BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Calibration of the EAS Radio Pulse Height DTSTART;VALUE=DATE-TIME:20070706T153000Z DTEND;VALUE=DATE-TIME:20070706T154200Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-1-119@cern.ch DESCRIPTION:Speakers: Dr. HORNEFFER\, Andreas (RU Nijmegen)\nLOPES is one the pioneering experiments for the measurement of radio emission\nfrom air showers with digital radio receivers. It is set up at the site of the\nKA SCADE-Grande air shower array and takes data in conjunction with it. This\ ngives us the unique possibility to combine LOPES and KASCADE-Grande data. \n\nIn its second phase LOPES has been extended to 30 antennas\, which inc reases\nthe detection rate of well reconstructed events. Also a new\, abso lute\ncalibration of the radio antennas is now available. By correlating t he\nmeasured radio pulse height with air shower parameters measured by\nKA SCADE-Grande\, we have derived a formula that describes the radio pulse he ight\nas a function of air shower geometry and primary particle energy. Th us allowing\nus to estimate the cosmic ray energy from radio data.\n\nhttp s://indico.nucleares.unam.mx/event/4/session/55/contribution/119 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/119 END:VEVENT BEGIN:VEVENT SUMMARY:New approach to UHE cosmic ray investigations in the energy range 10^15 - 10^19 eV DTSTART;VALUE=DATE-TIME:20070706T154200Z DTEND;VALUE=DATE-TIME:20070706T155400Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-1-201@cern.ch DESCRIPTION:Speakers: Dr. YASHIN\, Igor (Moscow Engineering Physics Instit ute (State University))\nA new approach to investigations of ultra-high en ergy cosmic rays based on the new\nEAS observable - spectra of local densi ty of muons measured at ground level in a wide\nrange of zenith angles - i s considered. It is shown that muon density spectra are\nsensitive to the primary cosmic ray spectrum and composition\, and to features of the\nforw ard kinematic region of hadronic interaction\, and thus provide new inform ation\nthat can be used for verification of some hypotheses about UHE cosm ic ray spectra and\nof EAS simulation tools. For illustration of possibili ties of the new approach\, the\nexperimental data on muon bundles at zenit h angles from 30 degrees to horizon\nobtained with the Russian-Italian coo rdinate-tracking detector DECOR are used. The\nanalysis based on CORSIKA s imulation shows that measurements of muon density spectra\nin inclined EAS give the possibility to study characteristics of primary cosmic ray\nflux in a wide energy range from 10^15 to 10^19 eV by means of a single relati vely\nnot large detector with a single experimental technique.\n\nhttps:// indico.nucleares.unam.mx/event/4/session/55/contribution/201 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/201 END:VEVENT BEGIN:VEVENT SUMMARY:Zenith angle dependence of the size spectrum of air showers around the knee observed with the Tibet air shower array DTSTART;VALUE=DATE-TIME:20070706T155400Z DTEND;VALUE=DATE-TIME:20070706T160600Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-1-268@cern.ch DESCRIPTION:Speakers: Dr. HUANG\, Jing (Institute for Cosmic Ray Research\ , the University of Tokyo)\nThe air shower size (Ne) spectrum of cosmic ra ys around the knee at different zenith\nangles has been studied with the T ibet-III air-shower array. The air shower size is\nestimated by fitting t he lateral density distribution of the shower particles using\nthe modifie d NKG function\, which is optimized by the Monte Carlo simulation by using \ninteraction models of QGSJET01c and SIBYLL2.1 taking into account of the detector\nconfigurations. It is shown that the model dependence in the ai r shower size\ndetermination is not significant being less than 10% in th e absolute flux value and\nthe location of the break Ne* (or ''knee'') is seen to move to larger Ne* with\nincreasing zenith angle. In this paper\, we also show that for both models the\nobserved air shower size spectra ar e wholly compatible with the heavy-enriched\ncomposition in the knee energ y region.\n\nhttps://indico.nucleares.unam.mx/event/4/session/55/contribut ion/268 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/268 END:VEVENT BEGIN:VEVENT SUMMARY:Evidences for the Influence of the Earth's Magnetic Field on EAS M uon Component DTSTART;VALUE=DATE-TIME:20070706T160600Z DTEND;VALUE=DATE-TIME:20070706T161800Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-1-203@cern.ch DESCRIPTION:Speakers: Dr. YASHIN\, Igor (Moscow Engineering Physics Instit ute (State University))\nThe dependence of the intensity of muon bundles d etected at the Earth's surface by\nmeans of the coordinate-tracking detect or DECOR on the angle between muon arrival\ndirection and geomagnetic fiel d vector (pitch angle) has been analysed. It is found\nthat muon bundle in tensity decreases with the increase of the transverse component of\nthe ma gnetic field in comparison with calculations performed under assumption of \nazimuthal symmetry of the flux\, the effect being enhanced with the incr ease of zenith\nangle. Comparison with CORSIKA-based simulations has shown that this effect is\nexplained by changes in EAS muon lateral distributio n functions caused by propagation\nof particles in the Earth's magnetic fi eld. Another effect - appearance of a\ncoplanar component in directions of EAS muons in a plane determined by shower axis\nand Lorentz force vector - has been also observed.\n\nhttps://indico.nucleares.unam.mx/event/4/sess ion/55/contribution/203 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/203 END:VEVENT BEGIN:VEVENT SUMMARY:All-particle cosmic ray energy spectrum in the 3-200 PeV energy ra nge DTSTART;VALUE=DATE-TIME:20070706T133000Z DTEND;VALUE=DATE-TIME:20070706T134200Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-0-515@cern.ch DESCRIPTION:Speakers: Dr. MARTIROSOV\, R.M. (Yerevan Physics Institute)\nW e present the all-particle primary cosmic ray energy spectrum obtained by a \nparametric event-by-event determination of the primary energy. The res ults are \nobtained on the basis of an expanded experimental data from the GAMMA \nexperiment. The method was developed using the CORSIKA EAS simula tion \ncode with the SYBILL interaction model and taking into account the response of \nthe GAMMA detectors and reconstruction uncertainties of the EAS parameters.\n\nhttps://indico.nucleares.unam.mx/event/4/session/55/con tribution/515 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/515 END:VEVENT BEGIN:VEVENT SUMMARY:Preliminary results of the Moon shadow using the ARGO-YBJ experime nt DTSTART;VALUE=DATE-TIME:20070706T134200Z DTEND;VALUE=DATE-TIME:20070706T135400Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-0-458@cern.ch DESCRIPTION:Speakers: Dr. WANG\, Bo (Key Laboratory of Particle Astrophysi cs\, Institute of High Energy Physics\, Chinese Academy of Sciences\, Beij ing 100049\, China)\nARGO-YBJ is a "full coverage" air shower detector con sisting of \na carpet of Resistive Plate Chambers\, located at Yangbajing (4300m a.s.l.). \nUsing the data collected by the central detector (5800m^ 2 area) \nthe cosmic ray shadowing effect due to the Moon is studied. \nT he comparison of experimental results with Montecarlo simulations is \nals o discussed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/55/contr ibution/458 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/458 END:VEVENT BEGIN:VEVENT SUMMARY:The cosmic ray all-particle spectrum in the wide energy range from 10^{14} eV to 10^{17} eV observed with the Tibet-III air shower array DTSTART;VALUE=DATE-TIME:20070706T135400Z DTEND;VALUE=DATE-TIME:20070706T140600Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-0-277@cern.ch DESCRIPTION:Speakers: Mr. CHEN\, Ding (Faculty of Engineering\, Yokohama N ational University)\nWe present an updated all-particle energy spectrum us ing data set collected in the\nperiod from 2000 November through 2004 Oct ober by Tibet-III air-shower array. The\nenergy determination of the air s howers is made by fitting the lateral density\ndistribution of the shower particles to the modified NKG function which is optimized\nby simulation c alculation using interaction models of QGSJET01c \nand SIBYLL2.1 taking in to account of the detector configurations. It is shown that\nthe model dep endence in the energy determination is not significant being less than\n10 % in the absolute flux value and we obtained the cosmic ray energy spectru m in a\nwide range over 3 decades between 10^{14} eV and 10^{17} eV\, in which the position\nof the knee is clearly seen at around 4 PeV. Based on \nthese calculations\, we briefly discuss the systematic errors involved i n our\nexperimental results due to the Monte Carlo simulation.\n\nhttps:// indico.nucleares.unam.mx/event/4/session/55/contribution/277 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/277 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Rays in IceCube: Composition-Sensitive Observables DTSTART;VALUE=DATE-TIME:20070706T140600Z DTEND;VALUE=DATE-TIME:20070706T141800Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-0-1294@cern.ch DESCRIPTION:Speakers: Dr. SONG\, Chihwa (Department of Physics\, Universit y of Wisconsin\, Madison\, WI 53706)\nCosmic ray showers that trigger the IceTop surface array generate high energy muons\nthat are measured by the IceCube in-ice detector. The large surface and underground\narea of this 3 -dimensional instrument at completion guaranties significant statistics\nf or shower energy up to about 1 EeV. Since the number of muons is sensitive to the\ntype of the primary cosmic ray nucleus these events can be used f or the measurement\nof cosmic ray composition. Using the data taken in the existing array we measure the\nobsevables sensitive to the primary mass as a function of shower energy estimate\nwith the surface array. The resul t is compared to simulations of the coincident\nevents with different type s of primary nuclei.\n\nhttps://indico.nucleares.unam.mx/event/4/session/5 5/contribution/1294 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/1294 END:VEVENT BEGIN:VEVENT SUMMARY:Study of cosmic ray showers front and time structure with ARGO-YBJ DTSTART;VALUE=DATE-TIME:20070706T141800Z DTEND;VALUE=DATE-TIME:20070706T143000Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-0-1100@cern.ch DESCRIPTION:Speakers: Dr. MARSELLA\, Giovanni (Department of Innovation En gineering\,University of Salento and INFN\, Lecce\, ITALY)\nARGO-YBJ is a full coverage Extensive Air Shower array located by the\nhigh-altitude cos mic rays laboratory of Yangbajing (4300 m a.s.l.\, Tibet\,\nChina). The de tector consists of a layer of Resistive Plate Counters covering an area of \nabout 5800 m^2 with 58x62 cm^2 unit cells. This design allows a detaile d\ncharacterization of cosmic ray showers induced by primaries with energy in the range\nfrom 300 GeV up to 100 TeV.\nA set of well reconstructed da ta has been used in order to study the shower\nphenomenology and front str ucture with high time resolution (1 ns accuracy) and fine\ngranularity.\nS imulated CORSIKA showers have been used and the detector response is taken into\naccount in detail for this analysis. Several observables have been investigated in\nboth real and simulated data and compared\, aiming to der ive hints on cosmic ray\nshower age\, energy and mass composition. Results are presented and discussed.\n\nhttps://indico.nucleares.unam.mx/event/4/ session/55/contribution/1100 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/1100 END:VEVENT BEGIN:VEVENT SUMMARY:LOPES30 data analysis DTSTART;VALUE=DATE-TIME:20070706T143000Z DTEND;VALUE=DATE-TIME:20070706T144200Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-0-825@cern.ch DESCRIPTION:Speakers: Mr. NEHLS\, Steffen (Forschungszentrum Karlsruhe)\nL OPES30 is a digital radio antenna array working in the frequency range 40 -- 80 MHz\nwith 30 dipole antennas triggered by the air shower experiment KASCADE-Grande. From\nan absolute calibration the measured field strength of the LOPES30 antenna system is\nknown and the invesitigation of a large data set taken in east-west polarisation is\nperformed.\nThe reconstructed pulse height of the radio emission in extensive air showers is the\nmeasu red quantity to be compared with the KASCADE-Grande reconstruction paramet ers\,\nlike primary energy or shower geometrie on a single air hower basis . The resulting\ncorrelations will also be compared with expectations from detailed Monte Carlo\nsimulations.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/55/contribution/825 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/825 END:VEVENT BEGIN:VEVENT SUMMARY:Using the ARGO-YBJ experiment to determine the attenuation and the absorption lengths DTSTART;VALUE=DATE-TIME:20070706T144200Z DTEND;VALUE=DATE-TIME:20070706T145400Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-0-904@cern.ch DESCRIPTION:Speakers: Dr. ZHA\, Min (Institute of High Energy Physics)\nUs ing the data taken by the ARGO-YBJ experiment (606 $g/cm^{2}$\, Tibet\, P. R.China)\nin the period of July to September 2006\, the first measurement of\nEAS size spectrum in the range of $N_{e}=5\\times10^{4}-5\\times10^{6} $\nis presented at different zenith angles. The attenuation and absorption \nlengths have been determined by applying different analysis methods.\nFu rthermore the proton-air inelastic cross section around few hundrend TeV\n is explored by using the factor $k=\\lambda_{abs}^{sim}/\\lambda_{pair}^{s im}$\nobtained on the base of Monte Carlo simulation.\n\nhttps://indico.nu cleares.unam.mx/event/4/session/55/contribution/904 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/904 END:VEVENT BEGIN:VEVENT SUMMARY:Reconstruction of primary mass group energy spectra with KASCADE DTSTART;VALUE=DATE-TIME:20070706T170500Z DTEND;VALUE=DATE-TIME:20070706T171700Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-2-178@cern.ch DESCRIPTION:Speakers: Dr. ULRICH\, Holger (Forschungszentrum Karlsruhe)\nT he KASCADE-Grande experiment\, located at the area of the Forschungszentru m\nKarlsruhe\, Germany\, measures extensive air showers in the energy rang e between\n10^{14} and 10^{18} eV\, thus covering the first and the second knee of cosmic rays.\n\nFormer analyses of electron and muon data of the original KASCADE experiment revealed\nknee-like features in the energy spe ctra of light elements causing the knee in the\nall particle energy spectr um. Furthermore\, these analyses showed the limited\ncapability of the int eraction models QGSJet 01 and SIBYLL 2.1 to consistently\ndescribe the who le measured data range.\n\nAn update of the continuation of the analysis i s given\, presenting results for\ndifferent data sets and the use of the F LUKA model instead of the GHEISHA code in the\nsimulations. In addition\, features of improved and new interaction models (like\nQGSJet II and EPOS) and their impact on the analysis results will be discussed.\n\nhttps://in dico.nucleares.unam.mx/event/4/session/55/contribution/178 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/178 END:VEVENT BEGIN:VEVENT SUMMARY:Muon Production Height in the Air-Shower Experiment KASCADE-Grande . DTSTART;VALUE=DATE-TIME:20070706T171700Z DTEND;VALUE=DATE-TIME:20070706T172900Z DTSTAMP;VALUE=DATE-TIME:20260517T215533Z UID:indico-contribution-55-2-514@cern.ch DESCRIPTION:Speakers: Dr. DOLL\, Paul (scientist)\nA large area streamer t ube detector (128m^2)\, located within the KASCADE-\nGrande Experiment\, h as been built with the aim to identify muons\n(E>0.8GeV) and their directi on in extensive air showers. Besides the\ninvestigation of the muon pseudo rapitity in EAS\, the application of the\ntracking detector in reconstruct ing the muon production height is\nevaluated. The combination of the muon production height with shower\nparameters from the surface array is demons trated. Almost model independent\nenergy spectra for different mass groups are obtained. The muon\nproduction height distributions are reproduced di fferently by different\ninteraction models which are employed in the air-s hower simulation code\nCORSIKA.\n\nhttps://indico.nucleares.unam.mx/event/ 4/session/55/contribution/514 LOCATION:Merida\, Mexico Yucatan II+III+IV (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/55/contribution/514 END:VEVENT END:VCALENDAR