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trunk/Dwarf/Documents/ApplicationDFG/application.bib
r8773 r8777 2933 2933 @MASTERSTHESIS{Deeg:Dipl, 2934 2934 author = {Deeg, M.}, 2935 title = "{Prototypenentwicklung eines Detektorsystems f ür ultrahochenergetische Kosmische Strahlung}",2935 title = "{Prototypenentwicklung eines Detektorsystems f\"ur ultrahochenergetische Kosmische Strahlung}", 2936 2936 school = {Universit{\"a}t Dortmund}, 2937 2937 month = {Feb}, … … 2983 2983 2984 2984 @INPROCEEDINGS{Rueger, 2985 author = {R ueger, M. and Spanier, F.},2985 author = {R\"{u}ger, M. and Spanier, F.}, 2986 2986 booktitle = {Astronomische Nachrichten}, 2987 2987 volume = 328, … … 2997 2997 2998 2998 @INPROCEEDINGS{Ruegamer, 2999 author = {R uegamer, S. and others},2999 author = {R\"{u}gamer, S. and others}, 3000 3000 title = {Wide Range Multifrequency Observations of Northern TeV Blazars}, 3001 3001 booktitle = {Astronomische Nachrichten}, -
trunk/Dwarf/Documents/ApplicationDFG/application.tex
r8774 r8777 41 41 42 42 \maketitle 43 44 %\tableofcontents 43 \newpage 44 x 45 \thispagestyle{empty} 46 \cleardoublepage 47 \newpage 45 48 46 49 \section[1]{General Information (Allgemeine Angaben)} … … 61 64 {44221 Dortmund }&\multicolumn{2}{l|}{58285 Gevelsberg}\\ 62 65 {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)\,}\\66 {\parbox[t]{1.5cm}{Phone:}+49\,(231)\,755-3550}&\multicolumn{2}{l|}{\parbox[t]{1.5cm}{Phone:}+49\,(173)\,284\,79\,10}\\ 64 67 {\parbox[t]{1.5cm}{Fax:}+49\,(231)\,755-4547}&\multicolumn{2}{l|}{~}\\\hline\hline 65 68 \multicolumn{3}{|c|}{{\bf email}: wolfgang.rhode@udo.edu}\\\hline … … 79 82 {97074 W"urzburg }&\multicolumn{2}{l|}{97299 Zell am Main }\\ 80 83 {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: } }\\84 {\parbox[t]{1.5cm}{Phone:}+49\,(931)\,888-5031}&\multicolumn{2}{l|}{\parbox[t]{1.5cm}{Phone: +49\,(931)\,404\,81\,90} }\\ 82 85 {\parbox[t]{1.5cm}{Fax:}+49\,(931)\,888-4603}&\multicolumn{2}{l|}{~}\\\hline\hline 83 \multicolumn{3}{|c|}{{\bf email}: mannhei n@astro.uni-wuerzbueg.de}\\\hline86 \multicolumn{3}{|c|}{{\bf email}: mannheim@astro.uni-wuerzbueg.de}\\\hline 84 87 \end{tabular} 85 88 \originalTeX 86 89 \newpage 87 90 88 %\paragraph{1.2 Topic}~\\89 \subsection[1.2]{Topic}91 \paragraph{1.2 Topic}~\\ 92 %\subsection[1.2]{Topic} 90 93 Long-term VHE $\gamma$-ray monitoring of bright blazars with a dedicated Cherenkov telescope 91 94 92 %\paragraph{1.2 Thema}~\\93 \subsection[1.2]{Thema}95 \paragraph{1.2 Thema}~\\ 96 %\subsection[1.2]{Thema} 94 97 Langzeitbeobachtung von hellen VHE $\gamma$-Blazaren mit einem dedizierten Cherenkov Teleskop 95 98 96 %\paragraph{1.3 Discipline and field of work (Fachgebiet und Arbeitsrichtung)}~\\97 \subsection[1.3]{Discipline and field of work (Fachgebiet und Arbeitsrichtung)}99 \paragraph{1.3 Discipline and field of work (Fachgebiet und Arbeitsrichtung)}~\\ 100 %\subsection[1.3]{Discipline and field of work (Fachgebiet und Arbeitsrichtung)} 98 101 Astronomy and Astrophysics, Particle Astrophysics 99 102 100 %\paragraph{\bf 1.4 Scheduled duration in total (Voraussichtliche Gesamtdauer)}~\\101 \subsection[1.4]{Scheduled duration in total (Voraussichtliche Gesamtdauer)}103 \paragraph{\bf 1.4 Scheduled duration in total (Voraussichtliche Gesamtdauer)}~\\ 104 %\subsection[1.4]{Scheduled duration in total (Voraussichtliche Gesamtdauer)} 102 105 After successful completion of the three-year work plan developed in 103 106 this proposal, we will ask for an extension of the project for another … … 105 108 of supermassive binary black holes. 106 109 107 %\paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\108 \subsection[1.5]{Application period (Antragszeitraum)}110 \paragraph{\bf 1.5 Application period (Antragszeitraum)}~\\ 111 %\subsection[1.5]{Application period (Antragszeitraum)} 109 112 3\,years. The work on the project will begin immediately after the 110 funding. 113 funding. 111 114 112 115 \newpage 113 %\paragraph{\bf 1.6 Summary}~\\114 \subsection[1.6]{Summary}115 We propose to set up a robotic imaging air 116 cost, but high performance design for remote operation. The goal is to116 \paragraph{\bf 1.6 Summary}~\\ 117 %\subsection[1.6]{Summary} 118 We propose to set up a robotic imaging air-Cherenkov telescope with low 119 cost, but a high performance design for remote operation. The goal is to 117 120 dedicate this gamma-ray telescope to long-term monitoring observations 118 121 of nearby, bright blazars at very high energies. We will (i) search for … … 121 124 origin, and (iii) correlate the data with corresponding data from the 122 125 neutrino observatory IceCube to search for evidence of hadronic 123 emission processes. The observations will alsotrigger follow-up126 emission processes. The observations will furthermore trigger follow-up 124 127 observations of flares with higher sensitivity telescopes such as 125 MAGIC, VERITAS ,and H.E.S.S.\ Joint observations with the Whipple128 MAGIC, VERITAS and H.E.S.S.\ Joint observations with the Whipple 126 129 monitoring telescope will start a future 24\,h-monitoring of selected 127 130 sources with a distributed network of robotic telescopes. The telescope 128 design is based on a fulltechnological upgrade of one of the former131 design is based on a complete technological upgrade of one of the former 129 132 telescopes of the HEGRA collaboration (CT3) still located at the 130 133 Observatorio Roque de los Muchachos on the Canarian Island La Palma … … 135 138 136 139 \germanTeX 137 %\paragraph{\bf 1.6 Zusammenfassung}~\\138 \subsection[1.6]{Zusammenfassung}140 \paragraph{\bf 1.6 Zusammenfassung}~\\ 141 %\subsection[1.6]{Zusammenfassung} 139 142 {\bf Unser Vorhaben besteht darin, ein robotisches Luft-Cherenkov-Teleskop 140 143 mit geringen Kosten aber hoher Leistung fernsteuerbar in Betrieb zu 141 nehmen. Das Ziel ist es, dieses gamma-rayTeleskop ganz der144 nehmen. Das Ziel ist es, dieses Gammastrahlen Teleskop ganz der 142 145 Langzeitbeobachtung von nahen, hellen Blazaren bei sehr hohen Energien 143 146 zu widmen. Wir werden (i) nach Modulationen der Blazar-Emission durch … … 145 148 Statistik von gamma-Ausbr"uchen und deren physikalischen Ursprung 146 149 untersuchen und (iii) die Daten mit entsprechenden Daten von dem 147 Neutrino-Tel skop IceCube korrelieren, um Nachweise f"ur hadronische150 Neutrino-Teleskop IceCube korrelieren, um Nachweise f"ur hadronische 148 151 Emissionsprozesse zu finden. Die Beobachtungen werden zus"atzlich 149 152 Nachfolgebeobachtungen von gamma-Ausbr"uchen mit h"ohersensitiven 150 Teleskopen wie MAGIC, VERITAS und H.E.S.S.\ triggern. Auf 153 Teleskopen wie MAGIC, VERITAS und H.E.S.S.\ triggern. Aufeinander 151 154 abgestimmte Beobachtungen zusammen mit dem Whipple Teleskop werden der 152 155 Auftakt zu einer zuk"unftigen 24-Stunden-Beobachtung von selektierten … … 163 166 \newpage 164 167 165 \section[2]{S tand der Forschung, eigene Vorarbeiten\\(Science case, preliminary work by proposer)}168 \section[2]{Science case, preliminary work by proposer\\(Stand der Forschung, eigene Vorarbeiten)} 166 169 167 170 \subsection[2.1]{Science case (Stand der Forschung)} 168 171 169 172 Since the termination of the HEGRA observations, the succeeding 170 experiments MAGIC and H.E.S.S. have impressively extended the physical171 scope of gamma ray astronomy detecting tens of formerly unknown gamma172 ray sources and analyzing their energy spectra, morphology,and173 experiments MAGIC and H.E.S.S.\ have impressively extended the physical 174 scope of gamma-ray astronomy detecting tens of formerly unknown gamma-ray 175 sources and analyzing their energy spectra, morphology and 173 176 temporal behavior. This became possible by lowering the energy 174 177 threshold from 700\,GeV to less than 100\,GeV and increasing at the same 175 178 time the sensitivity by a factor of five. A diversity of astrophysical 176 179 source types such as pulsar wind nebulae, supernova remnants, 177 micro quasars, pulsars, radio galaxies, clusters of galaxies, gamma ray178 bursts and blazars have been studied with these telescopes.180 micro-quasars, pulsars, radio galaxies, clusters of galaxies, Gamma-Ray 181 Bursts and blazars have been studied with these telescopes. 179 182 180 183 The main class of extragalactic, very high energy gamma-rays sources … … 185 188 long-wavelength radio waves to multi-TeV gamma-rays. In addition, 186 189 blazars are characterized by rapid variability, high degrees of 187 polarization, and super -luminal motion of knots in their190 polarization, and superluminal motion of knots in their 188 191 high-resolution radio images. The observed behavior can readily be 189 192 explained assuming relativistic bulk motion and in situ particle 190 acceleration, e.g. at shock waves, leading to synchrotron193 acceleration, e.g.\ at shock waves, leading to synchrotron 191 194 (radio-to-x-ray) and self-Compton (gamma-ray) emission \citep{Blandford}. 192 195 Additionally, inverse Compton scattering of external photons may play a 193 role in producing the observed gamma 196 role in producing the observed gamma-rays \citep{Dermer,Begelman}. 194 197 Variability may hold the key to understanding the details of the 195 emission processes and the source geometry , and the development of196 time-dependent models is currently on the agenda of model builders198 emission processes and the source geometry. The development of 199 time-dependent models is currently under investigation 197 200 worldwide. 198 201 … … 204 207 ambient matter, will quickly dominate the momentum flow of the jet. 205 208 This {\em baryon pollution} has been suggested to solve the energy 206 transport problem in gamma ray bursts,and is probably present in209 transport problem in Gamma-Ray Bursts and is probably present in 207 210 blazar jets as well, even if they originate as pair jets in a black 208 211 hole ergosphere \citep{Meszaros}. Protons and ions accelerated in the 209 jets of blazars can reach extremely high energies before energy losses212 jets of blazars can reach extremely high energies, before energy losses 210 213 become important \citep{Mannheim:1993}. Escaping particles contribute 211 214 to the observed flux of ultrahigh energy cosmic rays in a major way. 212 215 Blazars and their unbeamed hosts, the radio galaxies, are thus the 213 216 prime candidates for origin of ultrahigh energy cosmic rays 214 \citep{Rachen} , and this can be investigated with the IceCube and AUGER217 \citep{Rachen}. This can be investigated with the IceCube and AUGER 215 218 experiments. Recent results of the AUGER experiment show a significant 216 219 anisotropy of the highest energy cosmic rays and point at either nearby … … 230 233 with magnetic confinement \citep{Mannheim:1995}. Short variability time 231 234 scales can result from dynamical changes of the emission zone, running 232 e.g. through an inhomogeneous environment.235 e.g.\ through an inhomogeneous environment. 233 236 234 237 The contemporaneous spectral energy distributions for hadronic and … … 237 240 model \citep{Mannheim:1999}. These properties allow conclusions 238 241 about the accelerated particles. Noteworthy, even for nearby blazars 239 the spectrum must be corrected for attenuation of the gamma 242 the spectrum must be corrected for attenuation of the gamma-rays due to 240 243 pair production in collisions with low-energy photons from the 241 244 extragalactic background radiation field \citep{Kneiske}. … … 252 255 generally showing the largest amplitudes and the shortest time scales 253 256 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 by256 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-rayflare, coined orphan flares, have been observed, questioning the257 has been observed in a flare of Mrk\,501 with the MAGIC telescope 258 \citep{Albert:501}. A giant flare of PKS\,2155-304 discovered by 259 H.E.S.S.\ \citep{Aharonian:2007pks} has shown similarly short doubling 260 time scales and a flux of up to 16 times the flux of the Crab Nebula. 261 Indications for TeV flares without evidence for an accompanying x-ray 262 flare, coined orphan flares, have been observed, questioning the 260 263 synchrotron-self-Compton mechanism being responsible for the 261 264 gamma-rays. Model ramifications involving several emission components, 262 265 external seed photons, or hadronically induced emission may solve the 263 problem \citep{Blazejowski}. Certainly, the database for contemporaneous264 multi-wavelength observations is still far from proving the 265 synchrotron-self-Compton model.266 problem \citep{Blazejowski}. Certainly, the database for 267 contemporaneous multi-wavelength observations is still far from proving 268 the synchrotron-self-Compton model. 266 269 267 270 Generally, observations of flares are prompted by optical or x-ray … … 297 300 wave luminosity is spectacularly high, even long before final 298 301 coalescence and the frequencies are favorable for the detectors under 299 consideration (LISA). Detection of gravitational waves relies on exact302 consideration (LISA). The detection of gravitational waves relies on exact 300 303 templates to filter out the signals and the templates can be computed 301 304 from astrophysical constraints on the orbits and masses of the black … … 307 310 Mrk\,501 during a phase of high activity in 1997 was reported by 308 311 HEGRA \citep{Kranich}, and was later confirmed including x-ray and 309 Tele acope Array data \citep{Osone}. The observations can be explained in312 Telescope Array data \citep{Osone}. The observations can be explained in 310 313 a supermassive black hole binary scenario \citep{Rieger:2000}. 311 314 Indications for helical trajectories and periodic modulation of optical … … 319 322 exposure simultaneous to the VHE observations, and this is a new 320 323 qualitative step for blazar research. For the same reasons, the VERITAS 321 Collaboration keeps the former Whipple telescope alive, albeit its324 collaboration keeps the former Whipple telescope alive, albeit its 322 325 performance seems to have strongly degraded. It is obvious that the 323 326 large Cherenkov telescopes such as MAGIC, H.E.S.S.\ or VERITAS are mainly … … 345 348 346 349 Assuming conservatively the performance of a single HEGRA-type 347 telescope, long-term monitor ing of at least the following known blazars348 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 a350 telescope, long-term monitor\-ing of at least the following known 351 blazars is possible: Mrk\,421, Mrk\,501, 1ES\,2344+514, 1ES\,1959+650, 352 H\,1426+428, PKS\,2155-304. We emphasize, that DWARF will run as a 350 353 facility dedicated to these targets only, providing a maximum 351 354 observation time for the program. Utilizing recent developments, such … … 364 367 of Amanda, IceCube, HEGRA and MAGIC the proposing groups contribute the 365 368 necessary knowledge and experience to build and operate a small imaging 366 air 369 air-Cherenkov telescope. 367 370 368 371 \paragraph{Hardware} … … 388 391 development departure of the faculty. 389 392 390 The ultra fast drive system of the MAGIC tel scopes, suitable for fast393 The ultra fast drive system of the MAGIC telescopes, suitable for fast 391 394 repositioning in case of Gamma-Ray Bursts, has been developed, 392 395 commissioned and programmed by the W\"{u}rzburg group … … 402 405 403 406 Mirror structures made of plastic material have been developed as 404 Winston Cones for balloon flight experiments previously by the group of407 Winston cones for balloon flight experiments previously by the group of 405 408 Wolfgang Dr\"{o}ge. W\"{u}rzburg has also participated in the development of 406 409 a HPD test bench, which has been setup in Munich and W\"{u}rzburg. With … … 413 416 flexible and modular enough to easily process DWARF data 414 417 \citep{Bretz:2005paris,Riegel:2005icrc,Bretz:2005mars}. A method for 415 absolute light calibration of the PMs based on Muon images has been 418 absolute light calibration of the PMs based on Muon images, especially 419 important for long-term monitoring, has been 416 420 adapted and further improved for the MAGIC telescope 417 421 \citep{Meyer:Diploma,Goebel:2005}. Both, data analysis and Monte Carlo … … 420 424 developed to be powerful and as robust as possible to be best suited 421 425 for automatic processing \citep{Dorner:2005paris}. Experience with 422 large amount of data (up to 15\,TB/month) has been gained over five423 years now.The datacenter is equipped with a professional multi-stage426 large amount of data (up to 8\,TB/month) has been gained since 2004. 427 The datacenter is equipped with a professional multi-stage 424 428 (hierarchical) storage system. Two operators are paid by the physics 425 429 faculty. Currently efforts in W\"{u}rzburg and Dortmund are ongoing to 426 turn the old inflexible Monte Carlo programs, used by the MAGIC427 collaboration, into modular packages which allowseasy simulation of430 turn the old, inflexible Monte Carlo programs, used by the MAGIC 431 collaboration, into modular packages allowing for easy simulation of 428 432 other setups. Experience with Monte Carlo simulations, especially 429 433 CORSIKA, is contributed by the Dortmund group, which has actively … … 432 436 model \citep{Haffke:Dipl,Schroeder:PhD} for the local atmosphere of La 433 437 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 438 for Lepton propagation in different media 439 %\citep{hepph0407075}. An 440 \citep{xxx}. 441 An energy unfolding method and program has been adapted for IceCube and 436 442 MAGIC data analysis \citep{Curtef:CM,Muenich:ICRC}. 437 443 438 444 \paragraph{Phenomenology} 439 445 440 Both groups furtherhave experience with source models and theoretical441 computations of gamma 446 Both groups have experience with source models and theoretical 447 computations of gamma-ray and neutrino spectra expected from blazars. 442 448 The relation between the two messengers is a prime focus of interest. 443 449 Experience with corresponding multi-messenger data analyses involving 444 450 MAGIC and IceCube data is available in the Dortmund group. Research 445 451 activities are also related with relativistic particle acceleration 446 \citep{Meli} and gamma 452 \citep{Meli} and gamma-ray attenuation \citep{Kneiske}. The W\"{u}rzburg 447 453 group has organized and carried out multi-wavelength observations of 448 bright blazars involving MAGIC, Suzaku, the IRAM telescopes ,and the449 optical KVAtelescope \citep{Ruegamer}. Signatures of supermassive454 bright blazars involving MAGIC, Suzaku, the IRAM telescopes and the 455 KVA optical telescope \citep{Ruegamer}. Signatures of supermassive 450 456 black hole binaries, which are most relevant also for gravitational 451 457 wave detectors, are investigated jointly with the German LISA 452 458 consortium (Burkart, Elbracht ongoing research, funded by DLR). 453 Secondary gammarays due to dark matter annihilation events are459 \mbox{Secondary} gamma-rays due to dark matter annihilation events are 454 460 investigated both from their particle physics and astrophysics aspects. 455 461 Another main focus of research is on models of radiation and particle … … 466 472 467 473 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 - with469 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.474 collaboration on the Roque de los Muchachos back into operation. It 475 will be setup, under the name DWARF, with an enlarged mirror surface 476 (fig.~\ref{DWARF}), a new camera with higher quantum efficiency and new 477 fast data acquisition system. The energy threshold will be lowered, and 478 the sensitivity of DWARF will be greatly improved compared to HEGRA CT3 479 (see fig.~\ref{sensitivity}). Commissioning and the first year of data 480 taking should be carried out within the three years of the requested 481 funding period. 476 482 477 483 \begin{figure}[ht] 478 484 \begin{center} 479 \includegraphics*[width=0.49 5\textwidth,angle=0,clip]{CT3.eps}480 \includegraphics*[width=0.49 5\textwidth,angle=0,clip]{DWARF.eps}481 \caption{ Left: The old HEGRACT3 telescope as operated within the482 HEGRA Sy tem. Right: A photomontage howthe revised CT3 telescope483 could look like with more and hexagonal mirrors.}485 \includegraphics*[width=0.496\textwidth,angle=0,clip]{CT3.eps} 486 \includegraphics*[width=0.496\textwidth,angle=0,clip]{DWARF.eps} 487 \caption{The old CT3 telescope as operated within the 488 HEGRA System (left) and a photomontage of the revised CT3 telescope 489 with more and hexagonal mirrors (right).} 484 490 \label{CT3} 485 491 \label{DWARF} … … 488 494 489 495 The telescope will be operated robotically to reduce costs and man 490 power demands. 496 power demands. Furthermore, we seek to obtain know-how for the 491 497 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. 498 monitoring array around the globe or CTA) or telescopes at sited 499 difficult to access. From the experience with the construction and 500 operation of MAGIC or HEGRA, the proposing groups consider the planned 501 focused approach (small number of experienced scientists) as optimal 502 for achieving the project goals. The available automatic analysis 503 package developed by the W\"{u}rzburg group for MAGIC is modular and 504 flexible, and can thus be used with minor changes for the DWARF 505 project. 499 506 500 507 \begin{figure}[htb] … … 502 509 \includegraphics*[width=0.7\textwidth,angle=0,clip]{visibility.eps} 503 510 \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 CrabNebula506 necessary for calibration and quality assurance. 511 considering a maximum observation zenith angle of 65$^\circ$ 512 for all sources which we want to monitor including the Crab Nebula, 513 necessary for calibration and quality assurance.} 507 514 \label{visibility} 508 515 \end{center} … … 510 517 511 518 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 519 of bright, nearby VHE emitting blazars. At least one of the proposed 520 targets will be visible any time of the year (see 521 fig.~\ref{visibility}). For calibration purposes, some time will be 522 scheduled for observations of the Crab Nebula.\\ 523 524 The blazar observations will allow 516 525 \begin{itemize} 517 \item to determine the duty cycle, the baseline emission,and the power526 \item to determine the baseline emission, the duty cycle and the power 518 527 spectrum of flux variations. 519 528 \item to cooperate with the Whipple monitoring telescope for an … … 521 530 \item to prompt Target-of-Opportunity (ToO) observations with MAGIC in 522 531 the case of flares increasing time resolution. Corresponding 523 ToO proposals to H.E.S.S.\ and Veritas are in 524 preparation. 532 ToO proposals to H.E.S.S.\ and VERITAS are in preparation. 525 533 \item to observe simultaneously with MAGIC which will provide an 526 534 extended bandwidth from below 100\,GeV to multi-TeV energies. 527 535 \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. 536 Mets\"{a}hovi Radio Observatory and the optical telescopes of the 537 Tuorla Observatory. The measurements will be correlated with INTEGRAL 538 and GLAST results, when available. X-ray monitoring using the SWIFT and 539 Suzaku facilities will be proposed. 540 532 541 \end{itemize} 533 542 … … 537 546 jets. We plan to interpret the data with models currently developed in 538 547 the context of the Research Training Group {\em Theoretical 539 Astrophysics} in W\"{u}rzburg (Graduiertenkolleg, GK\,1147), including 548 Astrophysics} in W\"{u}rzburg (Graduiertenkolleg, GK\,1147), including 540 549 particle-in-cell and hybrid MHD models. 541 550 \item the black hole mass and accretion rate fitting the data with 542 emission models. 543 hole mass from 551 emission models. Results will be compared with estimates of the black 552 hole mass from the Magorrian relation. 544 553 \item the flux of relativistic protons (ions) by correlating the rate 545 554 of neutrinos detected with the neutrino telescope IceCube and the rate 546 of gamma 555 of gamma-ray photons detected with DWARF, and thus the rate of escaping 547 556 cosmic rays. 548 557 \item the orbital modulation owing to a supermassive binary black hole. … … 557 566 period of one year, the following steps are necessary: 558 567 559 The work schedule assumes that the work will begin in January 2008,568 The work schedule assumes, that the work will begin in January 2008, 560 569 immediately after funding. Later funding would accordingly shift the 561 schedule. Each year is divided into quarters (see fig ure~\ref{schedule}).570 schedule. Each year is divided into quarters (see fig.~\ref{schedule}). 562 571 563 572 \begin{figure}[htb] 564 573 \begin{center} 565 \includegraphics*[ angle=0,clip]{schedule.eps}574 \includegraphics*[width=\textwidth,angle=0,clip]{schedule.eps} 566 575 % \caption{Left: The old HEGRA CT3 telescope as operated within the 567 576 % HEGRA Sytem. Right: A photomontage how the revised CT3 telescope … … 574 583 \paragraph{Software} 575 584 \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. 585 \item MC adaption (Do/W\"{u}): Due to the large similarities with the 586 MAGIC telescope, within half a year new Monte Carlo code can be 587 programmed using parts of the existing MAGIC Monte Carlo code. For 588 tests and cross-checks another period of six months is necessary. 589 \item Analysis adaption (W\"{u}): The modular concept of the Magic 590 Analysis and Reconstruction Software (MARS) allows a very fast adaption 591 of the telescope setup, camera and data acquisition properties within 592 half a year. 593 \item Adaption Drive software (W\"{u}): Since the new drive electronics 594 will be based on the design of the MAGIC~II drive system the control 595 software can be reused unchanged. The integration into the new slow 596 control system will take about half a year. It has to be finished at 597 the time of arrival of the drive system components in 2009/1. 598 \item Slow control/DAQ (Do): A new data acquisition and slow control 599 system for camera and auxiliary systems has to be developed. Based on 600 experiences with the AMANDA DAQ, the Domino DAQ developed for MAGIC~II 601 will be adapted and the slow control integrated within three quarters 602 of a year. Commissioning will take place with the full system in 603 2009/3. 580 604 \end{itemize} 581 605 582 \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. 606 \paragraph{Mirrors (W\"{u})} First prototypes for the mirrors are 607 already available. After testing (six months), the production will 608 start in summer 2008, and the shipment will be finished before the full 609 system assembly 2009/2. 610 \paragraph{Drive (W\"{u})} After a planning phase of half a year to 611 simplify the MAGIC~II drive system for a smaller telescope (together 612 with the delivering company), ordering, production and shipment should 613 be finished in 2009/1. The MAGIC~I and~II drive systems have been 614 planned and implemented successfully by the W\"{u}rzburg group. 615 \paragraph{Auxiliary (W\"{u})} Before the final setup in 2009/1, all 616 auxiliary systems (weather station, computers, etc.) will have been 617 specified, ordered and shipped. 618 \paragraph{Camera (Do)} The camera has to be ready six month after the 619 shipment of the other mechanical parts of the telescope. For this 620 purpose camera tests have to take place in 2009/2, which requires the 621 assembly of the camera within six months before. By now, a PM test 622 bench is set up in Dortmund, which allows to finish planning and 623 ordering of parts of the camera, including the PMs, until summer 2008, 624 before the construction begins. 625 In addition to the manpower permanently provided by Dortmund 626 for production and commissioning, two engineers will participate in the 627 construction phase. 628 \paragraph{Full System (Do/W\"{u})} The full system will be assembled 629 after the delivery of all parts in the beginning of spring 2009. Start of 630 the commissioning is planned four months later. First light is expected 631 in autumn 2009. This would allow an immediate full system test with a 632 well measured, strong and steady source (Crab Nebula). After the 633 commissioning phase will have been finished in spring 2010, complete 634 robotic operation will be provided. 587 635 588 636 Based on the experience with setting up the MAGIC telescope we estimate … … 600 648 \section[4]{Funds requested (Beantragte Mittel)} 601 649 602 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. 650 Summarizing, the expenses for the telescope are dominated by the camera 651 and data acquisition. We request funding for a total of three years. 605 652 %The financial volume for the complete hardware inclusive 606 653 %transport amounts to {\bf 372.985,-\,\euro}. … … 609 656 610 657 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 staff612 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.658 students, one in Dortmund and one in W\"{u}rzburg each (3\,x\,TV-L13).The 659 staff members shall fulfill the tasks given in the work schedule above. 660 To cover these tasks completely, one additional PhD and a various 661 number of Diploma students will complete the working group. 615 662 616 663 Suitable candidates interested in these positions are Dr.\ Thomas … … 623 670 At the Observatorio Roque de los Muchachos (ORM), at the MAGIC site, 624 671 the mount of the former HEGRA telescope CT3 now owned by the MAGIC 625 collaboration is still operational. One hut for electronics close to672 collaboration is still serviceable. One hut for electronics close to 626 673 the telescope is available. Additional space is available in the MAGIC 627 674 counting house. The MAGIC Memorandum of Understanding allows for … … 631 678 632 679 To achieve the planned sensitivity and threshold 633 (fig ure~\ref{sensitivity})the following components have to be bought.680 (fig.~\ref{sensitivity}), the following components have to be bought. 634 681 To obtain reliable results as fast as possible well known components 635 682 have been chosen. … … 640 687 \citep{Juan:2000,MAGICsensi,Vassiliev:1999} 641 688 and the expectation for DWARF, with both a PMT- and a 642 GAPD-camera . It is based onthe sensitivity of643 HEGRA~CT1 , scaledby the improvements mentioned in the text.689 GAPD-camera, scaled from the sensitivity of 690 HEGRA~CT1 by the improvements mentioned in the text. 644 691 } \label{sensitivity} } 645 692 \end{figure} 646 693 \clearpage 647 {\bf Camera}\dotfill 20 7.550,-\,\euro\\[-3ex]694 {\bf Camera}\dotfill 206.450,-\,\euro\\[-3ex] 648 695 \begin{quote} 649 696 To setup a camera with 313 pixels the following components are needed:\\ 650 697 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth} 651 698 Photomultiplier Tube EMI\,9083B\hfill 220,-\,\euro\\ 652 Active voltage divider ( {\bf !!!!})\hfill 80,-\,\euro\\653 High voltage support and control\hfill {\bf 300,-}\,\euro\\699 Active voltage divider (EMI)\hfill 80,-\,\euro\\ 700 High voltage support and control\hfill 300,-\,\euro\\ 654 701 Preamplifier\hfill 50,-\,\euro\\ 655 702 Spare parts (overall)\hfill 3000,-\,\euro\\ … … 659 706 criterion. To keep the systematic errors small, a good background 660 707 estimation is mandatory. The only possibility for a synchronous 661 determination of the background is the determinationfrom the night-sky708 determination of the background is the measurement from the night-sky 662 709 observed in the same field-of-view with the same instrument. To achieve 663 710 this, the observed position is moved out of the camera center which 664 711 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. 670 712 respect to the camera center (so called Wobble mode). This observation 713 mode increases the sensitivity by a factor of $\sqrt{2}$, because 714 spending observation time for dedicated background observations becomes 715 obsolete, i.e.\ observation time for the source is doubled. This 716 ensures in addition a better time coverage of the observed sources.\\ 671 717 A further increase in sensitivity can be achieved by better background 672 718 statistics from not only one but several independent positions for the 673 background estimation in the camera \citep{Lessard:2001}. For wobble mode674 observations allowing for this, the source positionshould be shifted719 background estimation in the camera \citep{Lessard:2001}. To allow for 720 this the source position in Wobble mode should be shifted 675 721 $0.6^\circ-0.7^\circ$ out of the camera center. 676 %} 677 678 A camera completely containing shower images of events in the energy 722 723 A camera completely containing the shower images of events in the energy 679 724 region of 1\,TeV-10\,TeV should have a diameter in the order of 680 725 5$^\circ$. To decrease the dependence of the measurements on the camera … … 686 731 \includegraphics*[width=0.495\textwidth,angle=0,clip]{cam271.eps} 687 732 \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$^\circ$.733 \caption{Left: Schematic picture of the 271 pixel CT3 camera with a field of view of 4.6$^\circ$. 689 734 Right: Schematic picture of the 313 pixel camera for DWARF with a field of view of 5$^\circ$.} 690 735 \label{camCT3} … … 693 738 \end{figure} 694 739 695 Therefor a camera with 313 pixel camera (see figure~\ref{camDWARF}) is740 Therefore a camera with 313 pixel camera (see fig.~\ref{camDWARF}) is 696 741 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)742 MAGIC. 19\,mm diameter Photomultiplier Tubes (PM, EMI\,9083B/KFLA-UD) 698 743 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 a744 a quantum efficiency improved by 25\% (see fig.~\ref{qe}) and ensure a 700 745 granularity which is enough to guarantee good results even below the 701 746 energy threshold (flux peak energy). Each individual pixel has to be … … 708 753 cameras. 709 754 710 {\bfAt ETH~Z\"{u}rich currently test measurements are ongoing to prove the755 At ETH~Z\"{u}rich currently test measurements are ongoing to prove the 711 756 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 e xtremely high quantum efficiency ($>$50\%), easier gain stabilization and715 simplified application compared to classical PMs. If these test 716 measurements are successfully finished until 8/2008 we consider to use 717 GAPDs in favor of classical PMs. The design of such a camera would take 718 place at University Dortmund in close collaboration with the experts 719 from ETH. Construction would also take place at the electronics 720 workshop of Dortmund.} 757 Geiger-mode APDs (GAPD) as photon detectors in the camera of a 758 Cherenkov telescope. The advantages are an extremely high quantum 759 efficiency ($>$50\%), easier gain stabilization and simplified 760 application compared to classical PMs. If these test measurements are 761 successfully finished until 8/2008, we consider to use GAPDs in favor 762 of classical PMs. The design of such a camera would take place at 763 University Dortmund in close collaboration with the experts from ETH. 764 The construction would also take place at the electronics workshop of 765 Dortmund. 721 766 722 767 \end{quote}\vspace{3ex} 723 768 724 {\bf Camera support}\dotfill 204.000,-\,\euro\\[-3ex]769 {\bf Camera support}\dotfill 7.500,-\,\euro\\[-3ex] 725 770 \begin{quote} 726 771 For this setup the camera holding has to be redesigned. (1500,-\,\euro) 727 772 The camera chassis must be water tight and will be equipped with an 728 automatic lid protecting the PMs at day-time. For further protection, a773 automatic lid, protecting the PMs at daytime. For further protection, a 729 774 plexi-glass window will be installed in front of the camera. By coating 730 775 this window with an anti-reflex layer of magnesium-fluoride, a gain in 731 transmission of {\bf 5\%}is expected. Each PM will be equipped with a732 light-guide (Winston Cone) as developed by UC Davis and successfully in733 operation in the MAGIC camera. (3000,-\,\euro\ for all winston cones). The776 transmission of 5\% is expected. Each PM will be equipped with a 777 light-guide (Winston cone) as developed by UC Davis and successfully in 778 operation in the MAGIC camera. (3000,-\,\euro\ for all Winston cones). The 734 779 current design will be improved by using a high reflectivity aluminized 735 780 Mylar mirror-foil, coated with a dialectical layer ($Si\,O_2$ … … 738 783 planned. 739 784 740 In total a gain of {\bf $\sim$15\%}in light-collection741 efficiency compared to the old CT3 system can be ach eived.785 In total a gain of $\sim$15\% in light-collection 786 efficiency compared to the old CT3 system can be achieved. 742 787 \end{quote}\vspace{3ex} 743 788 … … 751 796 %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ 752 797 For the data acquisition system a hardware readout based on an analog 753 ring buffer (Domino\ II/I II), currently developed for the MAGIC\II798 ring buffer (Domino\ II/IV), currently developed for the MAGIC~II 754 799 readout, will be used \citep{Barcelo}. This technology allows to sample 755 800 the pulses with high frequencies and readout several channels with a 756 801 single Flash-ADC resulting in low costs. The low power consumption will 757 allow to include the digitization near the signal source which makes758 the transfer of the analog signal obsolete. Th e advantage isless759 pick-up noise and lesssignal dispersion. By high sampling rates802 allow to include the digitization near the signal source making 803 the transfer of the analog signal obsolete. This results in less 804 pick-up noise and reduces the signal dispersion. By high sampling rates 760 805 (1.2\,GHz), additional information about the pulse shape can be 761 806 obtained. This increases the over-all sensitivity further, because the 762 807 short integration time allows for almost perfect suppression of noise 763 due to night-sky background photons. The estimated trigger- (readout-)764 r ate of the telescope is below 100\,Hz (HEGRA: $<$10\,Hz) which allows765 to use a low-cost industrial solution for readout of the system like 766 USB\,2.0.808 due to night-sky background photons. The estimated trigger-, i.e.\ 809 readout-rate of the telescope is below 100\,Hz (HEGRA: $<$10\,Hz) which 810 allows to use a low-cost industrial solution for readout of the system, 811 like USB\,2.0. 767 812 768 813 %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ 769 814 Current results obtained with the new 2\,GHz FADC system in the MAGIC 770 data acquisition show that for a single telescope a sensitivity815 data acquisition show, that for a single telescope a sensitivity 771 816 improvement of 40\% with a fast FADC system is achievable \citep{Tescaro:2007}. 772 817 773 Asfor the HEGRA telescopes a simple multiplicity trigger is818 Like for the HEGRA telescopes a simple multiplicity trigger is 774 819 sufficient, but also a simple neighbor-logic could be programmed (both 775 820 cases $\sim$100,-\,\euro/channel). 776 821 777 822 Additional data reduction and preprocessing within the readout chain is 778 provided. Assuming conservatively a readout rate of 30\,Hz the storage823 provided. Assuming conservatively a readout rate of 30\,Hz, the storage 779 824 space needed will be less than 250\,GB/month or 3\,TB/year. This amount 780 825 of data can easily be stored and processed by the W\"{u}rzburg … … 785 830 %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ 786 831 \begin{quote} 787 The existing mirrors are replaced by new plastic mirrors which are788 currently developed by Wolfgang Dr\"{o}ge's group. The cheap and 789 light-weight material has been formerly used for Winston cones in790 balloon experiments. The mirrors are copied from a mastercoated with a832 The existing mirrors will be replaced by new plastic mirrors currently 833 developed by Wolfgang Dr\"{o}ge's group. The cheap and light-weight 834 material has been formerly used for Winston cones in balloon 835 experiments. The mirrors are copied from a master and coated with a 791 836 reflecting and a protective material. Tests have given promising 792 837 results. By a change of the mirror geometry, the mirror area can be 793 838 increased from 8.5\,m$^2$ to 13\,m$^2$ (see picture~\ref{CT3} and 794 montage~\ref{DWARF}) ; this includes an increase of $\sim$10$\%$ per839 montage~\ref{DWARF}). This includes an increase of $\sim$10$\%$ per 795 840 mirror by using a hexagonal layout instead of a round one. A further 796 841 increase of the mirror area would require a reconstruction of parts of … … 803 848 804 849 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. 850 aluminized Mylar mirror-foil and a dialectical layer of $SiO_2$ as for 851 the Winston cones. By this, a gain in reflectivity of $\sim10\%$ is 852 achieved, see fig.~\ref{reflectivity} \citep{Fraunhofer}. Both 853 solutions would require the same expenses. 810 854 811 855 To keep track of the alignment, reflectivity and optical quality of the … … 814 858 adjustment system, as developed by ETH~Z\"{u}rich and successfully 815 859 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 a822 telescope located at 2000\,m above sea level. The mirror's reflectivity823 of a 300\,nm thick aluminum layer with a protection layer of 10\,nm and824 100\,nm thickness respectively. For comparison the reflectivity of825 HEGRA CT1's mirrors \citep{Kestel:2000} are shown. The bottom plot depicts826 the quantum efficiency of the prefered PMs (EMI) together with the827 predecessor used in CT1. A proper coating \citep{Paneque:2004} will828 further enhance its effciency. An even better increase would be the829 usage of Geiger-mode APDs.}830 831 \label{cherenkov}832 \label{reflectivity}833 \label{qe}834 }835 \end{figure}836 860 837 861 %<grey>The system … … 839 863 840 864 %{\bf For a diameter mirror of less than 2.4\,m, the delay between an 841 %parabolic (isochron us) and a spherical mirror shape at the edge is well865 %parabolic (isochronous) and a spherical mirror shape at the edge is well 842 866 %below 1ns (see figure). Thus for a sampling rate of 1.2\,GHz parabolic 843 867 %individual mirrors are not needed. Due to their small size the … … 846 870 \end{quote}\vspace{3ex} 847 871 848 {\bf Calibration System}\dotfill 6.650,-\,\euro+IPR?\\[-3ex]872 {\bf Calibration System}\dotfill 9.650,-\,\euro\\[-3ex] 849 873 \begin{quote} 850 874 Components\\ 851 875 \parbox[t]{1em}{~}\begin{minipage}[t]{0.6\textwidth} 852 876 Absolute light calibration\hfill 2.000,-\,\euro\\ 853 Individual pixel rate control\hfill ???,-\,\euro\\877 Individual pixel rate control\hfill 3.000,-\,\euro\\ 854 878 Weather station\hfill 500,-\,\euro\\ 855 879 GPS clock\hfill 1.500,-\,\euro\\ … … 858 882 %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ 859 883 For the absolute light calibration (gain-calibration) of the PMs a 860 calibration box as successfully used in the MAGIC telescopewill be884 calibration box, as successfully used in the MAGIC telescope, will be 861 885 produced. 862 886 863 887 To ensure a homogeneous acceptance of the camera, essential for 864 wobble-mode observations, the trigger rate of the individual pixels888 Wobble mode observations, the trigger rate of the individual pixels 865 889 will be measured and controlled. 866 890 867 To correct foraxis misalignments and possible deformations of the868 structure (e.g.\ bending of camera holding masts) ,a pointing correction869 algorithm as used in the MAGIC tracking system will be applied. It is891 For a correction of axis misalignments and possible deformations of the 892 structure (e.g.\ bending of camera holding masts) a pointing correction 893 algorithm will be applied, as used in the MAGIC tracking system. It is 870 894 calibrated by measurements of the reflection of bright guide stars on 871 895 the camera surface and ensures a pointing accuracy well below the pixel 872 896 diameter. Therefore a high sensitive low-cost video camera, as for 873 MAGIC\ I and~II, ( {\bf300,-\,\euro\ camera, 600,-\,\euro\ optics,874 300,-\,\euro\ housing, 250,-\,\euro\ Frame grabber}) will be installed.897 MAGIC\ I and~II, (300,-\,\euro\ camera, 600,-\,\euro\ optics, 898 300,-\,\euro\ housing, 250,-\,\euro\ frame grabber) will be installed. 875 899 876 900 A second identical CCD camera for online monitoring (starguider) will 877 901 be bought. 878 902 879 A GPS clock is necessary for an accurate tracking. The weather station903 For an accurate tracking a GPS clock is necessary. The weather station 880 904 helps judging the data quality. 881 905 %}\\[2ex] 882 906 \end{quote}\vspace{3ex} 883 884 907 885 908 {\bf Computing}\dotfill 12.000,-\,\euro\\[-3ex] … … 904 927 \end{quote}\vspace{3ex} 905 928 929 %%%%%%%%%%%%%% PLOTS HERE???? %%%%%%%%%%%%%%%%%%%%%%%%%% 930 906 931 {\bf Mount and Drive}\dotfill 17.500,-\,\euro\\[-3ex] 907 932 \begin{quote} 908 933 %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ 909 934 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 drivesystem should allow for relatively fast repositioning for three935 corrosion protection, cable ducts, etc. is needed (7.500,-\,\euro). 936 937 Motors, shaft encoders and control electronics in the order of 938 10.000,-\,\euro\ have to be bought. The costs have been estimated with 939 the experience from building the MAGIC drive systems. The DWARF drive 940 system should allow for relatively fast repositioning for three 916 941 reasons: (i)~Fast movement might be mandatory for future ToO 917 observations. (ii)~Wobble -mode observations will be done changing the918 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 t ime, the observed source will be changed in constant time intervals921 ($\sim$20\,min). 922 923 Thereforethree 150\,Watt servo motors are intended to be bought. A942 observations. (ii)~Wobble mode observations will be done changing the 943 Wobble-position continuously (each 20\,min) for symmetry reasons. 944 (iii)~To ensure good time coverage of more than one source visible at 945 the same time, the observed source will be changed in constant time 946 intervals. 947 948 For the drive system three 150\,Watt servo motors are intended to be bought. A 924 949 micro-controller based motion control unit (Siemens SPS L\,20) similar to 925 950 the one of the current MAGIC~II drive system will be used. For 926 communication with the readout-system, a standard ethernet connection951 communication with the readout-system, a standard Ethernet connection 927 952 based on the TCP/IP- and UDP-protocol will be setup. 928 953 %}\\[2ex] … … 940 965 telescope position at the time of sunrise. 941 966 942 A fence for protection in case of robotic movementwill be967 For protection in case of robotic movement a fence will be 943 968 installed.%}\\[2ex] 944 969 \end{quote}\vspace{3ex} … … 951 976 %\parbox[t]{1em}{~}\parbox[t]{0.955\textwidth}{ 952 977 For remote, robotic operation a variety of remote controllable electronic 953 components such as ethernet controlled sockets and switches will be978 components such as Ethernet controlled sockets and switches will be 954 979 bought. Monitoring equipment, for example different kind of sensors, is 955 980 also mandatory.%}\\[2ex] … … 957 982 \hspace*{0.66\textwidth}\hrulefill\\[0.5ex] 958 983 \hspace*{0.66\textwidth}\hspace{0.5ex}\hfill Sum 4.2:\hfill{\bf 959 34 2.235,-\,\euro}\hfill\hspace*{0pt}\\[-1ex]984 340.635,-\,\euro}\hfill\hspace*{0pt}\\[-1ex] 960 985 \hspace*{0.66\textwidth}\hrulefill\\[-1.9ex] 961 986 \hspace*{0.66\textwidth}\hrulefill\\ 987 988 \begin{figure}[p] 989 \centering{ 990 \includegraphics[width=0.57\textwidth]{cherenkov.eps} 991 \includegraphics[width=0.57\textwidth]{reflectivity.eps} 992 \includegraphics[width=0.57\textwidth]{qe.eps} 993 \caption{Top to bottom: The Cherenkov spectrum as observed by a 994 telescope located at 2000\,m above sea level. The mirror's reflectivity 995 of a 300\,nm thick aluminum layer with a protection layer of 10\,nm and 996 100\,nm thickness respectively. For comparison the reflectivity of 997 HEGRA CT1's mirrors \citep{Kestel:2000} are shown. The bottom plot depicts 998 the quantum efficiency of the preferred PMs (EMI) together with the 999 predecessor used in CT1. A proper coating \citep{Paneque:2004} will 1000 further enhance its efficiency. An even better increase would be the 1001 usage of Geiger-mode APDs.} 1002 1003 \label{cherenkov} 1004 \label{reflectivity} 1005 \label{qe} 1006 } 1007 \end{figure} 962 1008 963 1009 \subsection[4.3]{Consumables (Verbrauchsmaterial)} … … 966 1012 % \parbox[t]{1em}{~}\begin{minipage}[t]{0.9\textwidth} 967 1013 10 LTO\,4 tapes (8\,TB)\dotfill 750,-\,\euro\\ 968 Consumables (overalls) tools and materials\dotfill 10.000,-\,\euro1014 Consumables (overalls): tools and materials\dotfill 10.000,-\,\euro 969 1015 % \end{minipage}\\[-0.5ex] 970 1016 \end{quote} … … 976 1022 \hspace*{0.66\textwidth}\hrulefill\\ 977 1023 978 \subsection[4.4]{ Reisen (Travel expenses)}1024 \subsection[4.4]{Travel expenses (Reisen)} 979 1025 The large amount of travel funding is required due to the very close 980 1026 cooperation between Dortmund and W\"{u}rzburg and the work demands on … … 1009 1055 1010 1056 1011 \subsection[4.5]{Publi kationskosten (Publication costs)}1057 \subsection[4.5]{Publication costs (Publikationskosten)} 1012 1058 Will be covered by the proposing institutes. 1013 1059 … … 1037 1083 \setlength{\itemsep}{0pt} 1038 1084 \setlength{\parsep}{0pt} 1039 \item Prof.\ Dr.\ Dr.\ Wolfgang Rhode (Grundaust tattung)1085 \item Prof.\ Dr.\ Dr.\ Wolfgang Rhode (Grundauststattung) 1040 1086 \item Dr.\ Tanja Kneiske (Postdoc (Ph"anomenologie), DFG-Forschungsstipendium) 1041 1087 \item Dr.\ Julia Becker (Postdoc (Ph"anomenologie), Drittmittel) 1042 1088 \item Dipl.-Phys.\ Kirsten M"unich (Doktorand (IceCube), Drittmittel) 1043 \item Dipl.-Phys.\ Jens Dreyer (Doktorand (IceCube), Grundaust tattung)1089 \item Dipl.-Phys.\ Jens Dreyer (Doktorand (IceCube), Grundauststattung) 1044 1090 \item M.Sc.\ Valentin Curtef (Doktorand (MAGIC), Grundausstattung) 1045 1091 \item cand.\ phys.\ Michael Backes (Diplomand (MAGIC), zum F"orderbeginn diplomiert) … … 1078 1124 \originalTeX 1079 1125 1080 \subsection[5.2]{Co -operation with other scientists\\(Zusammenarbeit mit1126 \subsection[5.2]{Cooperation with other scientists\\(Zusammenarbeit mit 1081 1127 anderen Wissenschaftlern)} 1082 1128 1083 Both applying groups co -operate with the international1084 MAGIC -Collaboration and the institutes represented therein. (W\"{u}rzburg1129 Both applying groups cooperate with the international 1130 MAGIC collaboration and the institutes represented therein. (W\"{u}rzburg 1085 1131 funded by the BMBF, Dortmund by means of appointment for the moment). 1086 1132 … … 1096 1142 The group in Dortmund is involved in the IceCube experiment (BMBF 1097 1143 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. 1144 Moreover on the field of phenomenology good working contacts exist to 1145 the groups of Prof.~Dr.~Reinhard Schlickeiser, Ruhr-Universit\"{a}t 1146 Bochum and Prof.~Dr.~Peter Biermann, MPIfR Bonn. There are furthermore 1147 intense contacts to Prof.~Dr.~Francis Halzen, Madison, Wisconsin. 1103 1148 1104 1149 The telescope design will be worked out in close cooperation with the … … 1106 1151 Prof.~Dr.~Eckart Lorenz (ETH~Z\"{u}rich). They will provide help in design 1107 1152 studies, construction and software development. The DAQ design will be 1108 contributed by the group of Prof.~Dr.~Riccardo Paoletti (Universit àdi1153 contributed by the group of Prof.~Dr.~Riccardo Paoletti (Universit\`{a} di 1109 1154 Siena and INFN sez.\ di Pisa, Italy). 1110 1155 1111 The group of the newly appointed {\em Lehrstuhl f\"{u}r Physik und Ihre1156 The group of the newly appointed {\em Lehrstuhl f\"{u}r Physik und ihre 1112 1157 Didaktik} (Prof.~Dr.~Thomas Trefzger) has expressed their interest to 1113 1158 join the project. They bring in a laboratory for photo-sensor testing, … … 1120 1165 The work on DWARF will take place at the ORM on the Spanish island La 1121 1166 Palma. It will be performed in close collaboration with the 1122 MAGIC -Collaboration.1167 MAGIC collaboration. 1123 1168 1124 1169 \subsection[5.4]{Scientific equipment available (Apparative … … 1127 1172 storage as well as for data analysis are available. 1128 1173 1129 The faculty of physics at the University ofDortmund has modern1174 The faculty of physics at the University Dortmund has modern 1130 1175 equipped mechanical and electrical workshops including a department for 1131 1176 development of electronics at its command. The chair of astroparticle … … 1184 1229 \end{minipage}\hfill~ 1185 1230 1231 \thispagestyle{empty} 1232 \newpage 1233 x 1234 \thispagestyle{empty} 1186 1235 \newpage 1187 1236 \paragraph{8 List of appendices (Verzeichnis der Anlagen)} … … 1197 1246 \item Letter of Support from the IceCube collaboration 1198 1247 \item Letter of Support from KVA optical telescope 1248 \item Email with offer from EMI for the PMs 1199 1249 \end{itemize} 1200 1201 1250 \newpage 1202 %\section{References} 1203 1204 (References of our groups are marked by an asterix *) 1251 x 1252 \thispagestyle{empty} 1253 \newpage 1254 1255 %(References of our groups are marked by an asterix *) 1205 1256 \bibliography{application} 1206 1257 \bibliographystyle{plainnat}
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