"asser (Doktorand, Elitenetzwerk Bayern)
1067\item Dipl.-Phys.\ Daniela Dorner (Doktorand (MAGIC), BMBF)
1068\item Dipl.-Phys.\ Daniel H"ohne (Doktorand (MAGIC), Landesmittel)
1069\item Dipl.-Phys.\ Markus Meyer (Doktorand, DFG-GRK1147)
1070\item M.Sc.\ Surajit Paul (Doktorand, DFG-GRK1147)
1071\item Dipl.-Phys.\ Stefan R"ugamer (Doktorand (MAGIC), Landesmittel)
1072\item Dipl.-Phys.\ Michael R"uger (Doktorand, Elitenetzwerk Bayern)
1073\item Dipl.-Phys.\ Martina Wei"s (Doktorand, Elitenetzwerk Bayern)
1074\item cand.\ phys.\ Sebastian Huber
1075\item cand.\ phys.\ Tobias Hein
1076\item cand.\ phys.\ Tobias Viering
1077\end{itemize}
1078\originalTeX
1079
1080\subsection[5.2]{Co-operation with other scientists (Zusammenarbeit mit
1081anderen Wissenschaftlern)}
1082
1083Both applying groups co-operate with the international
1084MAGIC-Collaboration and the institutes represented therein. (W\"{u}rzburg
1085funded by the BMBF, Dortmund by means of appointment for the moment).
1086
1087W\"{u}rzburg is also in close scientific exchange with the group of
1088Prof.~Dr.~Victoria Fonseca, UCM Madrid and the University of Turku
1089(Finland) operating the KVA optical telescope at La Palma. Other
1090cooperations refer to the projects JEM-EUSO (science case), GRIPS
1091(simulation), LISA (astrophysical input for templates), STEREO (data
1092analysis), and SOLAR ORBITER (electron-proton telescope). A cooperation
1093with GLAST science team members (Dr.~Anita and Dr.~Olaf Reimer,
1094Stanford) is also relevant for the proposed project.
1095
1096The group in Dortmund is involved in the IceCube experiment (BMBF
1097funding) and maintains close contacts to the collaboration partners.
1098Moreover on the field of phenomenology there do exist good working
1099contacts to the groups of Prof.~Dr.~Reinhard Schlickeiser,
1100Ruhr-Universit\"{a}t Bochum and Prof.~Dr.~Peter Biermann, MPIfR Bonn.
1101There are furthermore intense contacts to Prof.~Dr.~Francis Halzen,
1102Madison, Wisconsin.
1103
1104The telescope design will be worked out in close cooperation with the
1105group of Prof.~Dr.~Felicitas Pauss, Dr.~Adrian Biland and
1106Prof.~Dr.~Eckart Lorenz (ETH~Z\"{u}rich). They will provide help in design
1107studies, construction and software development. The DAQ design will be
1108contributed by the group of Prof.~Dr.~Riccardo Paoletti (Università di
1109Siena and INFN sez.\ di Pisa, Italy).
1110
1111The group of the newly appointed {\em Lehrstuhl f\"{u}r Physik und Ihre
1112Didaktik} (Prof.~Dr.~Thomas Trefzger) has expressed their interest to
1113join the project. They bring in a laboratory for photo-sensor testing,
1114know-how from former contributions to ATLAS and a joint interest in
1115operating a data pipeline using GRID technologies.
1116
1117\subsection[5.3]{Work outside Germany, Cooperation with foreign
1118partners (Arbeiten im Ausland, Kooperation mit Partnern im Ausland)}
1119
1120The work on DWARF will take place at the ORM on the Spanish island La
1121Palma. It will be performed in close collaboration with the
1122MAGIC-Collaboration.
1123
1124\subsection[5.4]{Scientific equipment available (Apparative
1125Ausstattung)}
1126In Dortmund and W\"{u}rzburg extensive computer capacities for data
1127storage as well as for data analysis are available.
1128
1129The faculty of physics at the University of Dortmund has modern
1130equipped mechanical and electrical workshops including a department for
1131development of electronics at its command. The chair of astroparticle
1132physics possesses common technical equipment required for constructing
1133modern DAQ.
1134
1135The faculty of physics at the University of W\"{u}rzburg comes with a
1136mechanical and an electronic workshop, as well as a special laboratory
1137of the chair for astronomy suitable for photosensor testing.
1138
1139\subsection[5.5]{The institution's general contribution (Laufende
1140Mittel f\"{u}r Sachausgaben)}
1141Current total institute budget from the University Dortmund $\approx$
114220.000\,\euro\ per year.\\
1143
1144Current total institute budget from the University W\"{u}rzburg $\approx$
114530.000\,\euro\ per year.\\
1146
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}~\\
1149none
1150
1151\subsection[5.7]{Other requirements (Sonstige Voraussetzungen)}~\\
1152none
1153
1154\newpage
1155\thispagestyle{empty}
1156
1157\paragraph{6 Declarations (Erkl\"{a}rungen)}
1158
1159A request for funding this project has not been submitted to
1160any other addressee. In case we submit such a request we will inform
1161the Deutsche Forschungsgemeinschaft immediately. \\
1162
1163The corresponding persons (Vertrauensdozenten) at 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
1166submission of this proposal.
1167
1168\paragraph{7 Signatures (Unterschriften)}~\\
1169
1170\vspace{2.5 cm}
1171
1172\hfill
1173\begin{minipage}[t]{6cm}
1174W\"{u}rzburg,\\[3.0cm]
1175\parbox[t]{6cm}{\hrulefill}\\
1176\parbox[t]{6cm}{~\hfill Prof.\ Dr.\ Karl Mannheim\hfill~}\\
1177\end{minipage}
1178\hfill
1179\begin{minipage}[t]{6cm}
1180Dortmund,\\[3.0cm]
1181\parbox[t]{6cm}{\hrulefill}\\
1182\parbox[t]{6cm}{~\hfill Prof.\ Dr.\ Dr.\ Wolfgang Rhode\hfill~}\\
1183\end{minipage}\hfill~
1184
1185\newpage
1186\paragraph{8 List of appendices (Verzeichnis der Anlagen)}
1187
1188\begin{itemize}
1189\item
1190%Schriftenverzeichnis der Antragsteller seit dem Jahr 2000
1191List of refereed publications of the applicants since 2000
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
1198\end{itemize}
1199
1200\newpage
1201%\section{References}
1202
1203(References of our groups are marked by an asterix *)
1204\bibliography{application}
1205\bibliographystyle{plainnat}
1206%\bibliographystyle{alpha}
1207%\bibliographystyle{plain}
1208
1209\end{document}
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