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}
|
---|
7 |
|
---|
8 | \originalTeX
|
---|
9 |
|
---|
10 | \setlength{\parindent}{0pt}
|
---|
11 |
|
---|
12 | \label{dummy}
|
---|
13 |
|
---|
14 | %cleardoubleplain,liststotoc,bibtotoc,idxtotoc,
|
---|
15 |
|
---|
16 | %\documentclass[a4paper,12pt,oneside,german]{article}
|
---|
17 | %\usepackage[ansinew]{inputenc}
|
---|
18 |
|
---|
19 | \input library.def
|
---|
20 |
|
---|
21 | \frenchspacing
|
---|
22 |
|
---|
23 | \newcommand{\loi}{\large \textbf{LoI:}\normalsize}
|
---|
24 | \newcommand{\anmerk}[1]{ \marginpar
|
---|
25 | [{\parbox[t]{19.mm}{\footnotesize\sf {#1}}
|
---|
26 | \parbox[t]{2.mm}{\rule[-14.4mm]{1.mm}{17.mm}}}]
|
---|
27 | {\parbox[t]{2.mm}{\rule[-14.4mm]{1.mm}{17.mm}}\parbox[t]{17.mm}{
|
---|
28 | \footnotesize \sf {#1} } } }
|
---|
29 |
|
---|
30 |
|
---|
31 | %\textwidth17cm
|
---|
32 | %\oddsidemargin-0.5cm
|
---|
33 | %\oddsidemargin-1.cm
|
---|
34 | %\textheight25cm
|
---|
35 | %\topmargin=-1.5cm
|
---|
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}
|
---|
90 | Long-term VHE $\gamma$-ray monitoring of bright blazars with a dedicated Cherenkov telescope
|
---|
91 |
|
---|
92 | %\paragraph{1.2 Thema}~\\
|
---|
93 | \subsection[1.2]{Thema}
|
---|
94 | Langzeitbeobachtung 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)}
|
---|
98 | Astronomy 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)}
|
---|
102 | After successful completion of the three-year work plan developed in
|
---|
103 | this proposal, we will ask for an extension of the project for another
|
---|
104 | two years to carry out an observation program centered on the signatures
|
---|
105 | of supermassive binary black holes.
|
---|
106 |
|
---|
107 | %\paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\
|
---|
108 | \subsection[1.5]{Application period (Antragszeitraum)}
|
---|
109 | 3\,years. The work on the project will begin immediately after the
|
---|
110 | funding.
|
---|
111 |
|
---|
112 | \newpage
|
---|
113 | %\paragraph{\bf 1.6 Summary}~\\
|
---|
114 | \subsection[1.6]{Summary}
|
---|
115 | We propose to set up a robotic imaging air Cherenkov telescope with low
|
---|
116 | cost, but high performance design for remote operation. The goal is to
|
---|
117 | dedicate this gamma-ray telescope to long-term monitoring observations
|
---|
118 | of nearby, bright blazars at very high energies. We will (i) search for
|
---|
119 | orbital modulation of the blazar emission due to supermassive black
|
---|
120 | hole binaries, (ii) study the statistics of flares and their physical
|
---|
121 | origin, and (iii) correlate the data with corresponding data from the
|
---|
122 | neutrino observatory IceCube to search for evidence of hadronic
|
---|
123 | emission processes. The observations will also trigger follow-up
|
---|
124 | observations of flares with higher sensitivity telescopes such as
|
---|
125 | MAGIC, VERITAS, and H.E.S.S.\ Joint observations with the Whipple
|
---|
126 | monitoring telescope will start a future 24\,h-monitoring of selected
|
---|
127 | sources with a distributed network of robotic telescopes. The telescope
|
---|
128 | design is based on a full technological upgrade of one of the former
|
---|
129 | telescopes of the HEGRA collaboration (CT3) still located at the
|
---|
130 | Observatorio Roque de los Muchachos on the Canarian Island La Palma
|
---|
131 | (Spain). After this upgrade, the telescope will be operated
|
---|
132 | robotically, a much lower energy threshold below 350\,GeV will be
|
---|
133 | achieved and the observation time required for gaining the same signal
|
---|
134 | as 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
|
---|
140 | mit geringen Kosten aber hoher Leistung fernsteuerbar in Betrieb zu
|
---|
141 | nehmen. Das Ziel ist es, dieses gamma-ray Teleskop ganz der
|
---|
142 | Langzeitbeobachtung von nahen, hellen Blazaren bei sehr hohen Energien
|
---|
143 | zu widmen. Wir werden (i) nach Modulationen der Blazar-Emission durch
|
---|
144 | Bin"arsysteme von supermassiven Schwarzen L"ochern suchen, (ii) die
|
---|
145 | Statistik von gamma-Ausbr"uchen und deren physikalischen Ursprung
|
---|
146 | untersuchen und (iii) die Daten mit entsprechenden Daten von dem
|
---|
147 | Neutrino-Telskop IceCube korrelieren, um Nachweise f"ur hadronische
|
---|
148 | Emissionsprozesse zu finden. Die Beobachtungen werden zus"atzlich
|
---|
149 | Nachfolgebeobachtungen von gamma-Ausbr"uchen mit h"ohersensitiven
|
---|
150 | Teleskopen wie MAGIC, VERITAS und H.E.S.S.\ triggern. Auf einander
|
---|
151 | abgestimmte Beobachtungen zusammen mit dem Whipple Teleskop werden der
|
---|
152 | Auftakt zu einer zuk"unftigen 24-Stunden-Beobachtung von selektierten
|
---|
153 | Quellen mit einem verteilten Netzwerk robotischer Cherenkov-Teleskope
|
---|
154 | sein. Das Teleskop-Design basiert auf einem kompletten technologischen
|
---|
155 | Upgrade eines der Teleskope der fr"uheren HEGRA-Kollaboration, welches
|
---|
156 | noch immer am Observatorio Roque de los Muchachos auf der kanarischen
|
---|
157 | Insel La Palma (Spanien) gelegen ist. Nach diesem Upgrade wird das
|
---|
158 | Teleskop robotisch betrieben werden und eine wesentlich geringere
|
---|
159 | Energieschwelle von unter 350\,GeV aufweisen, w"ahrend gleichzeitig die
|
---|
160 | notwendige Beobachtungszeit, um dasselbe Signal wie CT3 zu erhalten, um
|
---|
161 | einen 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 |
|
---|
169 | Since the termination of the HEGRA observations, the succeeding
|
---|
170 | experiments MAGIC and H.E.S.S. have impressively extended the physical
|
---|
171 | scope of gamma ray astronomy detecting tens of formerly unknown gamma
|
---|
172 | ray sources and analyzing their energy spectra, morphology, and
|
---|
173 | temporal behavior. This became possible by lowering the energy
|
---|
174 | threshold from 700\,GeV to less than 100\,GeV and increasing at the same
|
---|
175 | time the sensitivity by a factor of five. A diversity of astrophysical
|
---|
176 | source types such as pulsar wind nebulae, supernova remnants,
|
---|
177 | microquasars, pulsars, radio galaxies, clusters of galaxies, gamma ray
|
---|
178 | bursts and blazars have been studied with these telescopes.
|
---|
179 |
|
---|
180 | The main class of extragalactic, very high energy gamma-rays sources
|
---|
181 | detected with imaging air-Cherenkov telescopes are blazars, i.e.\
|
---|
182 | accreting supermassive black holes exhibiting a relativistic jet that
|
---|
183 | is closely aligned with the line of sight. The non-thermal blazar
|
---|
184 | spectrum covers up to 20 orders of magnitude in energy, from
|
---|
185 | long-wavelength radio waves to multi-TeV gamma-rays. In addition,
|
---|
186 | blazars are characterized by rapid variability, high degrees of
|
---|
187 | polarization, and super-luminal motion of knots in their
|
---|
188 | high-resolution radio images. The observed behavior can readily be
|
---|
189 | explained assuming relativistic bulk motion and in situ particle
|
---|
190 | acceleration, e.g. at shock waves, leading to synchrotron
|
---|
191 | (radio-to-x-ray) and self-Compton (gamma-ray) emission \citep{Blandford}.
|
---|
192 | Additionally, inverse Compton scattering of external photons may play a
|
---|
193 | role in producing the observed gamma rays \citep{Dermer,Begelman}.
|
---|
194 | Variability may hold the key to understanding the details of the
|
---|
195 | emission processes and the source geometry, and the development of
|
---|
196 | time-dependent models is currently on the agenda of model builders
|
---|
197 | worldwide.
|
---|
198 |
|
---|
199 | Although particle acceleration inevitably affects electrons and protons
|
---|
200 | (ions), the electrons are commonly believed to be responsible for
|
---|
201 | producing the observed emission owing to their lower mass and thus much
|
---|
202 | stronger energy losses (at the same energy). The relativistic protons,
|
---|
203 | which could either originate from the accretion flow or from entrained
|
---|
204 | ambient matter, will quickly dominate the momentum flow of the jet.
|
---|
205 | This {\em baryon pollution} has been suggested to solve the energy
|
---|
206 | transport problem in gamma ray bursts, and is probably present in
|
---|
207 | blazar jets as well, even if they originate as pair jets in a black
|
---|
208 | hole ergosphere \citep{Meszaros}. Protons and ions accelerated in the
|
---|
209 | jets of blazars can reach extremely high energies before energy losses
|
---|
210 | become important \citep{Mannheim:1993}. Escaping particles contribute
|
---|
211 | to the observed flux of ultrahigh energy cosmic rays in a major way.
|
---|
212 | Blazars and their unbeamed hosts, the radio galaxies, are thus the
|
---|
213 | prime candidates for origin of ultrahigh energy cosmic rays
|
---|
214 | \citep{Rachen}, and this can be investigated with the IceCube and AUGER
|
---|
215 | experiments. Recent results of the AUGER experiment show a significant
|
---|
216 | anisotropy of the highest energy cosmic rays and point at either nearby
|
---|
217 | AGN or sources with a similar spacial distribution as their origin
|
---|
218 | \citep{AUGER-AGN}.
|
---|
219 |
|
---|
220 | In some flares, a large ratio of the gamma-ray to optical luminosity is
|
---|
221 | observed. This is difficult to reconcile with the primary leptonic
|
---|
222 | origin of the emission, since the accelerated electron pressure would
|
---|
223 | largely exceed the magnetic field pressure. For shock acceleration to
|
---|
224 | work efficiently, particles must be confined by the magnetic field for
|
---|
225 | a time longer than the cooling time. The problem vanishes in the
|
---|
226 | following model: Photo-hadronic interactions of accelerated protons and
|
---|
227 | synchrotron photons induce electromagnetic cascades, which in turn
|
---|
228 | produce secondary electrons causing high energy synchrotron
|
---|
229 | gamma-radiation. This demands much stronger magnetic fields in line
|
---|
230 | with magnetic confinement \citep{Mannheim:1995}. Short variability time
|
---|
231 | scales can result from dynamical changes of the emission zone, running
|
---|
232 | e.g. through an inhomogeneous environment.
|
---|
233 |
|
---|
234 | The contemporaneous spectral energy distributions for hadronic and
|
---|
235 | leptonic models bear many similarities, but also marked differences,
|
---|
236 | such as multiple bumps which are possible even in a one-zone hadronic
|
---|
237 | model \citep{Mannheim:1999}. These properties allow conclusions
|
---|
238 | about the accelerated particles. Noteworthy, even for nearby blazars
|
---|
239 | the spectrum must be corrected for attenuation of the gamma rays due to
|
---|
240 | pair production in collisions with low-energy photons from the
|
---|
241 | extragalactic background radiation field \citep{Kneiske}.
|
---|
242 | Ultimately, the hadronic origin of the emission must be probed with
|
---|
243 | correlated gamma-ray and neutrino observations, since the pion decay
|
---|
244 | initiating the cascades involves a fixed ratio of electron-positron
|
---|
245 | pairs, gamma-rays, and neutrinos. A dedicated monitoring campaign
|
---|
246 | jointly with IceCube has the best chance for success. Pilot studies
|
---|
247 | done with MAGIC and IceCube indicate that the investigation of neutrino
|
---|
248 | event triggered gamma-ray observations are statistically
|
---|
249 | inconclusive \citep{Leier:2006}.
|
---|
250 |
|
---|
251 | The variability time scale of blazars ranges from minutes to months,
|
---|
252 | generally showing the largest amplitudes and the shortest time scales
|
---|
253 | at the highest energies. Recently, a doubling time scale of two minutes
|
---|
254 | has been observed in a flare of Mrk\,501 with the MAGIC
|
---|
255 | telescope \citep{Albert:501}. A giant flare of PKS\,2155-304 discovered by
|
---|
256 | H.E.S.S.\ \citep{Aharonian:2007pks} has shown similarly short
|
---|
257 | doubling time scales and a flux of up to 16 times the flux of the Crab
|
---|
258 | Nebula. Indications for TeV flares without evidence for an accompanying
|
---|
259 | x-ray flare, coined orphan flares, have been observed, questioning the
|
---|
260 | synchrotron-self-Compton mechanism being responsible for the
|
---|
261 | gamma-rays. Model ramifications involving several emission components,
|
---|
262 | external seed photons, or hadronically induced emission may solve the
|
---|
263 | problem \citep{Blazejowski}. Certainly, the database for contemporaneous
|
---|
264 | multi-wavelength observations is still far from proving the
|
---|
265 | synchrotron-self-Compton model.
|
---|
266 |
|
---|
267 | Generally, observations of flares are prompted by optical or x-ray
|
---|
268 | alerts, leading to a strong selection bias. The variability presumably
|
---|
269 | reflects the non-steady feeding of the jets and the changing interplay
|
---|
270 | between particle acceleration and cooling. In this situation,
|
---|
271 | perturbations of the electron density or the bulk plasma velocity are
|
---|
272 | traveling down the jet. The variability could also reflect the changing
|
---|
273 | conditions of the external medium to which the jet flow adapts during
|
---|
274 | its passage through it. In fact, a clumpy, highly inhomogeneous
|
---|
275 | external medium is typical for active galactic nuclei, as indicated by
|
---|
276 | their clumpy emission line regions, if visible against the
|
---|
277 | Doppler-enhanced blazar emission. Often the jets bend with a large
|
---|
278 | angle indicating shocks resulting from reflections off intervening
|
---|
279 | high-density clouds. Changes in the direction of the jet flow lead to
|
---|
280 | large flux variations due to differential Doppler boosting.
|
---|
281 |
|
---|
282 | Helical trajectories, as seen in high-resolution radio maps resulting
|
---|
283 | from the orbital modulation of the jet base in supermassive black hole
|
---|
284 | binaries, would lead to periodic variability on time scales of months
|
---|
285 | to years \citep{Rieger:2007}. Binaries are expected to be the most
|
---|
286 | common outcome of the repeated mergers of galaxies which have
|
---|
287 | originally built up the blazar host galaxy. Each progenitor galaxy
|
---|
288 | brings its own supermassive black hole as expected from the
|
---|
289 | Magorrian-Kormendy relations. It is subject to stellar dynamical
|
---|
290 | evolution in the core of the merger galaxy, of which only one pair of
|
---|
291 | black holes is expected to survive near the center of gravity.
|
---|
292 | Supermassive black hole binaries close to coalescence are thus expected
|
---|
293 | to be generic in blazars. Angular momentum transport by collective
|
---|
294 | stellar dynamical processes is efficient to bring them to distances
|
---|
295 | close to where the emission of gravitational waves begins to dominate
|
---|
296 | their further evolution until coalescence. Their expected gravitational
|
---|
297 | wave luminosity is spectacularly high, even long before final
|
---|
298 | coalescence and the frequencies are favorable for the detectors under
|
---|
299 | consideration (LISA). Detection of gravitational waves relies on exact
|
---|
300 | templates to filter out the signals and the templates can be computed
|
---|
301 | from astrophysical constraints on the orbits and masses of the black
|
---|
302 | holes. TeV gamma-rays, showing the shortest variability time scales,
|
---|
303 | probe deepest into the jet and are thus the most sensitive probe of the
|
---|
304 | orbital modulation at the jet base. Relativistic aberration is helpful
|
---|
305 | in bringing down the observed periods to below the time scale of years.
|
---|
306 | A tentative hint for a 23-day periodicity of the TeV emission from
|
---|
307 | Mrk\,501 during a phase of high activity in 1997 was reported by
|
---|
308 | HEGRA \citep{Kranich}, and was later confirmed including x-ray and
|
---|
309 | Teleacope Array data \citep{Osone}. The observations can be explained in
|
---|
310 | a supermassive black hole binary scenario \citep{Rieger:2000}.
|
---|
311 | Indications for helical trajectories and periodic modulation of optical
|
---|
312 | and radio lightcurves on time scales of tens of years have also been
|
---|
313 | described in the literature (e.g. \cite{Hong,Merrit}).
|
---|
314 |
|
---|
315 | To overcome the limitations of biased sampling, a complete monitoring
|
---|
316 | database for a few representative bright sources needs to be obtained.
|
---|
317 | Space missions with all-sky observations at lower photon energies, such
|
---|
318 | as GLAST, GRIPS, or eROSITA, will provide significant multi-wavelength
|
---|
319 | exposure simultaneous to the VHE observations, and this is a new
|
---|
320 | qualitative step for blazar research. For the same reasons, the VERITAS
|
---|
321 | Collaboration keeps the former Whipple telescope alive, albeit its
|
---|
322 | performance seems to have strongly degraded. It is obvious that the
|
---|
323 | large Cherenkov telescopes such as MAGIC, H.E.S.S.\ or VERITAS are mainly
|
---|
324 | used to discover new sources at the sensitivity limit. Thus they will
|
---|
325 | not perform monitoring observations of bright sources with complete
|
---|
326 | sampling during their visibility. However, these telescopes will be
|
---|
327 | triggered by monitoring telescopes and thus improve the described
|
---|
328 | investigations. In turn, operating a smaller but robotic telescope is
|
---|
329 | an essential and cost-effective contribution to the plans for
|
---|
330 | next-generation instruments in ground-based gamma-ray astronomy.
|
---|
331 | Know-how for the operation of future networks of robotic Cherenkov
|
---|
332 | telescopes, e.g. a monitoring array around the globe or a single-place
|
---|
333 | array like CTA, is certainly needed given the high operating shift
|
---|
334 | demands of the current installations.
|
---|
335 |
|
---|
336 | In summary, there are strong reasons to make an effort for the
|
---|
337 | continuous monitoring of the few exceptionally bright blazars. This can
|
---|
338 | be achieved by operating a dedicated monitoring telescope of the
|
---|
339 | HEGRA-type, referred to in the following as DWARF (Dedicated
|
---|
340 | multiWavelength Agn Research Facility). Its robotic design will keep
|
---|
341 | the demands on personal and infrastructure on the low side, rendering
|
---|
342 | it compatible with the resources of University groups. The approach is
|
---|
343 | also optimal to educate students in the strongly expanding field of
|
---|
344 | astroparticle physics.
|
---|
345 |
|
---|
346 | Assuming conservatively the performance of a single HEGRA-type
|
---|
347 | telescope, long-term monitoring of at least the following known blazars
|
---|
348 | is possible: Mrk\,421, Mrk\,501, 1ES\,2344+514, 1ES\,1959+650,
|
---|
349 | H\,1426+428, PKS\,2155-304. We emphasize that DWARF will run as a
|
---|
350 | facility dedicated to these targets only, providing a maximum
|
---|
351 | observation time for the program. Utilizing recent developments, such
|
---|
352 | as improvements of the light collection efficiency due to an improved
|
---|
353 | mirror reflectivity and a better PM quantum efficiency, a 30\%
|
---|
354 | improvement in sensitivity and a lower energy-threshold is reasonable.
|
---|
355 | Current studies show that with a good timing resolution (2\,GHz) a
|
---|
356 | further 40\% increase in sensitivity (compared to a 300\,MHz system) is
|
---|
357 | feasible. Together with an extended mirror area and a large camera, a
|
---|
358 | sensitivity improvement compared to a single HEGRA telescope of a
|
---|
359 | factor of 2.5 and an energy threshold below 350\,GeV is possible.
|
---|
360 |
|
---|
361 | \subsection[2.2]{Preliminary work by proposers (Eigene Vorarbeiten)}
|
---|
362 |
|
---|
363 | From the experience with the construction, operation and data analysis
|
---|
364 | of Amanda, IceCube, HEGRA and MAGIC the proposing groups contribute the
|
---|
365 | necessary knowledge and experience to build and operate a small imaging
|
---|
366 | air Cherenkov telescope.
|
---|
367 |
|
---|
368 | \paragraph{Hardware}
|
---|
369 |
|
---|
370 | The Dortmund group is working on experimental and phenomenological
|
---|
371 | astroparticle physics. In the past, the following hardware components
|
---|
372 | were successfully developed: a Flash-ADC based DAQ (TWR, transient
|
---|
373 | waveform recorder), currently in operation for data acquisition in the
|
---|
374 | AMANDA subdetector within the IceCube telescope \citep{Wagner:PhD}, an
|
---|
375 | online software Trigger for the TWR-DAQ system \citep{Messarius:PhD},
|
---|
376 | online data compression mechanisms (TWR DAQ) \citep{Refflinghaus:Dipl},
|
---|
377 | monitoring software for the TWR-DAQ-data \citep{Dreyer:Dipl} and
|
---|
378 | in-ice-HV-power-supply for IceCube. This development was done with the
|
---|
379 | companies CAEN, Pisa, Italy and Iseg, Rossendorf, Germany. The HV
|
---|
380 | modules were long time tested under different temperature conditions
|
---|
381 | connected to operating photomultipliers \citep{Bartelt:Dipl}. Prototypes
|
---|
382 | for the scintillator counters of the planned Air Shower Array {\em
|
---|
383 | SkyView} were developed and operated for two years \citep{Deeg:Dipl}.
|
---|
384 | Members of the group (engineers) were involved in the fast trigger
|
---|
385 | development for H1 and are involved in the FPGA-programming for the
|
---|
386 | LHCb data read out. The group may further use the well equipped
|
---|
387 | mechanical and electronic workshops in Dortmund and the electronic
|
---|
388 | development departure of the faculty.
|
---|
389 |
|
---|
390 | The ultra fast drive system of the MAGIC telscopes, suitable for fast
|
---|
391 | repositioning in case of Gamma-Ray Bursts, has been developed,
|
---|
392 | commissioned and programmed by the W\"{u}rzburg group
|
---|
393 | \citep{Bretz:2003drive,Bretz:2005drive}. To correct for axis
|
---|
394 | misalignments and possible deformations of the structure (e.g.\ bending
|
---|
395 | of camera holding masts), a pointing correction algorithm was developed
|
---|
396 | \citep{Dorner:Diploma}. Its calibration is done by measurement of the
|
---|
397 | reflection of bright guide stars on the camera surface and ensures a
|
---|
398 | pointing accuracy well below the pixel diameter. Hardware and software
|
---|
399 | (CCD readout, image processing and pointing correction algorithms) have
|
---|
400 | also been developed and are in operation successfully since more than
|
---|
401 | three years \citep{Riegel:2005icrc2}.
|
---|
402 |
|
---|
403 | Mirror structures made of plastic material have been developed as
|
---|
404 | Winston Cones for balloon flight experiments previously by the group of
|
---|
405 | Wolfgang Dr\"{o}ge. W\"{u}rzburg has also participated in the development of
|
---|
406 | a HPD test bench, which has been setup in Munich and W\"{u}rzburg. With
|
---|
407 | this setup, HPDs for future improvement of the sensitivity of the MAGIC
|
---|
408 | camera are investigated.
|
---|
409 |
|
---|
410 | \paragraph{Software}
|
---|
411 |
|
---|
412 | The W\"{u}rzburg group has developed a full MAGIC analysis package,
|
---|
413 | flexible and modular enough to easily process DWARF data
|
---|
414 | \citep{Bretz:2005paris,Riegel:2005icrc,Bretz:2005mars}. A method for
|
---|
415 | absolute light calibration of the PMs based on Muon images has been
|
---|
416 | adapted and further improved for the MAGIC telescope
|
---|
417 | \citep{Meyer:Diploma,Goebel:2005}. Both, data analysis and Monte Carlo
|
---|
418 | production, have been fully automatized, such that both can run with
|
---|
419 | sparse user interaction \citep{Dorner:2005icrc}. The analysis was
|
---|
420 | developed to be powerful and as robust as possible to be best suited
|
---|
421 | for automatic processing \citep{Dorner:2005paris}. Experience with
|
---|
422 | large amount of data (up to 15\,TB/month) has been gained over five
|
---|
423 | years now. The datacenter is equipped with a professional multi-stage
|
---|
424 | (hierarchical) storage system. Two operators are paid by the physics
|
---|
425 | faculty. Currently efforts in W\"{u}rzburg and Dortmund are ongoing to
|
---|
426 | turn the old inflexible Monte Carlo programs, used by the MAGIC
|
---|
427 | collaboration, into modular packages which allows easy simulation of
|
---|
428 | other setups. Experience with Monte Carlo simulations, especially
|
---|
429 | CORSIKA, is contributed by the Dortmund group, which has actively
|
---|
430 | implemented changes into the CORSIKA program, such as an extension to
|
---|
431 | large zenith angles, prompt meson production and a new atmospheric
|
---|
432 | model \citep{Haffke:Dipl,Schroeder:PhD} for the local atmosphere of La
|
---|
433 | Palma. Furthermore the group has developed high precision Monte Carlos
|
---|
434 | for Lepton propagation in different media \citep{hepph0407075}. An
|
---|
435 | energy unfolding method and program has been adapted for IceCube and
|
---|
436 | MAGIC data analysis \citep{Curtef:CM,Muenich:ICRC}.
|
---|
437 |
|
---|
438 | \paragraph{Phenomenology}
|
---|
439 |
|
---|
440 | Both groups further have experience with source models and theoretical
|
---|
441 | computations of gamma ray and neutrino spectra expected from blazars.
|
---|
442 | The relation between the two messengers is a prime focus of interest.
|
---|
443 | Experience with corresponding multi-messenger data analyses involving
|
---|
444 | MAGIC and IceCube data is available in the Dortmund group. Research
|
---|
445 | activities are also related with relativistic particle acceleration
|
---|
446 | \citep{Meli} and gamma ray attenuation \citep{Kneiske}. The W\"{u}rzburg
|
---|
447 | group has organized and carried out multi-wavelength observations of
|
---|
448 | bright blazars involving MAGIC, Suzaku, the IRAM telescopes, and the
|
---|
449 | optical KVA telescope \citep{Ruegamer}. Signatures of supermassive
|
---|
450 | black hole binaries, which are most relevant also for gravitational
|
---|
451 | wave detectors, are investigated jointly with the German LISA
|
---|
452 | consortium (Burkart, Elbracht ongoing research, funded by DLR).
|
---|
453 | Secondary gamma rays due to dark matter annihilation events are
|
---|
454 | investigated both from their particle physics and astrophysics aspects.
|
---|
455 | Another main focus of research is on models of radiation and particle
|
---|
456 | acceleration processes in blazar jets (hadronic and leptonic models),
|
---|
457 | leading to predictions of correlated neutrino emission \citep{Rueger}.
|
---|
458 | This includes simulations of particle acceleration due to the Weibel
|
---|
459 | instability \citep{Burkart}. Much of this research at W\"{u}rzburg is
|
---|
460 | carried 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 |
|
---|
467 | The aim of the project is to put the former CT3 of the HEGRA
|
---|
468 | collaboration on the Roque de los Muchachos back into operation - with
|
---|
469 | an enlarged mirror surface, a new camera with higher quantum
|
---|
470 | efficiency, and new fast data acquisition system, under the name of
|
---|
471 | DWARF. The energy threshold will be lowered, and the sensitivity of
|
---|
472 | DWARF will be greatly improved compared to HEGRA CT3 (see
|
---|
473 | figure~\ref{sensitivity}). Commissioning and the first year of data taking
|
---|
474 | should be carried out within the three years of the requested funding
|
---|
475 | period.
|
---|
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 |
|
---|
489 | The telescope will be operated robotically to reduce costs and man
|
---|
490 | power demands. Furthermore, we seek to obtain know-how for the
|
---|
491 | operation of future networks of robotic Cherenkov telescopes (e.g. a
|
---|
492 | monitoring array around the globe or CTA) or telescopes at inaccessible
|
---|
493 | sites. From the experience with the construction and operation of MAGIC
|
---|
494 | or HEGRA, the proposing groups consider the planned focused approach
|
---|
495 | (small number of experienced scientists) as optimal for achieving the
|
---|
496 | project goals. The available automatic analysis package developed by
|
---|
497 | the W\"{u}rzburg group for MAGIC is modular and flexible, and can thus be
|
---|
498 | used 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 |
|
---|
511 | The scientific focus of the project will be on the long-term monitoring
|
---|
512 | of bright, nearby VHE emitting blazars. At least one of the proposed
|
---|
513 | targets will be visible any time of the year (see figure~\ref{visibility}). For
|
---|
514 | calibration purposes, some time will be scheduled for observations of
|
---|
515 | the Crab nebula. The blazar observations will allow
|
---|
516 | \begin{itemize}
|
---|
517 | \item to determine the duty cycle, the baseline emission, and the power
|
---|
518 | spectrum of flux variations.
|
---|
519 | \item to cooperate with the Whipple monitoring telescope for an
|
---|
520 | extended time coverage.
|
---|
521 | \item to prompt Target-of-Opportunity (ToO) observations with MAGIC in
|
---|
522 | the case of flares increasing time resolution. Corresponding
|
---|
523 | ToO proposals to H.E.S.S.\ and Veritas are in
|
---|
524 | preparation.
|
---|
525 | \item to observe simultaneously with MAGIC which will provide an
|
---|
526 | extended bandwidth from below 100\,GeV to multi-TeV energies.
|
---|
527 | \item to obtain multi-frequency observations together with the
|
---|
528 | Mets\"{a}hovi Radio Observatory and the optical Tuorla Observatory. The
|
---|
529 | measurements will be correlated with INTEGRAL and GLAST results, when
|
---|
530 | available. x-ray monitoring using the SWIFT and Suzaku facilities will
|
---|
531 | be proposed.
|
---|
532 | \end{itemize}
|
---|
533 |
|
---|
534 | Interpretation of the data will yield crucial information about
|
---|
535 | \begin{itemize}
|
---|
536 | \item the nature of the emission processes going on in relativistic
|
---|
537 | jets. We plan to interpret the data with models currently developed in
|
---|
538 | the context of the Research Training Group {\em Theoretical
|
---|
539 | Astrophysics} in W\"{u}rzburg (Graduiertenkolleg, GK\,1147), including
|
---|
540 | particle-in-cell and hybrid MHD models.
|
---|
541 | \item the black hole mass and accretion rate fitting the data with
|
---|
542 | emission models. Results will be compared with estimates of the black
|
---|
543 | hole mass from the Magorrian relation.
|
---|
544 | \item the flux of relativistic protons (ions) by correlating the rate
|
---|
545 | of neutrinos detected with the neutrino telescope IceCube and the rate
|
---|
546 | of gamma ray photons detected with DWARF, and thus the rate of escaping
|
---|
547 | cosmic rays.
|
---|
548 | \item the orbital modulation owing to a supermassive binary black hole.
|
---|
549 | Constraints on the binary system will allow to compute most accurate
|
---|
550 | templates of gravitational waves, which is a connected project at
|
---|
551 | W\"{u}rzburg in the German LISA consortium funded by DLR.
|
---|
552 | \end{itemize}
|
---|
553 |
|
---|
554 | \subsection[3.2]{Work schedule (Arbeitsprogramm)}
|
---|
555 |
|
---|
556 | To complete the mount to a functional Cherenkov telescope within a
|
---|
557 | period of one year, the following steps are necessary:
|
---|
558 |
|
---|
559 | The work schedule assumes that the work will begin in January 2008,
|
---|
560 | immediately after funding. Later funding would accordingly shift the
|
---|
561 | schedule. 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 |
|
---|
588 | Based on the experience with setting up the MAGIC telescope we estimate
|
---|
589 | this workschedule as conservative.
|
---|
590 |
|
---|
591 | \subsection[3.3]{Experiments with humans (Untersuchungen am Menschen)}
|
---|
592 | none
|
---|
593 | \subsection[3.4]{Experiments with animals (Tierversuche)}
|
---|
594 | none
|
---|
595 | \subsection[3.5]{Experiments with recombinant DNA (Gentechnologische Experimente)}
|
---|
596 | none
|
---|
597 |
|
---|
598 | \clearpage
|
---|
599 |
|
---|
600 | \section[4]{Funds requested (Beantragte Mittel)}
|
---|
601 |
|
---|
602 | We request funding for a total of three years. Summarizing, the
|
---|
603 | expenses for the telescope are dominated by the camera and data
|
---|
604 | acquisition.
|
---|
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 |
|
---|
610 | For this period, we request funding for two postdocs and two PhD
|
---|
611 | students, one in Dortmund and one in W\"{u}rzburg each. The staff
|
---|
612 | members shall fulfill the tasks given in the work schedule above. To
|
---|
613 | cover these tasks completely, one additional PhD and a various number
|
---|
614 | of Diploma students will complete the working group.
|
---|
615 |
|
---|
616 | Suitable candidates interested in these positions are Dr.\ Thomas
|
---|
617 | Bretz, Dr.\ dest.\ Daniela Dorner, Dr.\ dest.\ Kirsten M\"{u}nich,
|
---|
618 | cand.\ phys.\ Michael Backes, cand.\ phys.\ Daniela Hadasch and cand.\
|
---|
619 | phys.\ Dominik Neise.
|
---|
620 |
|
---|
621 | \subsection[4.2]{Scientific equipment (Wissenschaftliche Ger\"{a}te)}
|
---|
622 |
|
---|
623 | At the Observatorio Roque de los Muchachos (ORM), at the MAGIC site,
|
---|
624 | the mount of the former HEGRA telescope CT3 now owned by the MAGIC
|
---|
625 | collaboration is still operational. One hut for electronics close to
|
---|
626 | the telescope is available. Additional space is available in the MAGIC
|
---|
627 | counting house. The MAGIC Memorandum of Understanding allows for
|
---|
628 | operating DWARF as an auxiliary instrument (see appendix). Also
|
---|
629 | emergency support from the shift crew is guaranteed, although
|
---|
630 | autonomous robotic operation is the primary goal.
|
---|
631 |
|
---|
632 | To achieve the planned sensitivity and threshold
|
---|
633 | (figure~\ref{sensitivity}) the following components have to be bought.
|
---|
634 | To obtain reliable results as fast as possible well known components
|
---|
635 | have 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}
|
---|
641 | as well as the expectations for DWARF, with both a PMT- and a
|
---|
642 | GAPD-camera. These expectations are based on the sensitivity of
|
---|
643 | HEGRA~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}{
|
---|
658 | For long-term observations, the stability of the camera is a major
|
---|
659 | criterion. To keep the systematic errors small, a good background
|
---|
660 | estimation is mandatory. The only possibility for a synchronous
|
---|
661 | determination of the background is the determination from the night-sky
|
---|
662 | observed in the same field-of-view with the same instrument. To achieve
|
---|
663 | this, the observed position is moved out of the camera center which
|
---|
664 | allows the estimation of the background from positions symmetric with
|
---|
665 | respect to the camera center (so called wobble-mode). This observation
|
---|
666 | mode increases the sensitivity by a factor of $\sqrt{2}$,
|
---|
667 | because spending observation time for dedicated background observations
|
---|
668 | becomes obsolete, i.e.\ observation time for the source is doubled. This
|
---|
669 | ensures in addition a better time coverage of the observed sources.
|
---|
670 |
|
---|
671 | A further increase in sensitivity can be achieved by better background
|
---|
672 | statistics from not only one but several independent positions for the
|
---|
673 | background estimation in the camera \citep{Lessard:2001}. For wobble mode
|
---|
674 | observations allowing for this, the source position should be shifted
|
---|
675 | $0.6^\circ-0.7^\circ$ out of the camera center.
|
---|
676 | %}
|
---|
677 |
|
---|
678 | A camera completely containing shower images of events in the energy
|
---|
679 | region of 1\,TeV-10\,TeV should have a diameter in the order of
|
---|
680 | 5$^\circ$. To decrease the dependence of the measurements on the camera
|
---|
681 | geometry, a camera layout as symmetric as possible will be chosen.
|
---|
682 | Consequently a camera allowing to fulfill these requirements should be
|
---|
683 | round 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 |
|
---|
695 | Therefor a camera with 313 pixel camera (see figure~\ref{camDWARF}) is
|
---|
696 | chosen. The camera will be built based on the experience with HEGRA and
|
---|
697 | MAGIC. 19\,mm diameter Photomultiplier Tubes (PM, EMI\,9083\,KFLA-UD)
|
---|
698 | will be bought, similar to the HEGRA type (EMI\,9083\,KFLA). They have
|
---|
699 | a 25\% improved quantum efficiency (see figure~\ref{qe}) and ensure a
|
---|
700 | granularity which is enough to guarantee good results even below the
|
---|
701 | energy threshold (flux peak energy). Each individual pixel has to be
|
---|
702 | equipped with a preamplifier, an active high-voltage supply and
|
---|
703 | control. The total expense for a single pixel will be in the order of
|
---|
704 | 650,-\,\euro.
|
---|
705 |
|
---|
706 | All possibilities of borrowing one of the old HEGRA cameras for a
|
---|
707 | transition time have been probed and refused by the owners of the
|
---|
708 | cameras.
|
---|
709 |
|
---|
710 | {\bf At ETH~Z\"{u}rich currently test measurements are ongoing to prove the
|
---|
711 | ability, i.e.\ stability, aging, quantum efficiency, etc., of using
|
---|
712 | Geiger-mode APDs (GAPD) as photon
|
---|
713 | detector in the camera of a Cherenkov telescope. The advantages are
|
---|
714 | extremely high quantum efficiency ($>$50\%), easier gain stabilization and
|
---|
715 | simplified application compared to classical PMs. If these test
|
---|
716 | measurements are successfully finished until 8/2008 we consider to use
|
---|
717 | GAPDs in favor of classical PMs. The design of such a camera would take
|
---|
718 | place at University Dortmund in close collaboration with the experts
|
---|
719 | from ETH. Construction would also take place at the electronics
|
---|
720 | workshop of Dortmund.}
|
---|
721 |
|
---|
722 | \end{quote}\vspace{3ex}
|
---|
723 |
|
---|
724 | {\bf Camera support}\dotfill 204.000,-\,\euro\\[-3ex]
|
---|
725 | \begin{quote}
|
---|
726 | For this setup the camera holding has to be redesigned. (1500,-\,\euro)
|
---|
727 | The camera chassis must be water tight and will be equipped with an
|
---|
728 | automatic lid protecting the PMs at day-time. For further protection, a
|
---|
729 | plexi-glass window will be installed in front of the camera. By coating
|
---|
730 | this window with an anti-reflex layer of magnesium-fluoride, a gain in
|
---|
731 | transmission of {\bf 5\%} is expected. Each PM will be equipped with a
|
---|
732 | light-guide (Winston Cone) as developed by UC Davis and successfully in
|
---|
733 | operation in the MAGIC camera. (3000,-\,\euro\ for all winston cones). The
|
---|
734 | current design will be improved by using a high reflectivity aluminized
|
---|
735 | Mylar mirror-foil, coated with a dialectical layer ($Si\,O_2$
|
---|
736 | alternated with Niobium Oxide), to reach a reflectivity in the order of
|
---|
737 | {\bf 98\%}. An electric and optical shielding of the individual PMs is
|
---|
738 | planned.
|
---|
739 |
|
---|
740 | In total a gain of {\bf $\sim$15\%} in light-collection
|
---|
741 | efficiency 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}
|
---|
746 | 313 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}{
|
---|
752 | For the data acquisition system a hardware readout based on an analog
|
---|
753 | ring buffer (Domino\ II/III), currently developed for the MAGIC\ II
|
---|
754 | readout, will be used \citep{Barcelo}. This technology allows to sample
|
---|
755 | the pulses with high frequencies and readout several channels with a
|
---|
756 | single Flash-ADC resulting in low costs. The low power consumption will
|
---|
757 | allow to include the digitization near the signal source which makes
|
---|
758 | the transfer of the analog signal obsolete. The advantage is less
|
---|
759 | pick-up noise and less signal dispersion. By high sampling rates
|
---|
760 | (1.2\,GHz), additional information about the pulse shape can be
|
---|
761 | obtained. This increases the over-all sensitivity further, because the
|
---|
762 | short integration time allows for almost perfect suppression of noise
|
---|
763 | due to night-sky background photons. The estimated trigger- (readout-)
|
---|
764 | rate of the telescope is below 100\,Hz (HEGRA: $<$10\,Hz) which allows
|
---|
765 | to use a low-cost industrial solution for readout of the system like
|
---|
766 | USB\,2.0.
|
---|
767 |
|
---|
768 | %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
|
---|
769 | Current results obtained with the new 2\,GHz FADC system in the MAGIC
|
---|
770 | data acquisition show that for a single telescope a sensitivity
|
---|
771 | improvement of 40\% with a fast FADC system is achievable \citep{Tescaro:2007}.
|
---|
772 |
|
---|
773 | As for the HEGRA telescopes a simple multiplicity trigger is
|
---|
774 | sufficient, but also a simple neighbor-logic could be programmed (both
|
---|
775 | cases $\sim$100,-\,\euro/channel).
|
---|
776 |
|
---|
777 | Additional data reduction and preprocessing within the readout chain is
|
---|
778 | provided. Assuming conservatively a readout rate of 30\,Hz the storage
|
---|
779 | space needed will be less than 250\,GB/month or 3\,TB/year. This amount
|
---|
780 | of data can easily be stored and processed by the W\"{u}rzburg
|
---|
781 | Datacenter (current capacity $>$80\,TB, $>$40\,CPUs).
|
---|
782 | \end{quote}\vspace{3ex}
|
---|
783 |
|
---|
784 | {\bf Mirrors}\dotfill 15.000,-\,\euro\\[-3ex]
|
---|
785 | %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
|
---|
786 | \begin{quote}
|
---|
787 | The existing mirrors are replaced by new plastic mirrors which are
|
---|
788 | currently developed by Wolfgang Dr\"{o}ge's group. The cheap and
|
---|
789 | light-weight material has been formerly used for Winston cones in
|
---|
790 | balloon experiments. The mirrors are copied from a master coated with a
|
---|
791 | reflecting and a protective material. Tests have given promising
|
---|
792 | results. By a change of the mirror geometry, the mirror area can be
|
---|
793 | increased from 8.5\,m$^2$ to 13\,m$^2$ (see picture~\ref{CT3} and
|
---|
794 | montage~\ref{DWARF}); this includes an increase of $\sim$10$\%$ per
|
---|
795 | mirror by using a hexagonal layout instead of a round one. A further
|
---|
796 | increase of the mirror area would require a reconstruction of parts of
|
---|
797 | the mount and will therefore be considered only in a later phase of the
|
---|
798 | experiment.
|
---|
799 |
|
---|
800 | If the current development of the plastic mirrors cannot be finished in
|
---|
801 | time, a re-machining of the old glass mirrors (8.5\,m$^2$) is possible
|
---|
802 | with high purity aluminum and quartz coating.
|
---|
803 |
|
---|
804 | In both cases the mirrors can be coated with the same high reflectivity
|
---|
805 | aluminized Mylar mirror-foil, and a dialectical layer of SiO2 as for
|
---|
806 | the Winston Cones. By this, a gain in reflectivity of $\sim10\%$ is
|
---|
807 | achieved, see figure~\ref{reflectivity} \citep{Fraunhofer}.
|
---|
808 |
|
---|
809 | Both solutions would require the same expenses.
|
---|
810 |
|
---|
811 | To keep track of the alignment, reflectivity and optical quality of the
|
---|
812 | individual mirrors and the point-spread function of the total mirror
|
---|
813 | during long-term observations, the application of an automatic mirror
|
---|
814 | adjustment system, as developed by ETH~Z\"{u}rich and successfully
|
---|
815 | operated 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
|
---|
822 | telescope located at 2000\,m above sea level. The mirror's reflectivity
|
---|
823 | of a 300\,nm thick aluminum layer with a protection layer of 10\,nm and
|
---|
824 | 100\,nm thickness respectively. For comparison the reflectivity of
|
---|
825 | HEGRA CT1's mirrors \citep{Kestel:2000} are shown. The bottom plot depicts
|
---|
826 | the quantum efficiency of the prefered PMs (EMI) together with the
|
---|
827 | predecessor used in CT1. A proper coating \citep{Paneque:2004} will
|
---|
828 | further enhance its effciency. An even better increase would be the
|
---|
829 | usage 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}
|
---|
850 | Components\\
|
---|
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}{
|
---|
859 | For the absolute light calibration (gain-calibration) of the PMs a
|
---|
860 | calibration box as successfully used in the MAGIC telescope will be
|
---|
861 | produced.
|
---|
862 |
|
---|
863 | To ensure a homogeneous acceptance of the camera, essential for
|
---|
864 | wobble-mode observations, the trigger rate of the individual pixels
|
---|
865 | will be measured and controlled.
|
---|
866 |
|
---|
867 | To correct for axis misalignments and possible deformations of the
|
---|
868 | structure (e.g.\ bending of camera holding masts), a pointing correction
|
---|
869 | algorithm as used in the MAGIC tracking system will be applied. It is
|
---|
870 | calibrated by measurements of the reflection of bright guide stars on
|
---|
871 | the camera surface and ensures a pointing accuracy well below the pixel
|
---|
872 | diameter. Therefore a high sensitive low-cost video camera, as for
|
---|
873 | MAGIC\ I and~II, ({\bf 300,-\,\euro\ camera, 600,-\,\euro\ optics,
|
---|
874 | 300,-\,\euro\ housing, 250,-\,\euro\ Frame grabber}) will be installed.
|
---|
875 |
|
---|
876 | A second identical CCD camera for online monitoring (starguider) will
|
---|
877 | be bought.
|
---|
878 |
|
---|
879 | A GPS clock is necessary for an accurate tracking. The weather station
|
---|
880 | helps 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}{
|
---|
893 | For on-site computing three standard PCs are needed ($\sim$8.000,-\,\euro).
|
---|
894 | This includes readout and storage, preprocessing and telescope control.
|
---|
895 | For safety reasons, a firewall is mandatory. For local cache-storage
|
---|
896 | and backup, two RAID\,5 SATA disk arrays with one Terabyte capacity
|
---|
897 | each will fulfill the requirement ($\sim$4.000,-\,\euro). The data will be
|
---|
898 | transmitted as soon as possible after data taking via Internet to the
|
---|
899 | W\"{u}rzburg Datacenter. Enough storage capacity and computing power
|
---|
900 | is available there and already reserved for this purpose.
|
---|
901 |
|
---|
902 | Monte Carlo production and storage will take place at University
|
---|
903 | Dortmund.%}\\[2ex]
|
---|
904 | \end{quote}\vspace{3ex}
|
---|
905 |
|
---|
906 | {\bf Mount and Drive}\dotfill 17.500,-\,\euro\\[-3ex]
|
---|
907 | \begin{quote}
|
---|
908 | %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
|
---|
909 | The present mount is used. Only a smaller investment for safety,
|
---|
910 | corrosion protection, cable ducts, etc. is needed (7.500,-\,\euro).
|
---|
911 |
|
---|
912 | For the movement, motors, shaft encoders and control electronics in the
|
---|
913 | order of 10.000,-\,\euro\ have to be bought. The costs have been estimated
|
---|
914 | with the experience from building the MAGIC drive systems. The DWARF
|
---|
915 | drive system should allow for relatively fast repositioning for three
|
---|
916 | reasons: (i)~Fast movement might be mandatory for future ToO
|
---|
917 | observations. (ii)~Wobble-mode observations will be done changing the
|
---|
918 | wobble-position continuously (each 20\,min) for symmetry reasons. (iii)~To
|
---|
919 | ensure good time coverage of more than one source visible at the same
|
---|
920 | time, the observed source will be changed in constant time intervals
|
---|
921 | ($\sim$20\,min).
|
---|
922 |
|
---|
923 | Therefore three 150\,Watt servo motors are intended to be bought. A
|
---|
924 | micro-controller based motion control unit (Siemens SPS L\,20) similar to
|
---|
925 | the one of the current MAGIC~II drive system will be used. For
|
---|
926 | communication with the readout-system, a standard ethernet connection
|
---|
927 | based 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}{
|
---|
938 | A UPS with 5\,kW-10\,kW will be
|
---|
939 | installed to protect the equipment against power cuts and ensure a safe
|
---|
940 | telescope position at the time of sunrise.
|
---|
941 |
|
---|
942 | A fence for protection in case of robotic movement will be
|
---|
943 | installed.%}\\[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}{
|
---|
952 | For remote, robotic operation a variety of remote controllable electronic
|
---|
953 | components such as ethernet controlled sockets and switches will be
|
---|
954 | bought. Monitoring equipment, for example different kind of sensors, is
|
---|
955 | also 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
|
---|
959 | 342.235,-\,\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
|
---|
974 | 10.750,-\,\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)}
|
---|
979 | The large amount of travel funding is required due to the very close
|
---|
980 | cooperation between Dortmund and W\"{u}rzburg and the work demands on
|
---|
981 | the construction site.\\[-2ex]
|
---|
982 |
|
---|
983 | \begin{quote}
|
---|
984 | %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{
|
---|
985 | Per year one senior group member from Dortmund and W\"{u}rzburg should
|
---|
986 | present the status of the work in progress at an international workshop
|
---|
987 | or conference:\\
|
---|
988 | 2 x 3\,years x 1.500,-\,\euro\dotfill 9.000,-\,\euro\\[-2ex]
|
---|
989 |
|
---|
990 | One participation at the biannual MAGIC collaboration meeting:\\
|
---|
991 | 2 x 3\,years x 1.000,-\,\euro\dotfill 6.000,-\,\euro\\[-2ex]
|
---|
992 |
|
---|
993 | PhD student exchange between W\"{u}rzburg and Dortmund:\\
|
---|
994 | 1\,student x 1\,week x 24 (every six weeks) x 800,-\,\euro\dotfill
|
---|
995 | 19.200,-\,\euro\\[-2ex]
|
---|
996 |
|
---|
997 | For setup of the telescope at La Palma the following travel expenses
|
---|
998 | are necessary:\\
|
---|
999 | 4 x 2\,weeks at La Palma x 2\,persons x 1.800,-\,\euro\dotfill
|
---|
1000 | 28.800,-\,\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
|
---|
1006 | 72.200,-\,\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)}
|
---|
1012 | Will be covered by the proposing institutes.
|
---|
1013 |
|
---|
1014 |
|
---|
1015 | \subsection[4.6]{Other costs (Sonstige Kosten)}
|
---|
1016 | \begin{quote}
|
---|
1017 | Storage container (for shipment of the mirrors)\dotfill 5.000,-\,\euro\\
|
---|
1018 | Transport\dotfill 15.000,-\,\euro\\
|
---|
1019 | Dismantling (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
|
---|
1024 | 20.000,-\,\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}
|
---|
1031 | none
|
---|
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
|
---|
1081 | anderen Wissenschaftlern)}
|
---|
1082 |
|
---|
1083 | Both applying groups co-operate with the international
|
---|
1084 | MAGIC-Collaboration and the institutes represented therein. (W\"{u}rzburg
|
---|
1085 | funded by the BMBF, Dortmund by means of appointment for the moment).
|
---|
1086 |
|
---|
1087 | W\"{u}rzburg is also in close scientific exchange with the group of
|
---|
1088 | Prof.~Dr.~Victoria Fonseca, UCM Madrid and the University of Turku
|
---|
1089 | (Finland) operating the KVA optical telescope at La Palma. Other
|
---|
1090 | cooperations refer to the projects JEM-EUSO (science case), GRIPS
|
---|
1091 | (simulation), LISA (astrophysical input for templates), STEREO (data
|
---|
1092 | analysis), and SOLAR ORBITER (electron-proton telescope). A cooperation
|
---|
1093 | with GLAST science team members (Dr.~Anita and Dr.~Olaf Reimer,
|
---|
1094 | Stanford) is also relevant for the proposed project.
|
---|
1095 |
|
---|
1096 | The group in Dortmund is involved in the IceCube experiment (BMBF
|
---|
1097 | funding) and maintains close contacts to the collaboration partners.
|
---|
1098 | Moreover on the field of phenomenology there do exist good working
|
---|
1099 | contacts to the groups of Prof.~Dr.~Reinhard Schlickeiser,
|
---|
1100 | Ruhr-Universit\"{a}t Bochum and Prof.~Dr.~Peter Biermann, MPIfR Bonn.
|
---|
1101 | There are furthermore intense contacts to Prof.~Dr.~Francis Halzen,
|
---|
1102 | Madison, Wisconsin.
|
---|
1103 |
|
---|
1104 | The telescope design will be worked out in close cooperation with the
|
---|
1105 | group of Prof.~Dr.~Felicitas Pauss, Dr.~Adrian Biland and
|
---|
1106 | Prof.~Dr.~Eckart Lorenz (ETH~Z\"{u}rich). They will provide help in design
|
---|
1107 | studies, construction and software development. The DAQ design will be
|
---|
1108 | contributed by the group of Prof.~Dr.~Riccardo Paoletti (Università di
|
---|
1109 | Siena and INFN sez.\ di Pisa, Italy).
|
---|
1110 |
|
---|
1111 | The group of the newly appointed {\em Lehrstuhl f\"{u}r Physik und Ihre
|
---|
1112 | Didaktik} (Prof.~Dr.~Thomas Trefzger) has expressed their interest to
|
---|
1113 | join the project. They bring in a laboratory for photo-sensor testing,
|
---|
1114 | know-how from former contributions to ATLAS and a joint interest in
|
---|
1115 | operating a data pipeline using GRID technologies.
|
---|
1116 |
|
---|
1117 | \subsection[5.3]{Work outside Germany, Cooperation with foreign
|
---|
1118 | partners (Arbeiten im Ausland, Kooperation mit Partnern im Ausland)}
|
---|
1119 |
|
---|
1120 | The work on DWARF will take place at the ORM on the Spanish island La
|
---|
1121 | Palma. It will be performed in close collaboration with the
|
---|
1122 | MAGIC-Collaboration.
|
---|
1123 |
|
---|
1124 | \subsection[5.4]{Scientific equipment available (Apparative
|
---|
1125 | Ausstattung)}
|
---|
1126 | In Dortmund and W\"{u}rzburg extensive computer capacities for data
|
---|
1127 | storage as well as for data analysis are available.
|
---|
1128 |
|
---|
1129 | The faculty of physics at the University of Dortmund has modern
|
---|
1130 | equipped mechanical and electrical workshops including a department for
|
---|
1131 | development of electronics at its command. The chair of astroparticle
|
---|
1132 | physics possesses common technical equipment required for constructing
|
---|
1133 | modern DAQ.
|
---|
1134 |
|
---|
1135 | The faculty of physics at the University of W\"{u}rzburg comes with a
|
---|
1136 | mechanical and an electronic workshop, as well as a special laboratory
|
---|
1137 | of the chair for astronomy suitable for photosensor testing.
|
---|
1138 |
|
---|
1139 | \subsection[5.5]{The institution's general contribution (Laufende
|
---|
1140 | Mittel f\"{u}r Sachausgaben)}
|
---|
1141 | Current total institute budget from the University Dortmund $\approx$
|
---|
1142 | 20.000\,\euro\ per year.\\
|
---|
1143 |
|
---|
1144 | Current total institute budget from the University W\"{u}rzburg $\approx$
|
---|
1145 | 30.000\,\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}~\\
|
---|
1149 | none
|
---|
1150 |
|
---|
1151 | \subsection[5.7]{Other requirements (Sonstige Voraussetzungen)}~\\
|
---|
1152 | none
|
---|
1153 |
|
---|
1154 | \newpage
|
---|
1155 | \thispagestyle{empty}
|
---|
1156 |
|
---|
1157 | \paragraph{6 Declarations (Erkl\"{a}rungen)}
|
---|
1158 |
|
---|
1159 | A request for funding this project has not been submitted to
|
---|
1160 | any other addressee. In case we submit such a request we will inform
|
---|
1161 | the Deutsche Forschungsgemeinschaft immediately. \\
|
---|
1162 |
|
---|
1163 | The corresponding persons (Vertrauensdozenten) at the
|
---|
1164 | Universit\"{a}t Dortmund (Prof.\ Dr.\ Gather) and at the Universit\"{a}t
|
---|
1165 | W\"{u}rzburg (Prof.\ Dr.\ G.\ Bringmann) have been informed about the
|
---|
1166 | submission of this proposal.
|
---|
1167 |
|
---|
1168 | \paragraph{7 Signatures (Unterschriften)}~\\
|
---|
1169 |
|
---|
1170 | \vspace{2.5 cm}
|
---|
1171 |
|
---|
1172 | \hfill
|
---|
1173 | \begin{minipage}[t]{6cm}
|
---|
1174 | W\"{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}
|
---|
1180 | Dortmund,\\[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
|
---|
1191 | List 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}
|
---|