BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:PoGOLite: a balloon-borne soft gamma-ray polarimeter. DTSTART;VALUE=DATE-TIME:20070706T170500Z DTEND;VALUE=DATE-TIME:20070706T171700Z DTSTAMP;VALUE=DATE-TIME:20260716T101824Z UID:indico-contribution-93-0-1177@cern.ch DESCRIPTION:Speakers: Prof. PEARCE\, Mark (KTH\, Department of Physics\, S tockholm)\nPolarized gamma-rays are expected from a wide variety of source s including \nrotation-powered pulsars\, accreting black holes and neutron stars\, and jet-\ndominated active galaxies. Polarization measurements pr ovide a powerful \nprobe of the gamma-ray emission mechanism and the distr ibution of magnetic \nand radiation fields around the source. No measureme nts have been performed \nin the soft gamma-ray band where non-thermal pro cesses are expected to \nproduce high degrees of polarization. The PoGOLit e experiment applies well-\ntype phoswich detector technology to polarizat ion measurements in the 25 - \n100 keV energy range. The instrument uses C ompton scattering and \nphotoabsorption in an array of 217 phoswich detect or cells made of plastic and \nBGO scintillators\, and surrounded by activ e BGO shields. A prototype of the \nflight instrument has been tested with polarized gamma-rays and background \ngenerated with radioactive sources. The test results and computer simulations \nconfirm that the instrument c an detect 10% polarization of a 100 mCrab source \nin one 6 hour balloon o bservation. In flight\, targets are constrained to within \nbetter than 5% of the field-of-view (~5 degrees squared) in order to maximize \nthe effe ctive detection area during observations. The pointing direction on the \n sky is determined by an attitude control system comprising star trackers\, \ndifferential GPS receiver system\, gyroscopes\, accelerometers and \nma gnetometers which provide correction signals to a reaction wheel and \ntor que motor system. Additionally\, the entire polarimeter assembly rotates \ naround its viewing axis to minimize systematic bias during observations. Flights \nare foreseen to start in 2009 and will target northern sky sourc es including the \nCrab pulsar/nebula\, Cygnus X-1\, and Hercules X-1. The se observations will \nprovide valuable information about the pulsar emiss ion mechanism\, the \ngeometry around the black hole\, and photon transpor tation in the strongly \nmagnetized neutron star surface\, respectively. F uture goals include a long \nduration balloon flight from the Esrange faci lity in the North of Sweden to \nCanada.\n\nhttps://indico.nucleares.unam. mx/event/4/session/93/contribution/1177 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/93/contribution/1177 END:VEVENT BEGIN:VEVENT SUMMARY:Energy cross-calibration from the first CREAM flight : transition radiation detector versus calorimeter DTSTART;VALUE=DATE-TIME:20070706T171700Z DTEND;VALUE=DATE-TIME:20070706T172900Z DTSTAMP;VALUE=DATE-TIME:20260716T101824Z UID:indico-contribution-93-0-309@cern.ch DESCRIPTION:Speakers: Dr. MAESTRO\, Paolo (University of Siena adn INFN)\, ZEI\, Riccardo (University of Siena - INFN)\nThe Cosmic Ray Energetics an d Mass (CREAM) balloon experiment had two successful\nflights in 2004/05 a nd 2005/06. It was designed to perform energy measurements from\na few Ge V up to 1000 TeV\, taking advantage of different detection techniques. The \nfirst instrument\, CREAM-I\, combined a transition radiation detector (e quipped with an\narray of proportional tubes and an acrylic Cherenkov devi ce) with a calorimeter to\nprovide independent energy measurements of cosm ic ray nuclei. Each detector was\ncalibrated with particle beams in a limi ted range of energies. In order to assess the\nabsolute energy scale of th e whole instrument and to investigate the systematic\neffects of each tech nique\, a cross-calibration was performed by comparing the\nindependent en ergy estimates on selected samples of Oxygen and Carbon nuclei.\n\nhttps:/ /indico.nucleares.unam.mx/event/4/session/93/contribution/309 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/93/contribution/309 END:VEVENT BEGIN:VEVENT SUMMARY:Measuring 10-1000GeV Cosmic-ray Electrons with GLAST/LAT DTSTART;VALUE=DATE-TIME:20070706T172900Z DTEND;VALUE=DATE-TIME:20070706T174100Z DTSTAMP;VALUE=DATE-TIME:20260716T101824Z UID:indico-contribution-93-0-1014@cern.ch DESCRIPTION:Speakers: Dr. MOISEEV\, Alexander (CRESST/NASA/Goddard Space F light Center)\nWe present here the capabilities of the GLAST Large Area Te lescope to detect cosmic\nray high-energy (HE) electrons in the energy ran ge from 10 GeV to 1 TeV. We also\ndiscuss the science topics that can be i nvestigated with HE electron data and\nquantify the results with LAT instr ument simulations. The science topics include CR\npropagation\, calibratio n of the IC gamma-ray model\, testing hypotheses regarding the\norigin of HE energy cosmic-ray electrons\, searching for any signature of Kaluza Kle in\nDark Matter annihilation\, measuring the HE electron anisotropy\, and forming links\nwith radio astronomy. We expect to detect ~ 10^7 electrons above 20 GeV in 1 year of\nLAT operations.\n\nhttps://indico.nucleares.una m.mx/event/4/session/93/contribution/1014 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/93/contribution/1014 END:VEVENT BEGIN:VEVENT SUMMARY:High Resolution Measurements of Cosmic-ray Air Showers with the Tr ack Imaging Cerenkov Experiment DTSTART;VALUE=DATE-TIME:20070706T174100Z DTEND;VALUE=DATE-TIME:20070706T175300Z DTSTAMP;VALUE=DATE-TIME:20260716T101824Z UID:indico-contribution-93-0-1172@cern.ch DESCRIPTION:Speakers: HAYS\, Elizabeth (University of Chicago and Argonne National Laboratory)\nThe Track Imaging Cerenkov Experiment (TrICE) is an air Cerenkov telescope designed\nto use a high resolution method for measu ring cosmic-ray composition at TeV-PeV\nenergies. The method aims to sepa rate the fast and compact direct Cerenkov signal\nproduced by primary cosm ic ray nuclei in the upper atmosphere from the light produced\nby the subs equent air shower cascade. Efficient discrimination of the direct Cerenkov \nsignal benefits from the use of small camera pixels to improve the angul ar resolution\nof the air shower image. Multi-anode photomultipliers are used in the TrICE camera\nto achieve 0.086 degree pixel spacing over a 1.5 degree field of view. The telescope\nwas completed in late 2006 at Argonn e National Laboratory. We present the results\nfrom the first observation s with TrICE.\n\nhttps://indico.nucleares.unam.mx/event/4/session/93/contr ibution/1172 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/93/contribution/1172 END:VEVENT BEGIN:VEVENT SUMMARY:Studies of Direct Cerenkov Emission with VERITAS DTSTART;VALUE=DATE-TIME:20070706T175300Z DTEND;VALUE=DATE-TIME:20070706T180500Z DTSTAMP;VALUE=DATE-TIME:20260716T101824Z UID:indico-contribution-93-0-732@cern.ch DESCRIPTION:Speakers: Ms. WISSEL\, Stephanie (University of Chicago)\nGrou nd-based composition measurements of high-energy cosmic rays can be signif icantly\nimproved by using the direct Cerenkov method. This technique tar gets the Cerenkov\nlight produced by the primary particle prior to its pro duction of an extensive air\nshower. With the appropriate time and angula r resolution\, the direct Cerenkov\nphotons can be separated from those pr oduced in the extensive air shower. By\nutilizing the 0.15deg angular and 2 nanosecond timing resolution of the very high\nenergy gamma-ray telesco pe system\, VERITAS\, the charge and energy of cosmic rays at\nTeV energie s can be identified on an event-by-event basis. Results from a preliminary \nsearch for direct Cerenkov events are discussed.\n\nhttps://indico.nucle ares.unam.mx/event/4/session/93/contribution/732 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/93/contribution/732 END:VEVENT BEGIN:VEVENT SUMMARY:A Direct Cerenkov Observatory for High-Energy Cosmic Rays DTSTART;VALUE=DATE-TIME:20070706T180500Z DTEND;VALUE=DATE-TIME:20070706T181700Z DTSTAMP;VALUE=DATE-TIME:20260716T101824Z UID:indico-contribution-93-0-380@cern.ch DESCRIPTION:Speakers: Prof. WAKELY\, Scott (University of Chicago)\nA desi gn concept for a future ground-based cosmic-ray observatory using the Dire ct\nCerenkov technique will be presented. This technique can provide high precision\,\nlargely model-independent\, measurements of the energy and c harge of heavy cosmic-ray\nprimaries in the region of the knee. It does s o by exploiting the direct component\nof Cerenkov radiation emitted by the se primaries prior to their first hadronic\ninteraction in the atmosphere. The promise of the technique has recently been\nverified with measuremen ts made by gamma-ray observatories.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/93/contribution/380 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/93/contribution/380 END:VEVENT BEGIN:VEVENT SUMMARY:Future plan for observation of cosmic gamma rays in the 100 TeV en ergy region with the Tibet air shower array : physics goal and overview DTSTART;VALUE=DATE-TIME:20070706T181700Z DTEND;VALUE=DATE-TIME:20070706T182900Z DTSTAMP;VALUE=DATE-TIME:20260716T101824Z UID:indico-contribution-93-0-416@cern.ch DESCRIPTION:Speakers: Mr. SAKO\, Takashi (Institute for Cosmic Ray Researc h\, University of Tokyo)\nAlthough SNRs are theoretically considered to be the most plausible candidates for\nthe acceleration of cosmic-ray hadrons up to PeV energies\, no observations have\nsucceeded in definitely specif ying those objects so far.\nSince accelerated electrons have difficulty pr oducing very high-energy gamma rays\nwith energies above 100 TeV via brems strahlung or inverse Compton scattering\, it can\nbe an effective way of o btaining clear evidence for hadronic acceleration to detect\nsuch high-ene rgy gamma rays generated via the decay of neutral pions produced in\ninter actions of accelerated hadrons with ambient material.\nThe Tibet air showe r array has been observing air showers induced by cosmic rays with\nenergi es above a few TeV. We are planning to add a large muon detector array to it\nand to improve its sensitivity to cosmic gamma rays with energies arou nd 100 TeV by\ndiscriminating them from background cosmic-ray hadrons. The possibility of detection\nof gamma rays in the 100 TeV energy region in o ur field of view is discussed\, based\non the improved sensitivity of our air shower array.\n\nhttps://indico.nucleares.unam.mx/event/4/session/93/c ontribution/416 LOCATION:Merida\, Mexico Kabah (Holiday Inn) URL:https://indico.nucleares.unam.mx/event/4/session/93/contribution/416 END:VEVENT END:VCALENDAR