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ISAPP Poster

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ISAPP Summer Institute 2009 at the Karlsruhe Institute of Technology

Program

Participants of the Summer Institute will meet at campus North on 20th of July 13:00h, for registration and introduction.

All lectures are given at KIT-Campus-north, either in the FTU ("Mittlerer Hörsaal"), or Building 401 , Room 410 (4th floor).
FTU = Traning center of the Research Center, located in front of the main entrance of campus north.

Overview lectures - - - - special lectures - - - - time table - - - - practical work

Overview lectures:

speaker
topic
affiliation
Johannes Blümer
Introduction to ISAPP-SI09
KIT, KCETA
Steen Hannestad
Introduction to modern cosmology
University of Aarhus
Guido Drexlin
Phenomenology of neutrinos & neutrino masses
KIT, KCETA
Christian Weinheimer
Single ß decay experiments: overview&KATRIN
University of Münster
Hans Kraus
Dark Matter in Cosmology and Astrophysics
University of Oxford
Klaus Eitel
Direct DM search and cryogenic bolometers
KIT, KCETA
Ralph Engel
The physics of Cosmic Rays
KIT. KCETA
Markus Roth
Overview of the Pierre Auger Observatory
KIT, KCETA
Dieter Zeppenfeld
Particle Physics Programme at LHC
KIT, KCETA
Thomas Müller
Overview of the CMS detector system
KIT, KCETA
     
   

Special lectures:

Wolfgang Menn,
Indirect DM search -- balloons, satellites, ISS
University of Siegen
Tim Huege
Advanced techniques for detection of UHE CR´s
KIT, KCETA
Andreas Heiss
Grid computing
KIT, SCC
Frank Hartmann
Silicon detector technology
CERN & KIT
Joachim Wolf
Vacuum technology
KIT, KCETA
Michal Kreps
data analysis & neural networks
KIT, KCETA
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Time table:

lectures
practical work
students
excursions
 
           
 
Mo 20. 07
Tue
Wed
Thurs
Fri
09:00 FTU
  practical work
10:15
 
     
coffee break
   
10:45 FTU
  in small groups

Dieter
Zeppenfeld

12:00
 
     
lunch break
   
13:00 Bd 401
registration
students presentations
 
(15min)
KATRIN
bioliq
14:30
Introduction
15:00
       
         
 
 
practical work in small groups
 
17:30
       
           
 
Mo 27. 07
Tue
Wed
Thurs
Fri
09:00 FTU

excursion to
MPIK Heidelberg

Talks:

Lindner

Bezrukov

 
10:15
   
coffee break
 
10:45/11:00
11:00 Bd 401
Tim Huege part I part II
12:00/12:15
     
lunch break
 
13:00
ANKA
research reactor FR2
 

KASCADE Grande

14:30
 
   
 

   
practical work in small groups
free time in Heidelberg
 
         
17:30
       
   
joint dinner
   
         
           
 
Mo 03. 08.
Tue
Wed
Thurs
Fri
09:00
   
 
reports
10:45
practical work
 
(ct´d)
         
discussion
résumé
11:00 Bd 401
12:15
     
lunch break
   
13:00
         
   
practical work in small groups
reports from
 
       
lab works
 
           
17:30
         
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Practical work:

Please note that the program of practical work may change. When applying, you can give preference for a few topics. Typically 2 participants are working on one topic.
 

Determination of the top quark mass

Using CDF data corresponding to an integrated luminosity of 1/fb top pair candidates with lepton+jets signature are selected. To extract the fraction of top pair events in data a fit to the events total transverse energy is performed. Then the top mass is determined by reconstructing the kinematics of the top pair event.

 

Characterisation of silicon strip detectors

The participants will get an introduction in the functionality of silicon strip detectors. They will characterize test structures as well as unirradiated and irradiated strip sensors, before real data will be taken with a full module. A short analysis of the data will complete the exercise.


 

Measuring cosmic muon flux with a VME DAQ system

In this topic, you will develop a readout system based on 8” PMT´s immersed in a 125liter liquid scintillator chamber read out via a VME data acquisition system. After initialising VME components, testing the PMT performance and connecting the hardware you will measure cosmic muons and deduce the muon flux from the acquired data.


 

Calibration of the LOPES experiment for radio detection of cosmic rays

The LOPES experiment is an array of 30 radio detectors designed to measure pulsed radio emission from cosmic ray air showers in coincidence with the KASCADE-Grande experiment. For a precise measurement of these radio signals, the absolute calibration of the individual detector channels and the positions of the 30 LOPES antennas have to be known with high accuracy. In this project, we will perform a calibration of LOPES in the field using an external reference source and a differential GPS system, followed by a complete analysis of the measured raw data leading to the production of the final calibration quantities.


 

Study of the arrival direction distribution of UHECRs

It is expected that the deflection of cosmic rays due to magnetic fields decreases with energy and above 60 EeV might be smaller than a few degrees. Such small deflection angles allow the search for point sources or source regions. The aim of the project will be the discussion and application of different methods to search for point sources and the evaluation of the statistical significance of possible signals of anisotropy. 


 

Composition analysis using FADC traces recorded by the surface detector array of Auger

 

The surface detector array of the Auger Observatory consists of 1600 water Cherencov stations. Each station is equipped with 12t of water and is overlooked by 3 9"PMTs. The time traces recorded by the FADC system allow us, to derive quantities which are strongly correlated with the mass of the initiating primary cosmic particle. The aim is the separation of the prompt muon signal from the delayed electron/photon signal.

 

Inclusive flux of muons and its relation to hadronic interactions

After an introduction to analytic estimates of the inclusive muon flux, an explicit flux calculation is carried out. The influcence of the characteristics of hadronic multiparticle production on the muon flux predictions is investigated by modifying the extrapolation of the interaction model to very high energy. The resulting uncertainty of the flux is estimated.


 

Mass & energy analysis of cosmic rays

This topic is related to data analysis of air-shower measurements with KASCADE-Grande. The multi-detector experiment KASCADE-Grande detects air-showers generated by high-energy cosmic ray particles entering the Earth’s Atmosphere. The energy and mass of the incoming primary particle have to be deduced from the information of the measured secondary particles. 


 

DETECTORS: a cosmic ray demonstration experiment

Simple coffee cans are equipped with photo-multipliers and work as Water-Cherenkov-Detectors. In a stand alone mode or coupled for coincidence measurements the full portable detection system can be used for demonstration of a cosmic ray detector. The simple electronics will be learned, and experiments like muon rate determination below different absorbers, air-shower measurements, or estimation of the muon life time will be performed in this practical work.    

 

KATRIN pre-spectrometer measurements

Besides its function as a high pass filter for the main spectrometer, the pre-spectrometer is used as a test bed for the final KATRIN setup. Practical work can be either measurements of background to identify its sources, transmission functions by means of an e-gun or improvement of the electrode configuration. Students get involved in XUHV-technology (p< 10^-13 bar), high speed multichannel data acquisition, particle tracking in electromagnetic fields and other topics.   

 

Investigation of the earth magnetic field and the magnetic materials in the KATRIN main spectrometer building

 

Properties like the value and the symmetry of the magnetic field in the centre of the KATRIN main spectrometer define the high resolution, the transmission, and the low background of the precise energy filter for determining the electron anti-neutrino mass. Since with 0.3 mT the magnetic field is rather low there, any external influence like the earth magnetic field or magnetic materials in the vicinity of the main spectrometer have to be considered. You'll take part in systematic magnetic field measurements across the KATRIN main spectrometer building.


 

Installation of the inner electrode High Voltage system at the KATRIN main spectrometer

 

The electromagnetic properties of the KATRIN main spectrometer are of essential importance for the determination of the mass of the electron anti-neutrino. In this context a wire electrode system is being installed, in order to create and shape the high precision analyzing potential. You'll take part in the quality assurance activities during installation and test of the precision high voltage system.


 

Influence of magnetic fields on the rotor temperature of turbo molecular pumps

If turbo molecular pumps (TMP) are operated within a magnetic field environment, rotating materials (as the pump rotor) are heated up due to induced eddy currents. If the temperature exceeds a critical limit the pump can be destroyed. For experiments with many TMP´s operating in magnetic fields (as for KATRIN) it is essential to know this critical limit which corresponds to a maximum allowed magnetic field to ensure save operation of the pumps. The work will include the calibration of an infrared camera, which will be used for the temperature measurement and the performance of a few measurements at various magnetic fields. 

 

Commissioning of the KATRIN differential pumping section

The Tritium source of KATRIN is windowless and operated at a pressure of about 0,003 mbar, whereas the pressure in the spectrometers must not exceed 10 fbar. This is achieved by an elaborate transport section which is opaque for Tritium, but transparent to beta-electrons. At the time of the SI, commissioning of the DPS is scheduled to begin. Students will participate in commissioning measurements or the preparation of these. Commissioning will comprise the determination of the gas flow reduction factor, magnetic field measurements and other topics.

 

grid computing

We will set up a Grid site including all necessary services and run Astroparticle Physics or HEP software on the Grid.

 

cloud computing

We will generate a virtual machine image with HEP or Astroparticle physics software and run it in the Cloud. Software from the 'own' experiment or alternatively, CMS Monte Carlo software can be used to do this practical work. Either the SCC Eucalyptus Cloud test bed or the Amazon Computing Cloud will be used. 

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