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BEGIN:VEVENT
SUMMARY:First events of the CNGS beam detected by LVD
DTSTART;VALUE=DATE-TIME:20070710T153000Z
DTEND;VALUE=DATE-TIME:20070710T154200Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-1-1031@cern.ch
DESCRIPTION:Speakers: SARTORELLI\, Gabriella (INFN and Department of Physi
 cs\, University of Bologna)\nThe Cern Neutrinos to Gran Sasso (CNGS) proje
 ct aims to produce a high \nenergy\, wide band muon neutrino beam at Cern 
 and send it towards the INFN \nGran Sasso National Laboratory (LNGS). Its 
 main goal is the observation of the \ntau neutrino appearance.\nThe beam s
 tarted its operation in August 2006: a total amount of $7.6~10^\n{17}$ pro
 tons were delivered to the target.\nThe LVD detector\, installed at LNGS a
 nd mainly dedicated to the study of \nsupernova neutrinos\, can detect CNG
 S neutrinos through the internal CC and \nNC interactions in the apparatus
  and through the muons generated by CC \ninteractions in the rock upstream
  the detector.\nLVD was fully operating during the whole CNGS running time
 \, with 950 t of \nactive mass. A total number of about 570 events were de
 tected in coincidence \nwith the beam spill time. This is in good agreemen
 t with the expected number \nof events.\n\nhttps://indico.nucleares.unam.m
 x/event/4/session/67/contribution/1031
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/1031
END:VEVENT
BEGIN:VEVENT
SUMMARY:The atmosphere UV background phenomena measured by detector on-boa
 rd “Universitetsky-Tatiana” satellite.
DTSTART;VALUE=DATE-TIME:20070710T154200Z
DTEND;VALUE=DATE-TIME:20070710T155400Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-1-138@cern.ch
DESCRIPTION:Speakers: Mr. KLIMOV\, Pavel (Skobeltsyn Institute of Nuclear 
 Physics)\nNear UV detector on-board the “Universitetsky-Tatiana” satel
 lite has observed \nthe atmosphere glow at night side of the Earth. Digita
 l oscilloscopes help to \nselect transient luminous events and to measure 
 their temporal profiles in time \nscale of 1-64 ms. Data from those detect
 ors were analyzed for prediction the \nduty cycle of future space detector
 s of ultra high energy cosmic rays.\n\nhttps://indico.nucleares.unam.mx/ev
 ent/4/session/67/contribution/138
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/138
END:VEVENT
BEGIN:VEVENT
SUMMARY:In-Ice radio detection of air shower cores
DTSTART;VALUE=DATE-TIME:20070710T155400Z
DTEND;VALUE=DATE-TIME:20070710T160600Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-1-806@cern.ch
DESCRIPTION:Speakers: Dr. SECKEL\, David (University of Delaware)\nRadio r
 eceivers (RICE\, AURA) have been deployed to detect impulsive emissions fr
 om\nneutrino interactions in ice at South Pole. An alternative source of p
 ulses is the\ncores of cosmic ray induced air showers. AIRES and CORSIKA s
 imulations suggest that\n>10% of the primary cosmic ray energy enters the 
 ice within 20 cm of the primary axis\nimpact point. The resulting 5-10 m c
 ascade will make Askaryan type pulses that can be\ndetected by in-ice rece
 ivers. Strategies are discussed for deploying a modest number\nof antennas
  which could operate in coincidence with IceCube to validate the in-situ\n
 detection of Askaryan pulses and produce a new discriminant for studying c
 osmic ray\nprimary composition for energies above 10^16 eV.\n\nhttps://ind
 ico.nucleares.unam.mx/event/4/session/67/contribution/806
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/806
END:VEVENT
BEGIN:VEVENT
SUMMARY:Calibration of TA Surface Detectors
DTSTART;VALUE=DATE-TIME:20070710T160600Z
DTEND;VALUE=DATE-TIME:20070710T161800Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-1-772@cern.ch
DESCRIPTION:Speakers: Dr. NONAKA\, Toshiyuki (Institute for Cosmic Ray Res
 erch\,University of Tokyo)\nThe surface detector of Telescope Array(TA) ex
 periment are deployed in desert of\nwestern utah\,USA.  The detector consi
 sts of two layers of plastic\nscintillators of 3m2 area with wave length s
 hifter fiber(WLSfiber). \nAnd at each layer\,PMT are connected with WLS fi
 bers.\nAt each layer \,2 LEDs are also equipped to check PMT linearity.\n 
 To estimate number of shower particles with good accuracy\, it is needed t
 oknow the\nresponse for 1 minimum ionization particle and the environmenta
 l effect on it. PMT\nlinearity are also needed to be monitored and calibra
 ted.\n Here we report observed variation on detector response and its cali
 bration. And the\nresult of linearity check with LEDs also will be reporte
 d.\n\nhttps://indico.nucleares.unam.mx/event/4/session/67/contribution/772
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/772
END:VEVENT
BEGIN:VEVENT
SUMMARY:Air fluorescence yield dependence on atmospheric parameters
DTSTART;VALUE=DATE-TIME:20070710T161800Z
DTEND;VALUE=DATE-TIME:20070710T163000Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-1-387@cern.ch
DESCRIPTION:Speakers: Dr. RODRIGUEZ FERNANDEZ\, Gonzalo (University of Rom
 a Tor Vergata and INFN)\nThe fluorescence detection of ultra high energy (
 $\\gtrsim 10^{18}$ eV) cosmic rays\nrequires a detailed knowledge of the f
 luorescence light emission from nitrogen\nmolecules\, which are  excited b
 y the cosmic ray shower particles along their path in\nthe atmosphere. We 
 have made a precise measurement of the fluorescence light spectrum\nexcite
 d by MeV electrons in dry air. We measured the relative intensities of 34\
 nfluorescence lines in the wavelength range from 284 to 429 nm with a high
  resolution\nspectrograph. The fluorescence spectrum dependence on pressur
 e\, temperature and\nhumidity was also measured.  The details and precisio
 n of the AIRFLY measurements\nsurpass that of previous experiments and red
 uce significantly the systematic\nuncertainty in the determination of the 
 cosmic ray shower energy with the\nfluorescence technique.\n\nhttps://indi
 co.nucleares.unam.mx/event/4/session/67/contribution/387
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/387
END:VEVENT
BEGIN:VEVENT
SUMMARY:The search for UHECR and Neutrinos from Space: a "Vision" for the 
 next decade
DTSTART;VALUE=DATE-TIME:20070710T163000Z
DTEND;VALUE=DATE-TIME:20070710T164200Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-1-1308@cern.ch
DESCRIPTION:Speakers: Dr. SANTANGELO\, Andrea (IAAT University of Tuebinge
 n\, Germany)\nUltra High Energy Cosmic Rays and Neutrinos\, with energies 
 from a few  10^18 eV to\nbeyond the decade of 10^20 eV\, and Cosmic Rays w
 ith E >= 5 10^19 eV appear to be the\nonly suitable messengers to explore 
 the Universe at frontier energies\, where\nradiation is expected to be pro
 duced under the most extreme physical conditions.\nObservations of these U
 HE particles will certainly provide new information 1) on the\nsources\; a
 nd 2) on the physical mechanisms able to accelerate these extreme\nmesseng
 ers to macroscopic energies. Moreover\, UHE particles may also\, provide\n
 evidence of yet unknown physics or of exotic particles\, relics of the ear
 ly Universe.\nTo reach these\ngoals\, innovative experiments with larger e
 ffective aperture (A_eff >= 10^5 km^2 sr)\nand good understanding of syste
 matic uncertainties (less than ~10%) must be\ndeveloped. Space-based obser
 vatories can reach the effective area necessary to\nsystematically explore
  the UHE Universe. In the present paper  1.) we present the\nScience Ratio
 nale behind UHE studies from space\; 2.) we briefly discuss the  science\n
 goals\, the requirements\, the instrument and mission profile of  a  'next
 -generation"\nspace-based mission for UHE observations to be  designed and
  developed in the\nframework of the ESA "Cosmic Vision  2015-2025" long te
 rm plan.\n\nhttps://indico.nucleares.unam.mx/event/4/session/67/contributi
 on/1308
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/1308
END:VEVENT
BEGIN:VEVENT
SUMMARY:The Northern Site of The Pierre Auger Observatory
DTSTART;VALUE=DATE-TIME:20070710T164200Z
DTEND;VALUE=DATE-TIME:20070710T165400Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-1-180@cern.ch
DESCRIPTION:Speakers: Prof. NITZ\, David (Michigan Technological Universit
 y)\nThe Pierre Auger Observatory is a multi-national project for research 
 on ultra-high\nenergy cosmic rays.  The Southern Auger Observatory in Mend
 oza province\, Argentina\,\nis approaching completion in 2007 with an inst
 rumented area of 3\,000 square\nkilometers.  It will accurately measure th
 e spectrum and composition of ultra-high\nenergy cosmic rays up to and bey
 ond the predicted GZK feature.  We have obtained\nfirst results on the ene
 rgy spectrum\, mass composition and distribution of arrival\ndirections on
  the southern sky.\n\nThe Northern Auger Observatory is designed to comple
 te and extend the investigations\nbegun in the south. It will establish ch
 arged particle astronomy and thus open a new\nwindow into the universe. Th
 e distribution of arrival directions of the highest\nenergy events will po
 int the way to unveiling the almost century old mystery of the\norigin and
  nature of ultra-high energy cosmic rays.  Achieving this goal requires\nc
 ollecting many more events in spite of the steeply falling energy spectrum
 . The\nplanned northern site will have an instrumented area of 4\,000 squa
 re miles (10\,370\nsquare kilometers) in South-East Colorado\, USA. The pr
 esentation covers the science\nof particle astronomy\, the layout and the 
 technical implementation of the Northern\nAuger Observatory.\n\nhttps://in
 dico.nucleares.unam.mx/event/4/session/67/contribution/180
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/180
END:VEVENT
BEGIN:VEVENT
SUMMARY:Livio Scarsi in memoriam
DTSTART;VALUE=DATE-TIME:20070710T133000Z
DTEND;VALUE=DATE-TIME:20070710T134200Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-0-1346@cern.ch
DESCRIPTION:Speakers: \nhttps://indico.nucleares.unam.mx/event/4/session/6
 7/contribution/1346
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/1346
END:VEVENT
BEGIN:VEVENT
SUMMARY:The JEM-EUSO Mission
DTSTART;VALUE=DATE-TIME:20070710T134200Z
DTEND;VALUE=DATE-TIME:20070710T135400Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-0-831@cern.ch
DESCRIPTION:Speakers: Dr. EBISUZAKI\, Toshikazu (RIKEN)\nJEM-EUSO is a sci
 ence mission to explore extremes of the Universe.　It\nobserves the dark-
 side of the Earth and detects UV photons emitted from\nthe giant air showe
 r caused by an extremely high energy particle (about\n10^20 eV). Such a pa
 rticle arrives almost straightly through our Milky\nWay Galaxy and is expe
 cted to allow us to trace the source location by\nits arrival direction. T
 his will open the door to the new astronomy with\ncharged particles: JEM-E
 USO can determine the arrival direction of the\nparticles within several d
 egrees and energy of them within 30%. In its\nfive years operation includi
 ng the tilt mode\, JEM-EUSO will detect at\nleast 1\,000 events with E>7x1
 0^19 eV and determine the energy spectrum\nof trans-GZK region with a stat
 istical accuracy of several percent.\nJEM-EUSO is planned to be transporte
 d with HTV (H2 Transfer Vehicle) and\nattached to the Japanese Experiment 
 Module/ Exposure Facility (JEM/EF)\nof International Space Station. JAXA r
 eleased the call for proposals for\nthe mission candidates of the second p
 hase utilization of JEM/EF for the\nlaunch of 2011 and 2013. Two years of 
 phase-A study will be carried out\nunder JAXA for selected candidates.\n*t
 he JEM-EUSO Collaboration: the list of authors is attached.\n\nhttps://ind
 ico.nucleares.unam.mx/event/4/session/67/contribution/831
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/831
END:VEVENT
BEGIN:VEVENT
SUMMARY:Status of the TUS space detector preparation for UHECR study
DTSTART;VALUE=DATE-TIME:20070710T135400Z
DTEND;VALUE=DATE-TIME:20070710T140600Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-0-146@cern.ch
DESCRIPTION:Speakers: Dr. TKACHEV\, LEONID (JOINT INSTITUTE FOR NUCLEAR RE
 SEARCH\, Dubna)\nThe space TUS detector of UV fluorescence light radiated 
 by EAS of Ultra \nHigh Energy Cosmic Rays (UHECR) is under preparation for
  the launch in 2009-\n2010. The TUS instrument will have ~2 sq. m.  mirror
  - concentrator area and \n256 PMT pixels in the photo receiver at the mir
 ror focal surface. The TUS mission \nis now planned for operation at the S
 mall Space Apparatus separated from the \nmain Foton-4 satellite launched 
 by SCB “Progress”. The “Universitetsky-\nTatiana” satellite data o
 n the night atmosphere UV glow helps to organize the \ntrigger system effe
 ctively separating EAS events from the background \natmospheric events. Th
 e TUS detector will be used not only for UHECR study \nbur also for observ
 ation of other atmospheric phenomena of UV radiation.\n\nhttps://indico.nu
 cleares.unam.mx/event/4/session/67/contribution/146
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/146
END:VEVENT
BEGIN:VEVENT
SUMMARY:Fluorescence Yield Results of FLASH (SLAC-E165)
DTSTART;VALUE=DATE-TIME:20070710T140600Z
DTEND;VALUE=DATE-TIME:20070710T141800Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-0-1264@cern.ch
DESCRIPTION:Speakers: Dr. REIL\, Kevin (Stanford Linear Accelerator Center
 )\, Dr. HUENTEMEYER\, Petra (Los Alamos National Laboratory)\nThe yield of
  fluorescence photons in an extensive air shower allows\nthe observer to d
 etermine the number of shower particles by measuring\nthe number of photon
 s produced. As the systematic uncertainties in\nboth ground array and fluo
 rescence detectors improve our need to\nbetter understand this calibration
  is required. Additionally\, as more\nsensitive fluorescence detectors obs
 erve further into the atmosphere\,\nour understanding of the spectral dist
 ribution of the yield is\nrequired in order to properly handle the lambda^
 -4 effect of\nRayleigh scattering.\n\nIn the first phase of SLAC's experim
 ent E-165\, "Fluorescence in Air\nfrom Showers/FLASH"\, a 28.5 GeV beam of
  electrons was used to measure\nthe total yield (photons per charged parti
 cle per meter) between 300\nand 400 nm as well as the spectral distributio
 n of the light. Our\nobjective was to make this measurement to better than
  10% total\nuncertainty and the calibration efforts required to achieve th
 is will\nbe outlined with details presented in the poster session.\n\nhttp
 s://indico.nucleares.unam.mx/event/4/session/67/contribution/1264
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/1264
END:VEVENT
BEGIN:VEVENT
SUMMARY:Science Objectives of the JEM EUSO mission on International Space 
 Station
DTSTART;VALUE=DATE-TIME:20070710T141800Z
DTEND;VALUE=DATE-TIME:20070710T143000Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-0-1227@cern.ch
DESCRIPTION:Speakers: Prof. TAKAHASHI\, Yoshiyuki (The University of Alaba
 ma in Huntsville)\nJEM-EUSO space observatory will have a very large expos
 ure factor in several years\, which is far exceeding the \ncritical exposu
 re factor required for observation of most of the sources within a few hun
 dred Mpc. The main \nscience objective is the source identifying atsronomy
  in particle channel. Quasi-linear tracking of the sources \nbecomes feasi
 ble at energy > 10^20 eV for all-sky. Acceleration mechanism may be studie
 d by the energy \nspectra of individual multiplets and that of all particl
 es. In addition\, JEM-EUSO has three exploratory test \nobservations: \n(i
 ). extremely high energy neutrinos\, beginning at E > 1019 eV: neutrinos a
 t such high energies are expected to \nhave an increased cross section in 
 the Standard Model\, and in particular\, in extra-dimension models\, \ncha
 racterizable by their possible detection or failure. \n(ii). fundamental p
 hysics at extreme energies at several decades higher than the Super LHC (L
 arge Hadronic \nCollider) energies\, \n(iii). global atmospheric observati
 on\, including large-scale and local plasma discharges\, night-glow\, mete
 orites\, and \nothers.\n\nhttps://indico.nucleares.unam.mx/event/4/session
 /67/contribution/1227
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/1227
END:VEVENT
BEGIN:VEVENT
SUMMARY:Instrument Overview of the JEM-EUSO Mission
DTSTART;VALUE=DATE-TIME:20070710T143000Z
DTEND;VALUE=DATE-TIME:20070710T144200Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-0-914@cern.ch
DESCRIPTION:Speakers: Prof. KAJINO\, Fumiyoshi (Konan University)\nJEM-EUS
 O with a large and wide-angle telescope mounted on ISS has been \nplaned a
 s a space mission to explore extremes of the universe through the \ninvest
 igation of ultra-high-energy cosmic rays by detecting photons which \nacco
 mpany air showers developed in the earth's atmosphere.  JEM-EUSO will \nbe
  launched by Japanese H-II Transfer Vehicle(HTV) and mounted at the \nExpo
 sed Facility of Japanese Experiment Module(JEM/EF) of ISS in the second \n
 phase of utilization plan. The telescope consists of high transmittance op
 tical \nFresnel lenses with a diameter of 2.5m\, 200k channels of multiano
 de-\nphotomultiplier tubes\, focal surface front-end\, readout\,  trigger 
 and system \nelectronics. An infrared camera and a LIDAR system will be al
 so used to monitor \nthe earth's atmosphere.\n\nhttps://indico.nucleares.u
 nam.mx/event/4/session/67/contribution/914
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/914
END:VEVENT
BEGIN:VEVENT
SUMMARY:Status of the LHCf experiment
DTSTART;VALUE=DATE-TIME:20070710T144200Z
DTEND;VALUE=DATE-TIME:20070710T145400Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-0-982@cern.ch
DESCRIPTION:Speakers: Mr. MENJO\, Hiroaki (Nagoya University\, Japan)\nThe
  uncertainty of hadron interaction models of Monte Carlo simulations have 
 caused\nsome systematic errors of energy reconstruction and the determinat
 ion of composition\nin ultra high energy cosmic ray measurements. The unce
 rtainty is due to the lack of\nthe experimental data on the nuclear intera
 ctions in the energy region over\n2x10^14eV. The LHCf experiment will prov
 ide crucial calibration points at 10^17eV\nthat are indispensable for the 
 hadron interaction models in the ultra-high energy\nregion. The production
  spectra of photons and neutral pion will be measured in the\nvery forward
  region of a LHC interaction point. The first data will be taken during\nb
 eam commissioning of the LHC with 450GeV+450GeV proton-proton collisions\,
  which is\nscheduled to start at the end of 2007. The final data set will 
 be taken with\n7TeV+7TeV collisions\, corresponding to 10^17eV cosmic ray 
 collisions in the\n"laboratory frame". LHC is scheduled to start 7TeV+7TeV
  collisions in the Spring of\n2008. In the meantime the preparation of the
  LHCf experiment is on going. The Arm#1\ndetector was fully assembled in J
 uly 2006. The Arm#2 detector will be finally\nassembled in April 2007. In 
 this talk\, we will present a progress report of the LHCf\nexperiment.\n\n
 https://indico.nucleares.unam.mx/event/4/session/67/contribution/982
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/982
END:VEVENT
BEGIN:VEVENT
SUMMARY:Performance of the IceTop array
DTSTART;VALUE=DATE-TIME:20070705T142000Z
DTEND;VALUE=DATE-TIME:20070705T143200Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-3-758@cern.ch
DESCRIPTION:Speakers: Prof. GAISSER\, Tom (Bartol Research Institute)\nThe
  surface air-shower array above the IceCube neutrino telescope now \nconsi
 sts of 52 ice Cherenkov tanks at 26 stations spread over an area of 0.22 \
 nsquare kilometer.  This paper reports on experience with deployment and \
 noperation of IceTop and describes data that verify the performance\, thre
 shold \nand energy response of the array.\n\nhttps://indico.nucleares.unam
 .mx/event/4/session/67/contribution/758
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/758
END:VEVENT
BEGIN:VEVENT
SUMMARY:Trigger Strategy for Radio Detection in Atmospheric Air Showers wi
 th LOPES^STAR
DTSTART;VALUE=DATE-TIME:20070710T170500Z
DTEND;VALUE=DATE-TIME:20070710T171700Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-2-923@cern.ch
DESCRIPTION:Speakers: Mr. ASCH\, Thomas (Research Centre Karlsruhe\, IPE)\
 nIn the framework of LOPES (LOFAR PrototypE Station)\, a Self-Triggered Ar
 ray of Radio\ndetectors (STAR) is developed. The challenge of LOPES^STAR i
 s to provide an\nindependent self-trigger on radio emission of extensive a
 ir showers with primary\nenergy above approximate 5*10^17 eV.\nMeasurement
 s are done both with an external and self-trigger in radio loud and quiet\
 nareas. Based on these data the self-trigger is optimised and higher level
  triggers\nare developed\, as well as algorithms for reconstruction of sho
 wer observables.\nThe methods and first results from LOPES^STAR are descri
 bed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/67/contribution/9
 23
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/923
END:VEVENT
BEGIN:VEVENT
SUMMARY:Energy dependence of air fluorescence yield
DTSTART;VALUE=DATE-TIME:20070710T171700Z
DTEND;VALUE=DATE-TIME:20070710T172900Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-2-388@cern.ch
DESCRIPTION:Speakers: Dr. CAZON\, Lorenzo (University of Chicago)\nIn the 
 fluorescence detection of ultra high energy ($\\gtrsim 10^{18}$ eV) cosmic
 \nrays\, it is assumed that the number of emitted fluorescence photons is 
 proportional\nto the energy deposited in air by shower particles. We have 
 performed measurements of\nthe fluorescence yield in atmospheric gases exc
 ited by electrons over a wide energy\nrange. AIRFLY has collected data  be
 tween 1 and 3 MeV at a Van de Graaff electron\naccelerator\, and between 3
  and 15 MeV at the AWA LINAC\, both located at the Argonne\nNational Labor
 atory. Fluorescence yield induced by electrons in the range 50 to 500\nMeV
  was studied with an extracted beam at the Beam Test Facility of Laborator
 i\nNazionali di Frascati. The large flux of photons from the APS synchrotr
 on radiation\nsource at the Argonne National Laboratory allowed us to expl
 ore the fluorescence\nemission from keV electrons produced by  X-ray inter
 action in air. Results of these\nmeasurements are summarised.\n\nhttps://i
 ndico.nucleares.unam.mx/event/4/session/67/contribution/388
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/388
END:VEVENT
BEGIN:VEVENT
SUMMARY:Current status of the expanded GRAPES collaboration at Ooty in Ind
 ia
DTSTART;VALUE=DATE-TIME:20070710T172900Z
DTEND;VALUE=DATE-TIME:20070710T174100Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-2-1058@cern.ch
DESCRIPTION:Speakers: Prof. GUPTA\, Sunil (Tata Institute of Fundamental R
 esearch)\nGRAPES-3 experiment employs a high-density array of scintillator
 s and a\nlarge area tracking muon telescope. The GRAPES collaboration is b
 eing\nexpanded with addition of several major facilities. These include a\
 nCerenkov telescope and low frequency dipole array for the measurement of\
 nshower energy. Addition of several modules of muon telescopes to cover a\
 nlarger area\, expansion of the scintillator array with greater separation
 \nbetween detectors. Installation of a neutron monitor is also planned. Th
 e\ncurrent status of the experiment would be summarized.\n\nhttps://indico
 .nucleares.unam.mx/event/4/session/67/contribution/1058
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/1058
END:VEVENT
BEGIN:VEVENT
SUMMARY:SiPM development for astroparticle physics applications
DTSTART;VALUE=DATE-TIME:20070710T174100Z
DTEND;VALUE=DATE-TIME:20070710T175300Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-2-688@cern.ch
DESCRIPTION:Speakers: Prof. TESHIMA\, Masahiro (Max-Planck-Institute for P
 hysics)\nSiPM is the novel solid state photodetector which can be operated
  \nin the single photon counting mode. It has excellent features\, \nhigh 
 quantum efficiency\, good charge resolution\, fast response\, \nvery compa
 ct\, high gain of 10^6\, very low power consumption\, \nimmune to the magn
 etic field and low bias voltage\, typically 60V. \nDrawbacks of this devic
 e are currently the large dark current\, \ncrosstalk between micro pixels 
 and relatively low sensitivity to \nUV and blue light. Last several years\
 , we have developed large size \nSiPM (9mm^2 and 25mm^2) for the applicati
 ons in the imaging atmospheric\ncherenkov telescopes (MAGIC and CTA) and i
 n the fluorescence telescope\n(EUSO). In the conference\, the current stat
 us of SiPM development by MPI\nand MEPhI will be presented.\n\nhttps://ind
 ico.nucleares.unam.mx/event/4/session/67/contribution/688
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/688
END:VEVENT
BEGIN:VEVENT
SUMMARY:A radio air shower detector as an extension for IceCube and IceTop
DTSTART;VALUE=DATE-TIME:20070710T175300Z
DTEND;VALUE=DATE-TIME:20070710T180500Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-2-293@cern.ch
DESCRIPTION:Speakers: Dr. KARG\, Timo (Bergische Universität Wuppertal)\n
 The IceCube neutrino detector is built into the Antarctic ice sheet at the
  South Pole to measure high energy \nneutrinos. For this\, 4800 PMTs are b
 eing deployed at depths between 1\,450 and 2\,450 meters into the ice to \
 nmeasure neutrino induced charged particles like muons. IceTop is a surfac
 e air shower detector consisting of 160 \nCherenkov ice tanks located on t
 op of IceCube. To extend IceTop\, a radio air shower detector could be bui
 lt to \nincrease the sensitivity at higher shower energies and for incline
 d showers significantly. As air showers induced by \ncosmic rays are a maj
 or part of the muonic background in IceCube\, IceTop is not only an air sh
 ower detector\, but \nalso a veto to reduce the background of IceCube. Air
  showers are detectable by radio signals with a radio surface \ndetector. 
 The major emission process is the coherent synchrotron radiation (geosynch
 rotron effect)\, emitted by e^+ \ne^- shower particles in the Earths magne
 tic field. Simulations of the expected radio signals of air showers are \n
 shown. The efficiency and the energy threshold of antenna field configurat
 ions are estimated.\n\nhttps://indico.nucleares.unam.mx/event/4/session/67
 /contribution/293
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/293
END:VEVENT
BEGIN:VEVENT
SUMMARY:The EEE Project
DTSTART;VALUE=DATE-TIME:20070710T180500Z
DTEND;VALUE=DATE-TIME:20070710T181700Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-2-644@cern.ch
DESCRIPTION:Speakers: SBARRA\, C. (Museo Storico della Fisica\, Centro Stu
 di e Ricerche "E. Fermi"\, Roma and INFN and Department of Physics\, Unive
 rsity of Bologna)\nThe EEE (/Extreme Energy Event/) Project is an experime
 nt for the study of very\nhigh-energy extensive air showers\, actually sta
 rting in Italy. It is based on the\ndetection of the shower muon component
  by means of a network of tracking detectors\,\ninstalled in Italian High 
 Schools.\n\nThe Project\, supported by the Ministero dell’Università e 
 della Ricerca (MIUR)\,\nIstituto Nazionale di Fisica Nucleare (INFN)\, Eur
 opean Organization for Nuclear\nResearch (CERN) and Museo Storico della Fi
 sica e Centro Studi e Ricerche “E. Fermi”\nhas been conceived by its l
 eader Professor Antonino Zichichi.\n\nIn its first phase the detector tele
 scopes will be installed in 21 High Schools in 7\npiloting cities all over
  Italy. The network will soon be heavily upgraded by\nincreasing the numbe
 r of High Schools and cities.\n\nThe single tracking telescope is composed
  by 3 large (~ 2 m2 ) Multi-gap Resistive\nPlate Chambers (MRPC)\, realize
 d with float glass electrodes. The use of particle\ndetectors based on suc
 h MRPCs will allow to determine with a very high accuracy the\ndirection o
 f the axis of cosmic ray showers initiated by primaries of ultra-high\nene
 rgy\, together with a high temporal resolution.\n\nThe first MRPC telescop
 e\, installed in the Liceo Scientifico “B.Touschek” in\nGrottaferrata 
 near the LNF-INFN site (nearby Rome)\, is successfully running. By the\nen
 d of year 2007\, the installation of the other telescopes will open the wa
 y for the\nfirst search of high-energy cosmic rays distant coincidences.\n
 \nIn the future\, serving many High Schools scattered all over the Italian
  territory\,\nthe EEE Project will also allow to investigate coincidences 
 between multiple\nprimaries producing distant showers. Here we present the
  experimental apparatus and\nits tasks.\n\nhttps://indico.nucleares.unam.m
 x/event/4/session/67/contribution/644
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/644
END:VEVENT
BEGIN:VEVENT
SUMMARY:Physics of the TALE Experiment
DTSTART;VALUE=DATE-TIME:20070710T181700Z
DTEND;VALUE=DATE-TIME:20070710T182900Z
DTSTAMP;VALUE=DATE-TIME:20260415T192852Z
UID:indico-contribution-67-2-1133@cern.ch
DESCRIPTION:Speakers: Prof. THOMSON\, Gordon (Rutgers\, The State Universi
 ty of New Jersey\, USA)\nThe Telescope Array Low Energy Extension (TALE) E
 xperiment consists of\nthree detectors which will extend the sensitivity i
 n energy of the\nTelescope Array (TA) experiment by two orders of magnitud
 e\, from\n18.5\n\nhttps://indico.nucleares.unam.mx/event/4/session/67/cont
 ribution/1133
LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana)
URL:https://indico.nucleares.unam.mx/event/4/session/67/contribution/1133
END:VEVENT
END:VCALENDAR