Changeset 8610 for trunk

Timestamp:

06/26/07 12:25:25 (17 years ago)

Author:

tbretz

Message:

*** empty log message ***

File:

• trunk/Dwarf/Documents/ApplicationDFG/application.tex (modified) (19 diffs)

trunk/Dwarf/Documents/ApplicationDFG/application.tex

@@ -192 +192 @@
 \section[2]{Stand der Forschung, eigene Vorarbeiten\\State of the art, preliminary work by proposer}
 
-\subsection[2.1]{Stand der Forschung/State of the art}
+\subsection[2.1]{State of the art (Stand der Forschung)}
 
 {\em
@@ -203 +203 @@
 }
 
-\textbf{Introduction:} Since the termination of the HEGRA observations,
-the succeeding experiments MAGIC and H.E.S.S.\ have impressively extended
-the physical scope of gamma ray observations by detecting tens of
-formerly unknown gamma ray sources and analyzing their energy spectra
-and temporal behavior. This became possible by lowering the energy
-threshold from 700 GeV to less than 100 GeV and increasing at the same
-time the sensitivity by a factor of five.\\ To fully exploit the
-discovery potential of the improved sensitivity, the discovery of new,
-faint objects has become the major task for the new telescopes. A
-diversity of astrophysical source types such as pulsar wind nebulae,
-supernova remnants, microquasars, pulsars, radio galaxies, clusters of
-galaxies, gamma ray bursts, and blazers can be studied with these
-telescopes and limits their availability for monitoring purposes of
-well-known bright sources.\\ There are strong reasons to make an effort
-for the continuous monitoring of the few exceptionally bright blazars.
-This can be achieved by operating a dedicated monitoring telescope of
-the HEGRA-type, referred to in the following as DWARF (Dedicated
+\paragraph{Introduction:} Since the termination of the HEGRA
+observations, the succeeding experiments MAGIC and H.E.S.S.\ have
+impressively extended the physical scope of gamma ray observations by
+detecting tens of formerly unknown gamma ray sources and analyzing
+their energy spectra and temporal behavior. This became possible by
+lowering the energy threshold from 700 GeV to less than 100 GeV and
+increasing at the same time the sensitivity by a factor of five.
+
+To fully exploit the discovery potential of the improved sensitivity,
+the discovery of new, faint objects has become the major task for the
+new telescopes. A diversity of astrophysical source types such as
+pulsar wind nebulae, supernova remnants, microquasars, pulsars, radio
+galaxies, clusters of galaxies, gamma ray bursts, and blazers can be
+studied with these telescopes and limits their availability for
+monitoring purposes of well-known bright sources.
+
+There are strong reasons to make an effort for the continuous
+monitoring of the few exceptionally bright blazars. This can be
+achieved by operating a dedicated monitoring telescope of the
+HEGRA-type, referred to in the following as DWARF (Dedicated
 multiWavelength Agn Research Facility). The reasons are outlined in
 detail below.
 
+\textbf{The science case:} The variability of blazars, seen across the
+entire electromagnetic spectrum, arises from the dynamics of
+relativistic jets and the particle acceleration going on in them. The
+jets are launched from the vicinity of accreting supermassive black
+holes, and theoretical models predict variability arising from the
+interplay between jet expansion, particle injection, acceleration and
+cooling.\\
+
+Long-term monitor observations of bright blazars are the key to obtain
+a solid and complete data base for variability investigations. 
+
+{\bf Hier sollte ganz klar rauskommen warum man unbedingt ein 
+long-term monitoring IACT braucht}
+
+{\bf Geigermde APDs?}
 
 \subsubsection{High energy gamma and neutrino sources}
 
-%============================================================
-%Der TeV-Photon-Astronomie ist es in den letzten Jahrzehnten gelungen, {\bf 14}
-%extragalaktische und {\bf ???} galaktische Objekte am Himmel zu
-%identifizieren. Hinzu kommt die Detektion von zwei diffusen Regionen in der
-%Galaxie, die von H.E.S.S. {\bf ZITAT!} und Milagro {\bf ZITAT!!!} gesehen
-%wurden. Die erste Quelle wurde im Jahr {\bf 19??} von {\bf HEGRA ???}
-%beobachtet. Im Vergleich zu R\"ontgen-Messungen, die den Himmel nach Quellen
-%abscannen k\"onnen und dementsprechend mehr als {\bf 1000 ???} Quellen
-%katalogisiert haben {\bf ZITAT KATALOG XMM Newton/Chandra}, scheint diese
-%Anzahl jedoch sehr niedrig. Ein Grund ist das kleine Sichtfeld, was
-%Luft-Cherenkov Teleskope besitzen, ein weiterer, dass das TeV-Photon Signal weit entfernter Quellen
-%($z>0.2$) vom extragalaktischen Hintegrundlicht absorbiert wird.  
-%Aufgrund der geringen Statistik an Quellen ist es zu diesem Zeitpunkt ist es notwendig, dass sich hochsensitive Instrumente
-%prim"ar auf die Untersuchung neuer Objekte am TeV-Photon-Himmel konzentrieren
-%und nicht auf die quantitative, permanente Beobachtung von schon bekannten
-%Quellen. Selbst wenn eine Quelle "uber einen l"angeren Zeitraum beobachtet
-%wurde, handelt es sich hier um einen Zeitraum von {\bf $<3$~Monaten ????}. In
-%dieser Zeit fallen jedoch sowohl Schlechtwetter-Perioden wie auch Phasen mit
-%starker Mond-Einstrahlung weg. Au{\ss}erdem muss beachtet werden, dass die
-%Quelle nur eine geringe Anzahl an Stunden sichtbar am Himmel ist.  
+{\bf Aus den folgenden beiden Abschnitten kann man vielleicht einen 
+(k"urzeren) machen?}
 
 The TeV photon astronomy succeeded in discovering {\bf 14}
 extragalactic and {\bf ???} galactic objects at the sky during the past
 decades. Additionally there are two diffuse regions within our galaxy
-which have been detected by H.E.S.S.\cite{Aharonian:2006} and Milagro {\bf ZITAT!!! }
- {\it Neues Millagro Papier mit "TeV Gamma-Ray Sources from a Survex
- of the Galactic Plane with Milagro} 4+ Quellregionen: "TeV
-Gamma-Ray Sources from a Survey of the Galactic  Plane with Milagro"
-Arxiv-Nr.: 0705.0707 The first source was discovered in the year
-19{\bf??} by the {\bf HEGRA} collaboration {\it (War das nicht wer
+which have been detected by H.E.S.S.\cite{Aharonian:2006} and Milagro
+{\bf ZITAT!!! } {\it Neues Millagro Papier mit "TeV Gamma-Ray Sources
+from a Survex of the Galactic Plane with Milagro} 4+ Quellregionen:
+"TeV Gamma-Ray Sources from a Survey of the Galactic  Plane with
+Milagro" Arxiv-Nr.: 0705.0707 The first source was discovered in the
+year 19{\bf??} by the {\bf HEGRA} collaboration {\it (War das nicht wer
 anders, die zu allererst den Crab sahen?...ZITAT?)}. In comparison to
 x-ray measurments, which are able to scan the entire sky for sources
@@ -268 +268 @@
 sources. Even when a source was observed over a longer period of time
 this does mean {\bf  less than three month ???? {\it Viel l"anger sind
-die Quellen am St"uck doch gar nicht sichtbar, oder? Sinnvoller w"are es
-wom"oglich die wenigen Beobachtungsstunden in diesen X Monaten
+die Quellen am St"uck doch gar nicht sichtbar, oder? Sinnvoller w"are
+es wom"oglich die wenigen Beobachtungsstunden in diesen X Monaten
 hervorzuheben.}} But one has to take into account that during this time
 also periods of bad weather and times with strong moon light can
-significantly reduce  observation time. Furthermore on has to consider
-that the sources are visible in the sky for few hours only. {\it Kann
-man das wirklich so sagen?}
-
-%Bei den bisher beobachteten galaktischen Objekten handelt es sich um
-%Mikroquasare und Supernova \"Uberreste, die identifizierten extragalaktischen
-%Objekte sind Aktive Galaxien (AGN). Die Objekte sind in Tabelle~\ref{tev_objects}
-%aufgelistet {\bf TESHIMAS VORTRAG IN MADISON}. Bei den AGN handelt es sich um
-%13 BLLacs und um eine FR-I Galaxie, M87. 
+significantly reduce  observation time. Furthermore one has to consider
+that the sources are visible in the sky only for a few hours each night.
 
 The so far observed galactic objects are microqasars and supernova
@@ -292 +285 @@
 new sources (luminosity function, redshift distribution).
 
-%Im Falle von hadronischer Teilchenbeschleunigung in den TeV Quellen, kann das
-%TeV Signal von $\pi^0$-Zerf"allen herr"uhren. Die neutralen Pionen kommen
-%von Delta-Resonanz Zerf"allen, die durch Proton-Photon Wechselwirkungen
-%entstehen. Ein weiterer Kanal im Zerfall der Delta-Resonanz f"uhrt zur
-%Produktion von geladenen Pionen und damit zur Produktion von Neutrinos in
-%koinzidenz mit TeV Photonen. Daher sind TeV Quellen auch immer interessant
-%f"ur Hochenergie-Neutrinoteleskope.
-
 In case of hadronic particle acceleration within the TeV emitters, the
 TeV signal may arise from $\pi^0$-decays. These neutral pions are decay
@@ -309 +294 @@
 telescopes.
 
-%Die hohe Variabilit"at in der zeitlichen Entwicklung der AGN
-%TeV-Photon-Spektren kann bisher noch nicht schl"ussig erkl"art
-%werden
 The strong variability in the temporal evolution of the AGN TeV photon
-spectra cannot be explained conclusively yet,
-
-{\it .... blabla quantitative Untersuchungen, d.h.
-Langzeituntersuchungen notwendig.}
-
-{\bf SENSITIVIT\"ATSPLOT}\\
-{\bf TABELLE QUELLEN}\\
-{\bf AGN Physik kann man nicht ohne die unteren Paragraphen erkl"aren}\\
+spectra cannot be explained conclusively yet, {\it warum braucht man
+f"ur die Untersuchung Langzeitbeobachtungen?}
+
+{\bf SENSITIVIT\"ATSPLOT, Was hat der hier zu suchen?}\\
+{\bf TABELLE QUELLEN, Was bringt das f"ur den Antrag oder den Referee?}\\
+{\bf AGN Physik kann man nicht ohne die unteren Paragraphen erkl"aren,
+Muss man die hier erkl"aren? Wir m"ussen nur deutlich machen warum wir 
+Langzeitbeobachtungen brauchen, nicht, dass wir die Physik verstehen}\\
 {\it Die Frage ist, ob man galaktische Quellen mit in die
 Langzeit-Beobachtung nehmen will, dann mu"s man das einzeln
-durchgehen. Ich bau die Argumentation gerade nur auf AGN auf:}
+durchgehen. Ich bau die Argumentation gerade nur auf AGN auf,
+keine galaktischen Quellen!}
 
 \begin{itemize}
 \item Welche Quellen wurden oberhalb von 1 TeV bislang beobachtet?
 \item Welche Sensitivit"at braucht man?
-\item Warum braucht man Langzeitbeobachtungen?
-\item Warum stehen diese Beobachtungen nicht auf der Speisekarte der
-gro"sen neuen Telekope?
+\item $\to$ Hier muesste doch der Abschnitt aus Ziele und ein Verweis
+darauf reichen, das HEGRA die Quellen detektiert hat und wir besser
+sein werden, oder?
 \end{itemize}
 
 \paragraph{Physikalische Modelle}
 Erkl"are die verschiedenen Szenarien:
+{\bf Ist das wirklich n"otig. Da sollten doch referenzen reichen...
+das ist ja wirklich nichts aktuelles!}
 \begin{itemize}
 \item Inverse Compton
@@ -347 +332 @@
 
 Au"serdem: Stand der Dinge, um die Variabilit"at zu erkl"aren
+{\bf (Wichtig?) }
 
 \paragraph{Ergebnisse von Multiwavelangth-Kampangen}
@@ -363 +349 @@
 
 \paragraph{Die Photon-Neutrino-Verbindung}
-BLABLA-\\
-
-\textbf{The science case:} The variability of blazars, seen across the
-entire electromagnetic spectrum, arises from the dynamics of
-relativistic jets and the particle acceleration going on in them. The
-jets are launched from the vicinity of accreting supermassive black
-holes, and theoretical models predict variability arising from the
-interplay between jet expansion, particle injection, acceleration and
-cooling.\\
-
-Long-term monitor observations of bright blazars are the key to obtain
-a solid data base for variability investigations. 
+{\bf Steht das nicht oben schon {\em AGNs are interstng
+Targets for Neutrino Teleskops}?}
 
 \subsection{Eigene Vorarbeiten/Preliminary work by proposer}
@@ -387 +363 @@
 }
 
-
-\subsubsection{Quellphysik}
+Hie sollte was stehen zu (Ich denke der Abschnitt ist wichtig um zu
+zeigen, dass man auch leisten kann was man verspricht)
+\begin{itemize}
+\item Aufbau von Drive und Starguider (W"urzburg)
+\item Erfahrungen mit Spiegeln (Dr"oge, W"urzburg)
+\item Erfahrungen mit PMTs/HV (Dortmund)
+\item Erfahrungen mit HPDs (W"urzburg)
+\item Die modulare und powerfull Analyse Software (W"urzburg)
+\item Das bestreben die MCs modular umzuschreiben (W"urzburg, Dortmund?)
+\item Erfahrungen mit MCs: Unfolding, Athmosphaere, Corsika? (Dortmund)
+\item Die Automatisierung der Analyse und MCs, wichtig! (W"urzburg)
+\item Neutrino Studien, um zu zeigen, dass die angestrebten 
+Korrelationen auch wirklich von jemandem ausgewertet werden k"onnen 
+(Dortmund)
+\item Multi-Wellenl"angen Kampagnen (Suzaku, Swift), W"urzburg/Dortmund?
+\item Bestehende Monitoring Proposal (MAGIC)
+\item Die SSC Modellrechnungen aus W"urzburg
+\item LISA? (W"urzburg)
+\end{itemize}
+
 
 \subsubsection{Beteiligung an Experimenten}
@@ -403 +397 @@
 group for MAGIC is modular and flexible, and can thus be used with
 minor changes for the DWARF project.\\
-
-Ring-Methode f"ur wobble-modus aus W"urzburg?
 
 Monte Carlo production and storage will take place at Universit"at
@@ -438 +430 @@
 telescope. \textbf{WHIPPLE wird aber noch benutzt!!!}
 
-The layout of the telescope shall be carried out modular in
-such a sense that components of future telescopes (mirror, camera, DAQ)
-can be tested and optimized at this bodywork.
+The layout of the telescope shall be carried out modular in such a
+sense that components of future telescopes (mirror, camera, DAQ) can be
+tested and optimized at this bodywork.
 
 %Wissenschaftlich sollen folgende Punkte realisiert werden:
-Scientifically the following aims shall be realized:
-
-\begin{itemize}
-%\item[(1)] Langzeitbeobachtungen zeitlicher Variationen von TeV-Gamma-Ray-Quellen.\\
-\item[(1)] Long-term observations of temporal variations of TeV gamma
+With the upgraded instrument the following scientific aims shall be
+realized:
+
+\begin{enumerate}
+\item Long-term observations of temporal variations of TeV gamma
 ray sources.\\
 An understanding of this variability will deepen our knowledge about
+
   \begin{itemize}
   \item the composition and generation of the jets, intimately connected
@@ -467 +460 @@
 \item Rieger; On the geometric origin of periodicity in blazar-type sources
 }}
-  \end{itemize} 
+  \end{itemize}
+
 Long-term monitor observations of bright blazars are the key to obtain
 a solid data base for variability investigations. Assuming
@@ -477 +471 @@
 \textbf{\textit{oder ist dieser Abschnitt doch besser in 3.2.
 aufgehoben?!}} 
-\item[(2)] Coincident observations with gamma telescopes in different
+
+\item Coincident observations with gamma telescopes in different
 energy ranges:\\ Flux variations will be determined and compared with
 variability properties in other wavelength ranges. 
-\item[(3)] Coincident observations with the neutrino telescope
+
+\item Coincident observations with the neutrino telescope
 IceCube:\\ Hadronic emission processes and possible coincidences
 between VHE-gamma and neutrino-emission will be studied. 
-\item [(5)] Furthermore, we seek to obtain know-how for the operation
+
+\item Furthermore, we seek to obtain know-how for the operation
 of future networks of Cherenkov telescopes (e.g. a monitoring array
 around the globe or CTA) or telescopes at inaccessible sites. 
-\end {itemize}
+\end {enumerate}
 
 \subsection{Arbeitsprogramm/Work schedule}
@@ -513 +510 @@
 determined and compared with variability properties in other wavelength
 ranges.
+
 \item The lightcurves will be interpreted using models for the
 nonthermal emission from relativistically expanding plasma jets. In
@@ -519 +517 @@
 (Graduiertenkolleg, GK1147) shall be used. Particle acceleration is
 studied with hybrid MHD and particle-in-cell methods.
+
 \item {The black hole mass and accretion rate will be determined from
 the emission models. Estimates of the black hole mass from emission
@@ -525 +524 @@
 galaxy) will be compared.
 \textbf{\item Rieger, Mannheim; On the central black hole mass in Mkn 501}}
-\item \textbf{To achieve a maximal database for these studies the observation 
-schedule will be arranged together with the one for Whipple. (Letter of 
-support?) ($\rightarrow$ collaboration with Veritas)}
+
+\item \textbf{To achieve a maximal database for these studies the
+observation  schedule will be arranged together with the one for
+Whipple. (Letter of  support?) ($\rightarrow$ collaboration with
+Veritas)}
+
 \item When flaring states will be discovered during the monitor
 program, MAGIC will issue a Target of Opportunity observation to obtain
@@ -533 +535 @@
 Target-of-Opportunity (ToO) proposals to H.E.S.S.\ and Veritas are in
 preparation.
-\item
-\textbf{Additionally DWARF observations will be combined with
-simultaneous MAGIC observations via a software coincidence trigger.
-Recent simulations for CTA ref{MAGIC-CTA-Simulationen} show that by
-this kind of observation the energy range of the larger telescope can
-hugely be stretched to higher energies. This in turn leads to the so
-far unique possibility to cover an energy range of tens of GeV to
-several tens of TeV at the same time leading to the possibility of
-studying inverse compton peaks as well as absorption due to EBL
-simultaneously.} 
+
+\item DWARF observations will be combined with simultaneous MAGIC
+observations. By this kind of observation the energy range of the MAGIC
+telescope can be stretched to higher energies. This in turn leads to
+the so far unique possibility to cover an energy range of tens of GeV
+to several tens of TeV at the same time allowing the study of the
+inverse compton peaks as well as absorption due to EBL simultaneously.
+By a software coincidence trigger the sensitivity in the overlapping
+energy region might be improved further.
 
 \item Correlating the arrival times of neutrinos detected by the
@@ -550 +551 @@
 sources. The investigation proposed here is complete for both, neutrino
 and gamma observations, and can therefore lead to conclusive results.
+
 \item The diffusive fluxes of escaping UHE cosmic rays obtained from
 AUGER or flux limits of neutrinos from IceCube, respectively, will be
 used to constrain models of UHE cosmic ray origin and large-scale
 magnetic fields.
+
 \item Multi-frequency observations together with the Mets"ahovi Radio
 Observatory and the optical Tuorla Observatory are planned (Letters of
@@ -559 +562 @@
 and GLAST results, when available. X-ray monitoring using the SWIFT and
 Suzaku facilities will be proposed.
+
 \item The most ambitious scientific goal of this proposal is the search
 for signatures of binary black hole systems from orbital modulation of
@@ -1252 +1256 @@
 %\section{References}
 
-\vskip0.3cm
-
 %\bibliographystyle{alpha}
 \newpage