BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Posters 2 + Coffee DTSTART;VALUE=DATE-TIME:20070707T194500Z DTEND;VALUE=DATE-TIME:20070707T211500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-event-39-1@cern.ch DESCRIPTION:OG 2.1-2.4\; HE 1.5\, 1.6\; SH 1.8\, 3.6\n\nhttps://indico.nuc leares.unam.mx/event/4/session/39/?slotId=1 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/?slotId=1 END:VEVENT BEGIN:VEVENT SUMMARY:About the possibility for estimation of the atmospheric transparen cy on the basis of EAS Cherenkov light registration DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-57@cern.ch DESCRIPTION:Speakers: Dr. MISHEV\, alexander (Institute for Nuclear Resear ch and Nuclear Energy\, Bulgarian Academy of Sciences)\nThe transparency i s one of the primary measures of the atmospheric state. The precise\nlong term series of atmospheric transparency measurements gives the possibility for\nquantitative estimate of the variability of air circulation and to m ake climatologic\nconclusions with regard to contamination\, cloud formati on\, humidity and radiative\nexchange. It seems to be possible to estimate the atmospheric transparency on the\nbasis of atmospheric Cherenkov light registration and corresponding Monte Carlo\nsimulations. Measuring the Ch erenkov light flux produced in extensive air shower in\ndifferent atmosphe ric conditions one obtains different amplitude spectra. This\nreflects on the slope of the reconstructed spectrum. The different slopes of the\nreco nstructed spectra correspond obviously to different atmospheric conditions . In\nthis work are presented several CORSIKA simulations of the expected density spectra\nat sea level and high mountain altitude observation level s. Several preliminary\nmeasurements with atmospheric Cherenkov telescope and estimates are shown. The\npossibility to study different atmospheric p rofiles is discussed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/ 39/contribution/57 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/57 END:VEVENT BEGIN:VEVENT SUMMARY:HEAT : Enhancement Telescopes for the Pierre Auger Southern Observ atory in Argentina DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-65@cern.ch DESCRIPTION:Speakers: \nThe southern part of the Pierre Auger Observatory is nearing completion in the \nprovince of Mendoza\, Argentina. The instru ment has been used to take air \nshower data at the highest energies since 2004. The energy threshold for high \nquality shower data is about 3 10** 18 eV for the surface array of particle \ndetectors (SD). The data of the Auger fluorescence telescopes (FD) enable \nprecise event reconstruction even below 10**18 eV.\nAfter the completion of the southern observatory th e Pierre Auger Collaboration \nintends to further expand its energy range down to nearly 10**17 eV by three \nadditional fluorescence telescopes (H EAT) with an elevated field of view from 30 \nto nearly 60 degree. It is p lanned to use these telescopes in the hybrid mode \nin combination with an infilled detector array with fourfold sampling density and \nadditional m uon detection capabilities (AMIGA).\nThese enhancements will enable the so uthern Pierre Auger Observatory to \ncover the energy range of interest fo r the transition from galactic to \nextragalactic cosmic rays as well as t he highest energy domain in a common \nexperiment with good energy and mas s resolution. \nThe Pierre Auger Observatory in Argentina will thus be ext ended to have a \nbroad overlap with the data range of the KASCADE Grande experiment. The \nHEAT layout and the estimated properties of the enhancem ent telescopes will \nbe discussed.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/39/contribution/65 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/65 END:VEVENT BEGIN:VEVENT SUMMARY:A Macroscopic description of Coherent Geo-Magnetic Radiation from Cosmic rays DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-69@cern.ch DESCRIPTION:Speakers: SCHOLTEN\, Olaf (KVI / RUG)\nIn an air shower induce d by a cosmic ray\, due to the high velocities\, most of\nthe particles ar e concentrated in the relatively thin shower front\, which\, for\nobvious reasons\, is called the 'pancake'. This pancake\, which for the present\nd iscussion is assumed to be charge neutral\, contains large numbers of elec trons\nand positrons. It has a typical thickness of a few meters and is mo ving to the\nsurface of the Earth with (almost) the velocity of light\, $c $. When this\npancake is moving through the Earth magnetic field the Loren tz force on the\ncharged particles induces a drift velocity and thus an el ectric current in a\ndirection which is perpendicular to the magnetic fiel d and the shower axis.\nThis fast-moving electrical current induces an ele ctromagnetic pulse which can\nbe detected at the Earth surface. Because of the typical length and time scales\ninvolved\, the intensity of the radia tion is maximal in the frequency range of\n1-10 MHz\, and can thus be dete cted with radio receivers.\n\nTo show the basic principles of the Macrosco pic Geo-Magnetic Radiation (MGMR)\nmodel and we confine ourselves to a rat her simple geometry where the cosmic\nshower moves straight to the Earth s urface and where the Earth magnetic field\nis parallel to the Earth surfac e. In the limit where the thickness of the\npancake is shrinked to zero ev en a simple analytic form for the electric pulse\ncan be derived. This sho ws that the pulse height falls rapidly with distance to\nthe shower core\, that with increasing distance the pulse lengthens\, and that\nthe leading part of the pulse carries the information on the earlier parts of\nthe ai r shower.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribut ion/69 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/69 END:VEVENT BEGIN:VEVENT SUMMARY:The new large-sized scintillation charged particles detector for e xtensive air shower experiments at Tien-Shan. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-86@cern.ch DESCRIPTION:Speakers: SHEPETOV\, A.L. (P.N.Lebedev Physical Institute\, Ti en-Shan Mountain Station)\nFor the newly build extensive air shower array of the Tien-Shan mountain complex ATHLET \nis designed the new type of a l arge-size charged particles detector on the basis of the thin \nmolded pol ystyrene scintillator in conjunction with the wavelength shifting fibers. The 10 mm \nthick scintillation plates have a 1x1 m^2 sensitive area\, a 9 9% registration efficiency of the \ncharged particles and a homogeneity of the scintillation light output better than 90%. Due to \ntheir relatively low mass and cost characteristics\, the absence of the external high-volt age \nfeeding and a wide dynamic range of the registered signal amplitudes (about 10^6) \ndetectors of the described type suit well for the use in w ide-spread multi-channel extensive \nair shower installations.\n\nhttps:// indico.nucleares.unam.mx/event/4/session/39/contribution/86 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/86 END:VEVENT BEGIN:VEVENT SUMMARY:16-point DCT as the spectral 1st level surface detector trigger in the Pierre Auger Observatory DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-112@cern.ch DESCRIPTION:Speakers: Dr. SZADKOWSKI\, Zbigniew (University of Lodz)\nHadr on induced\, very inclined EAS\, starting their development early \nin the atmosphere produce narrow\, relatively flat muonic fronts on \nthe Pierre Auger detection level. The signatures of FADC traces \n(very short rise t ime with fast exponential attenuation) from water \nCherenkov tanks can be used for their detection. Currently used \ntriggers in the Pierre Auger s urface detector (Threshold and Time \nover Threshold triggers) have been s elected to detect showers with \npossibly wide range of distances from the core\, angles and energies. \nHowever they are not optimized for horizont al and very inclined \nshowers\, interesting as potentially generated by n eutrinos. \nThe paper describes the algorithm of 16-point discrete cosine transform \nas the spectral 1st level trigger implemented into a progressi ve FPGA\, \nused in the 4th generation of the surface detector.\n\nhttps:/ /indico.nucleares.unam.mx/event/4/session/39/contribution/112 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/112 END:VEVENT BEGIN:VEVENT SUMMARY:100 MHz sampling 1st level SD trigger for Infill Array and Auger N orth based on a single progressive FPGA DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-122@cern.ch DESCRIPTION:Speakers: Dr. SZADKOWSKI\, Zbigniew (University of Lodz)\nThe proposal of a new 4th generation of the Front-End with the advanced 1st \n level triggers for the Infill Array of the Pierre Auger Observatory and fo r the \nAuger North is described. Newest FPGA chips offer much higher capa city of logic \nregisters and memories\, as well as DSP blocks. The calibr ation channel\, \npreviously supported by an external dual-port RAM\, has been fully implemented \ninto FPGA chip\, through a large internal memory. In turn DSP blocks allowed on \nimplementation of much more sophisticated spectral trigger algorithms.\nA single chip simplified board design\, new er architecture of FPGA reduced \nresouces utilization and power consumpti on. Higher sampling in the new Front-\nEnd in comparison with previous 40 MHz designs as well as free resources for \nnew detection algotithms can b e a good platform for CR radio detection \ntechnique at Auger enhancing a duty cycle for the detection of UHECR’s.\n\nhttps://indico.nucleares.una m.mx/event/4/session/39/contribution/122 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/122 END:VEVENT BEGIN:VEVENT SUMMARY:Sigma-Delta compensation of pedestals in the First Level SD Trigge r of the Pierre Auger Observatory DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-124@cern.ch DESCRIPTION:Speakers: Dr. SZADKOWSKI\, Zbigniew (University of Lodz)\nDail y temperature variation in the electronic box of the surface detector in t he \nPierre Auger Observatory may reach more than 40ºC\, which causes a s ignificant \nvariation of the pedestal of FADC traces. Pedestal variation\ , more than 5 ADC–\ncounts in full temperature range\, could significant ly affect the trigger conditions \nespecially for the Time-over-Threshold Trigger working at very low thresholds \nabove the pedestals. In the curre ntly used algorithm\, the thresholds are being \nadjusted by the calibrati on channel in order to keep required trigger conditions. \nHowever\, keepi ng a stable pedestal seems to be better approach than \nthresholds tuning via the slow calibration loop. The algorithm\, implementation \nand prelim inary results from the climate chamber for the compensation of the \npedes tal drift in the First Level SD Trigger are presented. Results are \nsatis factory. The algorithm will be activated for testing in the real environme nt \nin a full hexagon of test tanks equipped with the Cyclone Front-End.\ n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/124 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/124 END:VEVENT BEGIN:VEVENT SUMMARY:Pinhole camera for study of atmospheric UV flashes as a source of background in the TUS experiment. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-148@cern.ch DESCRIPTION:Speakers: Mr. PONCE\, Epifanio (Moscow State University)\nThe near UV glow of the night atmosphere and near UV transient events in the \natmosphere are sources of the background phenomena in search for ultra h igh \nenergy cosmic ray fluorescence signals in the atmosphere. Nature of the UV \natmospheric transient events is not known yet and more experimen tal data on \nthem are needed. Study of space-time development of UV tran sient events is \nsuggested with the help of a new fast imaging detector: pinhole camera with \nthe multi anode photomultiplier tube. Design and co nstruction of the pinhole \ncamera to be installed at the satellite is pr esented. The camera mountain \ntesting and calibration are suggested.\n\n https://indico.nucleares.unam.mx/event/4/session/39/contribution/148 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/148 END:VEVENT BEGIN:VEVENT SUMMARY:FANSY: a code for simulations of coplanar particle generation in h adron interactions DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-158@cern.ch DESCRIPTION:Speakers: Prof. MUKHAMEDSHIN\, Rauf (Institute for Nuclear Res earch of Russian Academy of Science)\nThe phenomenon of alignment of most energetic structures of gamma-ray-hadron families\nfound in mountain and s tratospheric X-ray - emulsion chamber experiments cannot be\nexplained wit hout a coplanar particle generation with large transverse momenta in\nhadr on interactions at superhigh energies. A phenomenological model\, which ma kes it\npossible to simulate such interactions\, is presented. Different v ersions of this\nmodel are considered\, their features are described and c ompared with those of models\napplied by the CORSIKA package.\n\nhttps://i ndico.nucleares.unam.mx/event/4/session/39/contribution/158 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/158 END:VEVENT BEGIN:VEVENT SUMMARY:R&D of the Fresnel optical system for the TUS space detector DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-162@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. Th e TUS optical system \nwill consist of the Fresnel mirror-concentrator of ~2 sq. m. and 256 PMT pixels \nas the photo receiver at the mirror focal s urface. The 2 PMT pixel prototypes \nwere tested and used for data taken a t the “Universitetsky-Tatiana” and \nCompass-2 satellites. The R&D stu dy of the Fresnel mirror production is \npresented.\n\nhttps://indico.nucl eares.unam.mx/event/4/session/39/contribution/162 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/162 END:VEVENT BEGIN:VEVENT SUMMARY:Radio detection of high-energy cosmic rays at the Pierre Auger Obs ervatory DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-176@cern.ch DESCRIPTION:Speakers: Dr. VAN DEN BERG\, Ad (Kernfysisch Versneller Instit uut)\nThe Southern Auger Observatory provides an excellent test bed to stu dy the \nradio detection of extensive air showers as an alternative\, cost -effective\, and \naccurate tool for cosmic-rays physics. The data from th e radio setup can be \ncorrelated with those from the well-calibrated Auge r baseline detectors. \nFurthermore\, human-induced radio noise levels at the Southern Auger site are \nrelatively low. We have started an R&D progr am to test various radio-detection \nconcepts. Our studies will reveal Rad io Frequency Interferences (RFI) caused by \nnatural effects such as day-n ight variations\, thunderstorms\, and by human-\nmade disturbances. These RFI studies are required to optimise detection \nparameters such as antenn a design\, frequency interval\, antenna spacing and \nsignal processing. T he data from our initial setups\, which presently consist of \ntypically 3 -4 antennas\, will be used to characterise the shower from radio \nsignals and to optimise the initial concepts. Furthermore\, the operation of a \n large detection array requires autonomous detector stations. The current \ ndesign is aiming at stations with antennas for two polarizations\, solar power\, \nwireless communication\, and local trigger logic. The results of this initial phase \nprovides an important stepping stone for the design of a few tens kilometers \nsquare engineering array.\n\nhttps://indico.nuc leares.unam.mx/event/4/session/39/contribution/176 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/176 END:VEVENT BEGIN:VEVENT SUMMARY:The LOFAR air shower front evolution library DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-181@cern.ch DESCRIPTION:Speakers: Mr. LAFEBRE\, Sven (Dept. of Astrophysics\, IMAPP\, Radboud University)\nThe LOFAR radio telescope\, under construction in the Netherlands\, will be a powerful instrument \nto measure extensive air showers through their radio signal. In order to fully understand the \np roperties of these signals\, we are building a library of CORSIKA simulati ons of showers at \n10^16--10^20.5 eV on the LOFAR BlueGene supercompute r. This library contains histogrammed \ndata on the particle energy and spatial and angular distributions throughout the course of the air \nsho wers. The REAS2 code is used to calculate geosynchrotron radio emission fr om these \nsimulations. We present parametrisations of various character istics of the particle distributions and \nradio signal from showers in this library.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contr ibution/181 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/181 END:VEVENT BEGIN:VEVENT SUMMARY:Design Considerations for the Next Generation of Atmospheric Imagi ng Cherenkov Telescopes DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-189@cern.ch DESCRIPTION:Speakers: Dr. BUGAEV\, Viatcheslav (Washington University\, De partment of Physics\, Campus Box 1105\, 1 Brookings Dr. St. Louis\, MO 631 30\, USA)\nThe HESS\, MAGIC and VERITAS experiments are now fully operatio nal\nand are detecting and discovering a large number of high-energy gamma -ray\nsources. This is a good time to work on the design of the next gener ation of IACT\nexperiments.\n\nWe estimate the limiting angular resolution and detection area for an\narray of 3 large-aperture IACTs. We consider a n idealized IACT system in order to\nunderstand the limitations imposed by the intrinsic nature of the atmospheric showers\nfor such a configuration . The idealization includes the assumptions of a perfect\noptical system\, the absence of the night sky background and a wide field\nof view.\n\nThe showers are simulated using the ALTAI code. A number of values of altitud e and\nmagnetic field intensity are tested corresponding to possible futur e sites for a new\nnorthern-hemisphere array. The optimal design depends o n the target\nenergy range\; for each energy we tune both the cell length and the image processing\nin order to maximize the signal-to-noise-ratio a nd present the resulting values of\nthe detection area and the angular res olution. We discuss the dependence of these\nquantities on the mirror size and the field of view of the telescopes.\n\nhttps://indico.nucleares.unam .mx/event/4/session/39/contribution/189 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/189 END:VEVENT BEGIN:VEVENT SUMMARY:A New Parallel Processing Scheme Enabling Full Monte Carlo EAS Si mulation in the GZK Energy Region DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-199@cern.ch DESCRIPTION:Speakers: Prof. KASAHARA\, katsuaki kasahara (Advanced Researc h Institue For Science And Engineering\, Waseda University)\nWe developed a new parallel processing method enabling full M.C EAS simulation (say\, with minimum energy of \n500 keV) without using thin sampling even at 10^ 19 eV. Normally\, distributed-parallel processing needs a \nspecific sof tware and programs must be organized to match with such system. During t he computation such a \nscheme also requires complex communications among many computer hosts. \n Our scheme first creates a skeleton of a shower \, and smashes it into n-peaces and distributes the peaces to n-\ncpu to flesh them. After each peace is completely fleshed\, they are assembled to make a complete picture of the \nshower. Thus\, during the computation need no communication. With n=50\, a 10^19 eV shower can be \nsimulated in ~10 days. For a 10^20 eV shower\, we may randomly sample a fraction of n-peases (say\, 100 for \nn=1000)\, and safely econstruct whole picture of the shower. The scheme dose not use any weight on each \nparticle and very much stable. \n The scheme has been implemented in Cosmos code. T o produce a number of showers with full fluctuations\, \nwe have also dev eloped a new method which utilizes the present result. The latter is u sed for the TA \nexperiment and is described in an accompanying paper.\n\ nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/199 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/199 END:VEVENT BEGIN:VEVENT SUMMARY:A Fast and Accurate Monte Carlo EAS Simulation Scheme in the GZK Energy Region and Some Results for the TA experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-200@cern.ch DESCRIPTION:Speakers: Prof. KASAHARA\, katsuaki kasahara (Advanced Researc h Institue For Science And Engineering\, Waseda University)\nAs described in an accompanying paper (kasahara)\, full M.C simulation of air showers in the GZK region is \npossible by a distributed-parallel processing m ethod. However\, this still needs a long computation time even \nwith ~ 50 to ~100 cpu's which may be available in many pc cluster environments. Air showers always fluctuate \nevent to event largely\, and only 1 or fe w events are not appropriate for practical application.\n However\, we ma y note that the fluctuations appear only in the longitudinal development\ ; if we look into the \ningredients (energy spectrum\, angular distributio n\, arrival time distribution etc and their correlations) at the \nsame "a ge" of the shower\, they are almost the same (or at least can be scaled\; e.g\, for the lateral distribution\, \nwe may use appropriate Moliere len gth ). In some cases (for muons and hadrons)\, we may use another \npar ameter instead of the "age". \n Based on this fact\, we developed a n ew fast and accurate M.C simulation scheme which utilizes a database in \n which full M.C\nresults are stored (FDD). We generate a number of air sho wers by using the usual thin sampling method. The \nthin sampling is some times very dangerous when we discuss detailed ingredient (say\,lateral di stribution\, energy \nspectrum\, their correlations etc) but is safely em ployed to see the total number of particles in the longitudinal \ndevelop ment (LDD\; we can generate ~1000 LDD showers by 50 cpu's in a day). The n\, for a given 1 particular \nsuch an event at a certain depth\, we can e xtract every details from FDD by a correspondence rule such as the \none u sing "age" etc. \n We describe the method\, its current status and show some results for the TA experiment.\n\nhttps://indico.nucleares.unam.mx/e vent/4/session/39/contribution/200 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/200 END:VEVENT BEGIN:VEVENT SUMMARY:Performance of the 1.5*10^5 front-end electronics channels of the ARGO-YBJ experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-218@cern.ch DESCRIPTION:Speakers: Prof. CARDARELLI\, Roberto (INFN Roma Tor Vergata)\n By using an 8-channel custom chip in GaAs technology\, over 1.5*10^5 front -end \nelectronics channels were built\, tested and installed in the resis tive plate \nchambers (RPCs) of the ARGO-YBJ experiment. These channels we re designed \nto obtain 1 ns time resolution over about 6000 m^2 of sensit ive area. Here we \npresent the design features\, the performance and the results during a long \noperational time at an altitude of 4300 meters a.s .l.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/21 8 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/218 END:VEVENT BEGIN:VEVENT SUMMARY:Long-term study of the environmental effects on the ARGO-YBJ RPC a rray DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-219@cern.ch DESCRIPTION:Speakers: Dr. CAMARRI\, Paolo (University of Roma "Tor Vergata " and INFN Roma Tor Vergata - Italy)\nAfter a 1-year-long running time\, m uch information has been collected on the \nperformance of the ARGO-YBJ de tector. In particular\, increased expertise on the \ndetector behaviour in the peculiar environmental conditions of the experimental \nsite (4300 me ters a.s.l.) has been reached. Here we show and discuss the \ncorrelation between the detector operating parameters and the environmental \nfactors\ , exploiting the statistical significance provided by a long-term monitori ng \nof the whole full-coverage central array of 1560 Resistive Plate Cham bers.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/ 219 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/219 END:VEVENT BEGIN:VEVENT SUMMARY:Laser Calibration of the Air Fluorescence Yield Experiment AIRLIGH T DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-228@cern.ch DESCRIPTION:Speakers: Dr. GONZALEZ\, Danays (University of Karlsruhe)\nThe relative fluorescence efficiency for MeV electrons in nitrogen and air ha s \nbeen measured with high precision by the AIRLIGHT experiment. The rang e \nfrom 300nm to 400nm was spanned using a 300nm to 400nm broad-band (M-\ nUG6) filter and 5 narrow-band filters. Fluorescence photons were detected by \nseven 2” PMTs in coincidence with the signals of a plastic scintil lator which \nstopped the collimated beam from a 90Sr electron source. \nT he main source of errors for the absolute scale of the fluorescence yield is the \nuncertainty of the efficiency of the PMTs for single photon detec tion in the UV \ndomain.\nTherefore\, using the original AIRLIGHT set-up\, the 90Sr electron beam was \nsubstituted by a pulsed N2 laser beam with a wavelength of 337nm and similar \ngeometry. The scintillator at the beam stop was replaced by a calibrated power \nprobe to measure the laser inten sity in each pulse. The beam intensity is \nreduced by neutral density fil ters to achieve count rates from the Rayleigh \nscattering similar to the fluorescence measurements. A narrow-band filter \n(337nm)\, a M-UG6 broad- band filter\, and a quartz window are applied to three \noriginal PMTs of the fluorescence measurements. The experimental procedures \nand first res ults are discussed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39 /contribution/228 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/228 END:VEVENT BEGIN:VEVENT SUMMARY:Deployment of an array of water-Cherenkov detectors for Extensive Air Shower Experiments DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-262@cern.ch DESCRIPTION:Speakers: Ms. SHEIDAEI\, Farzaneh (Sharif University of Techno logy)\nA new small array of cherenkov detectors is deployed in Tehran\, 12 00 m \nabove sea level. This array contains of four tanks full of distille d water with \ndiameter of 60 cm and height of 120 cm. The effective area of each tank is \nabout 0.6 . They are used to detect the air showers and to record the arrival \ntime of the secondary particles. We have collected about 200000 EAS in 1894 h \nof observation time from nov-2005 to Feb-200 6. We find zenith and azimuth \ndistribution of EAS with this array. A d istribution with n=5.70.1 was obtained \nfor zenith angle and a West-Ea st asymmetry has been observed in the \nazimuthal distribution of EAS of c osmic rays because of the magnetic field of the \nEarth. This asymmetry is about 1%.\n Since this tank of distilled water is cheaper and more ava ilable than \nScintillators it is preferable to use them instead of Scinti llators in our future \nlarger array. Result of data analysis and computer simulation with CORSIKA \ncode is presented in this paper.\n\nhttps://ind ico.nucleares.unam.mx/event/4/session/39/contribution/262 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/262 END:VEVENT BEGIN:VEVENT SUMMARY:3D Reconstruction of Extensive Air Showers from Fluorescence Data DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-282@cern.ch DESCRIPTION:Speakers: Prof. PIMENTA\, Mario (LIP)\, Dr. ANDRINGA\, Sofia ( LIP)\nA method to reconstruct the 3-dimensional structure of extensive air showers\, \nseen by fluorescence detectors\, is described.\nThe observati on of the shower is done in 2-dimensional pixels\, for consecutive \ntime bins. Time corresponds to a third dimension. Assuming that the cosmic ray \nshower propagates as a plane wave front moving at the speed of light\, a \ncomplex 3D volume in space can be associated to each measured charge (p er \npixel and time bin). The 3D description in space allows a simultaneou s access to \nthe longitudinal and lateral profiles of each shower. In cas e several eyes \nobserve the same shower\, the method gives a straight-for ward combination of \nall the information.\n\nhttps://indico.nucleares.una m.mx/event/4/session/39/contribution/282 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/282 END:VEVENT BEGIN:VEVENT SUMMARY:RADIODETECTION OF ASTRONOMICAL AND ATMOSPHERIC PHENOMENA IN THE CO SMIC RAY DEDICATED CODALEMA EXPERIMENT DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-337@cern.ch DESCRIPTION:Speakers: Mr. LAMBLIN\, Jacob (SUBATECH)\nThe main goal of the CODALEMA experiment\, located in the Station de Radioastronomie\nde Nanç ay\, France\, is the radiodetection of extensive air showers initiated by high\nenergy cosmic rays using log-periodic antenna and short active dipol es in the 1-200\nMHz bandwidth.\nFirst results showed that both antennas a re able to detect the transient radio\nsignals emitted by extensive air sh owers.\nIn addition to the detection of cosmic rays\, astronomical observa tions have been also\nperformed with these antennas allowing an estimation of the absolute CODALEMA\nperformances and a calibration of the antennas. \nAfter a brief technical description of both antennas\, the radio observ ation of a\nsolar flare during January 2005 is presented and the possibili ty to use the sun to\nestimate the CODALEMA angular resolution is shown. I n a second part\, the CODALEMA\nsensitivity to the galactic radio signal i s demonstrated and a method to calibrate\neach antenna with this signal is described. Finally\, it is shown that the wide\ndetection acceptance and frequency range offer a strong sensitivity to distant\natmospheric electri c-field evolutions like thunderstorms and related phenomena.\n\nhttps://in dico.nucleares.unam.mx/event/4/session/39/contribution/337 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/337 END:VEVENT BEGIN:VEVENT SUMMARY:EAS radio detection at large impact parameter: the inverse problem and the design of a giant array DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-338@cern.ch DESCRIPTION:Speakers: GOUSSET\, Thierry (Subatech)\nRadio electric field s trengths associated with extensive air shower can be \nevaluated at large impact parameter with analytical expressions. Such a \ntheoretical tool is most valuable in the present stage of development of the \nradio detectio n technique when the capabilities of the latter for comic-ray \nphysics ar e under investigations. It provides a manageable tool which can help \nin devising new ideas for the analysis of radio detection data. It can also b e \nused to perform non trivial tests of much more detailed numerical appr oaches \nwhich are currently under development.\n\nThe approximation leadi ng to such a formulation will be presented and two \napplications will be discussed: the inverse problem of how to go from a \nsampling of the radio electric field on a few antennas to the main characteristics \nof the ext ensive air shower\, and the question of the antenna spacing of a giant \na rray for ultra high energy cosmic rays.\n\nhttps://indico.nucleares.unam.m x/event/4/session/39/contribution/338 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/338 END:VEVENT BEGIN:VEVENT SUMMARY:Design and performances of a fully autonomous antenna for radio de tection of extensive air showers DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-339@cern.ch DESCRIPTION:Speakers: Dr. REVENU\, Benoit (APC/SUBATECH)\nThe use of the r adio-detection technique in a wide area cosmic-ray detector requires\nauto nomous antenna stations\, in terms of power feeding\, triggering and data\ ntransmission. A\nprototype has been tested at the Nançay Radio Observato ry (France).\nIt uses the broadband (1-200 MHz) active dipoles installed o n the CODALEMA\nexperiment (see other contributions in this conference)\, together with a solar power\nsupply\,\nan independent trigger electronics and a dedicated communication system. We\npresent here the complete setup and the performances of this new kind of detector.\n\nhttps://indico.nucle ares.unam.mx/event/4/session/39/contribution/339 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/339 END:VEVENT BEGIN:VEVENT SUMMARY:Optical and data acquisition system for the SPHERE-2 detector DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-435@cern.ch DESCRIPTION:Speakers: Dr. CHERNOV\, Dmitry (Skobeltsyn Institute of Nuclea r Physics of Moscow State University)\nA new method for high energy cosmic ray detection was suggested by A.E.Chudakov in\n1972. According to this m ethod a reflected from the snow surface Cherenkov light is\nobserved by an optical camera lifted above the surface on the balloon.\n\nOptical system of the SPHERE-2 detector consists of 1500mm diameter spherical mirror\nan d has 1sr view angle. Shmidt aperture diaphragm allows to reach 109 pixel optical\nresolution on the focal surface of the mirror. Electronic part of the detector\nconsists of 109 pulse shape acquisition FADC channels with 25 ns steps. The dynamic\nrange in each channel is equal to 10000 due to u sing of two 10-order ADC. PMTs have\n109 autoranging high-voltage power s upplies that allow to set optimal PMT sensitivity\naccording to the light conditions of\nmeasurements. Trigger system allows to separate on the PMTs mosaic light spot images\nof Cherenkov light reflected from the snow surf ace.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/4 35 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/435 END:VEVENT BEGIN:VEVENT SUMMARY:Experiment SPHERE-2 status 2007 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-438@cern.ch DESCRIPTION:Speakers: Dr. CHERNOV\, Dmitry (Skobeltsyn Institute of Nuclea r Physics of Moscow State University)\nNew SPHERE-2 detector basic paramet ers are described.\n\nNew calorimetric method is used to study the primary cosmic rays energy spectrum and\nchemical composition at energy region 10 PeV - 1 EeV. The method is practically\nindependent of the particle inter action model. Results of CORSIKA simulation of\ndetector are presented.\n\ nLifted by tied balloon to the 1 km altitude detector will detect EAS Cher enkov light\nreflected from the snow frozen surface of Baikal lake. First measurements are planned\nto the beginning of 2008.\n\nhttps://indico.nucl eares.unam.mx/event/4/session/39/contribution/438 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/438 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Tau Neutrino Telescope (CRTNT) Prototype Experiment at Yangbajing DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-456@cern.ch DESCRIPTION:Speakers: Prof. HE\, Huihai (Institute of High Energy Physics\ , CAS)\nCosmic Ray Tau Neutrino Telescope (CRTNT) is designed to detect ta u lepton \nshowers initiated from Earth-skimming tau neutrinos. A potentia l site is located \nat Balikun\, Xinjiang\, China. Two CRTNT Cerenkov imag ing telescopes are \ninstalled at Yangbajing\, Tibet (4300m a.s.l.) near t he ARGO-YBJ RPC carpet \ndetector\, with which coincident observation of c osmic ray showers above \n10^14 eV is performed for telescope testing. Det ector status and operational \nresults are reported in this paper.\n\nhttp s://indico.nucleares.unam.mx/event/4/session/39/contribution/456 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/456 END:VEVENT BEGIN:VEVENT SUMMARY:Fluorescence in air with moisture and its effect on the energy det ermination of ultrahigh-energy cosmic rays DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-465@cern.ch DESCRIPTION:Speakers: Dr. SAKAKI\, Naoto (Aoyama Gakuin University)\nPhoto n yields in moist air are measured with Sr90 beta source\nand compared wit h those in dry air. \nConsiderable reduce in the photon yields is found du e to water vapor.\nSince the ultrahigh energy cosmic ray observatories (Hi Res\, Auger\, TA)\nwith fluorescence technique on ground are at high altit ude\,\nthe effect of the water vapor may be negligible.\nHowever\, for the experiments from space like JEM-EUSO\,\nthe decrease of photon yield in m oist air should be\ntaken into account to interpret the longitudinal devel opments of\nextensive air showers near the sea surface\, although the effe cts\naround the shower maximum for most showers may be small.\nIn this pap er\, the pressure dependence of the photon yields in moist air\nwill be re ported and the effects on the energy determination of cosmic rays\nwill be discussed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contrib ution/465 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/465 END:VEVENT BEGIN:VEVENT SUMMARY:Simulations of a particle detector array for the Jicamarca Radio O bservatory to study extended air showers using radar DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-478@cern.ch DESCRIPTION:Speakers: Dr. WAHL\, David (Instituto Geofisico del Peru)\nIt has previously been suggested that the Jicamarca Radio Observatory (JRO) c ould be\nused for the detection of extended air showers using radar echo [ 1]. The use of radar\nis appealing as it could allow to map the longitudin al development of air showers\nthrough the atmosphere. This paper presents studies on the implementation of an array\nof particle detectors (scintil lator\, water tank) at the JRO. The particle detectors\nserve the purpose of providing a known method for the detection of extended air\nshowers aga inst which to compare radar observations. Secondly\, in a scenario where\n extended air showers can be detected by radar\, it will be unfeasible to m aintain the\nradar source continuously active. For this reason\, a particl e trigger which could set\noff the radar pulse to detect the ionisation tr ail would be a necessary addition to\nthe JRO if it is to be used for many hours as a cosmic ray detector. This paper\npresents studies on the desig n of a particle detector array for use as a trigger and\nproviding informa tion on air showers based on simulations.\n\n[1] T. Vinogradova et al. in 1st International Workshop on Radio Detection of High\nEnergy Particles. 2 000. University of California\n\nhttps://indico.nucleares.unam.mx/event/4/ session/39/contribution/478 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/478 END:VEVENT BEGIN:VEVENT SUMMARY:Partial reanimation of experimental complex ANI at Mt. Aragats (pr oposal). DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-483@cern.ch DESCRIPTION:Speakers: Prof. SHAULOV\, Sergey (P.N.Lebedev Physical Institu te\, Moscow\, Russia)\nWe present the proposal for reanimation of the half -built experimental complex \nANI at Mt. Aragats (Armenia\, 3200 m a.s.l.) . It is proposed as a first stage to \ncomplete the functioning GAMMA inst allation by big X-ray emulsion chamber for \ndetailed study of EAS cores a t energies 1-100 PeV. \nPreliminary data obtained in this fieled by the Ti en Shan “Hadron” installation \nare presented. \nThis proposal is an E FT and requests creation of an international cooperation.\n\nhttps://indic o.nucleares.unam.mx/event/4/session/39/contribution/483 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/483 END:VEVENT BEGIN:VEVENT SUMMARY:Balloon-borne measurement of UV nightglow and clouds for the JEM-E USO mission DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-497@cern.ch DESCRIPTION:Speakers: Dr. SAKAKI\, Naoto (Aoyama Gakuin University)\nUltra -high energy cosmic rays (UHECR's) above 100 EeV have been observed with\n several experiments. Their origin and propagation mechanism are still\nin mystery mainly due to the low statistics. In order to observe UHECR's\nwit h sufficient statistics\, the JEM-EUSO experiment is going on.\nIn the JEM -EUSO experiment\, fluorescence and Cherenkov light from the \nextensive a ir showers induced by UHECR's are observed with a telescope\nattached to t he International Space Station. It is important to study\nthe background i ntensity in near UV region (300-400nm)\nseen from the JEM-EUSO telescope.\ nWe launched a balloon at Sanriku Balloon Center of JAXA\nto investigate t he nightglow and the clouds on August 29\, 2005.\nThe upward and downward nightglow was measured through the eight near UV\nfilters and the clouds w ere recorded with infrared thermography.\nIn this paper\, the detail of th e experiment and the results will be reported.\n\nhttps://indico.nucleares .unam.mx/event/4/session/39/contribution/497 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/497 END:VEVENT BEGIN:VEVENT SUMMARY:A GEANT-based package for determination of the PAMIR experiment X- ray emulsion chamber response DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-508@cern.ch DESCRIPTION:Speakers: Prof. MUKHAMEDSHIN\, Rauf (Institute for Nuclear Res earch of Russian Academy of Science)\nAnalysis of various data accumulated in X-ray emulsion chamber experiments\,\nespecially\, data on gamma-ray –hadron families with unusual characteristics\n(Centauros\, aligned even ts etc.)\, requires a comprehensive program to simulate the\npropagation o f electromagnetic and various-type hadron particles through\nsandwich-like media of emulsion chambers as well as measuring procedures used for\nemul sion chamber data processing. Such a new computer code ECSim 2.0 has been\ nrecently elaborated on basis of the GEANT 3.21 package. As compared to th e latter\,\nthe ECSim 2.0 takes into account the LPM effect for gamma-rays and electrons\, uses\nnew cross sections of muon interactions of differen t types allowing also for the LPM\neffect in pair generation\, incorporate s QGSJET model for simulation of high-energy\nhadron interactions and acco unts for production and interactions of charm particles.\nBesides\, measur ing and data treatment procedures employed in the Pamir experiment are\nsi mulated properly. Main features of the ECSim 2.0 code and some results obt ained for\nthe Pamir emulsion chamber experiment are discussed. The ECSim 2.0 can be used widely\nfor data analysis in various X-ray emulsion chambe r experiments.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/cont ribution/508 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/508 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-Ray Astronomy around 100 TeV with a large muon detector oper ated at very high altitude. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-571@cern.ch DESCRIPTION:Speakers: Dr. DI SCIASCIO\, Giuseppe (INFN\, Sez. Napoli\, Ita ly)\nMeasurements at 100 TeV and above are an important goal for the\nnext generation of high energy $\\gamma$-ray astronomy experiments.\nIn fact\, the high energy end of $\\gamma$-ray source spectra might\nprovide clear discrimination between electron and hadron\nprocesses\, thus allowing the identification of cosmic "PeVatrons"\,\nthe sites of Cosmic Rays productio n and acceleration.\n\nThe most natural experimental solution to detect ve ry low\nradiation fluxes is provided by the Extensive Air shower (EAS)\nar rays. They benefit from a close 100$\\%$ duty cycle and a very\nlarge fiel d of view ($\\sim$2 sr). The exposure is large but the\nsensitivity is lim ited by their angular resolution and their poor\ncosmic ray background dis crimination. At energies above 10 TeV the\nstandard technique for rejectin g the hadronic background consists\nin looking for {\\it "muon-poor"} show ers.\n\nIn this paper we discuss the capability of a large muon detector\n ($\\sim$2500 m$^2$) operated with an EAS array at very high\naltitude ($>$ 4000 m a.s.l.) to detect $\\gamma$-ray fluxes around\n100 TeV. Simulation based estimates of energy ranges and\nsensitivities will be presented.\n\n https://indico.nucleares.unam.mx/event/4/session/39/contribution/571 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/571 END:VEVENT BEGIN:VEVENT SUMMARY:Tunka-133 EAS Cherenkov Array: Status of 2007 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-629@cern.ch DESCRIPTION:Speakers: Prof. PROSIN\, Vasily (Scobeltsyn Institut of Nuclea r Physics of MSU\, Moscow\, Russia)\nThe new EAS Cherenkov array Tunka-133 of a sensitive area about 1 km^2 is mounting in \nTunka valley since the end of 2005. The new array will permit a detailed study of cosmic ray \nen ergy spectrum and mass composition in the energy range 10^15 - 10^18 eV wi th the \nunique method. The array will consist of 19 clasters each contain ing 7 optical detectors. The \nfirst claster started operation since Octob er 2006. We discribe the data aqcuisition system \nof the array and presen t the preliminaty results of the test operation.\n\nhttps://indico.nuclear es.unam.mx/event/4/session/39/contribution/629 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/629 END:VEVENT BEGIN:VEVENT SUMMARY:Study of photo-sensor candidates for the MEMSTEL project DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-686@cern.ch DESCRIPTION:Speakers: Dr. LEE\, Moo Hyun (Institute for Physical Science a nd Technology\, University of Maryland)\nThe MEMSTEL (Micro Electro Mechan ical Systems Space Telescope) is a space \nbased experiment being designed to investigate the origin of extreme energy \ncosmic-ray (EECR) particles above 5 x 10^19 eV. The fluorescent light \ngenerated in extensive air sh owers (EAS) when EECRs hit the atmosphere can \nbe detected from low Earth orbit. MEMSTEL will implement a novel idea of a \ntracking mirror based o n semiconductor MEMS technology. The light signal will \nbe focused on a r elatively small area of readout photo-sensors using a tracking \nmirror. O ne candidate for MEMSTEL photo-sensors is the conventional multi-\nanode P MT. Recently\, a new type of photo-sensor was developed for particle \ndet ector readouts - the silicon photo multiplier (Si-PM). This compact photo- \nsensor is comprised of a large array of micro-cells operating in a limit ed Geiger \nmode\, and provides high gain (~10^6) with low operating volta ge (~50 V). The \ncompact design\, light weight and low power consumption make this device an \nexcellent photon-detector candidate for space-based experiments. In this \npaper\, we report on the comparative performance of a 2 x 2 mm^2 Si-PM\, a \nconventional PMT\, and a Hybrid Photo Diode (HPD ) in lab tests\, reading out light \ngenerated by Light Emitting Diodes (L ED) as well as by scintillating fibers \nexcited with a radioactive source .\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/686 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/686 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic-Ray Events as Background in Imaging Atmospheric Cherenkov T elescopes DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-704@cern.ch DESCRIPTION:Speakers: Dr. MAIER\, Gernot (McGill University\, Montreal)\nT he dominant background for observations of gamma-rays in the energy region above 50\nGeV with Imaging Atmospheric Cherenkov telescopes are cosmic- ray events. The images\nof most of the cosmic ray showers look significant ly different from those of\ngamma-rays and are therefore easily discrimina ted. However\, a small fraction of\nevents seems to be indistinguishable from gamma-rays. This constitutes an\nirreducible background to the obser vation of high-energy gamma-ray sources\, and\nlimits the sensitivity achi evable with a given instrument. Here\, a Monte Carlo study\nof gamma-like cosmic-ray events is presented. The nature of gamma-like cosmic-ray\neve nts\, the shower particles that are responsible for the gamma-like appeara nce\, and\nthe dependence of these results on the choice of the hadronic i nteraction model are\ninvestigated. Most of the gamma-like cosmic ray eve nts are characterised by the\nproduction of high-energy pi0 early in the shower development which dump most of the\nshower energy into electromagne tic sub-showers. Also Cherenkov light from single\nmuons can mimic gamma- rays in close-by pairs of telescopes. Differences of up to 25%\nin the col lection area for gamma-like proton showers between QGSJet/FLUKA and\nSiby ll/FLUKA simulations have been found.\n\nhttps://indico.nucleares.unam.mx/ event/4/session/39/contribution/704 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/704 END:VEVENT BEGIN:VEVENT SUMMARY:Spectral resolved Measurement of the Nitrogen Fluorescence Emissio ns in Air induced by Electrons DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-713@cern.ch DESCRIPTION:Speakers: Dr. WALDENMAIER\, Tilo (University of Delaware\, Dep artment of Physics and Astronomy)\nFor the calorimetric determination of t he primary energy of extensive air showers\,\nmeasured by fluorescence tel escopes\, a precise knowledge of the conversion factor\n(fluorescence yiel d) between the deposited energy in the atmosphere and the number of\nemitt ed fluorescence photons is essential. The fluorescence yield of the eight\ nstrongest nitrogen emission bands between 300 nm and 400 nm has been meas ured by the\nAirLight Experiment at Forschungszentrum Karlsruhe using elec trons from a Sr-90\nsource with energies between 250 keV to 2 MeV. Measure ments have been performed in\ndry air\, pure nitrogen\, and a nitrogen-oxy gen mixture at pressures ranging from 2 hPa\nto 990 hPa. Furthermore the i nfluence of water vapor has been studied. The resulting\nabsolute accuraci es for the single nitrogen bands are in the order of 15 %. In the\ninvesti gated energy range\, the fluorescence yield proved to be independent of th e\nenergy of the ionizing electrons.\n\nhttps://indico.nucleares.unam.mx/e vent/4/session/39/contribution/713 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/713 END:VEVENT BEGIN:VEVENT SUMMARY:Online monitoring for the fluorescence telescopes of the Pierre Au ger Observatory DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-717@cern.ch DESCRIPTION:Speakers: Prof. KAMPERT\, Karl-Heinz (Universität Wuppertal)\ nA new tool monitoring the status of the fluorescence telescopes has been\ ndeveloped to guarantee smooth operation of all detector components during \ndata taking. Monitoring data from FD telescopes are collected online\nre gularly during data acquisition as well as in dedicated modes such as\ncal ibration. They are stored locally in databases that are replicated on a\nd edicated central server. A web interface implemented on a this server can\ ndynamically generate graphs and specialised visualisations\, which are\na ccessible locally for the shift crew as well as remotely from anywhere in\ nthe world. An alarm warning is triggered automatically in case of\npredef ined conditions which require immediate action. This tool also\nprovides t he ability to monitor the long term stability of key quantities\nand data quality. The concept and its implementation are presented.\n\nhttps://indi co.nucleares.unam.mx/event/4/session/39/contribution/717 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/717 END:VEVENT BEGIN:VEVENT SUMMARY:A programmable hardware module for precise absolute time event gen eration and capture DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-733@cern.ch DESCRIPTION:Speakers: Mr. SMITH\, Jeremy (university of Utah)\, Mr. THOMAS \, Jason (University of Utah)\, Mr. THOMAS\, Stan (University of Utah)\, P rof. WIENCKE\, Lawrence (university of Utah)\nWe have designed and built a programmable hardware module for TTL pulse\ngeneration and capture in abs olute time. The time reference is an on-board GPS\n(Global Positioning Sy stem) receiver. Tests of a prototype performed at the US\nNational Institu te of Standards (NIST) found a nominal accuracy better than 20 ns\nrelativ e to the secondary US frequency standard. Potential applications for this \ndevice are numerous and include triggering calibration sources and laser s at\nspecific times for calibration of cosmic-ray observatories. The hard ware is\nconfigured in a standard PC104 layout for use with embedded syste ms. A Linux\nsoftware device driver interface featuring an extensive set of user commands was\nalso developed.\n\nhttps://indico.nucleares.unam.mx/ event/4/session/39/contribution/733 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/733 END:VEVENT BEGIN:VEVENT SUMMARY:Characteristics and Performances of the electronics for the fluore scence detectors of the Telescope Array experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-790@cern.ch DESCRIPTION:Speakers: Dr. TOKUNO\, Hisao (Institute for Cosmic Ray Researc h\, The University of Tokyo)\nThe three stations of the Telescope Array fl uorescence detectors (FDs)\ncontain 12 telescopes each\, and each of the t elescopes has a 256 pixel\nPMT camera with a field of view of 18 degree x 16 degrees.\nThe fluorescence signals of each pixel are digitized with the ir\nwaveforms by the Signal Digitizer/Finder modules (SDFs). The signal\na lerts from the SDFs are send to the Track Finder modules (TF) to\ngenerate first trigger signals for air shower events. When a shower\ntrack image i s found in one camera\, the Central Trigger Distributor\n(CTD) module send s the final trigger signal to all the telescopes to\nstore their data. Her e we will describe the characteristic features\nand performances of the el ectronics\, which are developed and measured\nthrough laboratory tests and actual fluorescence light measurements.\n\nhttps://indico.nucleares.unam. mx/event/4/session/39/contribution/790 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/790 END:VEVENT BEGIN:VEVENT SUMMARY:Calibration and monitoring of the air fluorescence detector for th e Telescope Array experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-792@cern.ch DESCRIPTION:Speakers: Dr. TOKUNO\, Hisao (Institute for Cosmic Ray Researc h\, The University of Tokyo)\nThe air fluorescence detectors (FDs) of the Telescope Array (TA) \nexperiment have been constructed in a dessert of Ut ah\, USA. \nWe can measure the longitudinal developments of EASs directly \nwith the FDs by detecting air fluorescence lights and determine\n the pr imary energies of ultra-high energy cosmic rays. \nIn order for accurate o bservation and measurements of EASs\, \nelaborate detector calibrations an d monitoring systems are required. \nWe will present the result of calibra tion and monitoring systems \nfor the reflectance and curvature radius of segment mirrors\, \nthe characteristics of PMT (absolute gain\, linearity\ , \ntemperature dependence of gain)\, and the uniformity of the \ncamera s urface\, etc.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contr ibution/792 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/792 END:VEVENT BEGIN:VEVENT SUMMARY:Data acquisition system of air fluorescence detectors for the Tele scope Array experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-795@cern.ch DESCRIPTION:Speakers: Dr. TOKUNO\, Hisao (Institute for Cosmic Ray Researc h\, The University of Tokyo)\nThe construction of the fluorescence detecto rs (FDs) of the \nTelescope Array (TA) experiment will be completed in Jun e 2007\, \nand the first observation with the full configuration is planne d \nin summer in this year. In this paper\, we describe the development \n of the data acquisition (DAQ) system for the TA FD observations. \nThe DAQ system of each TA FD station is comprised of 16 CPUs: \n13 for controls o f the FD front-end electronics and 1 for data \nstorage and 1 for environm ent monitoring\, and 1 for the central \ncontrol of the whole system. We e mploy the Network Shared Memory \nsystem (NSM) for communication of the CP Us. We will present the \ndetail of the system and the performance in the test observations \nand the first science run.\n\nhttps://indico.nucleares .unam.mx/event/4/session/39/contribution/795 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/795 END:VEVENT BEGIN:VEVENT SUMMARY:The Central Laser Facility at the Telescope Array DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-800@cern.ch DESCRIPTION:Speakers: Dr. UDO\, shigeharu (icrr\, university of tokyo)\nAt mospheric monitoring is indispensable to calibrate the\nreconstruction of extensive air shower that observed by air\nfluorescence telescope. The Te lescope Array (TA) experiment is using\nan air fluorescence technique alon g with a shower array system to\nobserve the ultra-high energy cosmic ray. And we adopted two laser\nsystems measuring the atmospheric transmittanc e to calibrate the\nFluorescence Detector (FD) of TA. One is a LIDAR syst em which will be\nreported other-where in this conference and another is a Central Laser\nFacility (CLF). The CLF located near the middle of three FD stations\nis equipped with a UV (355nm) laser and optical components th at direct\na calibrated pulsed beam into the sky. The scattering light fr om this\nbeam observed by FDs becomes a good calibration source of total\n attenuation caused by atmosphere between CLF and FDs. We will\ndescribe t he TA-CLF system along with some measurements briefly.\n\nhttps://indico.n ucleares.unam.mx/event/4/session/39/contribution/800 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/800 END:VEVENT BEGIN:VEVENT SUMMARY:Atmospheric Monitoring with LIDAR and Infra-red Camera at Black Ro ck Mesa in the Utah desert DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-803@cern.ch DESCRIPTION:Speakers: Prof. CHIKAWA\, Michiyuki (Kinki University)\nAn atm ospheric monitoring system has installed at Black Rock Mesa in the Utah\nd esert to study the properties of atmosphere using a LIDAR(Light Detection And\nRanging) system and an infra-red(IR) camera for cosmic rays experimen t. The aims of\natmospheric monitoring are to calibrate observed cosmic ra y's energy and to determine\ndetectable region of the fluorescence detecto rs. For these reasons\, the atmospheric\nextinction coefficient and the c loudiness should be determined precisely as possible. \n The LIDAR system consisits of a laser device and a light receiver with a photo\nmultiplier tube(PMT) mounting on a steerable base. The laser emits pulse lights\nsuc cessively into the atmoshere and the receiver detects scattered faint ligh ts by\nthe PMT. To determine the atmospheric extinction coefficient\, a la rge amount of data\nhas been\nacquired using LIDAR system at Black Rock Me sa commencing from July 2005.A lot of\ndata is analized by means of so-cal led the slope method and/or the Klett's method\nafter due consideration of atmospheric pressure effect. \nA result consistent with a calculation of the Rayleigh scattering is obtained for the\nvertical extinction coefficie nt above an altitude of several kilometres in a calm\nweather. It is also found that the one-dimentional atmospheric density model is\nreasonable as sumption on a limitative condition in the Utah desert. \n The current res ults from the atmospheric monitoring with the LIDAR and the IR\ncamera wil l be presented in full detail.\n\nhttps://indico.nucleares.unam.mx/event/4 /session/39/contribution/803 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/803 END:VEVENT BEGIN:VEVENT SUMMARY:Prompt Muons in Extended Air Showers DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-812@cern.ch DESCRIPTION:Speakers: Dr. RIDKY\, Jan (Institute of Physics Prague)\nWe pr esent results of simulations of muon content in the air showers induced \n by very high energy cosmic rays. Muon energy distributions and muon densit ies \nat ground level are given. We discuss a prompt muon component genera ted by \ndecays of charmed mesons. The method combines standard Monte Carl o \ngenerators incorporated in the CORSIKA code and phenomenological estim ates \nof charm hadroproduction.\n\nhttps://indico.nucleares.unam.mx/event /4/session/39/contribution/812 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/812 END:VEVENT BEGIN:VEVENT SUMMARY:Simulation of Horizontal Air shower DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-815@cern.ch DESCRIPTION:Speakers: Dr. LIU\, TsungChe (Institute of Physics\,National C hiao Tung University)\nEarth-skimming neutrino experiment such as NuTel or CRTNT detects air \nshower\, which is produced by decay of tau lepton\, f rom near horizontal \ndirection. Traditional shower simulations have diffi culty in simulating shower at \nzenith angle near 90 degree\, where some v ariables diverge to infinity. Recent \nCORSIKA simulation code had update s on simulation of horizontal air shower. \nWe also developed a method to simulate horizontal air shower. This talk will \ncompare results from both methods.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribut ion/815 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/815 END:VEVENT BEGIN:VEVENT SUMMARY:Advancement of the wide-angle JEM-EUSO optical system with hologra phic and Fresnel lenses DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-823@cern.ch DESCRIPTION:Speakers: TAKIZAWA\, Yoshiyuki (RIKEN\, Japan)\nExtreme Univer se Space Observatory on JEM/EF (JEM-EUSO) is a space mission to observe ex tremely high-energy \ncosmic rays. JEM-EUSO is a wide-angle refractive tel escope in near-ultraviolet wavelength region to observe time-\nresolved at mospheric fluorescence images of the extensive air showers from the Intern ational Space Station. \nThis paper will discuss the optical system of JEM -EUSO. We will report on an optimized optics design that maximizes \nthe s ensitivity of JEM-EUSO. We will describe this design and report on the res ults of optics manufacturing tests.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/39/contribution/823 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/823 END:VEVENT BEGIN:VEVENT SUMMARY:The Focal Surface of the JEM-EUSO Telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-824@cern.ch DESCRIPTION:Speakers: Dr. KAWASAKI\, Yoshiya (RIKEN)\nThe Extreme Universe Space Observatory on JEM/EF (JEM-EUSO) is a space mission to study extrem ely high-energy \ncosmic rays. The JEM-EUSO instrument is a wide-angle ref ractive telescope in near-ultraviolet wavelength region to \nobserve time- resolved atmospheric fluorescence images of the extensive air showers from the International Space \nStation. The focal surface is a spherical curve d surface\, and its area amounts to about 4.5 m2. The focal surface \ndete ctor is covered with about 6\,000 multi-anode photomultipliers (MAPMTs). T he focal surface detector consists of \nPhoto-Detector-Modules\, each of w hich consists of 9 Elementary Cells (ECs). The EC contains 4 units of the \nMAPMTs. Therefore\, about 1\,500 ECs or about 160 PDMS are arranged on t he whole of the focal surface of JEM-\nEUSO. The EC is a basic unit of the front-end electronics. The PDM is a basic unit of the data acquisition sy stem.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/ 824 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/824 END:VEVENT BEGIN:VEVENT SUMMARY:Thermal neutrons in EAS: a new method of EAS study DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-827@cern.ch DESCRIPTION:Speakers: Dr. STENKIN\, Yuri (Institute for Nuclear Research o f RAS)\nIt is shown that recording of thermal neutrons accompanying the EA S with\nspecific scintillator detectors for thermal neutron detection\ngiv es a new and very interesting additional information.\nResults of CORSIKA based Monte Carlo simulations as well as preliminary\nexperimental data ar e presented. A new method to study Extensive Air \nShowers is proposed.\n\ nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/827 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/827 END:VEVENT BEGIN:VEVENT SUMMARY:The trigger system of the JEM-EUSO Project DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-838@cern.ch DESCRIPTION:Speakers: Dr. BERTAINA\, Mario (Torino University)\nThe trigge r system of JEM-EUSO should face\ndifferent major challenging points: a) c ope with the limited down-link\ntransmission rate from the ISS to Earth\, by operating a severe on-board\nand on-time data reduction\; b) use very f ast\, low power consuming and radiation\nhard electronics\; c) have a high signal-over-noise performance and flexibility\nin order to lower as much as possible the energy threshold of the\ndetector\, adjust the system to a variable nightglow background\, and trigger on\ndifferent categories of e vents (images insisting on the same pixels or crossing\nhuge portions of t he entire focal surface). Based on the above stringent\nrequirements\, the main ingredients for the trigger logic are: the Gate Time\nUnit (GTU)\; t he minimum number Nthresh of photo-electrons\npiling up in a GTU in a pixe l to be fired\; the persistency level Npers\, in\nwhich fired pixels are o ver threshold\; the localization and correlation in\nspace and time of the fired pixels\, that distinguish a real EAS from an\naccidental background enhancement. The core of the trigger logic is the\nTrack Trigger Algorith m that has been specifically developed for this purpose. \nIts characteris tics\, preliminary performance and its possible implementation\non FPGA or DSP will be discussed together with a general overview of the\narchitectu re of the triggering system of JEM-EUSO.\n\nhttps://indico.nucleares.unam. mx/event/4/session/39/contribution/838 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/838 END:VEVENT BEGIN:VEVENT SUMMARY:Atmospheric Monitoring System of the JEM-EUSO Mission DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-846@cern.ch DESCRIPTION:Speakers: Dr. MITEV\, Valentin (Observatory of Neuchâtel\, S witzerland)\, Dr. SATO\, Mitsuteru (RIKEN\, Japan)\nJEM-EUSO will study ul tra-high-energy cosmic rays by their optical yield in the \natmosphere. To evaluate this yield it is important to monitor the atmosphere \ninside th e field-of-view (FOV) of the JEM-EUSO receiver. This monitoring shall \npe rmit the correction of the JEM-EUSO signal\, where the critical parameters are \nthe cloud presence and top altitude. The Atmospheric Monitoring Sys tem will be \nbased on a complex of sensors: infrared (IR) camera\, Lidar\ , and JEM-\nEUSO "slow-data". The IR camera consists of Ge dioptric lenses \, a band-pass \nfilter and an un-cooled micro-bolometer array. It will ac quire images of the cloud \ntop temperature covering the JEM-EUSO FOV. The cloud-top altitude will be \nevaluated from the temperature with relative ly low precision. High-precision \n(30m) Lidar cloud-top altitude measurem ents will be used to correct the cloud-\ntop altitude from the IR-camera. The Lidar will use laser at 355nm transmitted in \nthree fixed directions\ , as well as the JEM-EUSO receiver with \nthree dedicated detector. The op tical background signal in the UV\, detected by \nJEM-EUSO will allow imag ing of the cloud field inside its FOV (the JEM-\nEUSO "slow-data" operatio n). The "stereoscope" processing of this image will \nprovide additional l ow-resolution evaluation of the cloud top altitude.\n\nhttps://indico.nucl eares.unam.mx/event/4/session/39/contribution/846 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/846 END:VEVENT BEGIN:VEVENT SUMMARY:A GRID approach to ARGO-YBJ experiment data transfer and processin g. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-887@cern.ch DESCRIPTION:Speakers: STANESCU\, Cristian (INFN Roma Tre)\nSome aspects of the cosmic ray astronomy require the access and the \nprocessing of the d ata in the shortest possible time. We implemented a data \nfiles moving sy stem \, based on GRID tools and services\, to automatically \ntransfer the files from the high altitude ARGO-Yangbajing Laboratory in Tibet to \nthe Storage Elements at the processing sites in IHEP-Beijing (China) and CNAF -\nBologna (Italy). We describe also the GRID approach to an unified job \ nsubmission and proccessing system and the mirroring of the ARGO data file s \ncatalogs. This new approach allows our communities to cooperate more \ nefficiently in data analysis\, in sharing the available resources\, reali zing at the \nsame time the backup of the data.\n\nhttps://indico.nucleare s.unam.mx/event/4/session/39/contribution/887 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/887 END:VEVENT BEGIN:VEVENT SUMMARY:Nuclear Cosmic Ray Propagation in the Atmosphere between 10GeV and 10TeV per nucleon DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-888@cern.ch DESCRIPTION:Speakers: Dr. DEROME\, Laurent (LPSC/IN2P3/CNRS)\nThe future h igh energy nuclear cosmic ray flux measurements in the upper atmosphere\nw ill require large\, and thus accurate\, corrections for reliable Top of At mosphere\n(galactic) fluxes to be derived. In this perspective\, the atmos pheric corrections are\nevaluated from the transport calculations of the f lux in the atmosphere. The\ncontributions of these corrections to the accu racy of the experimental results are\ndiscussed for the B/C and subFe/Fe e lements ratios\, over the kinetic energy range 10\n- 10**4 GeV/n. These co ntributions become largely dominant at the highest energies\ninvestigated. The results and the prospects for the galactic flux measurements will\nbe discussed in the presentation.\n\nhttps://indico.nucleares.unam.mx/event/ 4/session/39/contribution/888 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/888 END:VEVENT BEGIN:VEVENT SUMMARY:REAS2: CORSIKA-based Monte Carlo simulations of geosynchrotron rad io emission DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-891@cern.ch DESCRIPTION:Speakers: Dr. HUEGE\, Tim (Forschungszentrum Karlsruhe)\nSimul ations of geosynchrotron radio emission from extensive air showers \nperfo rmed with the Monte Carlo code REAS1 used analytical parameterisations \nt o describe the spatial\, temporal\, energy and angular particle distributi ons \nin air showers. The successor REAS2 replaces these parameterisations with \nprecise\, multi-dimensional histograms derived from per-shower COR SIKA \nsimulations. REAS2 allows an independent selection between paramete risation \nand histogram for each of the relevant particle distributions\, enabling us to \nstudy the changes arising from using a more realistic ai r shower model in \ndetail. We describe the new simulation strategy and il lustrate the effects \nintroduced by the improved air shower model.\n\nhtt ps://indico.nucleares.unam.mx/event/4/session/39/contribution/891 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/891 END:VEVENT BEGIN:VEVENT SUMMARY:A Wide Angle Air Cherenkov Imaging Telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-895@cern.ch DESCRIPTION:Speakers: Dr. MIRZOYAN\, Razmick (Max-Planck-Institute for Phy sics)\nThe existing imaging air Cherenkov Telescopes (IACT) are using \nim aging cameras of aperture 2-4 degrees. These telescopes\nhave F/0.7 to F/1 .2 optics. The best optical resolution that one\ncan obtain with these opt ical designs is in the range of 3 minutes \nof arc\, and that only in the central region of the imaging camera. \nThere are indications from simulat ions that one can further improve \nthe sensitivity of the IACTs (the back ground rejection) if one could \nprovide an improved optical resolution of about 1 minute of arc. \nThe usual prime focus telescopes will need an op tical design of\nF/3 or even slower optics for achieving about 1 minute of arc resolution. \nIn this report we want to show an optical design of a t elescope can \noffer (12-20) degree wide field of view (FoV) and an optica l \nresolution of one minute of arc everywhere in the field of view. \nThe advantages and the drawbacks of the wide FoV telescopes will\nbe discusse d.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/895 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/895 END:VEVENT BEGIN:VEVENT SUMMARY:Status and performance of the ARGO-YBJ trigger system. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-900@cern.ch DESCRIPTION:Speakers: STANESCU\, Cristian (INFN Roma Tre)\nThe ARGO-YBJ gr ound-based detector allows to investigate many issues in \ngamma-ray astro nomy and cosmic ray physics spanning a large energy range \nby means of it s ability to operate down to a few hundreds of GeV up to a few \nPeV. The apparatus consists of a single layer of about 2000 Resistive Plate \nChamb ers (RPCs) for a total instrumented area of ~6700 m2. The whole \ndetector has been fully equiped with final front-end\, trigger and DAQ electronics \nand is in data taking since last February. The detection of small size showers is \none of main tasks of the ARGO-YBJ experiment. The maximum tri gger rate due \nto cosmic rays that the system can acquire is 15 KHz with a data transfer rate \nof about 16 MB/s. In this paper the design and perf ormance of the trigger \nsystem will be described.\n\nhttps://indico.nucle ares.unam.mx/event/4/session/39/contribution/900 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/900 END:VEVENT BEGIN:VEVENT SUMMARY:A Linear Accelerator for TA-FD calibration DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-903@cern.ch DESCRIPTION:Speakers: SHIBATA\, Tatsunobu (Institute for Cosmic Ray Resear ch\, University of Tokyo)\nThe energy of the primary cosmic ray can be cal culated from fluorescence\nphotons detected by fluorescence telescope. How ever\, since we can not know\nthe true energy of primary cosmic ray\, it i s difficult to calibrate between\nnumber of photons and energy directly. I n TA project\, we will create pseudo-\ncosmic ray events by using accelera ted electron beam which is injected in\nthe air. The injected electron bea m creates an air shower and fluorescence\nphotons are emitted. We can cali bate between electron beam energy which is\nknown exactry and detected pho tons. We are developping a small linear\naccelerator (Linac) at High Ener gy Accelerator Research Organization (KEK)\nin Japan. The maximum energy i s 40MeV\, the typical current is 0.16nC\, and\nthe intensity per pulse is 6.4mJ. The accuracy of beam energy is less than\n1%. The Linac consists of a -100kV pulse type electron gun\, a 1.5m pre-buncher\nand buncher tube\, a 2m S-band accelerator tube\, a quadrupole magnet\, a 90\ndegree bending magnet\, and a S-Band(2856MHz) 50MW high power klystron as \nRF source. W e chekced the performance of the electron beam\, energy \nresolution\, bea m spread\, beam current\, and beam loss by PARMELA simulation\, \nand chec ked the air shower by electron beam and number of the detected \nphotons b y detector simulation which are made by GEANT4. In this Spring\, we \nwill do the full beam test in KEK. The beam operation in Utah will be started \nfrom this Autumn. In this talk\, we will report about the results of the beam test \nand calibration method by this Linac.\n\nhttps://indico.nucle ares.unam.mx/event/4/session/39/contribution/903 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/903 END:VEVENT BEGIN:VEVENT SUMMARY:The architecture of DAQ system for the ARGO-YBJ experiment. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-910@cern.ch DESCRIPTION:Speakers: STANESCU\, Cristian (INFN Roma Tre)\nThe ARGO-YBJ ex periment has now reached its final design configuration. The \ndetector sy stem consists of a full coverage array ( about 5800 m2) of Resistive \nPla te Chambers (RPCs). At the nominal threshold the system must be able to \n sustain a maximum transfer rate of the order of 15 MB/s and an high peak d ata \nflow. Data are read out using a typical front-end acquisition chain built around a \ncustom bus. Specialized electronics have been designed an d efficient software \nhas been written to perform this task. In this pape r we described the \narchitecture of the DAQ system of the ARGO-YBJ experi ment and its \nperformances.\n\nhttps://indico.nucleares.unam.mx/event/4/s ession/39/contribution/910 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/910 END:VEVENT BEGIN:VEVENT SUMMARY:The Front-End Cards of the Pierre Auger Surface Detectors: Test Re sults and Performance in the Field DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-935@cern.ch DESCRIPTION:Speakers: KAMPERT\, Karl-Heinz (Bergische Universitaet Wuppert al)\nThe Pierre Auger Observatory\, presently under construction in Argent ina\, is nearing\ncompletion. The instrument is designed to\nmeasure the h ighest energy cosmic rays with unprecedented resolution and statistics.\nI ts surface array comprises 1600 water\nCherenkov detectors distributed ove r an area of 3000 km2. The Cherenkov light of each\ntank is detected by th ree 9-inch\nphotomultipliers from which the signals of the anode and last dynode are digitized\neach by 10 bit 40 MHz FADCs. An Altera\nCyclone FPGA is employed to generate different local triggers and to handle the data\n transfer to a communication board. The\nlow-power budget\, large environme ntal temperature variations\, and the long-term\noperation impose special constraints to the\nFront-End cards. After discussing the design of the ca rds we present an automized\ntest-bench including a climate chamber which\ nhas been set up in order to test the large number of boards prior to inst allation in\nthe field. The qualification procedure and\nthe results obtai ned in the laboratory are presented. Data collected during operation\nin t he field demonstrate a very good\nperformance and reliability of the Front -End cards.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contrib ution/935 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/935 END:VEVENT BEGIN:VEVENT SUMMARY:TUS space detector as a pathfinder for the next generation space d etectors DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-948@cern.ch DESCRIPTION:Speakers: Prof. KAJINO\, Fumiyoshi (Konan University)\nSpace d etectors of UV fluorescence and Cherenkov light radiated by ultra high \ne nergy extensive air showers (UHECR EAS) have advantages of high EAS \ndete ction aperture in observing the whole sky by one instrument and will be \n able to get statistically rich results on the UHECR arriving directions.\n At the same time the space environment and particularly variable UV \nback ground intensity put some restrictions to EAS measurements from the \nsate llites. Before making and launching the full scale fluorescence detectors like \nJEM-EUSO and TUS-M for UHECR measurements the TUS detector comprisi ng \nthe main parts of photo receivers of JEM-EUSO and TUS-M is planned to be \nlaunched in 2009-2010. Results of the TUS detector will help to make final \ndesign of the next generation of space UHECR detectors.\n\nhttps: //indico.nucleares.unam.mx/event/4/session/39/contribution/948 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/948 END:VEVENT BEGIN:VEVENT SUMMARY:Operation of LOPES-30 for Polarization Measurements of the Radio Emission of Cosmic Ray Air Showers DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-961@cern.ch DESCRIPTION:Speakers: Mr. NEHLS\, Steffen (Forschungszentrum Karlsruhe)\nT he LOPES-30 experiment\, located with the air shower experiment\nKASCADE-G rande at Forschungszentrum Karlsruhe\, Germany\, is an array of 30\ndipole antennas set-up to investigate the pulsed radio emission from\ncosmic ray air showers in the Earth's atmosphere. After one year of\nmeasurements of the East-West polarization by all 30 antennas\, recently\,\nthe LOPES-30 set-up was reconfigured to perform dual-polarization\nmeasurements. Half o f the antennas have been configured for measurements\nof the North-South p olarization direction. Only by measuring at the\nsame time both\, the E-W and N-S polarization components of the radio\nemission\, the geosynchrotro n effect as the dominant emission mechanism in air\nshowers can be verifie d. The status of the measurements\, including the\nabsolute calibration of the antennas\, the monitoring of the environmental\nconditions and a prel iminary analysis of the dual-polarized events are\nreported.\n\nhttps://in dico.nucleares.unam.mx/event/4/session/39/contribution/961 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/961 END:VEVENT BEGIN:VEVENT SUMMARY:Calculation of radio emission from high energy air showers DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-969@cern.ch DESCRIPTION:Speakers: Dr. ENGEL\, Ralph (Forschungszentrum Karlsruhe\, Kar lsruhe Institute of Technology\, 76021 Karlsruhe)\nFor a long time radio e mission accompanying extensive air showers (EAS) is considered\nas an alte rnative to traditional methods of high energy cosmic ray detection (> 10^1 7\neV). In this paper\, results of simulations of radio signals from air s howers with\nenergy greater than 10^17 eV are reported. The simulations ar e based on a\ntrack-by-track radio emission calculation using the EGSnrc M onte Carlo shower code.\nThe lateral distribution of the predicted radio e mission pattern is compatible with\nthe recent LOPES-10 experimental data at distances < 300 m. Perspectives of extending\nthe EAS radio emission ca lculation to ultra-high energy (up to 10^20 eV) are also\ndiscussed.\n\nht tps://indico.nucleares.unam.mx/event/4/session/39/contribution/969 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/969 END:VEVENT BEGIN:VEVENT SUMMARY:The performance of the LHCf detectors DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-981@cern.ch DESCRIPTION:Speakers: Mr. MENJO\, Hiroaki (Nagoya University\, Japan)\nThe LHCf is an early time physics experiment of the CERN Large Hadron Collide r. The\nLHCf will provide an indispensable data on the energy and transver se momentum spectra\nof neutral particles in the very forward region at 1x 10^17eV. The LHCf apparatus is\ncomposed of two independent detectors inst alled +/- 140m and at zero degree collision\nangle from the ATLAS interact ion point. Each detector has two sampling calorimeters\nwhich are composed of 44 radiation lengths of tungsten plates\, 16 layers of plastic\nscinti llators and 4 layers of position sensitive detectors ( scintillating fiber s for\nArm#1\, silicon tracker for Arm#2). The calibrations for all compon ents (all plastic\nscintillators\, PMTs\, scintillating fibers\, and MAPMT s) have been finished. The Arm#1\ndetector was fully assembled in July 200 6\, while the Arm#2 detector was pre-assembled\nin September 2006 and will be finally assembled in April 2007. The beam test for\noverall calibratio n was carried out at a CERN SPS in August 2006. A final beam test\nwill be made in September 2007. In this poster\, we report the performances of t he\ndetectors.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/cont ribution/981 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/981 END:VEVENT BEGIN:VEVENT SUMMARY:Astrophysics Motivation behind the Pierre Auger Southern Observato ry Enhancements DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-991@cern.ch DESCRIPTION:Speakers: Dr. MEDINA TANCO\, Gustavo (ICN-UNAM)\nThe Pierre Au ger Collaboration intends to extend the energy range of its southern\nobse rvatory in Argentina for high quality data from 0.1 to 3 EeV. The extensio ns\nproposed and described in accompanying papers\, include three addition al fluorescence\ntelescopes with a more elevated field of view (HEAT) and a nested surface array with\n750 and 433 m spacing respectively and additi onal muon detection capabilities\n(AMIGA). The enhancement of the detector will allow measurement of cosmic rays\, using\nthe same techniques\, from below the second knee up to the highest energies observed.\nThe evolution of the spectrum through the second knee and ankle\, and corresponding\npr edicted changes in composition\, are crucial to the understanding the end of\nGalactic confinement and the effects of propagation on the lower energ y portion of\nthe extragalactic flux. The latter is strongly related to th e cosmological\ndistribution of sources and to the composition of the inje cted spectrum. We discuss\nthe science motivation behind these enhancement s as well as the impact of combined\nHEAT and AMIGA information on the ass essment of shower simulations and reconstruction\ntechniques.\n\nhttps://i ndico.nucleares.unam.mx/event/4/session/39/contribution/991 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/991 END:VEVENT BEGIN:VEVENT SUMMARY:First generation Moon based CR experiments DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1011@cern.ch DESCRIPTION:Speakers: Prof. SPILLANTINI\, Piero (INFN and University\, Fir enze\, Italy)\nThe Moon based observation of cosmic rays must be part of t he complete \nprogram at the forefront of the space science and technology of the set of Moon \nbased observatories that will operate on the Moon in the next few decades. \nWhen compared with the cost of a dedicated vehicl e and its launch\, the \ninstallation of CR experiments on the Moon\, in a suitable equipped location\, \ncompensates for the cost of the Earth to M oon transportation. It will be \ndiscussed what could be obtained by insta lling on the Moon the experiments \nselected in the last two decades but n ever flown because of the shortage of \nflight occasions and of spacecraft s. Their evolution could constitute the ‘first \ngeneration Moon based C R experiments’. Examples of these experiments and \ntheir possible adapt ation to the Moon location are given for several important \nthematic of t he CR research\, such as the measurement of the flux of very high Z \nCR\, of a large number of isotopes and of rare CR components\, the hunt for \n antinuclei and the chemical composition at knee.\n\nhttps://indico.nuclear es.unam.mx/event/4/session/39/contribution/1011 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1011 END:VEVENT BEGIN:VEVENT SUMMARY:Data Acquisition System of Surface Detector Array of the Telescope Array experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1028@cern.ch DESCRIPTION:Speakers: Dr. OZAWA\, SHUNSUKE (ICRR\, University of Tokyo)\nT he Telescope Array(TA) experiment will investigate the origin of the ultra high\nenergy cosmic rays (UHECRs).\nThis experiment is a hybrid observatio n of an air shower array and fluorescence\ntelescopes installed in Utah\, USA.\nWe finised deploying about 500 Surface Detectors(SDs) for AS array t o our site in\nwinter of 2006-2007\,\nand start SD operation from April 20 07.\nEffective area of this array is 760km^2\, each detector set up at int ervals of 1.2km and\nhas 2 layers of 3m^2\, 1.2cm thick scintilator. Its e nergy threshold for air shower\nevent is 10^19eV or more.\nThe detector ha s the power supply to operate electronics and them for the data\ncollectio n respectively.\nThe data from detectors are transmited to a trigger cente r by wireless LAN modem. \nWe develop a data acquisition system for SDs on this wireless communication.\nIn this presentation\, we will report about the data acquisition system of SD array.\n\nhttps://indico.nucleares.unam .mx/event/4/session/39/contribution/1028 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1028 END:VEVENT BEGIN:VEVENT SUMMARY:A LED Flasher for TUNKA EAS experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1056@cern.ch DESCRIPTION:Speakers: Mr. SHAIBONOV\, Bator (Institute for Nuclear Researc h RAS)\nA LED flasher has been developed for TUNKA-133 EAS Cherenkov detec tor. Blue \nultra bright InGaN LED is used as a light source in the flashe r. The flasher's \ndriver based on a complementary pair of fast RF transis tors. The light yield of \nthe flasher is adjusted in a wide range from 0 to upt to 10**9 photons per \npulse. The results of studies of the flasher 's amplitude and timing parameters \nand their stabilities are presented.\ n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/1056 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1056 END:VEVENT BEGIN:VEVENT SUMMARY:Getting rid of artificial fluctuations in EAS simulated with thinn ing: estimate of artificial fluctuations and simple economical method to s uppress them DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1075@cern.ch DESCRIPTION:Speakers: Mr. RUBTSOV\, Grigory (Institute for Nuclear Researc h of the Russian Academy of Sciences)\nThe most common way to simplify ext ensive Monte-Carlo simulations of air showers is\nthe thinning approximati on. We study its effect on the physical parameters\nreconstructed from sim ulated showers. To this end\, we created a library of showers\nsimulated w ithout thinning with energies from $10^{17}$~eV to $10^{18}$~eV\, differen t\nzenith angles and primaries. This library is publicly available. Variou s physically\ninteresting applications of the showers simulated without th inning are discussed. \nObservables reconstructed from these showers are c ompared to those obtained with the\nthinning approximation. The amount of artificial fluctuations introduced by thinning\nis estimated. A simple me thod\, multisampling\, is suggested which results\nincontrollable suppress ion of artificial fluctuation and simultaneously conserves\ncomputational resources as compared to the usual thinning.\n\nhttps://indico.nucleares.u nam.mx/event/4/session/39/contribution/1075 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1075 END:VEVENT BEGIN:VEVENT SUMMARY:A system of medium resolution for monitoring the night sky backgro und in the visible and near UV range DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1105@cern.ch DESCRIPTION:Speakers: Mr. FOKITIS\, Emmanuel (National Technical Universit y of Athens\, Physics Department)\nWe address the problem of determining t he spectrum of night sky background \nin a spectral resolution which allow s understanding quick changes in the \nintensity and shape of these spectr a. One can use this information in EAS \nobservatories for carrying out po ssible corrective actions during the testing\, \ndesigning or normal opera tion phases. \nWe present a design of a low cost medium resolution telesco pe for the night \nsky background radiation\, based on an Oriel 77250 1/8 m monochromator. \nUsing two types of holographic gratings with 1200 and 2 400 grooves per mm \nwe are able to measure nightglow emissions in the vis ible and UV spectrum \nregion as well. The monochromators works in conjunc tion with a UV sensitive \nphotomultiplier tube and can achieve better th an 0.25 nm resolution.\nData acquisition and control of the facility are based mostly in custom-made \nhardware. The artificial light from mercury lamps in the near area of N.T.U.A. \ncampus can be clearly observed and used for calibration purposes and further \nimprovement of this setup. We present the contributions in the night sky \nbackground due to atmospheric \, zodiacal\, planetary\, moon and stellar \nradiations. We suggest possib le adaptation of this facility for use in ground \nbased and spaceborn EAS detectors.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contrib ution/1105 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1105 END:VEVENT BEGIN:VEVENT SUMMARY:Experimental Emulation of Air Fluorescence and study of its Yield at Low Pressure Electrical Discharges DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1108@cern.ch DESCRIPTION:Speakers: Mr. MALTEZOS\, Stavros (National Technical Universit y of Athens\, Physics Department)\nHaving high-resolution UV spectra produ ced from EAS fluorescence\, one can \ndetermine in a more accurate way th e effects of atmospheric attenuation of \nthese signals by including Rayle igh\, Mie-scattering as well as resonance \nabsorption inside the atmosphe re. For this reason\, we developed an \nexperimental setup for emulating t he air-fluorescence using high-resolution \nspectroscopy in the UV range f rom 300 to 400 nm. We used low pressure \nelectrical discharges in air \, as light source\, and registered the spectra with \nhigh resolution spectr ometers of 0.25\, 1\, 2 and 3 m focal lengths. These \npressure and temper ature conditions\, existing in the low pressure lamp used\, \nare far from the ones existing during EAS fluorescence but such data might be \nuseful for better understanding of the fluorescence emission\, and also in \nall owing to adapt such spectrometers in\ndedicated fluorescence yield experim ents in accelerators\, since in the relevant \nliterature there are not a vailable data with such high resolution. In addition\, \nthere are very fe w experimental data taking into account the parameter \ntemperature in spa ce and thus we designed a monochromator for \nmeasurements of\nair-fluores cence yield as a function of pressure and temperature\, using spectral \nl amps in which the above parameters can be controlled\, which is presented in \nthis work.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/con tribution/1108 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1108 END:VEVENT BEGIN:VEVENT SUMMARY:Experimental Details and Calibration of The FLASH Thin Target Expe riment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1113@cern.ch DESCRIPTION:Speakers: Dr. HUENTEMEYER\, Petra (Los Alamos National Laborat ory)\nThe thin target mode of the FLASH (Fluorescence in Air from Showers) \nexperiment was conducted at SLAC. The aim was to measure the total \nan d spectrally resolved fluorescence yield of charged particles \ntraveling through air to better than 10%. The setup consisted of a \n15.24 cm thick gas volume which was viewed by two PMT detectors \neach equipped with 15 r emotely interchangeable narrow band filters to \nmeasure the fluorescence spectrum between 300 and 445 nm. Final results of the FLASH\nexperiment wi ll be presented in a talk at this conference. The calibration \nof the exp erimental setup is crucial in minimizing the systematic uncertainty \nof t he measurement. We will describe how the physics of Rayleigh scattering \n is used to derive an absolute end-to-end calibration of the \nexperiment f rom first principles. In addition\, a method for a relative \ncalibration is presented using a setup with a mercury lamp\, a monochromator \nand a N IST calibrated photo diode in a light sealed black box. Finally\,\nthe tor oid measuring the beam charge had to be calibrated. The \ncombination of a ll three measurement uncertainties provided an absolute \ncalibration of t he FLASH experiment.\n\nhttps://indico.nucleares.unam.mx/event/4/session/3 9/contribution/1113 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1113 END:VEVENT BEGIN:VEVENT SUMMARY:A Fabry-Perot Interferometer prototype for use in Doppler LIDAR fo r atmospheric and night sky background monitoring in EAS detection DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1114@cern.ch DESCRIPTION:Speakers: Mr. FOKITIS\, Emmanuel (National Technical Universit y of Athens\, Physics Department)\nA Fabry-Perot interferometer prototype is studied\, as part of a Doppler LIDAR \n(DL) receiver\, for determining the aerosol to molecular scattering ratio for use \nin EAS Fluorescence D etectors. The etalon of this instrument has a Free \nSpectral Range of 0. 1 cm[-1] and resolution in wavenumber 0.04 cm[-1] .\nPossible additional u se of the proposed DL receiver can be as a spectrally \nselective detector to measure the aerosol phase function normalized to the \nmolecular phase function using a bi-static LIDAR. Both molecular and aerosol \ndata are c ollected by the same DL receiver simultaneously as opposed to the\nRayleig h or Raman LIDAR adopted in the atmospheric monitoring procedures in \nEAS fluorescence telescopes. We present preliminary laboratory results and \n evaluate their capabilities to meet the requirements of the above two \nca libration issues of EAS measurements. The results from the present \nproto type are expected to lead to a design for a DL receiver aiming to achieve \nmeasurements of the aerosol backscattering coefficient with accuracy of the \norder of 5%\, presenting a significant progress in comparison with the present \ntechniques used in atmospheric monitoring for EAS fluorescen ce or atmospheric \nCherenkov telescopes.\n\nhttps://indico.nucleares.unam .mx/event/4/session/39/contribution/1114 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1114 END:VEVENT BEGIN:VEVENT SUMMARY:The TALE Tower Detector DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1130@cern.ch DESCRIPTION:Speakers: Prof. BERGMAN\, Douglas (Rutgers University)\nThe TA Low Energy Extension will include a Tower FluorescenceDetector. Extensiv e air\nshowers at the lowest usful energies for fluorescence detectors wil l in general be\nclose to the detector. This requires viewing all elevati on angles to be able to\nreconstruct showers. The TALE Tower Detector\, o perating in conjunction with other\nTALE detectors will view elevation ang les up to above 70 degrees\, with an azimuthal\ncoverage of about 90 degre es. Results from a prototype mirror operated in\nconjunction with the HiR es detector will also be presented.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/39/contribution/1130 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1130 END:VEVENT BEGIN:VEVENT SUMMARY:Effect of the improved data acquisition system of IceCube on its n eutrino-detection capabilities DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1231@cern.ch DESCRIPTION:Speakers: Dr. CHIRKIN\, Dmitry (LBNL)\nIceCube data acquisitio n system is capable of recording information about all photons\nregistered by its photomultiplier tubes for up to 13 microseconds for each sensor\nw ith high precision. The time resolution of 3 ns and charge resolution of 3 0% of all\n1 photoelecton pulses within each sensor’s event record is ac hieved. The first\natmospheric neutrino analysis did not take full advanta ge of this\, as it used\ninformation of only one photon per hit DOM in the event\, much like the previous\ngeneration of the high-energy neutrino te lescopes. The improvement in quality of the\ndata reconstruction due to th e improved design of the experiment is estimated and its\neffect on the Ic eCube capabilities as a neutrino detector is discussed.\n\nhttps://indico. nucleares.unam.mx/event/4/session/39/contribution/1231 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1231 END:VEVENT BEGIN:VEVENT SUMMARY:Cloud Monitoring at HiRes Detector using Infra-Red Sensors DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1237@cern.ch DESCRIPTION:Speakers: FEDOROVA\, Yulia (University of Utah)\nThe monitorin g of atmospheric conditions is very important for \nfluorescence observati ons. Particularly\, the presence of clouds can \ndrastically distort the s ignal from the extensive air shower. Infra-red \n(IR) sensors\, measuring sky temperature\, can help to distinguish clouds\, \nwhich are usually sig nificantly warmer than clear skies. An array of such \nsensors\, covering the HiRes detector's field of view\, was installed\, and \nhas been collec ting data every minute of detector operation. Using this \ninformation\, a cloud database was created. This database is used to select \ncloud free CR events. In this paper we present a description of the array \nand the method to analyze IR data.\n\nhttps://indico.nucleares.unam.mx/event/4/ses sion/39/contribution/1237 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1237 END:VEVENT BEGIN:VEVENT SUMMARY:The Telescope Array's Middle Drum Observatory: The Detector and Fi rst Data DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1254@cern.ch DESCRIPTION:Speakers: Dr. MATTHEWS\, John Norman (University of Utah)\nThe Telescope Array Project (TA) is an Ultra High Energy Cosmic Ray\nObservat ory in central Utah. It performs a hybrid measurement of the\nextensive a ir showers induced by cosmic rays. The two detector systems\nare 1) an ar ray of 576 scintillation detectors and 2) three fluorescence\ntelescope ob servatories which overlook the ground array. The Telescope\nArray will me asure the study spectral shape\, chemical composition of\nprimary cosmic r ays\, and search for sources. Additionally\, it seeks to\nunderstand the difference between the HiRes (High Resolution Fly's Eye)\nand AGASA (Akeno Giant Air Shower Array) spectra. The Middle Drum\nObservatory has been i nstrumented using refurbished telescopes from\nthe HiRes-I Observatory at Dugway. We will discuss the\ndetectors\, modifications to aid calibration and analysis\, and the first\ndata from this observatory.\n\nhttps://indi co.nucleares.unam.mx/event/4/session/39/contribution/1254 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1254 END:VEVENT BEGIN:VEVENT SUMMARY:Reconstruction of Air Shower by TA Surface Array DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1257@cern.ch DESCRIPTION:Speakers: Dr. SAKURAI\, Nobuyuki (Institute for Cosmic Ray Res earch\, The University of Tokyo)\nTelescope Array (TA) is a EAS detector w hich is now building in the\nwestern desert in Utah\, USA.\nIn order to es timate the performance of TA\, a detailed detector\nsimulation is being de veloped in Java. The number\nof particles produced during the development of the EAS shower with\nvarious inclinations is calculated by\nCOSMOS code .\nSurface detector (SD) of TA consists of two layers of plastic\nscintill ator and wave form is recorded by 50MHz FADC.\nThe detection efficiency of each SD has been evaluated by using the\nvarious calibration data\nand th e results of GEANT4 simulation.\nThe analysis methods of the EAS data of S D are also being developed\nusing TA simulation.\nThis report describes th e structure of our SD simulation code\, the\nanalysis methods.\n\nhttps:// indico.nucleares.unam.mx/event/4/session/39/contribution/1257 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1257 END:VEVENT BEGIN:VEVENT SUMMARY:The Telescope Array Low-Energy Extension (TALE) Infill Ground Arra y DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1261@cern.ch DESCRIPTION:Speakers: Prof. BELZ\, John (University of Utah)\nThe physics goals of the The Telescope Array Low-Energy Extension (TALE) \ninclude the hybrid measurement of spectrum and composition of cosmic rays down \nto e nergies below 10^17 eV. To achieve composition measurements from \nobserva tion of extensive air showers\, a ground array detector must have the \nab ility to distinguish the muonic and electromagnetic components of a shower . \nHere\, we consider the design issues relevant to the infill ground arr ay \ncomponent of the TALE hybrid detector\, and present results of protot ype \nstudies as well as preliminary detector designs and the envisioned a rray \nlayout.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/cont ribution/1261 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1261 END:VEVENT BEGIN:VEVENT SUMMARY:Electromagnetic and muon primary discrimination from underground s cintillator signatures DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1276@cern.ch DESCRIPTION:Speakers: Mr. SANCHEZ\, Federico (Departamento de Altas Energi as\, Instituto de Ciencias Nucleares \, Universidad Nacional Autonoma de M exico\, Mexico\, D.F.\, C.P. 04510)\nWe discuss discrimination techniques and their quantitative efficiency that allow the\nseparation of high energ y electron/photon and muon primaries originated in cosmic ray\nextensive a ir showers impinging the ground. The experimental setup used in this study \nis detailed elsewhere in this volume (Sanchez et al.). Several approache s are\nanalyzed\, including track timing\, footprint characterization and neural networks.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/co ntribution/1276 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1276 END:VEVENT BEGIN:VEVENT SUMMARY:Buried plastic scintillator muon telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1277@cern.ch DESCRIPTION:Speakers: Mr. SANCHEZ\, Federico (Departamento de Altas Energi as\, Instituto de Ciencias Nucleares \, Universidad Nacional Autonoma de M exico\, Mexico\, D.F.\, C.P. 04510)\nMuon telescopes can have several appl ications\, ranging from astrophysical to\n solar-terrestrial interaction s tudies\, and fundamental particle physics. We\n show the design parameter s\, characterization and end-to-end simulations of a\n detector composed b y a set of three parallel dual-layer scintillator planes\,\n buried at fix depths ranging from 0.30 m to 3 m. Each layer is 4 m2 and is\n composed b y 50 rectangular pixels of 4cm x 2 m\, oriented at a 90 deg angle\n with r espect to its companion layer. The scintillators are MINOS extruded\n poly styrene strips with two Bicron wavelength shifting fibers mounted on\n mac hined grooves. Scintillation light is collected by multi-anode PMTs of\n 6 4 pixels\, accommodating two fibers per pixel. The front-end electronics h as\n a time resolution of 7.5 nsec. Any strip signal above threshold opens a\n GPS-tagged 2 micro-seconds data collection window. All data\, includi ng\n signal and background\, are saved to hard disk. Separation of extensi ve air\n shower signals from secondary cosmic-ray background muons and ele ctrons is\n done offline using the GPS-tagged threefold coincidence signal from surface\n water cerenkov detectors located nearby in a triangular ar ray. Cosmic-ray\n showers above 6 PeV are selected. The data acquisition s ystem is designed to\n keep both\, background and signals from extensive a ir showers for a\n detailed offline data.\n\nhttps://indico.nucleares.unam .mx/event/4/session/39/contribution/1277 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1277 END:VEVENT BEGIN:VEVENT SUMMARY:Comprison of hybrid and monte carlo shower generators on an event by event basis. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1278@cern.ch DESCRIPTION:Speakers: Mr. ALLEN\, Jeff (New York University)\nSENECA is a hybrid air shower simulation written by H. Drescher that utilizes both\nMo nte Carlo simulation and cascade equations. By using the cascade equations only in\nthe high energy portion of the shower\, where they are extremely accurate\, SENECA is\nable to utilize the advantages in speed from the ca scade equations yet still produce\ncomplete\, three dimensional particle d istributions at ground level. We present a\ncomparison\, on an event by ev ent basis\, of SENECA and CORSIKA\, a well trusted MC\nsimulation. By usin g the same first interaction in both SENECA and CORSIKA\, the\neffect of t he cascade equations can be studied within a single shower\, rather than\n averages over many showers. Our study shows that for showers produced in t his manner\,\nSENECA agrees with CORSIKA to a very high accuracy as to den sities\, energies\, and\ntiming information for individual species of grou nd-level particles from both iron\nand proton primaries with energies betw een 1EeV and 100EeV. Used properly\, SENECA\nproduces ground particle dist ributions virtually indistinguishable from those of\nCORSIKA in a fraction of the time. For example\, for a shower induced by a 40 EeV\nproton simul ated with 10^-6 thinning\, SENECA is 10 times faster than CORSIKA.\n\nhttp s://indico.nucleares.unam.mx/event/4/session/39/contribution/1278 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1278 END:VEVENT BEGIN:VEVENT SUMMARY:Description and preliminary test results of a detector prototype f or the TUS space fluorescence observatory DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1301@cern.ch DESCRIPTION:Speakers: Dr. SALAZAR\, Humberto (Fac. Cs. FIS-MAT\, BUAP)\nWe discuss a general scheme of the optics and electronics read out as well\n as preliminary test results of a detector prototype for the space fluoresc ence\ntelescope TUS (FD-TUS). The mirror of this prototype is coupled to a n 8 by 8 pixel\ncamera. Each of the 64 pixels is read by one PMT of 13 mm diameter (Hamamatsu model\nR1463) . The optics design is a multi-hexagonal segmented telescope with focal\ndistance of 1.5m and 2 square meter area. The optics design is optimized to have a\nlight collection\nefficiency g reater then 50% for all the pixel positions. The fluorescence detector\nis being tested at the high mountain site Sierra La Negra near Puebla City i n Mexico\n(600g/cm2). The FD-TUS will observe EAS tracks at energies of a bout 1 EeV at\ndistances 25-50km\,and zenith angles greater than 45 degre e with direction tracks\nperpendicular to the FD axis.\n\nhttps://indico.n ucleares.unam.mx/event/4/session/39/contribution/1301 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1301 END:VEVENT BEGIN:VEVENT SUMMARY:Electronics and Data Acquisition System of the Extensive Air Showe r Detector Array at the University of Puebla DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1302@cern.ch DESCRIPTION:Speakers: Dr. VILLASENOR\, Luis (Institute of Physica and Math ematics\, University of Michoacan)\nField programmable gate arrays (FPGAs) are playing an increasing role in\nDAQ systems in cosmic ray experiments due to their high speed and\nintegration and their low cost and low power comsumption. In this paper we\ndescribe in detail the new electronics and data acquisition system based on\nFPGA boards of the extensive air shower detector array built in the Campus of\nthe University of Puebla. The purpo se of this detector array is to measure\nthe energy and arrival direction of primary cosmic rays with energies\naround 10^15 eV. The array consists of 10 liquid scintillator detectors\nand 6 water Cherenkov detectors (of 1 .86 m2 cross section)\, distributed\nin a square grid with a detector spac ing of 20 m over an area of 4000 m2.\nThe electronics described also makes use of analog to digital converters\nwith a resolution of 10 bits and sa mpling speeds of 100 MS/s to digitize\nthe PMT signals. We also discuss th e advantages of discriminating the\nPMT signals inside the FPGAs with res pect to the conventional use of\ndedicated discrimination circuits.\n\nhtt ps://indico.nucleares.unam.mx/event/4/session/39/contribution/1302 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1302 END:VEVENT BEGIN:VEVENT SUMMARY:AMIGA: A muon detector and infilled array for the Auger Observator y DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1307@cern.ch DESCRIPTION:Speakers: Prof. ETCHEGOYEN\, Alberto (CNEA\, Buenos Aires)\nIt is planned to up-grade the Pierre Auger Observatory through some enhancem ents so\nthat the energy spectrum of cosmic rays can be studied down to 0. 1 EeV and the muon\ncomponent of showers can be determined. The former wi ll lead to a spectrum measured\nby one technique from 0.1 EeV to beyond 10 0 EeV while the latter will aid\nidentification of the primary particles. These enhancements consist of three high\nelevation telescopes (HEAT\, des cribed in a companion poster) and an infilled area\nhaving both surface de tectors and underground muon counters (AMIGA). \n\nThe surface array of t he Auger Observatory will be enhanced over a 23.5 km2 area by\n85 detector pairs laid out as a graded array of water-Cherenkov detectors and 30 m2\n buried muon scintillator counters. The spacings in the array will be 433 and 750 m .\nThe muon detectors will comprise highly segmented scintillato rs with optical fibres\nending on multi-anode phototubes. The AMIGA comple x will be centred 6.0 km away from\nthe fluorescence detector installation at Coihueco and will be overlooked by the HEAT\ntelescopes. \n\nWe descri be the design features and expected performance of the AMIGA enhancement.\ n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/1307 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1307 END:VEVENT BEGIN:VEVENT SUMMARY:A particle acceleration site in the Coma cluster? DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-5@cern.ch DESCRIPTION:Speakers: Mr. ECKERT\, Dominique (ISDC)\nObservations of the C oma cluster by Beppo-SAX have shown a hard X-ray excess in the\nspectrum t hat could be interpreted as the presence of a particle acceleration site.\ nHowever\, given that the hard X-ray instrument on board Beppo-SAX was non -imaging\,\nexistence of point sources could change this interpretation. T he better angular\nresolution of INTEGRAL allowed us to analyze the morpho logy of the hard X-ray\nemission. Our results show that contamination by a very hard point source embedded in\nthe cluster is highly unlikely\, whic h strengthens the hypothesis of a particle\nacceleration site in the Coma region.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contributio n/5 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/5 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-rays from globular clusters DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-26@cern.ch DESCRIPTION:Speakers: Dr. BEDNAREK\, Wlodek (Department of Experimental Ph ysics\, University of Lodz)\nThe millisecond pulsars in globular clusters can accelerate leptons at the shock waves\noriginated in collisions of th e pulsar winds and/or inside the pulsar magnetospheres.\nLeptons diffuse g radually through the globular cluster comptonizing stellar and \nmicrowave background radiation. We calculate the GeV-TeV $\\gamma$-ray spectra for\ ndifferent models of injection of leptons and parameters of the globular c lusters. \nThe results of calculations are shown for four specific globula r clusters (47 Tuc\,\nTer 5\, M13\, and M15) which might be potentially de tected by the present Cherenkov\ntelescopes and the planned satellite tele scopes (AGILE\, GLAST).\n\nhttps://indico.nucleares.unam.mx/event/4/sessio n/39/contribution/26 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/26 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-rays from young open cluster Ber 87 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-28@cern.ch DESCRIPTION:Speakers: Dr. BEDNAREK\, Wlodek (Department of Experimental Ph ysics\, University of Lodz)\nOpen clusters are concentrations of dense mat ter and young stars. It is expected that\nnon-thermal processes play impor tant role in these objects due to the observations of\nnon-thermal X-ray e mission and directional coincidence with some uniEGRET sources. We\ncalcul ate the gamma-ray spectra expected from the open cluster Ber 87 assuming that\nhadrons and leptons are accelerated inside this object.\n\nhttps://i ndico.nucleares.unam.mx/event/4/session/39/contribution/28 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/28 END:VEVENT BEGIN:VEVENT SUMMARY:Very high energy gamma-ray emission of close metagalactic sources Mkn421\, Mkn 501 amd NGC 1275. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-62@cern.ch DESCRIPTION:Speakers: Prof. SINITSYNA\, Vera Georgievna (Lebedev Physical Institute)\nExploration of the galactic and metagalactic objects in which the acceleration of\nprotons and nuclei is accompanying with generation of gamma-quanta and neutrinos is\nof great current interest for astroparticl e physics because the gammas and neutrinos\ndo not dissipate energy after propagation through the magnetic fields of the Universe\nproviding a uniqu e probe into these cosmic accelerators. These gamma-astronomical\nresearch es are carrying out with SHALON mirror telescope at the Tien-Shan\nhigh-mo untain observatory. During the period 1992 – 2007\, SHALON has been used for\nobservations of the metagalactic sources Mkn421\, Mkn501\, NGC1275\, 3c454.3\, 1739+522\nand galactic sources Crab Nebula\, Cygnus X-3\, Tycho 's SNR\, Geminga\, 2129+47XR. The\nobservation results of two type of met agalactic sources: BLLacs Mkn 421 (z = 0.031)\,\nMkn 501 (z = 0.034) and S eyfert galaxy NGC 1275 (z=0.0179) are presented. The\nintegral average gam ma-ray fluxes of Mkn 421 and Mkn 501 were estimated as $(0.63 \\pm\n0.14)\ \times10^{-12} cm^{-2}s^{-1}$ and $(0.86 \\pm 0.13)\\times10^{-12} cm^{-2} s^{-1}$\nrespectively. NGC 1275 is being intensively studied by SHALON and gamma-ray flux are\nfound to be $(0.78\\pm 0.13)\\times10^{-12} cm^{-2}s^ {-1}$. The integral spectra of\nevents from source - $k_on$ and background events\, observing simultaneously with\nsource's events - $k_off$\, and s ource image are presented. The increase of the flux\nover the average valu e was detected in 1997 and 2004 observations of Mkn 421 by\nSHALON and est imated to be $(1.01\\pm0.25)\\times10^{-12} cm^{-2}s^{-1}$ and\n(0.96\\pm0 .2)\\times10^{-12} cm^{-2}s^{-1}$\, respectively. The significant increase of\nMkn 501 flux was detected in 1997 with the VHE ground telescopes all over the world.\nThe integral gamma- ray flux by SHALON telescope was esti mated as $(1.21\\pm\n0.13)\\times10^{-12} cm^{-2}s^{-1}$ that is comparabl e with flux of powerful galactic\nsource Crab Nebula. The research of extr agalactic and galactic sources of very-high\nenergy gamma-quanta by method s\, including ones using mirror Cherenkov telescopes\nconcerns\, rather th an delicate problem of the cosmic ray nature and the role of our\nGalaxy a nd Extragalaxy in their generation.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/39/contribution/62 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/62 END:VEVENT BEGIN:VEVENT SUMMARY:Galactic sources at TeV energy: Flaring activity of Cygnus X-3 and new binary 2129+47XR DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-68@cern.ch DESCRIPTION:Speakers: SINITSYNA\, Vera Yurievna (Lebedev Physical Institut e)\nThe new galactic gamma-source neutron star 2129+47XR is detected at en ergy >0.8TeV\nwith flux (0.19\\pm0.9)×10^{-12}cm^{-2}s^{-1} and index of the integral spectrum is kγ\n= -1.05\\pm0.10. \nCygnus X-3 is peculiar X- ray binary system discovered about 40 years ago. The system\nhas been obse rved throughout wide range of the electromagnetic spectrum. It is one of\n the brightest Galactic X-ray sources\, displaying high and low states and rapid\nvariability in X-rays. It is also the strongest radio source among X-ray binaries and\nshows both huge radio outbursts and relativistic jets. The radio activity is closely\nlinked with the X-ray emission and the dif ferent X-ray states. Based on the\ndetections of ultra high energy gamma-r ays\, Cygnus X-3 has been proposed to be one of\nthe most powerful sources of charged cosmic ray particles in the Galaxy. The attempts\nof detection of TeV emission from Cygnus X-3 were first made in the mid of 1970s and\n continued through the mid 1980s. Two observations were particularly import ant: the\nKiel results and contemporaneous observation at Haverah Park. Th ese results indicated\na very large UHE flux from Cygnus X-3. The 10 year' s observation results of point\nsource Cygnus X-3 by mirror Cherenkov tele scope SHALON are presented. Cygnus X-3 has\nbeen regularly observed since a 1995 with average gamma-quantum flux of F(EO>0\,8\nTeV)=(6.8\\pm0.7)\\ti mes10^{-13}cm^{-2}s^{-1}. The energy spectrum of Cygnus X-3 at 0.8\n- 65 T eV F(>E_0) ~ E^{kγ}\, where kγ= -1.22\\pm0.04 is obtained for the first time with\nflux on the order the less than upper limits published before. The flux in 2003 year\nis (1.79\\pm0.33)\\times10^{-12}cm^{-2}s^{-1}. The index of integral spectrum is\nkγ=-1.28\\pm0.06. Earlier\, in 1997\, the increase of flux was also observed\n(1.2\\pm0.5)\\times10^{-12}cm^{-2}s^{- 1}. Thus\, among ten observable gamma-quantum\nobjects\, there is galactic source Cygnus X-3\, with periodic change of intensity. The\nvariability o f radiation can give essential information on a source nature. The\nbinary Cyg X-3 came to new period of flaring activity at radio- and X-ray energi es in\n2006. In May and July 2006 the significant increase of Cyg X-3 flux have detected\nwith SHALON at TeV energy.\n\nhttps://indico.nucleares.una m.mx/event/4/session/39/contribution/68 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/68 END:VEVENT BEGIN:VEVENT SUMMARY:A first synoptic blazar study comprising eleven blazars visible in E>100 GeV gamma rays DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-70@cern.ch DESCRIPTION:Speakers: Dr. WAGNER\, Robert (Max-Planck-Institute for Physic s)\nSince 2002\, the number of detected blazars at gamma-ray energies of 1 00 GeV and above\nhas more than doubled. A synoptic study of these objects therefore might reveal\nimportant collective characteristics. I present a study of all currently known\nhigh-frequency peaked BL Lac-type objects f or which photon energy spectra at E>100\nGeV have been inferred. The intri nsic energy spectra of the sources are reconstructed\nusing a contemporary model for the extragalactic background light. Then\, the\nproperties of t he observed emission are compared and correlated among each other\,\nwith X-ray data\, and with the individual estimated black hole masses. In addit ion\, I\nconsider temporal properties of the found VHE gamma-ray flux. Key findings concern\nthe flux-black hole mass and variability scale-black ho le mass connections and the\ncorrelation of the spectral slope and the lum inosity. The latter is also studied for\nsources for which individual dist inct flux states have been observed. As a specific\napplication\, the syno ptic study allows to constrain the redshift of PG 1553+113\, a\nTeV blazar s whose distance is unknown to date.\n\nhttps://indico.nucleares.unam.mx/e vent/4/session/39/contribution/70 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/70 END:VEVENT BEGIN:VEVENT SUMMARY:Detection of very high energy gamma-rays from the BL Lac object 1E S 2344+514 in a low emission state with the MAGIC telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-71@cern.ch DESCRIPTION:Speakers: Dr. WAGNER\, Robert (Max-Planck-Institute for Physic s)\nThe MAGIC telescope has observed very high energy gamma-ray emission f rom the AGN 1ES\n2344+514. A gamma-ray signal corresponding to an 11 sigma excess and an integral flux\nof (2.38+-0.30)*10^-11 cm^-2 s^-1 above 200 GeV has been obtained from 23.1 hours of\ndata taking between 2005 August 3 and 2006 January 1. The data confirm the previously\ndetected gamma-ray emission from this object during a flare seen by the Whipple\ncollaboratio n in 1995 and the evidence from long-term observations conducted by the\nW hipple and HEGRA groups. The MAGIC observations show a relatively steep di fferential\nphoton spectrum that can be described by a power law with a sp ectral index of\n-2.95+-0.12 between 140 GeV and 5.4 TeV. The observations reveal a low flux state\,\nabout six times below the 1995 flare seen by W hipple and comparable with the previous\nWhipple and HEGRA long term measu rements. During the MAGIC observations no\nsignificant time variability ha s been observed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/co ntribution/71 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/71 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma ray emission from PWN interacting with molecular clouds DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-91@cern.ch DESCRIPTION:Speakers: Dr. BARTKO\, Hendrik (MPI f. Physik\, Munich\, Germa ny)\nIn this work we consider the situation in which the pulsar (and its n ebula) is formed\ninside or close to the high density regions of a molecul ar cloud. Recent models for\nthe gamma radiation of pulsar wind nebula try to include not only radiation processes\ndue to the injected leptons but also processes due to injection of relativistic\nhadrons into the nebula. Hadrons accelerated during the lifetime of a pulsar can be\npartially capt ured in dense (10^3-10^5 cm^3)\, magnetized (10^{-5} 10^{-3} G)\nmolecular clouds\, producing gamma-rays for a relatively long time. We compare the \ntheoretical predictions with PWN candidates observed by MAGIC and HESS i n VHE gamma-rays.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/c ontribution/91 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/91 END:VEVENT BEGIN:VEVENT SUMMARY:MAGNETIC FIELD IN SUPERNOVA REMNANT SN 1987A DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-125@cern.ch DESCRIPTION:Speakers: Dr. KSENOFONTOV\, Leonid (Institue of Cosmophysical Research and Aeronomy\, Yakutsk\, RUSSIA)\nA nonlinear kinetic theory of c osmic-ray acceleration in supernova remnants is employed to investigate th e \nproperties of the remnant SN 1987A. It is shown that a large downstrea m magnetic field 10 mG is required to fit \nthe existing observational dat a. Such a strong field\, together with the strong shock modification due t o CR back-\nreaction\, provides the steep and concave radio-emission spect rum and considerable synchrotron cooling of high-\nenergy electrons that d iminish their X-ray synchrotron flux below the observed Chandra flux\, whi ch has to be \nconsidered as an upper limit for non-thermal X-ray emission .\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/125 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/125 END:VEVENT BEGIN:VEVENT SUMMARY:AN EVIDENCE FOR STRONG NON-THERMAL EFFECTS IN TYCHO SNR DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-127@cern.ch DESCRIPTION:Speakers: Dr. KSENOFONTOV\, Leonid (Institue of Cosmophysical Research and Aeronomy\, Yakutsk\, RUSSIA)\nWe present for the case of Tych o's supernova remnant the relation between the blast wave and contact \ndi scontinuity sizes calculated within the nonlinear kinetic theory of cosmic ray acceleration in SNRs. It is \ndemonstrated that they are very well co nfirmed by recently published Chandra measurements\, which show that \nthe observed contact discontinuity radius is so close to the shock radius\, t hat it can only be explained by the \nefficient CR acceleration which in t urn makes the medium more compressible.\n\nhttps://indico.nucleares.unam.m x/event/4/session/39/contribution/127 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/127 END:VEVENT BEGIN:VEVENT SUMMARY:Discovery of TeV Gamma-Ray Emission in the W28 Region from HESS Ob servations\, and Multiwavelength Comparisons DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-129@cern.ch DESCRIPTION:Speakers: Dr. ROWELL\, Gavin (School of Chemistry and Physics\ , University of Adelaide)\nH.E.S.S. observations of the old-age (more than 10000 yrs\; about 0.5 deg diameter) composite SNR W28 \nreveal TeV emissi on situated at its northeastern and southern boundaries. The northeastern TeV source is \nin an \narea where W28 is interacting with a dense molecul ar cloud\, containing OH masers\, local radio and X-ray \npeaks. The south ern TeV sources are found in a region occupied by several HII regions\, in cluding the ultra-\ncompact HII region W28-A2. Our analysis of NANTEN CO d ata also reveals a dense molecular cloud \nenveloping \nthis southern regi on. Further details concerning H.E.S.S.\, NANTEN\, and other multiwaveleng th results will \nbe \npresented at the conference.\n\nhttps://indico.nucl eares.unam.mx/event/4/session/39/contribution/129 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/129 END:VEVENT BEGIN:VEVENT SUMMARY:Looking for the high energy component of GRBs at the Large Apertur e GRB Observatory DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-175@cern.ch DESCRIPTION:Speakers: BERTOU\, Xavier (Centro Atomico Bariloche\, Institut o Balseiro. Argentina)\nThe LAGO project aims at the detection of high ene rgy photons from GRBs using the\nsingle particle technique in ground based water Cherenkov detectors. To reach a\nreasonable sensitivity\, high alti tude mountain sites have been selected and detectors\nare in operation in Mexico (Sierra Negra\, 4650m a.s.l.) and Bolivia (Chacaltaya\,\n5300m a.s. l.). We report on detector calibration and operation at high altitude\,\ns earch for bursts in 6 months of preliminary data\, as well as search for s ignal when\nsatellites report a burst.\n\nhttps://indico.nucleares.unam.mx /event/4/session/39/contribution/175 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/175 END:VEVENT BEGIN:VEVENT SUMMARY:Time variation of the flux of TeV gamma-rays from PKS 2155-304 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-205@cern.ch DESCRIPTION:Speakers: Prof. NISHIJIMA\, Kyoshi (Tokai University)\nObserav ations of neaby blazar PKS 2155-304(z=0.116) was performed\nin July and Au gust 2006 with the CANGAROO-III atmospheric Cherenkov\ntelescope in South Australia\, which was triggered by the H.E.S.S.\ngroup as a high state. St ereo observations with three telescopes\nwere performed except for the obs ervations done before culmination\nin each night of July periods due to me chanical tracking problem\nof one telescope. Only two-fold observations we re done in those periods.\nHere\, by combining three-fold data and two-fol d data\, the time\nvariation of the flux of VHE gamma-rays from PKS 2155-3 04 was studied.\nEffective live time for three-fold and two-fold obseravti ons\nin July is 15.0 hours and 9.4 hours\, respsctively\, and that for Aug ust\nis 17.1 hours. We detected averaged signals at the 6.8 sigma level fo r\nthree-fold data in July and at the 2.7 sigma level in August.\nMore tha n 4 sigma level signals are detected for two-fold obseravtions.\nThe light curve shows a clear nightly time variation of the flux\nfrom PKS 2155-304 \, particularly the flux in July 28 and 30 exceeds\n1 Crab.\n\nhttps://ind ico.nucleares.unam.mx/event/4/session/39/contribution/205 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/205 END:VEVENT BEGIN:VEVENT SUMMARY:HESSJ1023-575: Non-thermal particle acceleration associated with a young stellar cluster? DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-211@cern.ch DESCRIPTION:Speakers: Mr. RAUE\, Martin (Institut für Experimentalphysik\ , Universität Hamburg\, Germany)\nThe results from H.E.S.S. observations towards Westerlund 2 are presented. The\ndetection of very-high-energy gam ma-ray emission towards the young stellar cluster\nWesterlund 2 in the HII complex RCW49 by H.E.S.S. provides ample evidence that\nparticle accelera tion to extreme energies is associated with this region. A variety\nof pos sible emission scenarios will be reviewed\, ranging from high-energy gamma -ray\nproduction in the colliding wind zone of the massive Wolf-Rayet bina ry WR20a\,\ncollective wind scenarios\, diffusive shock acceleration at th e boundaries of\nwind-blown bubbles in the stellar cluster\, and outbreak phenomena from hot stellar\nwinds into the interstellar medium. These scen arios are compared to the\ncharacteristics of the associated new VHE gamma -ray source HESSJ1023-575\, and\nconclusions on the validity of existing e mission scenarios for high-energy gamma-ray\nproduction are drawn.\n\nhttp s://indico.nucleares.unam.mx/event/4/session/39/contribution/211 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/211 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of LSI+61303 with Swift DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-233@cern.ch DESCRIPTION:Speakers: Dr. HOLDER\, Jamie (University of Delaware)\nThe TeV emitting high-mass X-ray binary system LSI+61303 was observed with the\nS wift satellite from early September 2006 to early January 2007. Many of th ese\nobservations were contemporaneous with TeV observations. The data con sist of\nobservations on 24 separate days with durations ranging between 7 00s and\n4700s\, and cover 4.5 orbital periods of the binary system. We pr esent here a\ntemporal and spectral analysis of the 0.3 to 10keV X-ray dat a from the XRT\ninstrument\, as well as contemporaneous optical data from UVOT. Implications\nfor the models of high energy emission from this syste m are discussed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/co ntribution/233 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/233 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of Mrk 421 and Mrk 501 in Spring 2006 with VERITAS DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-234@cern.ch DESCRIPTION:Speakers: FEGAN\, Stephen (UCLA)\nVERITAS\, the Very Energetic Radiation Telescope Array System\, is an\narray of four imaging Atmospher eic Cherenkov telescopes in southern\nArizona. It is sensitive to gamma-ra ys at energies above 100GeV. Here\,\nwe discuss the results of observation s of two well known VHE blazars\,\nMarkarian 421 and Markarian 501\, durin g Spring 2006 which were made\nwith the first two telescopes during the co missioning phase of VERITAS\nDuring most of this time Mrk 421 was in an un usually active state\nwhile Mrk 501 was in a much lower flux state. As suc h\, these\nobservations provided an opportunity to test the sensitivity of the\ninstrument to strong and weak sources. We discuss implications of\n these observations on our understanding of these objects.\n\nhttps://indic o.nucleares.unam.mx/event/4/session/39/contribution/234 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/234 END:VEVENT BEGIN:VEVENT SUMMARY:A search for 100 TeV celetial gamma rays with the Tibet air shower array and a future prospect DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-241@cern.ch DESCRIPTION:Speakers: Dr. TAKITA\, Masato (Institute for Cosmic Ray Resear ch\, the University of Tokyo)\nStimulated by the recent HESS galactic surv ey which discovered 14 \nnew TeV gamma-ray sources\, it is now important t o measure 100 TeV \ngamma rays from celetial sources to locate possible c osmic-ray \naccelerators up to PeV energies in our galaxy.\nThe Tibet air shower array (37\,000m**2)\, located at 4\,300 m above\nsea levelin Tibet\ , is a wide field-of-view gamma-ray telescope \nabove TeV energies. We wi ll report on a search for 100 TeV celetial\ngamma rays with the Tibet air shower array. In addition\, we have\na plan aiming at 100 TeV gamma-ray astronomy by adding a large\nunderground water Cherenkov muon detector a rray (approximately \n10\,000m**2) to the existing Tibet air shower array. \n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/241 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/241 END:VEVENT BEGIN:VEVENT SUMMARY:Detection of 2006 TeV-outburst of PKS 2155-304 with the CANGAROO-I II telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-243@cern.ch DESCRIPTION:Speakers: Ms. SAKAMOTO\, Yukiko (Depertment of Physics\, Tokai University)\nObservations of PKS 2155-304 with the CANGAROO-III imaging a tmospheric \nCherenkov telescope were performed for 5 nights from July 28 to August 2 in \n2006\, just after H.E.S.S. reported that this target obje ct was at a strong active \nstate. Signal exceeding 6 sigma significance l evel was detected in the effective \nlive time of 15.0 hours using three-f old steroscopic data set. Obtained time \naveraged integral flux above 630 GeV is (2.3+-0.4)*10^-11cm^-2sec^-1\nwhich corresponds to ~60%Crab flux l evel. We found nightly variation of \ngamma-ray flux from PKS 2155-304.\n Follow up observations were done for 6 nights between August 17 and \n25.E ffective live time of this period is 17.1 hours and its activity settled d own to \n~20%Crab.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/ contribution/243 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/243 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-hadron separation of parent particles of air showers above s everal 10 TeV energies using Tibet-III air-shower array DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-278@cern.ch DESCRIPTION:Speakers: Mr. CHEN\, Ding (Faculty of Engineering\, Yokohama N ational University)\nThe recent advances in TeV gamma-ray astronomy are la rgely due to the ability to\ndistinguish between extensive air showers gen erated by gamma rays and hadronic cosmic\nrays. In this paper\, we report on a method to distinguish electromagnetic air showers\nfrom hadronic air showers in Tibet air-shower observation. An extensive Monte Carlo\nsimulat ion has been carried out and the secondary particles are also propagated\ nthrough the Tibet-III air shower array to study the detector response. So me\npreliminary results on the search for gamma-ray sources above several 10 TeV energies\nare discussed.\n\nhttps://indico.nucleares.unam.mx/event/ 4/session/39/contribution/278 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/278 END:VEVENT BEGIN:VEVENT SUMMARY:Supernova remnant evolution in uniform and non-uniform media DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-290@cern.ch DESCRIPTION:Speakers: Dr. FERREIRA\, Stefan (North-West University (Potche fstroom Campus))\nIn this work numerical simulations showing the time evol ution of a supernova \nremnant (SNR) in an uniform and non-uniform interst eller medium (ISM) are \npresented. For this we use a hydrodynamic model i ncluding a kinematic \ncalculation of the interstellar magnetic field. Imp ortant parameters include the \nejecta mass and energy of the remnant\, as well as interstellar medium density \nand adiabatic index. By varying the se we constructed an analytical expression \ngiving the return time of the reverse shock to the origin. We also computed the \nevolution of the remn ant in non-uniform media. As the SNR evolves from one \ninto another mediu m of higher density a reflection shock is created which is \ndriven back t oward the center. As the reflection shock moves inward it also \ndrags som e of the compressed ISM field lines with it and heats the inside of the \n SNR. When a SNR explodes in a medium with a high density and the blast \nw aves propagate into a medium with a lower density a cavity is being blown \naway changing the geometry of the high density region. Also\, once the f orward \nshock moves into the medium of less density\, a second reverse sh ock will start \nto form in this region.\n\nhttps://indico.nucleares.unam. mx/event/4/session/39/contribution/290 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/290 END:VEVENT BEGIN:VEVENT SUMMARY:Semi-analytical Modelling of Time-variable Blazar Jet Spectra DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-304@cern.ch DESCRIPTION:Speakers: Ms. MILOVANOVIC\, Ana (University of Leeds)\nWe pres ent a detailed leptonic model for the spectral evolution of TeV blazars.\n Synchrotron emission is modelled\, with the TeV component explained by bot h Inverse\nCompton upscattering of synchrotron photons and photons origina ting externally to the\njet. The Broad Line Region and accretion disc are considered for the source of soft\nexternal target photons. We investigate the effects on the emission region's passage\nthrough the BLR to the evol ution of the observed spectra. Taking into account\ntime-travel effects\, we have developed a fast kinetic-equation solving numerical code\nto fit t he time-resolved X-ray and gamma-ray (MeV to TeV) spectra from current\nsa tellite observatories and imaging Cherenkov telescopes. Predictions are pr esented\nfor the averaged TeV photon spectra on timescales of 10 - 30 minu tes. The possible\nscenario of orphan TeV flares due to the emission regio n's emergence from the BLR is\nproposed.\n\nhttps://indico.nucleares.unam. mx/event/4/session/39/contribution/304 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/304 END:VEVENT BEGIN:VEVENT SUMMARY:Observation of HESS J1303-631 with the CANGAROO-III telescopes DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-320@cern.ch DESCRIPTION:Speakers: Dr. KUSHIDA\, Junko (Tokai University)\nHESS J1303-6 31 is one of the unidentified TeV gamma-ray sources \nwhich H.E.S.S. group discovered as a diffuse source. \nWe observed HESS J1303-631 between Febr uary and May in 2006\nwith the CANGAROO-III imaging atmospheric Cherenkov telescope system. \nAfter considering the weather conditions\, the total e xposure is \nabout 35 hours live-time. Estimated threshold energy based on \nthe Monte Carlo simulation is about 1.3 TeV. \nAnalysis of this data se t yields more than 4 sigma excess events \nfrom the direction of HESS J130 3-631\, which corresponds to \n~20% Crab flux. \nHere we report our prelim inary results of the flux and \nthe spectrum of gamma-ray emission from th is target object.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/c ontribution/320 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/320 END:VEVENT BEGIN:VEVENT SUMMARY:Broadband gamma-ray observations: AGILE AND MAGIC DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-363@cern.ch DESCRIPTION:Speakers: Prof. DE ANGELIS\, Alessandro (INFN and University o f Udine)\nThe large FOV of the AGILE Gamma-Ray Imaging Detector (GRID)\, 2 .5 sr\, will allow the\nwhole sky to be surveyed once every 10 days in the 30 MeV - 50 GeV energy band down\nto 0.05 Crab Units. This fact gives the opportunity of performing the first\nflux-limited\, high-energy g-ray all -sky survey. The high Galactic latitude\npoint-source population is expect ed to be largely dominated by blazars. Several tens\nof blazars are expect ed to be detected by AGILE (e.g.\, Costamante & Ghisellini 2002)\,\nabout half of which accessible to the ground-based MAGIC Cherenkov telescope. Th e\nlatter can then carry out pointed observations of this subset of AGILE sources in the\n50GeV - 10TeV band. Given the comparable sensitivities of AGILE/GRID and MAGIC in\nadjacent energy bands where the emitted radiation is produced by the same (e.g.\, SSC)\nmechanism\, we expect that most of these sources can be detected by MAGIC. We expect\nthis broadband g-ray st rategy to enable discovery by MAGIC of 10-15 previously\nunknown TeV blaza rs.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/36 3 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/363 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of 1ES 0647+250 and 1ES 0806+524 with VERITAS DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-365@cern.ch DESCRIPTION:Speakers: Dr. COGAN\, Peter (McGill University)\nObservations of the blazars 1ES 0647+250 and 1ES 0806+524 with VERITAS\nare reported he re. These objects are among the favoured candidate\nextragalactic sources in the very high-energy regime due to the\npresence of high-energy electro ns and adequate seed photons. The\npresence of high-energy electrons is es tablished from the location of\nthe synrchrotron peak in the spectral ener gy distribution of the\nblazars. The presence of adequate seed photons is determined by the\nflux in the radio-through-optical wavebands. These are the key\ningredients for very high-energy gamma-ray emission in the contex t of\nthe synchrotron self-Compton model. The redshift of 1ES 0647+250 has \nbeen tentatively reported as 0.203 and the redshift of 1ES 0806+524 is\n 0.138\, thus the detection of very high-energy gamma-ray emission from\nth ese objects could make significant contributions to the\nunderstanding of the extragalactic infrared background light. The\nanalysis of these data r elies on standard techniques in very\nhigh-energy gamma-ray astronomy\, an d the results are compared to\npreviously reported upper limits and to the oretical predictions.\n\nhttps://indico.nucleares.unam.mx/event/4/session/ 39/contribution/365 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/365 END:VEVENT BEGIN:VEVENT SUMMARY:Future GLAST observations of Supernova remnants and Pulsar wind ne bulae DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-390@cern.ch DESCRIPTION:Speakers: Dr. FUNK\, Stefan (Kavli Institute for Particle Astr ophysics and Cosmology\, SLAC)\nShell-type Supernova remnants (SNRs) have long been known to harbour a population of\nultra-relativistic particles\, accelerated in the Supernova shock wave by the\nmechanism of Diffusive sh ock acceleration. Experimental evidence for the existence of\nelectrons up to energies of ~100 TeV was first provided by the detection of hard\nX-ra y synchrotron emission as e.g. in the shell of the young SNR SN1006. Furth ermore\nusing theoretical arguments shell-type Supernova remnants have lon g been considered\nas the main accelerator of protons - Cosmic rays - in t he Galaxy\; definite proof of\nthis process is however still missing. Pul sar Wind Nebulae (PWN) - diffuse\nstructures surrounding young pulsars - a re another class of objects known to be a\nsite of particle acceleration in the Galaxy\, again through the detection of hard\nsynchrotron X-rays su ch as in the Crab Nebula. Gamma-rays above 100 MeV provide a\ndirect acces s to\nacceleration processes. Ultra-relativistic electrons emit gamma-radi ation through\nInverse Compton scattering in ubiquitous photon fields (suc h as CMBR\, star light and\ndust emission or local synchrotron radiation)\ , protons emit gamma-radiation through\nthe decay of pi0s\, generated in p roton-proton interactions with Interstellar material\nsuch as gas clouds. Recent advances in ground-based gamma-ray astronomy e.g. made by\nCherenko v Telescopes above an energy threshold of 100 GeV have shown\, that both\n shell-type SNRs and PWN are classes\nof gamma-ray emitting objects in the Galaxy. The upcoming GLAST Large Area Telescope\n(LAT) will be operating i n the energy range between 30 MeV and 300 GeV and will\nprovide excellent sensitivity\, angular and energy resolution in a poorly investigated\nener gy band. Shell-type SNRs as well as PWN provide natural targets for GLAST\ nobservations and\ndetections. We will describe prospects for the investig ation of these Galactic\nparticle accelerators with GLAST.\n\nhttps://indi co.nucleares.unam.mx/event/4/session/39/contribution/390 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/390 END:VEVENT BEGIN:VEVENT SUMMARY:H.E.S.S. VHE Gamma-ray sources without identified counterparts DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-400@cern.ch DESCRIPTION:Speakers: Dr. KOSACK\, Karl (Max-Planck-Institut fuer Kernphys ik)\nScan-based observations of the Galactic plane and continuing\nre-obse rvations of known very-high-energy (VHE) gamma-ray sources with\nthe H.E.S .S. system of imaging atmospheric Cherenkov telescopes have\nrevealed a wi de variety of new VHE objects. While in many cases these\nobjects can be a ssociated with known sources in the X-ray\, radio\, or\noptical wavebands\ , a subset of them currently have no obvious\ncataloged lower-energy count erpart. Since at least weak X-ray and\nradio emission is predicted by most common VHE emission models\, the\nlack of lower-energy detections may pro vide substantial model\nconstraints and may even point to a new class of o bjects which emit\nprimarily in the VHE energy range. An analysis of 8 suc h unidentified\nsources will be presented here\, including a multi-wavelen gth\ndiscussion.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/co ntribution/400 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/400 END:VEVENT BEGIN:VEVENT SUMMARY:STACEE Observations of 1ES 1218+304 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-403@cern.ch DESCRIPTION:Speakers: MUKHERJEE\, Reshmi (Barnard College\, Columbia Unive rsity)\nWe present the analysis and results of recent high-energy gamma-ra y\nobservations of the high energy-peaked BL Lac (HBL) object 1ES 1218+304 with\nthe Solar Tower Atmospheric Cherenkov Effect Experiment (STACEE). 1ES\n1218+304 is an X-ray bright HBL at a redshift\nz=0.182\, and has been predicted to emit high energy gamma rays above\n100 GeV\, detectable by g round-based Cherenkov telescopes. Recently\,\nthis source has been detecte d by MAGIC and VERITAS\, confirming these\npredictions. STACEE's sensitivi ty to astrophysical sources at energies\nabove 100 GeV allows it to explor e high energy sources such as X-ray\nbright active galaxies and gamma-ray bursts. We will present results\nfrom STACEE observations of 1ES 1218+304 in the 2006-2007 observing\nseason.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/39/contribution/403 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/403 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray burst observations with the H.E.S.S. Air Cherenkov array DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-466@cern.ch DESCRIPTION:Speakers: TAM\, Pak Hin (Landessternwarte\, ZAH\, University o f Heidelberg\, Germany)\nGamma-ray bursts (GRBs) are among the potential v ery-high-energy (VHE) gamma-ray\nsources. VHE emission from GRBs is predic ted by most GRB models. Despite its\ngenerally fast-fading nature in many wavebands\, the time evolution of any VHE\nradiation is still not clear. T he highest energy radiation from GRBs ever detected\nfirmly by any instrum ent was a 18 GeV photon coming from GRB 940217 detected with\nEGRET about 1.5 hour after the onset of the GRB. There is also a tentative detection\n using MILAGRITO of TeV excess events from GRB 970417a. In order to probe t he largely\nunexplored VHE spectra of GRBs\, a GRB observing program has b een set up by the\nH.E.S.S. collaboration. With the high sensitivity of th e H.E.S.S. array\, VHE flux\nlevels predicted by GRB models are well withi n reach. Extra-galactic background light\nabsorption is taken into account in cases where redshifts are known. We will present\nthe H.E.S.S. observa tions of and results from some of the reported GRB positions\nduring the p ast few years.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/cont ribution/466 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/466 END:VEVENT BEGIN:VEVENT SUMMARY:A search for VHE gamma-ray binaries in the H.E.S.S. Galactic Plane Scan DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-467@cern.ch DESCRIPTION:Speakers: Mr. DICKINSON\, Hugh (University of Durham)\nUtilisi ng the unprecedented TeV sky coverage of the H.E.S.S. galactic plane scan\ , we present the results of a search \nfor Very High Energy gamma-ray sour ces coincident with the positions of known X-ray binaries. Although no \n significant detections were obtained\, upper limits to the TeV flux from 36 microquasars and X-ray binaries were \nderived.\n\nhttps://indico.nucle ares.unam.mx/event/4/session/39/contribution/467 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/467 END:VEVENT BEGIN:VEVENT SUMMARY:VHE gamma-ray observations of starburst galaxies with H.E.S.S. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-468@cern.ch DESCRIPTION:Speakers: Mr. NEDBAL\, Dalibor (Institute of Particle and Nucl ear Physics\, Charles University\, V Holesovickach 2\, 180 00\, Prague 8\, Czech Republic)\nStarburst galaxies are characterized by extremely high s tar-formation rates and\, as a\nconsequence\, very high supernova rates. T hese rates\, as well as the gas density\, are\norders of magnitude higher than in our Galaxy. Such an environment contains both a\nhigh cosmic ray f lux and high density of target material for pp and inverse compton\nintera ctions. These objects are therefore viable candidates for observable level s of\nVHE gamma-ray mission. Several starburst galaxies have been observed with H.E.S.S.\nstereoscopic array of atmospheric-Cherenkov telescopes. Re sults of these observations\nwill be presented.\n\nhttps://indico.nucleare s.unam.mx/event/4/session/39/contribution/468 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/468 END:VEVENT BEGIN:VEVENT SUMMARY:A Very High Energy gamma-ray survey of X-ray binaries using H.E.S. S. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-469@cern.ch DESCRIPTION:Speakers: Mr. DICKINSON\, Hugh (University of Durham)\nSince t he discovery of TeV emission from the LS 5039/RX J1826.2-1450 binary syste m\, microquasars are an \nestablished class of Very High Energy gamma-ray sources. Nonetheless\, the current catalog of gamma-ray binaries \nremains somewhat limited\, with only three examples known. We present the results of a systematic search for TeV \nemission from known X-ray binaries with similar properties to LS 5039/RX J1826.2-1450 using the H.E.S.S. \nAtmosph eric Cherenkov Telescope Array. Resultant constraints of the physical syst em characteristics required for \nbright TeV emission in gamma-ray binary systems are also derived.\n\nhttps://indico.nucleares.unam.mx/event/4/sess ion/39/contribution/469 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/469 END:VEVENT BEGIN:VEVENT SUMMARY:A search for VHE emission from passive supermassive black holes DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-470@cern.ch DESCRIPTION:Speakers: Ms. PEDALETTI\, Giovanna (LSW-Landessternwarte Heide lberg\, Germany)\nJets of Active Galactic Nuclei (AGN) are established emi tters of Very High\nEnergy (VHE\; >100 GeV) gamma rays. In addition\, VHE radiation is expected to be emitted\nfrom the vicinity of Supermassive Bla ck Holes (SMBH) irrespective of their\nactivity state. Accreting SMBH rota te and generate a dipolar magnetic field. In the\nmagnetosphere of the spi nning black hole acceleration\nof particles can take place in the field ga ps. VHE emission from these particles is\nfeasible via leptonic or\nhadron ic processes. Therefore quiescent systems\, where the lack of a strong pho ton\nfield allows the VHE emission to escape\, are candidates for emission . \nThe HESS experiment has observed passive \nSMBH in nearby galaxies of different masses. We describe the observations and the\nresults of searche s for VHE emission from those SMBH.\nWe will discuss the constraints set b y those observations in the context of\ndifferent models predicting VHE em ission from passive SMBH.\n\nhttps://indico.nucleares.unam.mx/event/4/sess ion/39/contribution/470 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/470 END:VEVENT BEGIN:VEVENT SUMMARY:Observation of VHE gamma rays from HESS J1804-216 with CANGAROO-II I Telescopes DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-477@cern.ch DESCRIPTION:Speakers: Mr. HIGASHI\, Yusuke (Kyoto University)\nThe H.E.S.S . collaboration has reported the detection of gamma-ray emission from\neig ht new sources located in the Galactic Plane. HESS J1804-216 is one of the \nbrightest of them\, and its size and photon index make it one of the lar gest and\nsoftest sources. The H.E.S.S. collaboration proposed two possibl e counter parts\,\nyoung Vela-like pulsar B1800-21 and the SNR G8.7-0.1\, but it does not perfectly line\nup with them. Recently\, the discovery of new supernova remnant\, G8.31-0.09\, with\nradio observation was reported\ ,which located within the error circle of H.E.S.S.\, but\nmore compact in size. Suzaku deep observations discovered new two X-ray sources\,\ncentere d on the HESS J1804-216.Using SWIFT data found three faint X-ray sources i n\nthe region of HESS J1804-216\, one of them near its center.\n\n\nWe obs erved HESS J1804-216 with CANGAROO-III telescopes from May to July in 2006 .We\ndetected gamma-ray signals with more than 5 sigma level during an eff ective exposure\nof 74.8 hours. The differential flux is consistent with t hat of H.E.S.S.. Its\nmorphology is under study\, but it seems extended co mpared to our PSF.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/ contribution/477 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/477 END:VEVENT BEGIN:VEVENT SUMMARY:Search for very high energy gamma-ray emission from parts of the G ould belt with the H.E.S.S. ground based Cherenkov telescopes DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-485@cern.ch DESCRIPTION:Speakers: Dr. HORNS\, D. (Institute for Astronomy and Astrophy sics\, Univ. Tuebingen)\, Dr. ROWELL\, G. P. (School of Chemistry&Physics\ , University of Adelaide)\nThe Gould belt\, a well-known region of enhance d star formation in the solar\nneighborhood\, is observed to be an expandi ng rim with a diameter of a few\nhundred parsecs and a width of approximat ely 100 pc. Most of the nearby\nOB stellar associations and molecular clo uds are found to be\naligned with the Gould belt. With the high star form ation rate along the\nGould belt\, the local supernova rate during the las t few million years is\nbelieved to be three to four times larger than the Galactic average. Under the\nassumption that supernova remnants are effic ient accelerators of cosmic rays\,\nthe Gould belt and its environment sho uld show an increased cosmic ray density\nwith respect to the Galactic ave rage. The cosmic rays are expected to interact\nwith the dense molecular g as which results mainly in pi-meson production with\nsubsequent decay in g amma-rays and neutrinos. We have searched for gamma-ray\nemission from var ious nearby (d=100-200 pc) parts of the Gould belt\nwith the HESS Cherenko v telescopes. Results will be presented at the\nconference.\n\nhttps://ind ico.nucleares.unam.mx/event/4/session/39/contribution/485 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/485 END:VEVENT BEGIN:VEVENT SUMMARY:Discovery of the candidate pulsar wind nebulae HESS J1718-385 in v ery-high-energy gamma-rays DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-494@cern.ch DESCRIPTION:Speakers: CARRIGAN\, Svenja (Max-Planck-Insitut für Kernphysi k)\nMotivated by recent detections of pulsar wind nebulae in very-high-ene rgy (VHE) gamma\nrays\, a systematic search for VHE gamma-ray sources asso ciated with energetic pulsars\nwas performed\,\nusing data obtained with t he H.E.S.S. (High Energy Stereoscopic System) instrument.\nThe search for VHE gamma-ray sources near the pulsar PSR J1718-3825 revealed the new\nVHE gamma-ray source HESS J1718-385. We report on the results from the HESS d ata\nanalysis of this source and on possible associations with the pulsar and at other\nwavelengths. Furthermore we investigate the energy spectrum of HESS J1718-385 that\nshows a clear peak. This is only the second time a VHE gamma-ray spectral maximum\nfrom a cosmic source was observed\, the f irst being the Vela X PWN.\n\nhttps://indico.nucleares.unam.mx/event/4/ses sion/39/contribution/494 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/494 END:VEVENT BEGIN:VEVENT SUMMARY:H.E.S.S. observations of the supernova remnant RX J0852.0-4622: sh ell-type morphology and spectrum of a widely extended VHE gamma-ray source DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-504@cern.ch DESCRIPTION:Speakers: Mrs. LEMOINE-GOUMARD\, Marianne (CENBG - CNRS - IN2P 3)\nThe shell-type supernova remnant RX J0852.0-4622 was detected in 2004 and re-observed\nbetween December 2004 and May 2005 with the High Energy S tereoscopic System\n(H.E.S.S.)\, an array of four Imaging Cherenkov Telesc opes located in Namibia and\ndedicated to the observations of gamma-rays a bove 100 GeV. The angular resolution of\n< 0.1° and the large field of vi ew of H.E.S.S. (5° diameter) are well adapted to\nstudying the morphology of the object in very high energy gamma-rays\, which exhibits\na remarkab ly thin shell very similar to the features observed in the radio range and \nin X-rays. The spectral analysis of the source from 300 GeV to 20 TeV wi ll be\npresented. Finally\, the possible origins of the very high energy g amma-ray emission\n(Inverse Compton scattering by electrons or the decay o f neutral pions produced by\nproton interactions) will be discussed\, on t he basis of morphological and spectral\nfeatures obtained at different wav elengths.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribut ion/504 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/504 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma Ray Extragalactic Excess in Coma direction DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-507@cern.ch DESCRIPTION:Speakers: Mrs. DAVOUDIFAR\, Pantea (PhD student in Astropartic le Physics/Kerman University)\nBy using Egret data\, considering a gamma r ay flux for Virgo suppercluster and a \ndetailed analysis on our postulate s\, with a new methode a gamma ray flux in \nComa direction reasults. \nso me analogy between the works has made\, is done. \na flux index for Coma d irection gamma rays has resulted which is in the favor of \nour informatio n from Coma supercluster.\n\nhttps://indico.nucleares.unam.mx/event/4/sess ion/39/contribution/507 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/507 END:VEVENT BEGIN:VEVENT SUMMARY:On pulsed emission of TeV gamma rays from Crab Pulsar DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-510@cern.ch DESCRIPTION:Speakers: Prof. ACHARYA\, Bannanje Sripathi (Tata Institute of Fundamental Research)\nWe have observed Crab pulsar in the TeV energy ban d using the Pachmarhi Array of\nCherenkov Telescopes for about 90 hours. O ur observations span about 6 year period\nfrom 2000 to 2006. We have analy sed our data with using TEMPO package for analysing\npulsar data. We have searched for eveidence of pulsed emission of gamma rays from\ncrab pulsar using the contemporaneous radio pulsar parameters. We do not see any\nevid ence for the pulsed emission at a threshold energy of 825 GeV. We present our\nresults on the light curve in the TeV energy band and set an upper li mit on the time\naveraged flux of TeV gamma rays.\n\nhttps://indico.nuclea res.unam.mx/event/4/session/39/contribution/510 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/510 END:VEVENT BEGIN:VEVENT SUMMARY:Multiwavelength observations of PKS 2005-489 and H 2356-309 with H.E.S.S. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-511@cern.ch DESCRIPTION:Speakers: Dr. COSTAMANTE\, Luigi (Max-Planck-Institut fuer Ker nphysik)\nSince their discovery as VHE emitters by H.E.S.S. in 2004\,\nthe high-energy peaked BL Lacs PKS 2005-489 and H 2356-309 have been monitore d \nat VHE to study their flux and spectral variability.\nTo sample their SED\, several multiwavelength campaigns with X-ray satellites have been\np erformed\, showing important spectral changes. Here we present the result s \nof 3 years of H.E.S.S. observations together with multiwavelength dat a\, in the context \nof the SED evolution and in comparison with the histo rical states.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contr ibution/511 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/511 END:VEVENT BEGIN:VEVENT SUMMARY:Search for pulsed emission of TeV gamma rays from Geminga Pulsar DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-517@cern.ch DESCRIPTION:Speakers: Prof. ACHARYA\, Bannanje Sripathi (Tata Institute of Fundamental Research)\nPulsed emission of gamma/X rays from Geminga pulsa r were detected earlier at the\nperiod of ~237 msec using EGRET/ROSAT ins truments. However\, there are conflicting\nreports about emission of pulse d gamma rays from this pulsar at very high energies.\nWe have observed thi s source for about 56 hours using the PACT setup during the last\n6 years spanning c. 2000 to 2006. This pulsar was found to undergo a glitch durin g\n1996-97 from X-ray observations as reported by Jackson et al. We have a nalysed our\ndata by extrapolaing the post-glitch pulsar elements to our e poch of observation and\nusing the "TEMPO" package for calculating the pul sar phase of each event. In this\npaper we describe our data\, analysis pr ocedure and the results.\n\nhttps://indico.nucleares.unam.mx/event/4/sessi on/39/contribution/517 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/517 END:VEVENT BEGIN:VEVENT SUMMARY:Search for very high energy gamma rays from possible ultra-high en ergy cosmic sources with MAGIC telescop DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-522@cern.ch DESCRIPTION:Speakers: Dr. SHINOZAKI\, Kenji Shinozaki (Max-Planck-Institut e for Physics)\nThe origin of the ultra-high energy cosmic rays (UHECRs\; several times 10^19 eV and\nhigher) is an open question \nin the astropart icle physics. So far no astrophysical object has been still\nidentified a s UHECR sources within a limited \nsource distance of several tens of Mpc by the Grisen-Zatsepin-Kuzmin effect. In\naccelation of such particles\, the \nvery high energy (VHE) gamma-ray emission is expected as well. In o rder to search\nfor such VHE gamma-rays\, we \nobserved nearby galaxies us ing the the MAGIC Telescope. Three possible sources had\nbeen selected fro m the \ncatalogue in the direction close to the UHECR event triplet-cluste r found by the\nAGASA experiment. In the present \npaper\, we will report the result of our observation and discuss the possible\ninterpretaion of t he UHECR origin models.\n\nhttps://indico.nucleares.unam.mx/event/4/sessio n/39/contribution/522 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/522 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of the Crab Nebula with the Whipple 10 m Telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-543@cern.ch DESCRIPTION:Speakers: Mr. GRUBE\, Jeffrey (University of Leeds)\nThe Crab nebula was observed with the Whipple 10 m telescope from September\n2000 t o March 2006 for a total exposure of nearly 200 hours. Standard \ncalibrat ion and gamma-ray reconstruction methods applied to Whipple 10 m data \nar e described in detail. Measurements of the total and yearly Crab nebula \n flux and energy spectrum are compared with recent results from Cherenkov \ ntelescope systems. Contributing factors are discussed for the >20% system atic \nerror in flux estimation. The long-term performance is presented\, relevant to \nthe ongoing TeV blazar monitoring campaign with the Whipple 10 m.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/ 543 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/543 END:VEVENT BEGIN:VEVENT SUMMARY:A Search for energy dependent morphology from the cocoon of Vela X with H.E.S.S. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-544@cern.ch DESCRIPTION:Speakers: Dr. KHELIFI\, Bruno (LLR\, Ecole Polytechnique)\nThe Vela Supernova remnant is a large\, nearby remnant with a complex morphol ogy\,\ncontaining a bright pulsar at its centre. This pulsar has an associ ated pulsar wind\nnebula (PWN)\, gamma-ray emission from which was detecte d by the H.E.S.S.\ncollaboration at very high energies. As the Vela remnan t is the closest known PWN to\nus\, detailed study of the spectral and mor phological characteristics of the emission\nassociated with the PWN can sh ed considerable light on the acceleration of particles\nto very high energ ies in this category of object. This question will be addressed\nhere in t he context of H.E.S.S. observations of the Vela region.\n\nhttps://indico. nucleares.unam.mx/event/4/session/39/contribution/544 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/544 END:VEVENT BEGIN:VEVENT SUMMARY:MAGIC upper limits on the high energy emission from GRBs DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-569@cern.ch DESCRIPTION:Speakers: Dr. GARCZARCZYK\, Markus (Max-Planck-Institut fuer P hysik\, Muenchen - GERMANY)\nDuring its first observation cycle\, between April 2005 and March 2006\,\nthe MAGIC telescope was able to observe nine different GRB events\nsince their early beginning. Other observations have been performed\nduring the following months in its second observation cyc le. \nThe observations\, with an energy threshold spanning from 80 to 200 GeV\, \ndid not reveal any gamma-ray emission.\nThe computed upper limits are compatible with a\npower law extrapolation\, where intrinsic fluxes a re evaluated taking\ninto account the attenuation due to the scattering in the Metagalactic\nRadiation Field (MRF).\n\nhttps://indico.nucleares.unam .mx/event/4/session/39/contribution/569 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/569 END:VEVENT BEGIN:VEVENT SUMMARY:Search for Pulsed VHE Gamma-Ray Emission from Pulsars with H.E.S.S . DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-572@cern.ch DESCRIPTION:Speakers: Mr. FUESSLING\, Matthias (Humboldt University Berlin )\nWe present recent results of a search for pulsed very-high-energy (VHE) gamma-ray\nemission from pulsars using data taken with the High Energy St ereoscopic System\n(H.E.S.S.)\, an array of imaging Cherenkov telescopes l ocated in Namibia. The data\nset\, accumulated during four years of operat ion until 2006\, comprises observations of\neleven young pulsars\, selecte d according to their spin-down luminosity relative to\ndistance\, and two millisecond pulsars. No evidence for pulsed emission was found in\nany dat a set and differential upper limits on pulsed energy flux were derived\, a nd\ncompared to a variety of model predictions on VHE gamma-ray emission f rom the\nvicinity of pulsar magnetospheres.\n\nhttps://indico.nucleares.un am.mx/event/4/session/39/contribution/572 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/572 END:VEVENT BEGIN:VEVENT SUMMARY:Observation of AE Aquarii with the MAGIC telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-577@cern.ch DESCRIPTION:Speakers: Ms. SIDRO MARTIN\, Nuria (Institut de Fisica d'Altes Energies IFAE)\nIn August 2005\, MAGIC telescope observed the cataclysmic variable AE Aquarii.\nObservations were done during four consecutive nigh ts within the context of a\ncoordinated quasi-simultaneous multiwavelength campaign covering radio\, optical\, UV\,\nand X-ray range. We report on t he results of this campaign.\n\nhttps://indico.nucleares.unam.mx/event/4/s ession/39/contribution/577 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/577 END:VEVENT BEGIN:VEVENT SUMMARY:Search for very high energy gamma-ray emission with H.E.S.S. from the young and massive stellar cluster Westerlund 1 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-599@cern.ch DESCRIPTION:Speakers: Dr. HORNS\, Dieter (Institute for Astronomy and Astr ophysics\, Univ. Tuebingen)\nWesterlund 1 is a unique case of a massive yo ung cluster with at least 11\nWolf-Rayet stars driving strong stellar wind s. It is possible that various\nconfigurations of these stellar winds (wi nd-wind interaction\, superposition of\nstellar winds etc.) can convert a fraction of the kinetic energy of the wind\ninto accelerated particles. Observations of spatially extended non-thermal\nX-ray emission from the h ighly reddened and nearby stellar cluster\nWesterlund 1 suggest that indee d stars are able to accelerate at least\nelectrons to TeV energies which t hen produce X-ray synchrotron emission. We\nreport on the results of H.E.S .S. observations of the Westerlund 1 cluster.\n\nhttps://indico.nucleares. unam.mx/event/4/session/39/contribution/599 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/599 END:VEVENT BEGIN:VEVENT SUMMARY:Inverse-Compton emission from halos around stars DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-606@cern.ch DESCRIPTION:Speakers: Mrs. ORLANDO\, Elena (MPE Garching)\nInverse Compton scattering by relativistic electrons produces a major component of\nthe d iffuse emission from the Galaxy. The photon fields involved are the cosmic \nmicrowave background and the interstellar radiation field from stars and dust.\nCalculations of the inverse Compton distribution have usually assu med a smooth ISRF\,\nbut in fact a large part of the Galactic luminosity c omes from the most luminous\nstars which are rare. Therefore we expect the ISRF\, and hence the inverse Compton\nemission\, to be clumpy. We also sh ow that some of the most luminous stars may be \nvisible to GLAST.\n\nhttp s://indico.nucleares.unam.mx/event/4/session/39/contribution/606 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/606 END:VEVENT BEGIN:VEVENT SUMMARY:A deconcolution technique for VHE gamma-ray astronomy and its appl ication to the morphological study of RXJ1713.7-3946 from the H.E.S.S. obs ervations DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-615@cern.ch DESCRIPTION:Speakers: Dr. MAURIN\, Gilles (SPP/DSM/CEA)\nDeconvolution alg orithms have been used successfully for \noptimization/restoration/deblurr ing of astronomical images in a variety of \nwavelengths\, especially in t he optical band (e.g.\, for HST). We present here an \niterative Richardso n-Lucy type method designed for treatment of images \nobtained with the Hi gh Energy Stereoscopy System (H.E.S.S.) array of ground-\nbased gamma-ray telescopes. Its application to extended source images\, with \nsufficient signal\, yields refined details relevant for the study of correlations wit h \nother wavelengths.\n\nIn this paper\, this algorithm is presented\, ap plied to the supernova remnant \nshell of RXJ1713.7-3946 and then interpre ted in terms either of hadronic or \nleptonic origin of the observed VHE g amma-ray emission.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/ contribution/615 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/615 END:VEVENT BEGIN:VEVENT SUMMARY:Long Duration Variability and Spectrum of Mrk 421 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-665@cern.ch DESCRIPTION:Speakers: Dr. SMITH\, Andrew (University of Maryland\, College Park)\nActive Galaxies such as Mrk 421 have been shown to be highly varia ble\nat all time scales. Atmospheric Cherenkov Telescopes (ACTs) have\nexc ellent instantaneous sensitivity and have observed short bright\nflares fr om Mrk 421. However\, long duration variability is difficult\nto monitor w ith ACTs due to their intermittent exposure. Milagro\,\nin contrast\, moni tors Mrk 421 with daily observations. While Milagro\nlacks the sensitivity to detect short duration flares\, it is capable\nof long duration monitor ing of the total flux of Mrk 421 on time\nscales from months to years. In this paper we present the long\nduration variability and total fluence of Mrk 421 using 6 years of\ndata from Milagro. We will also report the aver age spectrum above \n1 TeV.\n\nhttps://indico.nucleares.unam.mx/event/4/se ssion/39/contribution/665 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/665 END:VEVENT BEGIN:VEVENT SUMMARY:A Variability Study of Localized Sources Discovered by Milagro in the Galactic Plane DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-669@cern.ch DESCRIPTION:Speakers: WALKER\, Gary (Los Alamos National Laboratory)\nMila gro is a TeV gamma-ray observatory with a ~2 sr field of view and a >90% d uty\nfactor. A recent survey at 12 TeV of the Galactic Plane by Milagro h as discovered\nthree new sources\, along with four promising source candid ates. Each of the new\nsources and most of the candidates have likely cou nterparts in the EGRET GeV catalog\,\nsome of which are possibly associate d with pulsar wind nebulae (PWN) or supernova\nremnants (SNR). While such sources are not expected to be variable\, the\nidentification is not cert ain\, and so an examination of the variability may help to\ndifferentiate between steady sources like PWN and SNR\, and variable Galactic sources\ns uch as microquasars and x-ray binaries. A systematic search for variabili ty has\nbeen conducted on the Milagro sources and source candidates using time scales ranging\nfrom one day to two years. The results of this searc h\, along with some simple\nspectral studies\, will be presented.\n\nhttps ://indico.nucleares.unam.mx/event/4/session/39/contribution/669 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/669 END:VEVENT BEGIN:VEVENT SUMMARY:The effect of expansion on high-energy emission from AGN jets DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-682@cern.ch DESCRIPTION:Speakers: Prof. POHL\, Martin (Dept. of Physics and Astronomy\ , Iowa State University)\nWe present a detailed study of the impact\nof je t expansion on the emission properties of blazars\, in particular\ntheir g amma-ray lightcurves\, based on the notion that the radiation is produced in an\nemission zone that is travelling down the jet.\nUsing analytical es timates and numerical studies with a particular model\nof particle energiz ation\, we conclude that AGN jets must be very well\ncollimated with openi ng angles smaller than about 1 mrad\, if the emission\nseen over a few day s is caused by an emission zone that travels down the jet.\nOur findings s uggest that either this condition is not met or an unknown\nvery efficient mechanism collimates the jets of blazars.\n\nhttps://indico.nucleares.una m.mx/event/4/session/39/contribution/682 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/682 END:VEVENT BEGIN:VEVENT SUMMARY:Detecting a unique EBL signature with TeV Gamma Rays DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-683@cern.ch DESCRIPTION:Speakers: Mr. IMRAN\, Asif (Iowa State University)\nWe discuss the prospect of detecting a spectral break in the gamma-ray \nspectra of blazars due to the extragalactic background light in the near \nto mid-IR. A measurable break in the TeV spectra could arise from the \ndrop in the EBL density above ~ 1um. This change in the spectral index \nis mediated by the ratio of the near to mid-IR density of EBL. A detection \nof such a spectral feature could be understood as an unambiguous proof of \nEBL abs orption\, whereas the non-detection could be interpreted as a constraint \ nto the EBL spectrum. We present results from simulations of blazars at a range \nof redshifts and discuss the sensitivity of current TeV telescope s for detecting\na break.\n\nhttps://indico.nucleares.unam.mx/event/4/sess ion/39/contribution/683 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/683 END:VEVENT BEGIN:VEVENT SUMMARY:Observation of the binary system LSI +61 303 in Very High Energy G amma-Rays with VERITAS DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-700@cern.ch DESCRIPTION:Speakers: Dr. MAIER\, Gernot (McGill University\, Montreal)\nT he high mass x-ray binary LSI +61 303 was observed for several months in 2 006 and\n2007 by VERITAS\, an array of several imaging Cherenkov telescope s located at the Fred\nLawrence Whipple Observatory in southern Arizona. The unusual system of a black hole\nor neutron star orbiting a Be star pro ves to be an efficient particle accelerator.\nHere we present the detectio n of LSI +61 303 in very high energy gamma-rays during\nseveral orbital cy cles. The high sensitivity of VERITAS allows the determination of\nfluxes and energy spectra at different phases of the orbit\, revealing the high f lux\nvariability of this interesting source.\n\nhttps://indico.nucleares.u nam.mx/event/4/session/39/contribution/700 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/700 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray albedo of the moon DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-739@cern.ch DESCRIPTION:Speakers: Dr. MOSKALENKO\, Igor (Stanford University)\nWe calc ulate the production of gamma rays by cosmic ray interactions with the lun ar\nsurface. We show that the major contribution comes from neutral pions produced in\nproton interactions with the nuclei in the lunar surface whil e the electron\nbremsstrahlung is a minor component contributing mostly at low energies. Our\ncalculations show a good agreement with the EGRET obse rvations of the lunar albedo.\nWe are extending our predicted spectrum up to 300 GeV to cover the energy range\naccessible by the GLAST.\n\nhttps:// indico.nucleares.unam.mx/event/4/session/39/contribution/739 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/739 END:VEVENT BEGIN:VEVENT SUMMARY:The TeV Energy Spectrum of Mrk 421 Measured in a High Flaring Stat e DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-748@cern.ch DESCRIPTION:Speakers: Dr. KONOPELKO\, Alexander (Purdue University)\nThe B L Lac object (blazar) Mrk 421 was observed in a high emission state in Apr il\n2005 with the Whipple 10 m telescope for about 24.5 hrs. The measured gamma-ray rate\nvaried substantially over the range of 4 to 10 γ’s/min and eventually exceeded the\nsteady γ-ray rate of the Crab Nebula (the st andard candle) by a factor of 3. The\noverall significance of the gamma-ra y signal reached 50σ and the total number of\nexcess events was more than 10\,000. The Mrk 421 light curve does not display any\ndistinct variabili ty pattern. This unique Mrk 421 outburst enabled the measurement of\na hig h precision very high-energy γ-ray spectrum. The spectrum extends beyond 10 TeV\nand severely constrains the spectral energy distribution of the ex tra-galactic\nbackground light.\n\nhttps://indico.nucleares.unam.mx/event/ 4/session/39/contribution/748 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/748 END:VEVENT BEGIN:VEVENT SUMMARY:A Monte Carlo study of the irreducible background in the EGRET ins trument DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-762@cern.ch DESCRIPTION:Speakers: Dr. PORTER\, Troy (University of California\, Santa Cruz)\nThe diffuse extragalactic gamma-ray background (EGRB) has been deri ved by various\ngroups from observations by the EGRET instrument on CGRO. The derived\nEGRB consists of gamma-rays that may come from true astrophys ical components\, such\nas from unresolved extragalactic point sources (bl azars\, normal galaxies\, etc.) and\ntruly diffuse signals from the Galaxy and inverse Compton scattering on the solar\nradiation\nfield\, and an ir reducible instrumental background due to\ngamma rays produced by cosmic-ra y interactions in the EGRET instrument and\nCGRO spacecraft. Using a detai led Monte Carlo model of the EGRET instrument and\nCGRO\, we have investig ated the magnitude of the irreducible\ninstrumental background and have de veloped an extension to the effective\narea determination. We present the results of our study and its effect\non current estimates of the EGRB.\n\n https://indico.nucleares.unam.mx/event/4/session/39/contribution/762 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/762 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma Rays from Neutrino Pulsars DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-816@cern.ch DESCRIPTION:Speakers: Dr. BHADRA\, Arunava (University of North Bengal)\nY oung rotating neutron stars (pulsars) are considered as strong sources of TeV \nmuon neutrinos\, which are produced through the delta resonance in p roton-\ngamma photon interactions. In this presentation it is shown that t he observed \nupper limit of gamma ray fluxes from the young pulsars put l imit on fluxes of \nmuon neutrinos from the sources.\n\nhttps://indico.nuc leares.unam.mx/event/4/session/39/contribution/816 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/816 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of the pulsar PSR B1951+32 with the Solar Tower Atmos pheric Cherenkov Effect Experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-830@cern.ch DESCRIPTION:Speakers: KILDEA\, John (Department of Physics\, McGill Univer sity\, Montreal\, QC H3A\n2T8\, Canada (Current address: Fred Lawrence Whi pple Observatory\,\nHarvard-Smithsonian Center for Astrophysics\, Amado\, AZ 85645))\nWe present the analysis and results of 12.5 hours of high-ener gy\ngamma-ray observations of the EGRET-detected pulsar PSR B1951+32 using \nthe Solar Tower Atmospheric Cherenkov Effect Experiment (STACEE).\nSTACE E is an atmospheric Cherenkov detector\, in Albuquerque\, New\nMexico\, th at detects cosmic gamma rays using the shower front-sampling\ntechnique. S TACEE's sensitivity to astrophysical sources at energies\naround 100 GeV a llows it to investigate emission from gamma-ray\npulsars with expected pul sed emission cutoffs below 100 GeV. We\ndiscuss the observations and analy sis of STACEE's PSR 1951+32 data\,\naccumulated during the 2005 and 2006 o bserving seasons\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/co ntribution/830 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/830 END:VEVENT BEGIN:VEVENT SUMMARY:Search for pulsed multi-TeV gamma rays from the Crab pulsar with t he Tibet III air shower array DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-844@cern.ch DESCRIPTION:Speakers: Prof. HIBINO\, Kinya (Kanagawa University)\nWe obser ve the steady emission of multi-TeV gamma rays from \nthe crab nebula from observation of the Tibet air shower array.\nIn this conference\, we will also report that no evidence for long-term\nvariability of flux intensity from the Crab Nebula is found.\nIn this article\, we will present the resu lt that a search for pulsed \nmulti-TeV gamma rays emission from crab puls ar using data taken \nwith the Tibet III air shower array.\n\nhttps://indi co.nucleares.unam.mx/event/4/session/39/contribution/844 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/844 END:VEVENT BEGIN:VEVENT SUMMARY:Active Atmospheric Calibration for H.E.S.S. Applied to PKS 2155-30 4 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-853@cern.ch DESCRIPTION:Speakers: Dr. CHADWICK\, Paula (University of Durham)\nUsing d ata derived from the H.E.S.S. telescope system and the LIDAR facility on s ite\,\na method of correcting for changing atmospheric quality based on co smic-ray\nparameters is presented. The method was applied to data from the active galactic\nnucleus PKS 2155-304\, taken during August and September 2004 when the quality of the\natmosphere at the site was highly variable . Corrected and uncorrected fluxes are\nshown\, and the method is discusse d as a first step towards a more complete\natmospheric calibration.\n\nhtt ps://indico.nucleares.unam.mx/event/4/session/39/contribution/853 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/853 END:VEVENT BEGIN:VEVENT SUMMARY:H.E.S.S. sources possibly associated with massive star clusters DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-873@cern.ch DESCRIPTION:Speakers: Dr. MARCOWITH\, Alexandre (LPTA\, Université Montpe llier 2\, CNRS/IN2P3\, Montpellier\, France)\, Dr. KOMIN\, Nukri (LPTA\, U niversité Montpellier 2\, CNRS/IN2P3\, Montpellier\, France)\nIn view of the discovery of HESS J1023-575 (discussed in a separate \npresentation)\, we\nexamine other very high energy (VHE) gamma-ray\nsources possibly asso ciated with massive star clusters. Particle acceleration in\nmassive star forming regions can proceed at\nthe interface of two interacting winds or result from a collective process\; \nmultiple\nshock acceleration or MHD t urbulence. \nThe gamma-ray emission can either take place in the shell at the edge of the\nsuperbubble blown by the winds and multiple supernova exp losions. \nNon-thermal radiation from the shell structure then trace the i nteraction of\nenergetic particles (ions and/or electrons) with the \nsurr ounding interstellar matter. In particular\, HESS J1837-069 is spatially\n coincident with a recently discovered very massive star cluster. \nWe disc uss the VHE gamma-ray data resulting from H.E.S.S. observations on \nthis or\nother possible such associations. We consider data in other \nwaveleng th domains\, in particular in X-rays\, and examine the available \nevidenc e that\nthe VHE emission could originate in particles accelerated by\nthe above-mentioned mechanisms in massive star clusters.\n\nhttps://indico.nuc leares.unam.mx/event/4/session/39/contribution/873 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/873 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray emission associated with the Cluster-scale AGN Outbursts in the Hydra A system DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-882@cern.ch DESCRIPTION:Speakers: DOMAINKO\, Wilfried (Max-Planck-Institut für Kernph ysik\, Heidelberg\, Germany)\nRecent observations have revealed the existe nce of an enormously\nenergetic ~ 10^61 erg AGN outburst in the Hydra A cl uster of galaxies.\nThis outburst has produced cavities in the\nintra-clus ter medium\, apparently supported by pressure from\ncosmic rays. Here we a rgue that these particles are very\nlikely protons and nuclei. For a plaus ible\nspatial distribution of the target gas\, based on observations and\n hydrodynamical simulations\, we show that the pi0-decay gamma-rays\nfrom t hese cosmic-rays could be detectable with the H.E.S.S.experiment.\n\nhttps ://indico.nucleares.unam.mx/event/4/session/39/contribution/882 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/882 END:VEVENT BEGIN:VEVENT SUMMARY:The TeV-$\\gamma-radiation from the Galactic center observed by H. E.S.S. and a possible dark matter interpretation DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-886@cern.ch DESCRIPTION:Speakers: RIPKEN\, Joachim (Institut fuer Experimentalphysik\, Universitaet Hamburg)\nWith H.E.S.S.\, a system of four Cherencov telesco pes\, a signal of very high energy\nTeV-$\\gamma$-radiation from the direc tion of the Galactic center has been detected.\nThe interpretation of the signal due to dark matter annihilations is discussed and\nlimits on the an nihilation cross sections and density profiles are given. This is an\nupda te of earlier publications including recent observations of the Galactic c enter\nregion with H.E.S.S.\n\nhttps://indico.nucleares.unam.mx/event/4/se ssion/39/contribution/886 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/886 END:VEVENT BEGIN:VEVENT SUMMARY:Is the unidentified source HESS J1303-631 a dark matter clump? DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-890@cern.ch DESCRIPTION:Speakers: RIPKEN\, Joachim (Institut fuer Experimentalphysik\, Universitaet Hamburg)\nThe H.E.S.S. collaboration found several so far un identified sources of\nTeV-gamma-radiation without any known counterpart i n other wavelengths. One of those\nis HESS J1303-631 which was serendipiti ously found in the same field of view of PSR\nB1259-63 / SS 2883. The poss ibility that HESS J1303-631 is a clump of dark matter is\ndiscussed.\n\nht tps://indico.nucleares.unam.mx/event/4/session/39/contribution/890 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/890 END:VEVENT BEGIN:VEVENT SUMMARY:The Spectral Index Distribution of Blazars: Prospects for GLAST DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-894@cern.ch DESCRIPTION:Speakers: Ms. VENTERS\, Tonia (Department of Astronomy and Ast rophysics\, The University of Chicago)\nThe intrinsic distribution of spec tral indices in GeV energies of gamma-ray–loud\nblazars is a critical in put in determining the spectral shape of the unresolved\nblazar contributi on to the diffuse extragalactic gamma-ray background\, as well as an\nimpo rtant test of blazar emission theories. We present a maximum-likelihood me thod of\ndetermining the intrinsic spectral index distribution (ISID) of a population of\ngamma-ray emitters which accounts for error in measurement of individual spectral\nindices\, and we apply it to the case of Energeti c Gamma-Ray Experiment Telescope \n(EGRET) blazars. We find that the most likely Gaussian ISID for EGRET blazars has a\nmean of 2. 27 and a standard deviation of 0. 20. The most likely ISID is\nsignificantly narrower than one would conclude if measurement error had not been\ntaken into account. This in turn implies that the curvature of the unresolved blazar\nspectrum is expected to be relatively small. We additionally find some indication\ nthat FSRQs and BL Lacs may have different ISIDs (with BL Lacs being harde r). We also\ntest for spectral index hardening associated with blazar vari ability\, and for\ndependence of the spectral index on luminosity or redsh ift\, and we find no evidence\nfor any of these effects. Finally\, we prod uce simulated Gamma-ray Large Area Space\nTelescope (GLAST) spectral index datasets and perform the same analyses. We find that\nwith the improved s tatistics due to the much larger number of resolvable blazars\,\nGLAST dat a will help us determine the ISIDs with much improved accuracy. Should any \ndifference exist between the ISIDs of BL Lacs and FSRQs or between the I SIDs of\nblazars in the quiescent and flaring states\, GLAST data will be adequate to separate\nthese ISIDs at a significance better than 3 sigma.\n \nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/894 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/894 END:VEVENT BEGIN:VEVENT SUMMARY:First simultaneous multiwavelength observation for the BL Lac obje ct\, 1ES1959+650 in a low state with MAGIC and Suzaku/Swift DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-911@cern.ch DESCRIPTION:Speakers: Mr. HAYASHIDA\, Masaaki (Max-Planck-Institut fuer Ph ysik\, D-80805 Muenchen\, Germany)\nMultiwavelength observations provide v aluable information to estimate the physical parameters of AGN emission \n models. Since blazars show a strong flux variability\, it is important to derive these physical parameters in the \ndifferent states in order to und erstand the acceleration mechanism and in the jet. So far simultaneous bla zar \nobservations in X-rays and VHE gamma-rays could only be performed in their high states due to the limited \nsensitivity of conventional Imagin g Atmospheric Cherenkov telescopes (IACTs). Recently\, new IACTs\, like th e \nMAGIC telescope\, have made it possible to measure the flux within som e hours of observation even in the low \nstate of certain blazars.\nIn May 2006 we conducted simultaneous multiwavelength observations for the BL La c object\, 1ES1959+650 in \na low state with the MAGIC telescope\, togethe r with the X-ray satellites Suzaku and Swift. Swift also provided \nmulti- filter photometry in the UV-optical band. The source was clearly detected in all energy bands\, from the \noptical to TeV energies. 1ES1959+650 is a n interesting TeV BL Lac object that showed an “orphan” flare in VHE \ ngamma-rays in 2002 which can not be explained with a simple one-zone SSC model. In this presentation\, the\nresults from the MAGIC-Suzaku-Swift mul tiwavelength observations will be reported.\n\nhttps://indico.nucleares.un am.mx/event/4/session/39/contribution/911 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/911 END:VEVENT BEGIN:VEVENT SUMMARY:GRB without hard to soft evolution and high energy emission DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-926@cern.ch DESCRIPTION:Speakers: Dr. MIROSHNICHENKO\, Leonid (Instituto de Geofisica\ , UNAM\, Mexico)\nSpectral properties of some GRB with presence of high en ergy component \nwithin RHESSI\, HETE and \nSWIFT t90 intervals are discus sed. In some cases the temporal profiles of GRB \nin low and high \nenerg y bands are similar but in some cases they are different and maxima are \n not coincide. \nWe found the same type GRB in CGRO database too – for ex ample\, GRB930131. \nMoreover\, for some GRB\nfrom CGRO and AVS-F database in which spectra contradict Band model high \nenergy component are presen t the hard to soft spectral evolution is absent – \nfor example\, for GR B930506 (t90=22.144±0.091) Epeak on burst begin less \nthan Epeak during other burst parts - Epeak(1-3s)=540±58 keV\, \nEpeak(3-7s)=1064±38 keV\, Epeak(7-23s)=850±32 keV. All GRB with such \nproperties are long GRB for standatd BATSE and other classifications including \ntaking in account bu rst hardness ones.\nWe suppose that such type GRB consist a new subgroup o f long GRB.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contrib ution/926 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/926 END:VEVENT BEGIN:VEVENT SUMMARY:Long term monitoring of bright TeV Blazars with the MAGIC telescop e DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-928@cern.ch DESCRIPTION:Speakers: Dr. GOEBEL\, Florian (Max-Planck-Institute for Physi cs\, Munich)\nThe MAGIC telescope has performed long term monitoring obser vations of\nthe bright TeV Blazars Mrk421\, Mrk501 and 1ES1959+650. Up to 40\nobservations\, 30 minutes each have been performed for each source\nev enly distributed over the observable period of the year. The\nsensitivity of MAGIC is sufficient to establish a flux level of 25% of\nthe Crab flux for each measurement. These observations are well suited\nto trigger multi wavelength ToO observations\, and the overall collected\ndata allows an un biased study of the flaring statistics of the\nobserved AGNs.\n\nhttps://i ndico.nucleares.unam.mx/event/4/session/39/contribution/928 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/928 END:VEVENT BEGIN:VEVENT SUMMARY:Break in the Very High Energy Spectrum of PG 1553+113: New Upper L imit on Its Redshift? DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-940@cern.ch DESCRIPTION:Speakers: Mr. MAZIN\, Daniel (Max-Planck-Institute for Physics \, Munich)\nPG 1553+113 is a known BL Lac object\, newly detected in the G eVTeV energy\nrange by H.E.S.S. and MAGIC. The redshift of this source is unknown and a\nlower limit of z>0.09 was recently estimated. The very high energy (VHE)\nspectrum of PG 1553+113 is attenuated due to the absorption by the\nlow-energy photon field of the extragalactic background light (EB L). Here\nwe correct the combined H.E.S.S. and MAGIC spectrum of PG 1553+1 13 for\nthis absorption assuming a minimum density of the evolving EBL. We use an\nargument that the intrinsic photon index cannot be harder than Ga mma=1.5\nand derive an upper limit on the redshift of z<0.69. Moreover\, w e find\nthat a redshift above z=0.42 implies a possible break of the intri nsic\nspectrum at 200 GeV. Assuming that such a break is absent\, we deriv e a\nmuch stronger upper limit of z<0.42. Alternatively\, this break might be\nattributed to an additional emission component in the jet of PG 1553+ 113.\nThis would be the first evidence for a second component detected in the\nVHE spectrum of a blazar.\n\nhttps://indico.nucleares.unam.mx/event/4 /session/39/contribution/940 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/940 END:VEVENT BEGIN:VEVENT SUMMARY:Seven-year observation of multi-TeV gamma rays from the Crab Nebul a with the Tibet air shower array DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-954@cern.ch DESCRIPTION:Speakers: Dr. TAKITA\, Masato (Institute for Cosmic Ray Resear ch\, University of Tokyo)\nThe Tibet air shower array\, consisting of 533 scintillation counters\nwhich are placed in a lattice with 7.5 m spacing\, has been in\noperation since 1999 at Yangbajing in Tibet\, China at an al titude of\n4\,300 m above sea level. In this conference\, we will report on the\ncontinuous observation of multi-TeV gamma rays from the Crab Nebul a\nwith the Tibet air shower array. We found no evidence for time\nvariab ility of flux intensity from the Crab Nebula at multi-TeV\nenergies. Also the gamma-ray energy spectrum of the Crab Nebula is\nconsistent with our previous results and other observations by the\natmospheric imaging Cheren kov telescopes. In addition\, we will discuss\nour systematic errors\, su ch as the stability in pointing accuracy\,\nangular resolution and the abs olute energy scale error\, which have\nbeen checked by monitoring the Moon 's shadow in the cosmic-ray flux.\n\nhttps://indico.nucleares.unam.mx/even t/4/session/39/contribution/954 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/954 END:VEVENT BEGIN:VEVENT SUMMARY:The trigger unit of the space borne gamma-ray burst telescope ECLA IRs DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-979@cern.ch DESCRIPTION:Speakers: Dr. SCHANNE\, Stéphane (CEA Saclay\, DAPNIA)\nGamma -ray bursts (GRB) sign energetic explosions in the Universe\, occurring at \ncosmological distances. Multi-wavelength observations of GRB allow to st udy their\nproperties and to use them as cosmological tools.\n In 2011 th e space borne gamma-ray telescope ECLAIRs is expected to provide accurate\ nGRB localizations on the sky in near real-time\, necessary for ground-bas ed follow-up\nobservations. Led by CEA Saclay\, France\, the project is cu rrently in its technical\ndesign phase.\n ECLAIRs is optimized to detect highly red-shifted GRB thanks to a 4 keV low energy\nthreshold. A coded ma sk telescope with a 1024 cm2 detection plane of 80x80 CdTe\npixels permane ntly observes a 2 sr sky field. The on-board trigger detects GRB using\nco unt-rate increase monitors on multiple timescales and cyclic images. It co mputes\nsky images in the 4-50 keV energy range by de-convolving detector plane images with\nthe mask pattern and localizes newly detected sources w ith <10 arcmin accuracy. While\nindividual GRB photons are available hours later\, GRB alerts are transmitted over a\nVHF network within seconds to ground\, in particular to robotic follow-up telescopes\,\nwhich refine GRB localizations to the level needed by large spectroscopic telescopes.\n T his paper describes the ECLAIRs concept\, with emphasis on the GRB trigger ing scheme.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contrib ution/979 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/979 END:VEVENT BEGIN:VEVENT SUMMARY:Search for variability and QPO activity from Sgr A* from H.E.S.S. observations DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1021@cern.ch DESCRIPTION:Speakers: Prof. DE JAGER\, Ocker (North-West University\, Sout h Africa)\nOne interesting possibility is that the galactic center source HESS J1745-290\nis associated with the galactic center source Sgr A*\, the galactic center black \nhole\, in which case we may expect variability as seen in IR and X-rays\, with\nQPO frequencies predicted by Aschenbach et al. (2004). We will present the\nresults of a search for such variable sig natures using HESS observations of this\nsource.\n\nhttps://indico.nuclear es.unam.mx/event/4/session/39/contribution/1021 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1021 END:VEVENT BEGIN:VEVENT SUMMARY:Search for Gamma Ray Bursts with the ARGO-YBJ detector. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1034@cern.ch DESCRIPTION:Speakers: Dr. VALLANIA\, Piero (IFSI-INAF and INFN\, Torino)\n ARGO-YBJ is a "full coverage" air shower detector consisting of a 6700 m^2 \ncarpet of Resistive Plate Chambers\, located at Yangbajing (Tibet\, P.R . China\, \n4300 m a.s.l.).\nIts large field of view (~2 sr) makes ARGO-YB J particularly suitable to \ndetect unpredictable and short duration event s such as Gamma Ray Bursts.\nARGO-YBJ can search for GRBs using two detect ion techniques: the "Scaler \nMode"\, \nworking in the GeV energy range\, and the "Shower Mode"\, at energies above \na few hundreds of GeV. \nThe results of the search for emission from GRBs in coincidence with satellit e\ndetections are presented.\n\nhttps://indico.nucleares.unam.mx/event/4/s ession/39/contribution/1034 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1034 END:VEVENT BEGIN:VEVENT SUMMARY:Search for point sources of gamma rays using GRAPES-3 experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1054@cern.ch DESCRIPTION:Speakers: Mr. OSHIMA\, Akitoshi (Osaka City University in Japa n)\nThe GRAPES-3 experiment observes extensive air showers using a high-de nsity array of\nscintillators and a large area tracking muon detector. The array consists of 300\nscintillation detectors (each 1m^2 in area) and 16 modules of muon detectors having a\ntotal area of 560m^2. We have develop ed a new method of detector time offset\ncorrection to \nimprove the angul ar resolution of the array by using shower data. We have been able\nto det ermine the angular resolution of the array using the shadow of Sun and Moo n by\nusing this method. The showers due to charged cosmic rays are identi fied by measuring\ntheir muon content using large area muon detector. Here we report on the status of\nthe search for gamma rays from the `standard candle' CRAB nebula using the GRAPES-3 data.\n\nhttps://indico.nucleares.u nam.mx/event/4/session/39/contribution/1054 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1054 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of the Draco Dwarf Spheroidal Galaxy with STACEE DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1076@cern.ch DESCRIPTION:Speakers: COVAULT\, C. E. (Department of Physics\, Case Wester n Reserve University\, Cleveland\, OH 44106 USA)\nThe Draco dwarf spheroid al galaxy has garnered interest as a possible source for the\nindirect det ection of dark matter. Draco has a large mass-to-light ratio\, and its\nr elative proximity to the Earth provides favorable conditions for the produ ction of\ndetectable gamma-rays from dark matter self-annihilation in the galaxy's core. The\nSolar Tower Atmospheric Cherenkov Effect Experiment ( STACEE) is an air-shower\nCherenkov telescope located in Albuquerque\, NM capable of detecting gamma-rays with\nan energy threshold of about 250 GeV for this source. We present the results of the\nSTACEE observations of Dr aco during the 2005-2006 observing season totaling\napproximately 10 hours of livetime after cuts.\n\nhttps://indico.nucleares.unam.mx/event/4/sessi on/39/contribution/1076 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1076 END:VEVENT BEGIN:VEVENT SUMMARY:A New Analysis of the EGRET Effective Area and Implications for th e Galactic Diffuse Gamma-Ray Flux DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1116@cern.ch DESCRIPTION:Speakers: Prof. JOHNSON\, Robert (U.C. Santa Cruz)\nThe EGRET experiment onboard the Compton Gamma-ray Observatory have provided \nthe m ost precise measurements of the gamma-ray sky to date. EGRET measurements of \ndiffuse emission across the sky show an excess above 1 GeV. This “ GeV excess” has \nbeen a topic of great debate and interest since its or iginal discovery by Hunter et al. in \n1997. We have modified the GLAST s imulation and reconstruction software to model the \nEGRET instrument. Thi s detailed modeling has allowed us to explore the parameters of the \nEGRE T instrument\, in both its beam-test configuration and in-orbit on CGRO\, in greater \ndetail than has previously been published. We have found that the GeV excess is \nsignificantly increased when previously unaccounted f or instrumental effects are \nconsidered. We will present a new measureme nt of diffuse gamma-ray emission in the \ninner Galaxy.\n\nhttps://indico. nucleares.unam.mx/event/4/session/39/contribution/1116 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1116 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of the Giant Radio Galaxy M87 in the 100 GeV Energy D omain with the MAGIC Telescope DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1120@cern.ch DESCRIPTION:Speakers: Mr. MEYER\, Markus (Institut für Theoretische Physi k und Astrophysik\, Universität Würzburg)\nSince 2005 the giant radio ga laxy M87 has been observed in the 100 GeV energy domain\nwith the MAGIC Te lescope. Results from the analysis of those observations will be\npresente d.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/112 0 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1120 END:VEVENT BEGIN:VEVENT SUMMARY:Detecting GRBs and SNe with IceCube and follow-up observations DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1132@cern.ch DESCRIPTION:Speakers: Dr. KOWALSKI\, Marek (Humboldt-Unversity\, Berlin)\n We present a summary of AMANDA results obtained in searches for neutrinos from Gamma-Ray Bursts (GRBs). \nUsing simulations\, we show how the IceCub e detector\, which is currently being constructed at the South Pole\, will \nimprove the sensitivity of the search. In order to improve the prospec ts for detections of gamma-ray dark bursts\, as \nwell as core collapse Su pernovae (SNe)\, we discuss a novel follow-up scheme of high energy neutr ino events from \nIceCube. Triggered by neutrinos events from IceCube\, a network of small optical telescopes is meant to monitor the \nsky for SNe rising lightcurves and GRB afterglows. The observing program is outlined and its status discussed. Using \na realistic configuration of optical te lescopes\, we estimate the achievable gain in sensitivity of IceCube for d etections \nof neutrinos from GRBs and SNe.\n\nhttps://indico.nucleares.un am.mx/event/4/session/39/contribution/1132 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1132 END:VEVENT BEGIN:VEVENT SUMMARY:Radiation from internal shocks in magnetized flows DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1141@cern.ch DESCRIPTION:Speakers: Dr. MASTICHIADIS\, Apostolos (Physics Dpt\, Universi ty of Athens)\nWe consider the internal shock formation in magnetized outf lows and we\nexamine the plastic collision between such relativistic blobs taking\ninto account a possible dissipation of magnetic flux. We find th at\nafter the collision a large amount of energy is released in\nthermal f orm and consequently we assume that this is transferred\ninto protons whic h obtain a relativistic\nMaxwellian distribution. The relativistic thermal proton plasma is dense\nenough to suffer substantial energy losses throug h proton-proton\ninteractions and thus to transfer its initial energy into \nphotons\, electron-positron pairs and neutrinos. We estimate the radiate d\nspectrum by following the evolution of protons\, electrons and photons as they\ninteract with each other and with the magnetic field as well.\n\n https://indico.nucleares.unam.mx/event/4/session/39/contribution/1141 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1141 END:VEVENT BEGIN:VEVENT SUMMARY:Upper Limits from H.E.S.S. Observations of AGN in 2005-2007 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1205@cern.ch DESCRIPTION:Speakers: Dr. BENBOW\, Wystan (Max Planck Institut fuer Kernph ysik)\nA sample of selected active galactic nuclei (AGN) was observed \nfr om 2005 to 2007 with the High Energy Stereoscopic System (H.E.S.S.)\, \nan array of imaging atmospheric-Cherenkov telescopes in Namibia. \nSignifica nt detections for some of these objects are reported\nelsewhere. Integral flux upper limits for the other candidate \nvery-high-energy (VHE\; >100 GeV) gamma-ray emitters will be presented.\n\nhttps://indico.nucleares.un am.mx/event/4/session/39/contribution/1205 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1205 END:VEVENT BEGIN:VEVENT SUMMARY:Multi-wavelength Observations of PG 1553+113 with H.E.S.S. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1210@cern.ch DESCRIPTION:Speakers: Dr. BENBOW\, Wystan (Max Planck Institut fuer Kernph ysik)\nThe high-frequency peaked BL Lac PG 1553+113\nwas discovered by H.E .S.S. to be a emitter of VHE (>100 GeV)\ngamma rays during ~8 hours of obs ervations in 2005. \nThe AGN was observed again by H.E.S.S in 2006.\nA to tal of ~17 hours of additional data were taken.\nIn addition\, observation s using the VLT Sinfoni \ninstrument were made to determine the presently unknown\nredshift of PG 1553+113. Results of the H.E.S.S. observations\,\ nas well as from related multi-wavelength studies\, will be presented.\n\n https://indico.nucleares.unam.mx/event/4/session/39/contribution/1210 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1210 END:VEVENT BEGIN:VEVENT SUMMARY:GLAST Large Area Telescope Observations of Blazars DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1214@cern.ch DESCRIPTION:Speakers: Dr. CARSON\, Jennifer (Stanford Linear Accelerator C enter)\nThe Large Area Telescope (LAT\, 30 MeV < E < 300 GeV) aboard the G amma-ray Large Area\nSpace Telescope (GLAST)\, scheduled to launch in late 2007\, promises a factor of ~30\nincrease in sensitivity over its predece ssor\, EGRET. It is expected that the LAT will\ndetect over a thousand bla zars in its first year\, enabling the first detailed\npopulation studies o f these gamma-ray sources. The LAT’s sensitivity is sufficient to\nmeasu re the time-resolved spectra of dozens of blazars in flaring states over i ts\nlifetime and to study the time-averaged properties of hundreds more in quiescence. In\naddition\, the LAT’s large field of view (2.4 sr) and G LAST’s all-sky scanning mode\ntogether provide a uniform sky exposure an d even\, well-sampled light curves of every\nsource. In short\, the LAT is a sensitive probe of the parsec-scale jets of AGN and\nthe physics of the jets’ gamma-ray emitting regions. We present an overview of the\ncapabi lities of the LAT for timing and spectral studies and a discussion of how these\ncapabilities can constrain physical models of blazars. We also emph asize the\nimportant role of simultaneous observations at other wavelength s.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/121 4 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1214 END:VEVENT BEGIN:VEVENT SUMMARY:Limits on MeV Gamma-Ray Emission from Active Galaxies and Other Un identified High-Latitude Gamma-Ray Sources Observed with CGRO/COMPTEL DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1224@cern.ch DESCRIPTION:Speakers: Dr. STACY\, J. Gregory (LSU and Southern University\ , USA)\nWe have established cumulative flux limits in the COMPTEL energy r ange (0.75-30 MeV)\nfor a large sample of active galactic nuclei (AGN) of general interest. Our target\nlist consists of both known and unidentified gamma-ray sources at high Galactic\nlatitudes. Limits to the time-average d MeV-emission measured with COMPTEL are derived\nfrom all-sky maximum-lik elihood and flux maps produced using the full COMPTEL dataset\nspanning th e entire nine-year period of the CGRO mission (April 1991-June 2000). The\ nflux limits described here will be used to assess the contribution of AGN to the\ndiffuse gamma-ray background measured in the MeV regime\, and may serve to constrain\nthe emission processes operative in high-energy cosmi c sources.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribu tion/1224 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1224 END:VEVENT BEGIN:VEVENT SUMMARY:The role of GLAST in multiwavelength observations of bright TeV bl azars DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1229@cern.ch DESCRIPTION:Speakers: Dr. PANEQUE\, David (SLAC/Kipac)\nThe TeV blazars Mr k 421\, Mrk 501\, PSK 2155-304 and 1ES1959+650 are among the brightest kno wn blazars\, \nyet the existing experimental set of data does not allow on e to make unambiguous statements about the physical \nmechanisms responsib le for the electromagnetic emission. The lack of sensitive coverage in the energy range 1 \nMeV to 500 GeV (up to 2004)\, and the scarce truly simul taneous data result in a big inter-model and intra-model \ndegeneracy. The LAT instrument on board of the GLAST satellite\, which will start operati on in the fall 2007\, aims \nto perform gamma-ray astronomy in the energy range 20 MeV to 300 GeV. The sensitivity of LAT is about 25 \ntimes better than its predecessor\, EGRET. Together with the enhanced sensitivity of t he current generationn of \nImaging Air Cherenkov Telescopes (IACTs) in th e energy range 100 GeV – 500 GeV\, LAT observations offer \nunprecedent ed capabilities to study the high energy emission of these objects in both quiescent and flaring state. \n \nIn the conference we will present the c apabilities of the LAT instrument to study these objects\, as well as the \nplanned multiwavelength campaigns during the first year of GLAST operati on.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/12 29 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1229 END:VEVENT BEGIN:VEVENT SUMMARY:Sensitivity of the High Altitude Water Cherenkov Experiment to obs erve Gamma-Ray Bursts DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1239@cern.ch DESCRIPTION:Speakers: Dr. GONZALEZ SANCHEZ\, Maria Magdalena (Instituto de Astronomia\, Universidad Nacional Autonoma de Mexico)\nGround based teles copes have marginally observed very high energy emission (>100GeV)\nfrom g amma-ray bursts(GRB). For instance\, Milagrito observed GRB970417a with a\ nsignificance of 3.7 sigmas over the background. Milagro have not yet obse rved TeV\nemission from a GRB with its triggered and untriggered searches or GeV emission with\na triggered search using its scalers. These results suggest the need of new\nobservatories with higher sensitivity to transien t sources. The HAWC (High Altitute\nWater Cherenkov) observatory is propos ed as a combination of the Milagro tecnology\nwith a very high altitude (> 4000m over see level) site. The expected HAWC sensitivity\nfor GRBs is at least >10 times the Milagro sensitivity. In this work HAWC sensitivity\nfo r GRBs is discussed for different detector configurations such as altitude \,\ndistance between PMTs\, depth under water of PMTs\, number of PMTs req uired for a\ntrigger\, etc.\n\nhttps://indico.nucleares.unam.mx/event/4/se ssion/39/contribution/1239 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1239 END:VEVENT BEGIN:VEVENT SUMMARY:Capability of the scaler system of Milagro pond to observe Gamma R ay Burst DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1241@cern.ch DESCRIPTION:Speakers: Dr. ALVAREZ OCHOA\, Cesar (Facultad de Ciencias Fisi co Matematicas Benemerita Universidad Autonoma de Puebla)\nGamma-ray burst s (GRBs) have been observed up to energies of a few GeV by satellite\nobse rvatories. In particular\, GRB941017 showed a spectral component extending beyond\n200MeV and distinct from the previously observed at keV energies. Ground based\ntelescopes have marginally observed very high energy emissi on (>100GeV). For\ninstance\, the Milagrito observation of GRB970417a hint ed at a distinct higher-energy\ncomponent inconsistent with an extrapolati on of the observed emission at keV-MeV\nenergies. Therefore\, observations of gamma-ray bursts at GeV energies will bring new\ninsights about the em ission mechanisms and constrain the current GRB models. Milagro\nis a wide field (2sr) high duty cycle (>90%) ground based water Cherenkov detector. \nIt triggers mainly on extensive air showers (EAS) in the energy range fr om 100 GeV to\n100 TeV. However\, individual photomultiplier tube counting rates (scalers) are\nsensitive to EAS with energy as low as ~1GeV. In thi s work\, the capabilities of\nMilagro to detect the high energy component of GRBs using the scalers system are\npresented and compared with other ob servatories such as the Pierre Auger Water\nCherenkov tanks.\n\nhttps://in dico.nucleares.unam.mx/event/4/session/39/contribution/1241 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1241 END:VEVENT BEGIN:VEVENT SUMMARY:Emissions from supernova remnants in the presence of small-scale r andom and large-scale regular magnetic fields DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1268@cern.ch DESCRIPTION:Speakers: Dr. YOSHIDA\, Tatsuo (Faculty of Science\,Ibaraki Un iversity)\nWe study non-thermal emissions by relativistic electrons from 　supernova\nremnants(SNRs) in the presence of small-scale random and lar ge-scale regular magnetic\nfields. We extend our pure jitter and inverse C ompton emission models (Ogasawara et\nal. 2006) and construct the emission models with regular magnetic fields. We apply\nthem to the multi-waveleng th data of TeV gamma-ray sources SNRs RX J1713.7-3946\n(G347.3-0.5) and RX J0852.0-4622 (G266.6-1.2). The physical fit parameters of random\nand reg ular magnetic fields are discussed.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/39/contribution/1268 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1268 END:VEVENT BEGIN:VEVENT SUMMARY:Multiwavelength search for the first blazars DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1280@cern.ch DESCRIPTION:Speakers: Dr. CARRAMINANA\, Alberto (INAOE)\nHigh redshift mas sive protogalaxies\, the sites of early star formation\nin the Universe\, provided a suitable environment for the formation of\nthe first supermassi ve black holes. Mass accretion causes the black\nhole to grow and become a gamma-ray blazar for those observers \nprivileged by a line of sight parr alel to the jet. Possible\nevolutionary sequences are explored in terms of their visibility in\nthe millimeter\, optical and gamma-ray regimes.\n\nh ttps://indico.nucleares.unam.mx/event/4/session/39/contribution/1280 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1280 END:VEVENT BEGIN:VEVENT SUMMARY:Observation of the ULIRG Arp 220 with MAGIC DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1288@cern.ch DESCRIPTION:Speakers: Dr. VITALE\, vincenzo (dip. Fisica Udine)\nThe ultra -luminous infra red galaxies (ULIRGs) have an enhanced starburst\nrate whi ch might be related to a large emission of very high\nenergy gamma rays.\n Arp 220 is the nearest ULIRG (72 Mpc) and a well studied object.\nThis sou rce was observed with the stand alone imaging atmospheric\n Cherenkov tele scope MAGIC for more than 15 hours on-source.\nNo significant gamma ray ex cess was detected during the observations.\nThe first upper limits to the very high energy gamma ray flux\nwere obtained\, with an analysis energy t hreshold of 160 GeV.\nThe analysis results will be reported and compared to\n theoretical expectations.\n\nhttps://indico.nucleares.unam.mx/event/ 4/session/39/contribution/1288 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1288 END:VEVENT BEGIN:VEVENT SUMMARY:Variations of Angular Distribution of Cosmic Rays during GLE Perio d on January 20\, 2005. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-33@cern.ch DESCRIPTION:Speakers: Dr. STARODUBTSEV\, Sergey (Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy SB RAS\, Yakutsk\, Russia)\nThe varia tions of anisotropy of primary spectrum of cosmic rays (CR) during the \np eriod of CR intensity increasing on January 20\, 2005\, have been obtained \nusing the method of spectrographic global survey according to the data of \nground-based observations of CR at the world-wide network of stations . It is \nshown that in the flare main phase\, there was observed a CR str ong \nanisotropy and the particle flux to the south of the Sun. At a later time\, the \nanisotropy direction has periodically changed from north-sou thern to the \nopposite.\n\nhttps://indico.nucleares.unam.mx/event/4/sessi on/39/contribution/33 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/33 END:VEVENT BEGIN:VEVENT SUMMARY:Neutron Flux meter at Basic Environmental Observatory Moussala DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-58@cern.ch DESCRIPTION:Speakers: Dr. MISHEV\, alexander (Institute for Nuclear Resear ch and Nuclear Energy\, Bulgarian Academy of Sciences)\nThe space weather refers to conditions on the sun\, solar wind and Earth’s\nmagnetosphere and ionosphere. Several characteristic signatures in cosmic ray may be\nus ed for space weather applications on the basis of secondary cosmic ray neu tron\ndata. Good examples are the solar proton events and Geomagnetic stor ms. A possible\ntool for investigations from Earth the variation of cosmic ray flux is based on\nregistration of secondary cosmic ray neutrons and m uons. In this connection a neutron\nflux meter is developed at BEO Moussal a. The final design of neutron flux meter based\non gas-filled SNM-15 dete ctors is presented as well several preliminary experimental\nand Monte Car lo results. The aim of the complex is to provide with high statistics\nand precision measure of the absolute secondary neutron cosmic ray flux. The\ nscientific potential of detector complex is promising. Starting from esti mation of\nthe dose rate and finishing with space weather applications.\n\ nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/58 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/58 END:VEVENT BEGIN:VEVENT SUMMARY:Ground Level Events Recorded at Lomnicky Stit Neutron Monitor DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-172@cern.ch DESCRIPTION:Speakers: Prof. KUDELA\, Karel (IEP SAS Kosice\, Slovakia)\nAn update list of responses to relativistic solar particles and to particles \naccelerated in interplanetary space to high energies (Kudela et al\, Pr oc. 23rd \nICRC\, Calgary\, vol. 3\, p.71-74\, 1992) for the period 1966 u ntil December 2006 \nas recorded by a high mountain neutron monitor with n ominal vertical cut-off \nrigidity ~ 4 GV is presented. Selected events an d the specifics of high mountain \nneutron monitor measurements are discus sed.\nThis work was supported by Slovak Grant Agency APVV\, project no. 5 1-053805.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribut ion/172 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/172 END:VEVENT BEGIN:VEVENT SUMMARY:GCR-induced Photon Luminescence of the Moon: The Moon as a CR Det ector DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-209@cern.ch DESCRIPTION:Speakers: Dr. WILSON\, Thomas (NASA - Houston)\nWe report on t he results of a preliminary study of the GCR-induced photon \nluminescence of the Moon using the Monte Carlo program FLUKA. The model of \nthe lunar surface is taken to be the chemical composition of soils found \nat vario us landing sites during the Apollo and Luna programs\, averaged over \nall such sites to define a generic regolith for the present analysis. This \n then becomes the target that is bombarded by Galactic Cosmic Rays (GCRs) i n \nFLUKA to determine the photon fluence when there is no sunshine or Ear thshine. \nFrom the photon fluence we derive the energy spectrum which can be utilized to \ndesign an orbiting optical instrument for measuring the GCR-induced luminescence.\nThis is to be distinguished from the gamma-ray spectrum produced by the radioactive\ndecay of its radiogenic constituents lying in the surface and \ninterior. Also\, we investigate transient opti cal flashes from high-energy CRs \nimpacting the lunar surface (boulders a nd regolith). The goal is to determine \nto what extent the Moon could be used as a rudimentary CR detector. Meteor \nimpacts on the Moon have bee n observed for centuries to generate such flashes\, \nso why not CRs?\n\nh ttps://indico.nucleares.unam.mx/event/4/session/39/contribution/209 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/209 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Flux in the Presence of a Neutral Background DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-210@cern.ch DESCRIPTION:Speakers: Dr. WILSON\, Thomas (NASA - Houston)\nThe study of c osmic rays (CRs) is a very mature subject developed around \nthe concept o f radiative particle flux phi as a mono-variant function of \nenergy E\, t hat is phi = phi(E). This is based on the notion of the cosmos as \nbeing filled with cosmic radiation in the form of a collisionless exosphere \nof plasma. Neutrals\, however\, are likewise ubiquitous in space and planeta ry \ntrapped-radiation belts. It will be shown that in the presence of a n eutral \nbackground of density rho\, flux phi is actually bivariant in ene rgy E and rho\, \ncreating a surface phi(E\,rho). This is an intrinsic pro perty of charged-particle \nflux\, that flux is not merely a function of E but is dependent upon density rho \nwhen a background of neutrals is pres ent. The effect is produced by multiple \nscattering of charged particles off neutral and ionized atoms along with \nionization loss where charged a nd neutral populations interact. For the harder \nportion of CR spectra\, flux is mono-variant but at nonrelativistic energies \n(below ~350 MeV) it becomes sensitive to the presence of neutral backgrounds. \nThe dependenc e of phi(E\,rho) upon background neutrals is helpful in dicussing the \nan omalous CR (ACR) flux made up of ionized components of the heliospheric \n neutral atmosphere.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39 /contribution/210 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/210 END:VEVENT BEGIN:VEVENT SUMMARY:Atmospheric Transport Inferred from Seasonal Variations in Cosmoge nic Be-7 Concentrations DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-224@cern.ch DESCRIPTION:Speakers: Prof. YOSHIMORI\, Masato (Rikkyo University)\nA cosm ogenic radionuclide Be-7 (half life 53.3 days) results from nuclear intera ctions of galactic \ncosmic rays in the Earth's atmosphere. Most of Be-7 i s produced in the lower stratosphere and \nslowly tranported to the surfac e. Be-7 plays a role of atmospheric tracer and its measurements \nprovide an important clue on atmospheric air mass motions. Since 2002 we have con tinuously \nmeasured surface Be-7 concentrations in Tokyo. The data in 200 2-2006 indicated apparent \nincreases of the Be-7 concentrations in spring and autumn. It was found from analysis of \nprecipitation data that the s easonal variations are not associated with scavenging by precipitation. \n We suggested the possibility that the stratospheric Be-7 are brought to th e upper troposphere \nthrough a large-scale air mass exchange between the stratosphere and troposphere. The air mass \nexchange is inferred to occur in association with a periodic passage of a pair of traveling high \npres sure and extratropical low pressure over Japan in spring and autumn.\n\nht tps://indico.nucleares.unam.mx/event/4/session/39/contribution/224 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/224 END:VEVENT BEGIN:VEVENT SUMMARY:Observation of the gradual increases and bursts of energetic radia tion associated with the activity of the winter thunderstorm DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-265@cern.ch DESCRIPTION:Speakers: Dr. TORII\, Tatsuo (Japan Atomic Energy Agency)\nThe increase of the gamma-ray dose-rate in association with the activity of t he \nthunderstorm was observed by the detectors located at the ground leve l in the \nwinter of Japan. To investigate the particle acceleration mecha nism during \nwinter thunderstorms\, the four sets of radiation detectors were used which \nconsist of four long proportional counters (PRCs). These PRCs have a different \nresponse characteristic for the energy of inciden t particles by mounting shield \ncovers. The results were also compared wi th the data measured at the same \ntime by the environmental radiation mon itors using an NaI scintillator / \nionization chamber. Electric field was also measured by using a field mill. \nAs a result\, it was observed that the radiation intensity began to increase from \nbefore several 10 second s in which the radiation burst is generated. In \naddition\, the simultan eous radiation burst and a rapid increase of the electric \nfield indicate that the discharge by lightning was generated. From the observed \nresult s of the PRCs with different responses to the energy of incident particles \, \nthe gradual increase of counting rate is caused mainly by the irradia tion of \nphotons with energy of several MeV. Moreover\, it was considere d that the \nburst of the radiation was attributed to in the injection of high energy photons \nwith the energy over 10MeV.\n\nhttps://indico.nuclea res.unam.mx/event/4/session/39/contribution/265 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/265 END:VEVENT BEGIN:VEVENT SUMMARY:Interconnections Between Forbush Cosmic Ray Decreases and Atlantic Hurricanes Development. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-323@cern.ch DESCRIPTION:Speakers: Prof. KAVLAKOV\, Stilian (Bulgarian Academy of Scien ces)\nThe Forbush decreases\, recorded during 1951-2005 neutron measuremen ts on Climax\nCosmic Ray Station were used\, estimating their number per y ear F(n) and calculating\ntheir total yearly decrease F(t). They were inv estigated together with certain\nparameters of the hurricanes recorded ove r a large Atlantic Ocean area\, situated\nbetween 25 and 60 degrees West\, and 8 and 23 degrees North. In that area the water\nsurface temperature i s practically constant and the possibility of hurricane\nformation is equa lly distributed over it. The hourly data for hurricane maximum\nrotational wind velocity (W) was used to calculate: the kinetic energy as W2 and the \ntotal yearly accumulated hurricane increase of this velocity as dW/dt.\n It was found that both these parameters correlated well with F(n) and F(t) . That\nindicates the existence of some parallel or even interconnected hi gh atmosphere\nprocesses triggering the hurricane formation. From the othe r side that extend the\npossibilities for earlier hurricane forecasts.\n\n https://indico.nucleares.unam.mx/event/4/session/39/contribution/323 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/323 END:VEVENT BEGIN:VEVENT SUMMARY:Method and results of the analysis of data on vertical rigidities of cosmic rays cutoff in the geomagnetic field. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-340@cern.ch DESCRIPTION:Speakers: Dr. YUSHKOV\, Boris Yu. (Scobeltsyn Institute of Nuc lear Physics\, Lomonosov Moscow State University)\nThe method of the analy sis of data on vertical rigidities of cosmic rays cutoff is \ndescribed. T he essence of the method consists in the fact\, that both the \nexperiment al data and the calculation results are described in the form of \nchange of their value relative to the values related to IGRF. The value of these \nrelative changes quite certainly depends on the rigidity itself and on t he level of \ngeomagnetic field disturbance (the Kp-index). Systematic dis tinctions between \nthe experimental data and the results of calculations by Tsyganenko-89’s \nmagnetosphere model in the region of low rigidities (R < 0.5 GV) are revealed.\n\nhttps://indico.nucleares.unam.mx/event/4/se ssion/39/contribution/340 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/340 END:VEVENT BEGIN:VEVENT SUMMARY:Solar Cosmic Ray study with Neutron Monitors of a Various Design DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-349@cern.ch DESCRIPTION:Speakers: Dr. BALABIN\, Yury (Polar Geophysical Institute of R AS)\nThe modeled and observed responses of neutron monitors of two various \ntypes: the standard 3NM-64 and a leadless 4NMD one at the SANAE South \ nAfrican Antarctic station during a number of large GLE events were compar ed to \nprecise the specific yield of the NMD at low rigidity range. The p arameters of \nprimary relativistic solar protons outside magnetosphere: r igidity spectrum\, \nanisotropy direction and pitch angle distribution wer e determined on data of \nthe worldwide NM-64 neutron monitor network by m odeling technique. The \nmodeling included: definition of asymptotic vie wing cones of the NM stations \nunder study by the particle trajectory com putations in a model magnetosphere \nT01 (Tsyganenko (2001)\; calculation of the NM responses at variable primary \nsolar proton flux parameters\; d etermination of primary solar proton parameters \noutside the magnetospher e by a least square procedure at comparison of \ncomputed NM responses wi th observations. Then the response of both neutron \nmonitors NM64 and lea dless NMD was calculated using the specific yield \nfunctions (SYF) obtain ed earlier in the latitude and high-altitude survey of both \ninstruments (Stoker\, 1985\, 1994). By fitting to observations the SYF for the NMD \nd etector was adjusted so that it precisely described the response of leadle ss \nneutron monitor during a number of GLE events.\n\nhttps://indico.nucl eares.unam.mx/event/4/session/39/contribution/349 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/349 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of the December 2006 particle events at high latitude s with the KET aboard Ulysses DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-357@cern.ch DESCRIPTION:Speakers: Prof. STRUMINSKY\, A. (Institute of Space Research\, Russian Academy of Sciences\, Profsoyuznaya Street\, 84/32\, Moscow 11799 7\, Russia)\nAn unexpected rise of solar activity close to its minimum in December 2006 resulted\nin four X-class flares and four energetic particle events. These events were observed\nclose to Earth and above 70 degree So uth by the Ulysses spacecraft\, which was at a\nheliocentric distance of 2 .8 AU at that time. Three out of these four events produced\nsignificant i ntensity increases up to several hundred MeV/nucleon for protons and\nalph a-particles and several 10 MeV for electrons at high southern latitudes. T hey\nwere associated with X9.0\, X6.5\, and X3.4 flares from the AR 10930\ , coronal type II\nbursts and strong microwave emission on 5-th\, 6-th\, a nd 13-th December\, respectively.\nAlthough these flares have similar X-ra y and microwave time profiles\, the particle\nevent on December 13 is the weakest among the three at Ulysses\, but it is the largest\nnear Earth. It produced a ground level event leading to an intensity increase of\nabout 34 % in the Kiel neutron monitor. In contrast the December 6 particle even t was\nthe largest at Ulysses. We will discuss these events in context of previous Ulysses\nobservations and its consequences for particle propagati on to solar Polar Regions.\n\nhttps://indico.nucleares.unam.mx/event/4/ses sion/39/contribution/357 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/357 END:VEVENT BEGIN:VEVENT SUMMARY:Interaction of GeV Protons with Circumsolar Dust Grains DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-364@cern.ch DESCRIPTION:Speakers: KAHLER\, Stephen (Air Force Research Laboratory)\nA population of dust grains produced by asteroids and comets is continually \norbiting the Sun to within several Rsun. The grains scatter sunlight an d make \nup the solar F corona\, which shows only slow variations with tim e. Grain \ndynamics are due primarily to interactions with solar photons and the solar \nwind\, but they are also bombarded by the E > 1 MeV energe tic particles \npropagating antisunward after acceleration in CME-driven s hocks during SEP \nevents. We consider the effects of the interaction of high energy protons on \ndust grains during such events. To calculate the maximum expected effects\, we \ncalculate the proton energy spectrum of t he 20 January 2005 ground level \nevent (GLE) and consider the gamma ray f luxes produced in such an event. \nThe size distribution of the grains in the circumsolar environment is poorly \nknown\, so we use several popular models in our calculations.\n\nhttps://indico.nucleares.unam.mx/event/4/s ession/39/contribution/364 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/364 END:VEVENT BEGIN:VEVENT SUMMARY:Ground Level Enhancement of December 13\, 2006 by the Ground Measu rement Data DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-402@cern.ch DESCRIPTION:Speakers: Dr. STARODUBTSEV\, Sergey (Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy SB RAS\, Yakutsk\, Russia)\nOn the ba sis of neutron monitor world network data the GLE event of December 13\, 2 006\nis studied. Taking into account the initial differential spectrum of galactic cosmic\nrays\, viewing cones of the detectors\, integral multipli city of secondary neutrons at\nvarious latitudes and observation levels th e GLE spectrum is estimated. It is noted\nthat at the Yakutsk station this event has also been registered with the ionization\nchamber ASK-1.\n\nhtt ps://indico.nucleares.unam.mx/event/4/session/39/contribution/402 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/402 END:VEVENT BEGIN:VEVENT SUMMARY:Response of IceTop tanks to low-energy particles DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-408@cern.ch DESCRIPTION:Speakers: Mr. NIESSEN\, Peter (Department of Physics and Astro nomy\, University of Delaware)\nIceTop is the surface component of the Ice Cube neutrino telescope at the South Pole.\nIt will serve as an air-shower array that consists of cylindrical tanks of clear ice.\nElectrons\, posit rons\, gamma rays and muons produce Cherenkov radiation directly or\nthrou gh interaction products. It is therefore important to have a good understa nding\nof these processes. A thorough knowledge will permit the calculatio n of the response\nfunction\, allowing good estimates of the array trigger rates.\n\nThe continuous recording of a single tank rate also provides a means for IceTop to\nfunction as a large area low energy cosmic ray monito r. It serves the twofold purpose\nof detecting a) changes in the local int erplanetary medium environment and b) the\narrival of transient particles from solar events. We will present a simulation for\nthis detector configu ration and compare results to these measurements. The analysis\nwill attem pt to quantify the potential capabilities of IceTop as an observatory for\ nSolar and Heliospheric phenomena.\n\nhttps://indico.nucleares.unam.mx/eve nt/4/session/39/contribution/408 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/408 END:VEVENT BEGIN:VEVENT SUMMARY:Identification of solar cosmic ray ground level enhancements at th e middle latitudes. DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-471@cern.ch DESCRIPTION:Speakers: Dr. KRYAKUNOVA\, Olga (Institute of Ionosphere\, Min istry of Education and Science\, Republic of Kazakhstan)\nThis work is dir ected toward the experimental and theoretical investigation of \nthe groun d level solar cosmic ray enhancements (GLE). Relativistic protons (>1 \nGe V) are generated in powerful flares more often than they are observed at \ nthe Earth. Especially it concerns to observation at the middle latitudes. \nAlthough recorded magnitudes of ground level enhancements are usually v ery \nsmall at these geomagnetic latitudes the high statistical accuracy o f the 18-\ntube NM-64 Alma-Ata neutron monitor\, located at 3340 m altitud e\, make \npossible detection of these events at this point. Except for it the possible solar \nproton contribution into general flux of galactic co smic rays registered by means \nof Alma-Ata high altitude neutron monitor has been investigated in those \nevents when difficultly visually to notic e GLE events. GLE were investigated \nusing Student’s criterion. Some la st GLE on November 1997\, on August 1998 \nand December 2006 were analyzed . It is shown that using of Student’s \ncriterion allows to reveal effec tively GLE at the middle latitudes and to defined \nupper limit energy spe ctra of particles.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/ contribution/471 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/471 END:VEVENT BEGIN:VEVENT SUMMARY:Observations of primary\, trapped and quasi trapped particles with PAMELA experiment DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-503@cern.ch DESCRIPTION:Speakers: Dr. CASOLINO\, Marco (INFN ROma2)\nPAMELA was launc hed on June $15^{th}$ 2006 in a pressurized container on board the\nRuss ian Resurs-DK1 satellite. The satellite is flying in high inclination ($ 70^o$)\,\nlow Earth Orbit (350-600 km)\, performing measurements in diff erent points and\nconditions of the geomagnetosphere. The device is a mul ti-purpose apparatus \ncomposed of a permanent magnet spectrometer to prov ide particle charge\, rigidity and\nincoming angle. A series of six \ns cintillator counters arranged at its extremities provide redundant Time- of-Flight\nand charge data. Lepton/hadron identification is performed by a\nSilicon-Tungsten calorimeter and a Neutron detector placed at the\nb ottom of the device. An Anticounter system is used offline to\nreject fals e triggers coming from the satellite. \nPAMELA is capable of detecting pr otons (80 MeV- 700 GeV)\, antiprotons (80 MeV-190\nGeV)\, electrons (50 Me V - 400 GeV)\, positrons (50 MeV - 270 Gev) and nuclei\n($\\simeq 100 Me V/n 200GeV/nuc). In addition a tecnhique employing scintillator\ncounting rate and range energy methods allows to lower the minimum detectable\ne nergy range of the apparatus to 36 MeV and 3.5 MeV for protons and electro ns\nrespectively. \nThe orbit of the satellite and the characteristics of the magnet tracker allows\nPAMELA to perform a very detailed measurement of the nature and spectra of primary\n(above cutoff) and secondary partic les (sub-cutoff: trapped\, reentrant albedo\, etc.).\nThe precise measurem ents of particle distribution in different regions of the orbit\n provi des information on the processess of production\, propagation and interac tion\nof particles in Earth’s magnetosphere. In this work we will also discuss different\nmethods of calculation of geomagnetic coordinates and particle cutoff comparing them\nwith expected and measured fluxes.\n\nht tps://indico.nucleares.unam.mx/event/4/session/39/contribution/503 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/503 END:VEVENT BEGIN:VEVENT SUMMARY:The atmospheric muon flux in correlation with temperature variatio ns in the low stratosphere (50-200mb). DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-541@cern.ch DESCRIPTION:Speakers: Dr. BERTAINA\, Mario (Torino University)\nThe depend ence of the muon flux from the atmospheric parameters (pressure and\ntempe rature) is a well known effect since long time ago\, that is usually\ncorr ected for in cosmic ray measurements. We have correlated at EAS-TOP (LNGS) \nthe muon flux detected by the EMD detector (29 stations\, 10m^2 each\,\n E_thr>3MeV) with the atmospheric temperature (10-1000mb levels) monitored by\nthe radio-soundings of the Aeronautica Militare at Pratica di Mare (Ro me).\nA significant effect has been observed when the muon flux is correla ted with\nthe atmospheric temperature in the region 50-200mb (50-200gr/cm^ 2)\, as\nexpected\, since this is the region where the mesons of first gen eration are\nproduced. The effect becomes even larger (K_T=-9.5+/-1.1)x10^ -4 K-1) when the\nvariations of the cosmic ray primary flux is taken into account (Neutron\nMonitor\, Rome). Then\, the technique has been used to m onitor strong temperature\nvariations in the low stratosphere through the muon flux in two periods\,\nshowing that the average temperature variation s in the low stratosphere are\nreproduced with a ~2K uncertainty. The main results of this analysis will be\npresented.\n\nhttps://indico.nucleares. unam.mx/event/4/session/39/contribution/541 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/541 END:VEVENT BEGIN:VEVENT SUMMARY:Relativistic solar cosmic ray events (1956-2006) from GLE modeling studies DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-658@cern.ch DESCRIPTION:Speakers: Prof. VASHENYUK\, Eduard (Polar geophysical Institut e)\nThe modeling analysis of 15 large GLEs occurred in the period 1956-200 6 on \nthe data of the worldwide neutron monitors has been performed. In a ll studied \ncases two distinct RSP populations (components) were revealed : the early \nimpulse-like intensity increase with exponential energy spec trum (prompt \ncomponent\, PC)\, and the late gradual increase with a soft er energy spectrum of \nthe power law form (delayed component\, DC). The e xponential spectrum may \nbe an evidence of the acceleration by electric f ields arisingin the reconnecting \ncurrent sheets in the corona. The possi ble source of DC particles can be \nstochastic acceleration at the MHD tur bulence in expanding flare plasma.\nThe modeling analysis of pitch-angle d istributions and anisotropy dynamics \nallows also studying effects of RSP propagation in the IMF.\n\nhttps://indico.nucleares.unam.mx/event/4/sessi on/39/contribution/658 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/658 END:VEVENT BEGIN:VEVENT SUMMARY:WORLD GRID OF CALCULATED COSMIC RAY VERTICAL CUTOFF RIGIDITIES FOR EPOCH 1995.0 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-727@cern.ch DESCRIPTION:Speakers: Dr. SMART\, Don (Emeritus\, Air Force Research Labor atory)\nA world grid of vertical cosmic ray cutoff rigidities was calculat ed using the \nDefinitive International Geomagnetic Reference Field for Ep och 1995.0. These \ncutoff rigidity values show the effects of the contin ued evolution of the \ngeomagnetic field. The average cutoff values conti nue to decrease especially in \nthe South Atlantic and South American area s. However\, in some areas of the \nworld\, the cutoff values are increas ing. These temporal changes are particularly \napparent in the change of the location of the cosmic ray equator. These cutoff \nrigidity values hav e extensive use\, especially for computing aircraft radiation \ndose by th e CARI-6 software.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/ contribution/727 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/727 END:VEVENT BEGIN:VEVENT SUMMARY:WORLD GRID OF CALCULATED COSMIC RAY VERTICAL CUTOFF RIGIDITIES FOR EPOCH 2000.0 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-730@cern.ch DESCRIPTION:Speakers: Dr. SMART\, Don (Emeritus\, Air Force Research Labor atory)\nA world grid of vertical cosmic ray cutoff rigidities was calculat ed using the \nDefinitive International Geomagnetic Reference Field for Ep och 2000.0. These \ncutoff rigidity values were specifically computed for updating the aircraft \nradiation dose. These cutoff rigidity values sho w the effects of the continued \nevolution of the geomagnetic field. The average cutoff values continue to \ndecrease especially in the South Atlan tic and South American areas. However\, \nin the North Atlantic and the e ast coast of the North American continent\, the \ncutoff values are increa sing.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/ 730 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/730 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray induced ionization in the upper\, middle and lower atmo sphere simulated with CORSIKA code DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-916@cern.ch DESCRIPTION:Speakers: Prof. VELINOV\, Peter (Central solar terrestrial inf luences laboratory- BAS)\nPhysical model for calculation cosmic ray induce d ionization in the atmosphere is presented. The model is based on Monte C arlo simulation with CORSIKA 6.52 code using FLUKA and QGSJET hadronic int eraction subroutines. On the basis of the simulation results the ion pair production in the atmosphere and the impact of the different shower compon ents\, precisely the electromagnetic\, muon and hadronic is estimated. Th e simulations are carried out with realistic atmospheric model and followi ng steep spectrum. The model is applicable in the entire atmosphere from t he ground up to the upper atmosphere and ionosphere. A comparison with dir ect rocket measurements is provided. The validation of the proposed model is confirmed.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contr ibution/916 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/916 END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of Cosmic Ray Neutron Spectra in the Energy Region of 20-200 MeV at the Summit of Mauna Kea and Several Different Altitudes DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-966@cern.ch DESCRIPTION:Speakers: Dr. TAKASU\, Ryozo (Fujitsu Laboratories Ltd.)\nNowa days\, the information on the flux of cosmic ray neutrons has become very\ nimportant for the computer technology. Since the reduction of LSI (large scale\nintegrated circuit) scaling proceeds\, the effect of cosmic ray neu trons becomes\nsignificant. Neutrons hit the LSI of the computer and make pseudo signals and false\ndata. This phenomenon is known as the soft error of the computer. The soft error is\ndefined as spontaneous change of the digital information in the computer due to\n"radiation effects". For evalu ating the reliability of computer systems\, the accurate\nestimation of th e soft error rate has become essential. In this purpose\, the accurate\nob servation of the cosmic ray neutron spectra in the energy region up to sev eral\nhundreds of MeV has been anticipated.\nIn the conference\, we will r eport the energy spectra of neutrons in the energy range\nof ca. 20 MeV - 200 MeV at various altitudes including Mauna Kea\, Hawaii (4200 m) and\nMt . Norikura\, Japan (2770 m) and at the sea level. As far as we know\, thes e are quite\nimportant data to have measured the neutron spectra by the de tector that can measure\nthe energy of neutrons.\n\nhttps://indico.nuclear es.unam.mx/event/4/session/39/contribution/966 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/966 END:VEVENT BEGIN:VEVENT SUMMARY:Definition of the snow thickness from the absorption of cosmic ray neutron component DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1000@cern.ch DESCRIPTION:Speakers: Dr. YANKE\, Viktor (IZMIRAN)\nAn application of abso rption effect of the CR neutron component to the \nestimation of snow-wate r equivalent is considered in this work. The primary CR \nvariations\, cha nges of the atmospheric pressure and humidity concentration in \nbedding s urface are discussed as influence on the accuracy of the obtained \nresult s. Monitoring of the snow-cover during several seasons demonstrated an \ne fficiency of this method even for snow thickness of several meters. The \n accuracy of this thickness estimation is about several percentages. \n Des cribed method was approved for several cosmic ray stations \nwhere the acc umulation of large snow thickness is possible\, and for some \nFrench hydr ometeorological stations which were opened directly for the \nestimation o f snow-water equivalent.\n\nhttps://indico.nucleares.unam.mx/event/4/sessi on/39/contribution/1000 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1000 END:VEVENT BEGIN:VEVENT SUMMARY:The December 2006 GLE event as seen from LARC\, SVIRCO and OLC* DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1002@cern.ch DESCRIPTION:Speakers: Dr. STORINI\, MARISA (INAF/IFSI-Roma)\nDuring Decemb er 13 2006 a ground-level enhancement was recorded by the \nworld-wide net work of neutron monitors. This paper discusses the response of \nthree cos mic ray detectors characterized by different rigidity cutoffs: LARC (King \nGeorge Island - Antarctica)\, SVIRCO (Rome - Italy) and OLC (Santiago of Chile).\n\n\n*: Research partly supported by the Italian Antarctic Resear ch Program.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contrib ution/1002 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1002 END:VEVENT BEGIN:VEVENT SUMMARY:Characteristics of near real-time cutoff calculations on a local a nd global scale DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1032@cern.ch DESCRIPTION:Speakers: Dr. BUETIKOFER\, Rolf (Physikalisches Institut\, Uni versity of Bern)\nA procedure was developed to compute in near real-time t he effective vertical cutoff\nrigidities for a world grid with a mesh size of 5 x 5 degrees in geographic longitude\nand latitude. The evaluation is made every three hours. The cutoff rigidities are\ncalculated by the back ward trajectory tracing method\, where the geomagnetic field is\nrepresent ed by the IGRF model for the internal sources and by the Tsyganenko 1989\n model for the external part. The Kp indices derived at the U.S. Air Force Space\nForecast Center are used as input parameters for the Tsyganenko mod el to describe the\ncurrent degree of geomagnetic disturbance. In addition to the near real-time results\,\nthe procedure also allows to obtain the world grid for a specific time in the past as\nwell as the cutoff values a t a specific location during a specific time period. In\nthe paper we inve stigate the possibilities and limitations of these cutoff\ncalculations\, in particular during times with a strongly disturbed geomagnetosphere.\n\n https://indico.nucleares.unam.mx/event/4/session/39/contribution/1032 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1032 END:VEVENT BEGIN:VEVENT SUMMARY:Application of the NM-BANGLE model to GLE70 study DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1073@cern.ch DESCRIPTION:Speakers: Dr. EROSHENKO\, Eugenia (Cosmic Ray Department\, IZM IRAN)\nA new significant ground level enhancement was recorded by the worl dwide \nneutron monitor network during the minimum phase of the 23rd solar cycle\, on \n13 December\, 2006. The event\, also known as GLE70\, start ed at ~ 2:48 UT\, \nwhereas the neutron monitor flux in most stations reac hed its maximum in \n~3:00-3:10 UT. In northern Europe the event was regis tered with big \namplitudes that in some cases reached ~ 70-90%\, renderin g this recent \nenhancement in one of the greatest GLEs of the 23rd solar cycle. The low \nlatitude neutron monitor station in Athens seems to have recorded some \nenhancement during the time period of the event providing possible evidence \nof the existence of high energy solar particles. In th is work some preliminary \nresults of a ground level neutron monitor data analysis for the event of 13 \nDecember\, 2006\, are presented. The applic ation of the NM-BANGLE model to \nGLE 70\, using data from thirty four neu tron monitor stations widely distributed \naround the globe\, resulted in the determination of some GLE-parameters such \nas the rigidity spectrum a nd the location of the anisotropy source during \ndifferent moments of the event. The morphology of this event seems to have \nsimilarities with tha t of GLE69 in January 2005. It seems that during the initial \nphase of th e event the solar cosmic ray rigidity spectrum was quite hard \nwhereas la ter its evolution was rather complicated. Moreover the very first \nenerge tic particles seem to have arrived in a narrow beam.\n\nhttps://indico.nuc leares.unam.mx/event/4/session/39/contribution/1073 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1073 END:VEVENT BEGIN:VEVENT SUMMARY:Effect of solar protons on the middle atmosphere composition durin g GLE 13 December\, 2006 DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1083@cern.ch DESCRIPTION:Speakers: Dr. KIRILLOV\, Andrey (Polar Geophysical Institute o f RAS)\nThe effect of energetic solar protons on the middle atmosphere (20 -80 km ) \nchemical composition during SPE 13 December\, 2006 has been stu died. The \nsolar proton spectra were obtained from the neutron monitors\, balloons and \nspacecraft data. One-dimensional time-dependent model (Fad el et al.\, 2006\, \nASR\, 38\, p.1881-1886) has been used to calculate th e production and loss of \nminor atmospheric components during the GLE. De rived depletions of ozone \ncontent is in good agreement with experimental data obtained by the \nMicrowave Limb Sounder (MLS) instrument on the AUR A spacecraft.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contr ibution/1083 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1083 END:VEVENT BEGIN:VEVENT SUMMARY:Coupling functions for NM-64 and NM without lead derived on the ba sis of calculated apparent cutoff rigidities for CR latitude survey from A ntarctica to Italy in minimum of solar activity DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1093@cern.ch DESCRIPTION:Speakers: Prof. DORMAN\, Lev (Israel Cosmic Ray and Space Weat her Center\, Tel Aviv University)\nL. I. Dorman (1\,2)\, O. A. Danilova (3 )\, M. I. Tyasto (3)\, N. G. Ptitsina (3)\, G. \nVilloresi (4)\, N. Iucci (4) and M. Parisi (4)\n\n (1) Israel Cosmic Ray Center affiliated to T el Aviv University\, \nTechnion and Israel Space Agency\, Israel\; (2) IZM IRAN\, Troitsk\, Russia\; (3) \nSPbFIZMIRAN\, St. Petersburg\, Russia\; (4 ) Dipartimento di Fisica "E. Amaldi"\, \nUniversità "Roma Tre"\, Rome\, I taly\n\nIn Dorman et al. (2007) it was calculate the apparent cut-off rigi dities for the \nbackward route (Antarctica-Italy) of the CR latitude surv ey performed on a ship \nduring 1996-1997 solar minimum. These computation s were done on the basis \nof results of trajectory calculations for incli ned cut-off rigidities for various \nazimuth and zenith angles (0°\, 15° \, 30°\, 45°\, 60°) and azimuth directions \nchanging from 0° to 360° in steps of 45°. The information on integral \nmultiplicities of seconda ry neutrons detected by neutron monitor in dependence \nof zenith angle of incoming primary CR particles have been also used. This \ninformation is based on the theoretical calculations of meson-nuclear cascades \nof prima ry protons with different rigidities arriving to the Earth's atmosphere at \nzenith angles 0°\, 15°\, 30°\, 45°\, 60° and 75°. By using this i nformation and \ndata of CR latitude survey from Antarctica to Italy in mi nimum of solar activity \nwe determine coupling functions for NM-64 and NM without lead.\n\nReference: L.I. Dorman et al. “Apparent Cutoff Rigidit ies for Cosmic Ray Latitude \nSurvey from Antarctica to Italy in Minimum o f Solar Activity”\, Adv. Space Res.\, \n2007 (in press).\n\nhttps://indi co.nucleares.unam.mx/event/4/session/39/contribution/1093 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1093 END:VEVENT BEGIN:VEVENT SUMMARY:Electric Storm Effects on the soft and hard cosmic ray components observed in Mexico City DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1099@cern.ch DESCRIPTION:Speakers: Mr. ALVAREZ CASTILLO\, Jesús (Instituto de Geofísi ca)\nThe effects of electric thunderstorms on the electromagnetic and muon \ncomponents of the cosmic ray secondary flux were studied during severe \nstorms in 2004 and part of 2005 analyzing the variations of the counting rates \nshown in the upper and lower scintillators of the muon telescope installed in \nMexico City. Results show that for positive configurations of the electric field \nsoft component particles show an increase of flux that can be interpreted as \nparticle acceleration. For the hard component the inverse effect is observed\, \nthat is a decrease in the counting rat es for positive electric field storms. These \nresults are in agreement wi th those obtained by by Khaerdinov et al (1 and 2). \n(1) Khaerdinov N.S. \, Lidvansky A.S.\, Petkov V.B.\, and Surovetsky Yu P. 2003\, \nEffect of Disturbed Electric Field of the Atmosphere on Cosmic Rays: 1. Soft \nCompo nent\, Proc. 28th ICRC\, pp. 4169-4172. (2) Khaerdinov N.S.\, Lidvansky \ nA.S.\, Petkov V.B. 2003\, Effect of Disturbed Electric Field of the Atmos phere on \nCosmic Rays: 2. Hard Component\, Proc. 28th ICRC\, pp. 4173-417 6.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/109 9 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1099 END:VEVENT BEGIN:VEVENT SUMMARY:On the trend of Atlantic Hurricane with Cosmic Rays DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1165@cern.ch DESCRIPTION:Speakers: Prof. PEREZ-PERAZA\, JORGE (INSTITUTO DE GEOFISICA\, UNIVERSIDAD NACIONAL AUTONOMA DE MEXICO)\nOne of the main goals of Solar- Terrestrial Physics is to know how and when the \nperiodicities of Solar Activity do modulate terrestrial Climatic changes? The \npurpose of this s tudy is to examine the cosmophysical periodicities that could \npossible b e related with a modulation in the number and magnitude of \nhurricanes. \ nPrevious efforts on elucidating a plausible contribution of cosmophysical \nphenomena in the process of hurricanes development have been mostly \ nbased on Correlational analysis. Such an analysis indicates the possibili ty of a \ncertain relation between two time series\, however\, this is of global nature and \ndoes not furnish a precise information about when suc h a relation occurs: the \nfact that two series (cosmophysical and climati c) have similar periodicities does \nnot necessarily implies that one is t he cause and another is the effect. Besides\, \neven if the correlation co efficient is very low\, there is the possibility that an \nexisting relati on could be of non linear nature\, or there is a strong phase shift \namon g both phenomena. One of the ways to analyze two non-stationary \nseries\, to discern whether there is a linear relation or not is by means of the \ nCoherence Wavelet method\, which furnish valuable information about when \nand which periodicity do coincide in time\, and about its nature\, line ar or non-\nlinear relation\, provided there is not a noticeable diphase a mong them.\nIn the present work we use the Morlet wavelet technique fo r the annual \nnumber of North Atlantic hurricanes between 1851 and 2005.. The periodicities \nfound from this analysis\, with > 95 % confidence le vel are of 3.5\, 5.5 and 7 \nyrs.\, and with  95 % confidence level a re of 22 and 30 yrs. All these \nperiodicities\, are known in Cosmic Rays physics to be a consequence of Solar \nActivity modulation. To find the relationship between hurricanes and Cosmic Ray \nseries in time-frequency space\, we use then Wavelet Coherence analysis: it is \nfound that the more prominent periodicity in the case of hurricanes of \nmagnitude 3 and 4 is that of 30 years. The relationship with hurricanes of \nmagnitude 3 is a non-linear one in the period 1891-1944\, with a coherence > \n0.9\, w hile for hurricanes of magnitude 4 there is a linear relation between 188 9 \nand 1953 with a coherence of 0.9. . It is worth noting that Tropical Storms \nlanding into Mexico\, the Total Cyclonic Energy \, as well as the number of \ncategory 4-5 in the Northwest Pacific basin and the Potential Destruction \nIndex \, all them present also a cyclic behavior of 30 yea rs.\n\nhttps://indico.nucleares.unam.mx/event/4/session/39/contribution/11 65 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1165 END:VEVENT BEGIN:VEVENT SUMMARY:On a Plausible Relationship Between Cosmic Rays and the Ozone Hole Size DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T194500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-1222@cern.ch DESCRIPTION:Speakers: Dr. ALVAREZ-MADRIGAL\, MANUEL (IIE Department\, Tecn ológico de Monterrey\, Campus Estado de México)\nIt is well known that anthropogenic activity can modify the Earth environment \nin a global sca le. Several restrictions and policies may be adopted in order to \nattenua te the contamination effects and protect the environment. However\, in \no rder to design and evaluate the impact of these policies and restrictions in the \nhuman activity\, it is important to identify if exists other sour ces that affects the \nglobal phenomena. The extraterrestrial sources are interesting\, because we \ncan not modify their intensity\, we can only o bserve\, and try to understand \nwhy\, how and when these factors act ov er the Earth system. \n\nIn this work we are looking for an evidence of re lationships between the \nAntarctic Ozone Hole Size (OHS) and the Solar Cy cle (SC) periodicities\, as well \nas with the Cosmic Rays (CR) fluxes. Wi th this goal in mind we also analyze the \nAntarctic temperature anomalies \, linked with the OHS\, and their response to \nthe SC and CR variations. \nBy means of wavelet transformation based on the Morlet wavelet\, it is found \nthat (OHS) present a prominent periodicity frequency at ~ 3.5 yrs . Then\, \napplying the Wavelet Coherence analysis to two time-series\, it is found:\n(1) there is a common signal along time (September-november) o f ~ 3.5 yrs. \nbetween (OHS) and Cosmic Ray (CR): from 1988 to 1990 w ith a coherence \ncoefficient of 0.8 and from 1998 to 2002 with a cohere nce coefficient of 0.9. In \nboth periods the relationship is of non-lin ear nature. (2) the coherence \nbetween the time series of (OHS) and Antar ctic temperature (AT) is of linear \nnature (anticorrelation) with a coh erence factor > 0.85 in the periods 1985-\n1990 and 1998-2002. (3) the c oherence between the time series of (RC) and \n(AT) at polar altitude of 10-30 Km is of non-linear nature between 1986-1990 \nand of linear nature in the period 1991-1996 with coherence within in the \ninterval [0.65-0.7 ] in both cases. Between 1997-2002 there is a non-linear \nrelation with s coherence in the interval [0.7-0.9]. (4) the coherence between \n(SC) and (AT) is of non-linear nature is in the range [0.7-0.85] in the perio d \n1987-1992.\nPreliminary inferences seems to indicate that there is a relationship between \nthe the Ozone Hole Size and Cosmic Rays.\n\nhttps:/ /indico.nucleares.unam.mx/event/4/session/39/contribution/1222 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/1222 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Intensity Changes and Atlantic Hurricane Intensificatio n . DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T200500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-321@cern.ch DESCRIPTION:Speakers: Prof. KAVLAKOV\, Stilian (Bulgarian Academy of Scien ces)\nEarlier we have found a significant statistical relationship between geomagnetic\nactivity as measured by the Kp index and hurricane intensity as measured by the\nmaximum wind speed for a certain type of higher-latit ude hurricanes. Here we\nreexamine this relationship comparing changes in cosmic ray intensity and hurricane\nintensification rates (time derivative of hurricane intensity). Intensification is\ncomputed using a filter (Sav itzky-Golay) especially designed for derivative\ncalculations. We conside r only hurricanes over the North Atlantic Ocean away from\nland for two re gions\, one over the tropics and one over higher latitudes. The\nregions are chosen to control for effects of sea-surface temperature and shear on \nhurricane genesis. Data are taken from all tropical cyclones passing thr ough the\nregions during the period 1950-2006. We find that intensificati on rates peaks in the\nrange of 30-50 m/s. It appears that a slight differ ence exists between the\ninterconnection cosmic ray changes - hurricane in tensification in these two regions.\n\nhttps://indico.nucleares.unam.mx/ev ent/4/session/39/contribution/321 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/321 END:VEVENT BEGIN:VEVENT SUMMARY:Discovery of VHE gamma-rays from the BL Lac object PKS0548-322 (z= 0.069) with H.E.S.S DTSTART;VALUE=DATE-TIME:20070706T194500Z DTEND;VALUE=DATE-TIME:20070706T200500Z DTSTAMP;VALUE=DATE-TIME:20260916T025227Z UID:indico-contribution-39-0-331@cern.ch DESCRIPTION:Speakers: Dr. KHELIFI\, Bruno (LLR\, Ecole Polytechnique)\nThe extreme synchrotron BL Lac object PKS 0548-322 has been observed with the High Energy Stereoscopic System (H.E.S.S) array of atmospheric-Cherenkov telescopes. The observations were performed between October 2004 and Decem ber 2006 for a total exposure of nearly 25 hours live-time.\nWe will repor t the HESS detection and present a spectral energy distribution of this ob ject using a quasi-simultaneous X-ray spectrum from archival data. It will be used to estimate some general constraints on source parameters.\n\nhtt ps://indico.nucleares.unam.mx/event/4/session/39/contribution/331 LOCATION:Merida\, Mexico Regency (Hyatt) URL:https://indico.nucleares.unam.mx/event/4/session/39/contribution/331 END:VEVENT END:VCALENDAR