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  <organization>ICN-UNAM</organization>
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<supportEmail caption="Support">icrc2007@icrc2007.unam.mx</supportEmail>
<title>30th International Cosmic Ray Conference</title>
<description>The 30th International Cosmic Ray Conference will be held from July 3, 2007 to July 11, 2007 in Merida, Yucatan, Mexico.</description>
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 <name>Merida, Mexico</name>
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<startDate>2007-07-03T08:00:00</startDate>
<endDate>2007-07-11T19:00:00</endDate>
<creationDate>2005-09-26T05:04:53</creationDate>
<modificationDate>2024-04-12T17:46:55</modificationDate>
<timezone>Mexico/General</timezone>
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  <title>Dr.</title>
  <name first="José" middle="" last="Valdés"></name>
  <organization>IGeof-UNAM</organization>
  <emailHash>40af9343b8bb9d18708b4f0252d5f53c</emailHash>
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 <title>PoGOLite: a balloon-borne soft gamma-ray polarimeter.</title>
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   <title>Prof.</title>
   <name first="Mark" middle="" last="Pearce"></name>
   <organization>KTH, Department of Physics, Stockholm</organization>
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   <title>Prof.</title>
   <name first="Mark" middle="" last="Pearce"></name>
   <organization>KTH, Department of Physics, Stockholm</organization>
   <emailHash>b8056c84778dcbc0d7ab1bf12d008459</emailHash>
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  <name>Merida, Mexico</name>
  <address></address>
  <room>Kabah (Holiday Inn)</room>
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 <startDate>2007-07-06T12:05:00</startDate>
 <endDate>2007-07-06T12:17:00</endDate>
 <duration>00:12</duration>
 <abstract>Polarized gamma-rays are expected from a wide variety of sources including 
rotation-powered pulsars, accreting black holes and neutron stars, and jet-
dominated active galaxies. Polarization measurements provide a powerful 
probe of the gamma-ray emission mechanism and the distribution of magnetic 
and radiation fields around the source. No measurements have been performed 
in the soft gamma-ray band where non-thermal processes are expected to 
produce high degrees of polarization. The PoGOLite experiment applies well-
type phoswich detector technology to polarization measurements in the 25 - 
100 keV energy range. The instrument uses Compton scattering and 
photoabsorption in an array of 217 phoswich detector cells made of plastic and 
BGO scintillators, and surrounded by active BGO shields. A prototype of the 
flight instrument has been tested with polarized gamma-rays and background 
generated with radioactive sources. The test results and computer simulations 
confirm that the instrument can detect 10% polarization of a 100 mCrab source 
in one 6 hour balloon observation. In flight, targets are constrained to within 
better than 5% of the field-of-view (~5 degrees squared) in order to maximize 
the effective detection area during observations. The pointing direction on the 
sky is determined by an attitude control system comprising star trackers, 
differential GPS receiver system, gyroscopes, accelerometers and 
magnetometers which provide correction signals to a reaction wheel and 
torque motor system. Additionally, the entire polarimeter assembly rotates 
around its viewing axis to minimize systematic bias during observations. Flights 
are foreseen to start in 2009 and will target northern sky sources including the 
Crab pulsar/nebula, Cygnus X-1, and Hercules X-1. These observations will 
provide valuable information about the pulsar emission mechanism, the 
geometry around the black hole, and photon transportation in the strongly 
magnetized neutron star surface, respectively. Future goals include a long 
duration balloon flight from the Esrange facility in the North of Sweden to 
Canada.</abstract>
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