Search

Your search keyword '"Thornton, G. J."' showing total 18 results
Start Over Author "Thornton, G. J." Topic fos: physical sciences
18 results on '"Thornton, G. J."'

1. Atmospheric Monitoring for the Pierre Auger Fluorescence Detector

Author

Mostafa, M. A., Fick, B., Ave, M., Letessier, A., Bertou, X., Deligny, O., Lachaud, C., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Clay, R. W., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., Brunet, J. M., Capdevielle, J. N., Cohen, F., Courty, B., Guglielmi, L., Jaeger, J. J., Benoît Revenu, Tristram, G., Waisbard, J., Billoir, P., Boratav, M., Castera, A., Sylvie DAGORET, Genolini, B., Lefebvre, F., Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Argiro, S., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, D., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Roberts, M., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Sommers, P., Luis. Anchordoqui, Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Kajita T. Asaoka Y. Kawachi A. Matsubara M. Sasaki M., PIERRE AUGER, Lantz, Simone, and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract

Major uncertainties in the fluorescence energy measurement come from the precision of various atmospheric transmission, air Cerenkov subtraction, light multiple-scattering and cloud corrections. The Auger program for atmospheric monitoring, designed to measure these corrections and to minimize these uncertainties, is summarized in this paper., Four (4) pages, and three (3) EPS figures. Proceedings of the 28th International Cosmic Ray Conference, Universal Academy Press, Inc. Tokyo, Japan, HE (2003) 465-468

Published
2003

2. Shower Studies at around $10^{18}$ eV with the Surface Detector of the Pierre Auger Observatory

Author

P-L, Ghia, Mostafa, M. A., Fick, B., Ave, M., Letessier, A., Bertou, X., Deligny, O., Lachaud, C., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Clay, R. W., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., Brunet, J. M., Capdevielle, J. N., Cohen, F., Courty, B., Guglielmi, L., Jaeger, J. J., Benoît Revenu, Tristram, G., Waisbard, J., Billoir, P., Boratav, M., Castera, A., Sylvie DAGORET, Genolini, B., Lefebvre, F., Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Argiro, S., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, D., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Roberts, M., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Sommers, P., Luis. Anchordoqui, Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Kajita T. Asaoka Y. Kawachi A. Matsubara M. Sasaki M., PIERRE AUGER, and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

Three months of data taken by the Engineering Array Surface Detector of the Pierre Auger Observatory have been analyzed with the aim of setting a procedure for the study of showers at E_0 ~ 10^18 eV. We present the results, concerning: (i) the selection procedure and the check of its efficiency; (ii) the event rate and its stability; (iii) the characteristics of such events (i.e., angular direction, energy estimator S(1000), rise time vs core distance, correlation with pressure) showing their consistency with the expectations. The performances of the whole Surface Detector of the Auger Observatory are discussed., Comment: Talk given at 28th International Cosmic Ray Conferences (ICRC 2003), Tsukuba, Japan, 31 Jul - 7 Aug 2003

Published
2003

3. The Anisotropy Search Program For the Pierre Auger Observatory

Author

Clay, W., Ave, M., Letessier, A., Bertou, X., Deligny, O., Lachaud, C., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., Brunet, J. M., Capdevielle, J. N., Cohen, F., Courty, B., Guglielmi, L., Jaeger, J. J., Benoît Revenu, Tristram, G., Waisbard, J., Billoir, P., Boratav, M., Castera, A., Sylvie DAGORET, Genolini, B., Lefebvre, F., Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Argiro, S., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, D., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Roberts, M., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Fick, B., Sommers, P., Luis. Anchordoqui, Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Kajita T. Asaoka Y. Kawachi A. Matsubara M. Sasaki M., PIERRE AUGER, and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

The Pierre Auger Southern Observatory in Argentina has begun taking data as it is being developed up to a final enclosed area of 3000 square kilometres. A key aspect of the project is to provide information on the origin of the highest energy cosmic rays through understanding the arrival directions of those particles. To avoid claims of a spurious anisotropy detection because trials have not been properly accounted, the Auger Collaboration has agreed 'a priori' to the analysis prescription presented here. It specifies the following: 1. The accumulation time for the (future) data set to be analyzed. 2. The anisotropy 'targets', each assigned a chance probability level. 3. The analysis procedure for each trial. A positive result will be claimed for any target search only if its chance probability is less than its assigned level. The levels are chosen so that the total chance probability for one or more positive results is 0.001. Exploratory searches beyond this prescription will be encouraged, but the Auger Collaboration will not assign any confidence level to anisotropies that may be discovered that way. Any such discovery would identify a good target for a prescription to be used with a subsequent Auger data set., 4 pages

Published
2003

4. Calibration of the Pierre Auger fluorescence detector

Author

Roberts, M., Ave, M., Letessier, A., Bertou, X., Deligny, O., Lachaud, C., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Clay, R. W., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., Brunet, J. M., Capdevielle, J. N., Cohen, F., Courty, B., Guglielmi, L., Jaeger, J. J., Benoît Revenu, Tristram, G., Waisbard, J., Billoir, P., Boratav, M., Castera, A., Sylvie DAGORET, Genolini, B., Lefebvre, F., Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Argiro, S., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, D., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Fick, B., Sommers, P., Luis. Anchordoqui, Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Kajita T. Asaoka Y. Kawachi A. Matsubara M. Sasaki M., PIERRE AUGER, and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics
Abstract

The absolute calibration of an air fluorescence detector (FD) is an important element in correctly determining the energy of detected cosmic rays. The absolute calibration relates the flux of photons of a given wavelength at the detector aperture to the electronic signal recorded by the FD data acquisition system. For the Auger FDs, the primary absolute calibration method uses a diffusive surface which is placed in front of a telescope aperture to uniformly illuminate the telescope field of view with a known light signal. This single-wavelength measurement (375 nm) will be made at intervals of several months until the stability of the telescopes is determined. The relative wavelength dependence of the calibration is determined through independent measurements. The error in absolute calibration at a single wavelength is estimated to be less than 10%. Two other absolute calibration methods are used to provide an independent verification of the primary measurement. The stability of the calibration with time is monitored nightly by a relative calibration system. In this paper we will provide descriptions of the absolute and relative calibration methods used by the Auger air fluorescence observatory. Results from the calibration of the Auger Engineering Array telescopes will also be presented., Comment: 4 pages, no figures. Presented at the 28th International Cosmic Ray Conference

Published
2003
Full Text
View/download PDF

5. Hybrid Performance of the Pierre Auger Observatory and Reconstruction of Hybrid Events

Author

Kick, B., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Clay, R. W., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., J-M, Brunet, J-N, Capdevielle, Cohen, F., Courty, B., Guglielmi, L., J-J, Jaeger, Benoît Revenu, Tristram, G., Waisbard, J., Bertou, X., Billoir, P., Boratav, M., Castera, A., Dagoret-Campagne, S., Deligny, O., Lachaud, C., antoine letessier selvon, Genolini, B., Fabrice Lefebvre, Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Argiro, S., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R. P., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Roberts, M., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Fick, B., Sommers, P., Anchordoqui, L., Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Kajita T. Asaoka Y. Kawachi A. Matsubara Y. Sasaki M., PIERRE AUGER, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Lantz, Simone

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

The Pierre Auger Observatory is a``hybrid'' UHECR detector. The surface detector (SD) and air fluorescence detector (FD) of the observatory are designed for observation of cosmic ray showers in coincidence, with a 10% duty cycle. The resulting data are expected to be superior in quality to those of either the SD or FD operating individually. Hybrid operation, triggering, data acquisition, and event reconstruction were successfully demonstrated during the prototype phase of the project. This paper focuses on 75 hybrid events recorded during a four month period of running with the prototype detectors in late 2001 and early 2002. The geometric technique for reconstruction of the hybrid events is described and its advantages over the traditional FD-only method are demonstrated. A lateral distribution for the water Cherenkov signals, derived from these data, is presented., Comment: Talk given at 28th International Cosmic Ray Conferences (ICRC 2003), Tsukuba, Japan, 31 Jul - 7 Aug 2003

Published
2003
Full Text
View/download PDF

6. The SNR W28 at TeV Energies

Author

Rowell, G. P., Naito, T., Dazeley, S. A., Edwards, P. G., Gunji, S., Hara, T., Holder, J., Kawachi, A., Kifune, T., Matsubara, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Nishijima, K., Ogio, S., Patterson, J. R., Roberts, M. D., Sako, T., Sakurazawa, K., Susukita, R., Tamura, T., Tanimori, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Galaxy Astrophysics
Abstract

The southern supernova remnant (SNR)W28 was observed in 1994 and 1995 by the CANGAROO 3.8m telescope in a search formulti-TeV gamma ray emission, using the Cerenkov imaging technique. We obtained upper limits for a variety of point-like and extended features within a +-1 degree-region and briefly discuss these results, together with that of EGRET within the framework of a shock acceleration model of the W28 SNR., 5 pages, 2 figures, to appear in the proceedings of the GeV-TeV Gamma-Ray Astrophysics Workshop, "Towards a Major Atmospheric Cherenkov Detector VI" (Snowbird, Utah, August 13-16, 1999)

Published
1999
Full Text
View/download PDF

7. TeV gamma-ray observations of three X-ray selected BL Lacs

Author

Roberts, M. D., Mcgee, P., steven dazeley, Edwards, P. G., Hara, T., Holder, J., Kawachi, A., Kifune, T., Matsubara, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Ogio, S., Osaki, T., Patterson, J. R., Rowell, G. P., Sako, T., Sakurazawa, K., Susukita, R., Tamura, T., Tanimori, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

Despite extensive surveys of extragalactic TeV gamma-ray candidates only 3 sources have so far been detected. All three are northern hemisphere objects and all three are low-redshift X-ray selected BL Lacs (XBLs). In this paper we present the results of observations of the three nearest southern hemisphere XBLs (PKS0548-322, PKS2005-489 and PKS2155-304) with the CANGAROO 3.8m imaging telescope. During the period of observation we estimate that the threshold of the 3.8m telescope was around 1.5TeV. Searches for both steady and short timescale emission have been performed for each source. Additionally, we are able to monitor the X-ray state of each source on a daily basis and we have made contemporaneous measurements of optical activity for PKS0548-322 and PKS2155-304., Comment: 7 pages + 3 figures. Accepted by Astron. and Astrophys

Published
1999
Full Text
View/download PDF

8. Discovery of TeV Gamma Rays from SN1006: Further Evidence for the SNR Origin of Cosmic Rays

Author

Tanimori, T., Hayami, Y., Kamei, S., Dazeley, S. A., Edwards, P. G., Gunji, S., Hara, S., Hara, T., Holder, J., Kawachi, A., Kifune, T., Kita, R., Konishi, T., Masaike, A., Matsubara, Y., Matsuoka, T., Mizumoto, Y., Mori, M., Moriya, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Oda, S., Ogio, S., Patterson, J. R., Roberts, M. D., Rowell, G. P., Sakurazawa, K., Sako, T., Sato, Y., Susukita, R., Suzuki, A., Suzuki, R., Tamura, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, High Energy Physics::Experiment, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

This paper reports the first discovery of TeV gamma-ray emission from a supernova remnant made with the CANGAROO 3.8 m Telescope. TeV gamma rays were detected at the sky position and extension coincident with the north-east (NE) rim of shell-type Supernova remnant (SNR) SN1006 (Type Ia). SN1006 has been a most likely candidate for an extended TeV Gamma-ray source, since the clear synchrotron X-ray emission from the rims was recently observed by ASCA (Koyama et al. 1995), which is a strong evidence of the existence of very high energy electrons up to hundreds of TeV in the SNR. The observed TeV gamma-ray flux was $(2.4\pm 0.5(statistical) \pm 0.7(systematic)) \times 10^{-12}$ cm$^{-2}$ s$^{-1}$ ($\ge 3.0\pm 0.9$ TeV) and $ (4.6\pm 0.6 \pm 1.4) \times 10^{-12}$ cm$^{-2}$ s$^{-1}$ ($\ge 1.7\pm 0.5$ TeV) from the 1996 and 1997 observations, respectively. Also we set an upper limit on the TeV gamma-ray emission from the SW rim, estimated to be $ 1.1 \times 10^{-12}$ cm$^{-2}$ s$^{-1}$ ($\ge 1.7\pm 0.5$ TeV, 95% CL) in the 1997 data. The TeV gamma rays can be attributed to the 2.7 K cosmic background photons up-scattered by electrons of energies up to about 10$^{14}$ eV by the inverse Compton (IC) process. The observed flux of the TeV gamma rays, together with that of the non-thermal X-rays, gives firm constraints on the acceleration process in the SNR shell; a magnetic field of $6.5\pm2$ $\mu$G is inferred from both the synchrotron X-rays and inverse Compton TeV gamma-rays, which gives entirely consistent mechanisms that electrons of energies up to 10$^{14}$ eV are produced via the shock acceleration in SN1006., Comment: 17 pages, 3 figures, LaTeX2.09 with AASTeX 4.0 maros, to appear in Astrophys. J. Lett

Published
1998

9. TeV Gamma-ray Observations of Southern AGN with the CANGAROO 3.8m Telescople

Author

Roberts, M. D., Dazeley, S. A., Edwards, P. G., Hara, T., Hayami, Y., Kamei, S., Kifune, T., Kita, R., Konishi, T., Masaike, A., Matsubara, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Ogio, S., Patterson, J. R., Rowell, G. P., Sako, T., Sakurazawa, K., Susukita, R., Suzuki, A., Suzuki, R., Tamura, T., Tanimori, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

Since 1992 the CANGAROO 3.8m imaging telescope has been used to search for sources of TeV gamma-rays. Results are presented here for observations of four Southern Hemisphere BL-Lacs - PKS0521-365, PKS2316-423, PKS2005-489 and EXO0423-084. In addition to testing for steady DC emission, a night by night burst excess search has been performed for each source., 4 pages, 1 figure, LaTeX 2e with epsfig.sty, wrapfig.sty to appear in proceedings of the 25th ICRC, Durban, 1997

Published
1997

10. Observations of Pulsars, PSR 1509-58 and PSR 1259-63, by CANGAROO 3.8 m Telescope

Author

Sako, T., Dazeley, S. A., Edwards, P. G., Hara, T., Hayami, Y., Kamei, S., Kifune, T., Kita, R., Konishi, T., Masaike, A., Matsubara, Y., Matsuoka, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Ogio, S., Patterson, J. R., Roberts, M. D., Rowell, G. P., Sakurazawa, K., Susukita, R., Suzuki, A., Suzuki, R., Tamura, T., Tanimori, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The data for VHE (~TeV) gamma rays from young gamma-ray pulsar PSR1509-58 observed in 1996 with the CANGAROO 3.8m Cerenkov imaging telescope are presented, as well as the additional data from March to June of 1997. The high spin-down luminosity of the pulsar and the plerionic feature around the pulsar observed with radio and X-rays suggest that VHE gamma-ray emission is quite likely above the sensitivity of the CANGAROO telescope. The CANGAROO results on other pulsars, such as PSR1259-63, are also presented. PSR1259-63 is a highly eccentric X-ray binary system, which includes a high mass Be companion star, and a preliminary analysis on the data taken 4 months after the periastron in 1994 suggests emission of VHE gamma rays., 4 pages, 1 figure, LaTeX 2.09 with epsfig.sty, wrapfig.sty to appear in proceedings of the 25th ICRC, Durban, 1997

Published
1997

11. Very High Energy Gamma Rays from the Vela Pulsar/Nebula

Author

Yoshikoshi, T., Kifune, T., Dazeley, S. A., Edwards, P. G., Hara, T., Hayami, Y., Kamei, S., Kita, R., Konishi, T., Masaike, A., Matsubara, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Ogio, S., Patterson, J. R., Roberts, M. D., Rowell, G. P., Sako, T., Sakurazawa, K., Susukita, R., Suzuki, A., Suzuki, R., Tamura, T., Tanimori, T., Thornton, G. J., Yanagita, S., and Yoshida, T.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cherenkov telescope near Woomera, South Australia every year since 1992. This is the first concerted search for pulsed and unpulsed emission from the Vela region, and the imaging technique also allows the location of the emission within the field of view to be examined. A significant excess of gamma-ray-like events is found offset from the Vela pulsar to the southeast by about 0.13deg. The excess shows the behavior expected of gamma-ray images when the asymmetry cut is applied to the data. There is no evidence for the emission being modulated with the pulsar period -- in contrast to earlier claims of signals from the Vela pulsar direction., 4 pages, 2 figure, LaTeX2.09 with epsfig.sty, to appear in proceedings of the 25th ICRC, Durban, 1997

Published
1997

12. Observation of Spectrum of TeV Gamma Rays up to 60 TeV from the Crab at the Large Zenith Angles

Author

Sakurazawa, K., Tanimori, T., Dazeley, S. A., Edwards, P. G., Hara, T., Kamei, S., Kifune, T., Kita, R., Konishi, T., Masaike, A., Matsubara, Y., Matsuoka, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Ogio, S., Patterson, J. R., Roberts, M. D., Rowell, G. P., Sako, T., Susukita, R., Suzuki, A., Suzuki, R., Tamura, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

The CANGAROO experiment has observed gamma-ray above 7TeV from the Crab pulsar/nebula at large zenith angle in Woomera, South Australia. We report the CANGAROO data taken in 1992, 1993 and 1995, from which it appears that the energy spectrum extends at least up to 50 TeV. The observed integral spectrum is (8.4+-1.0) x 10^{-13}(E/7 TeV)^(-1.53+-0.15)cm^{-2}s^{-1} between 7 TeV and 50 TeV. In November 1996, the 3.8m mirror was recoated in Australia, and its reflectivity was improved to be about 90% as twice as before. Due to this recoating, the threshold energy of ~4 TeV for gamma rays has been attained in the observation of the Crab at large zenith angle. Here we also report the preliminary result taken in 1996., Comment: 4 pages, 2 figures, LaTeX 2.09 with epsfig.sty, to appear in proceedings of the 25th ICRC, Durban, 1997

Published
1997
Full Text
View/download PDF

13. Detection of Gamma Rays of Up to 50 TeV From the Crab Nebula

Author

Tanimori, T., Sakurazawa, K., Dazeley, S. A., Edwards, P. G., Hara, T., Hayami, Y., Kamei, S., Kita, R., Kifune, T., Konishi, T., Masaike, A., Matsubara, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Ogio, S., Patterson, J. R., Roberts, M. D., Rowell, G. P., Sako, T., Susukita, R., Suzuki, A., Suzuki, R., Tamura, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Physics::Accelerator Physics, FOS: Physical sciences, High Energy Physics::Experiment, Astrophysics
Abstract

Gamma rays with energies greater than 7 TeV from the Crab pulsar/nebula have been observed at large zenith angles, using the Imaging Atmospheric Technique from Woomera, South Australia. CANGAROO data taken in 1992, 1993 and 1995 indicate that the energy spectrum extends up to at least 50 TeV, without a change of the index of the power law spectrum. The observed differential spectrum is \noindent $(2.01\pm 0.36)\times 10^{-13}(E/{7 TeV})^{-2.53 \pm 0.18} TeV^{-1}cm^{-2}s^{-1}$ between 7 TeV and 50 TeV. There is no apparent cut-off. The spectrum for photon energies above $\sim$10 TeV allows the maximum particle acceleration energy to be inferred, and implies that this unpulsed emission does not originate near the light cylinder of the pulsar, but in the nebula where the magnetic field is not strong enough to allow pair creation from the TeV photons. The hard gamma-ray energy spectrum above 10 TeV also provides information about the varying role of seed photons for the inverse Compton process at these high energies, as well as a possible contribution of $\pi ^{\circ}$-gamma rays from proton collisions., Comment: 19 pages, 4 figures, LaTeX2.09 with AASTeX 4.0 maros, to appear in Astrophys. J. Lett

Published
1997
Full Text
View/download PDF

14. The Lateral Distribution Function of Shower Signals in the Surface Detector of the Pierre Auger Observatory

Author

Roth, M., Ave, M., Letessier, A., Bertou, X., Deligny, O., Lachaud, C., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Clay, R. W., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., Brunet, J. M., Capdevielle, J. N., Cohen, F., Courty, B., Guglielmi, L., Jaeger, J. J., Benoît Revenu, Tristram, G., Waisbard, J., Billoir, P., Boratav, M., Castera, A., Sylvie DAGORET, Genolini, B., Lefebvre, F., Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Argiro, S., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, D., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Roberts, M., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Fick, B., Sommers, P., Luis. Anchordoqui, Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Lantz, Simone, Kajita T. Asaoka Y. Kawachi A. Matsubara M. Sasaki M., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), PIERRE AUGER, and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

The surface detector (SD) array of the southern Pierre Auger Observatory will consist of a triangular grid of 1600 water Cherenkov tanks with 1.5 km spacing. For zenith angles less than 60deg the primary energy can be estimated from the signal S(1000) at a distance of about 1000m from the shower axis, solely on basis of SD data. A suitable lateral distribution function (LDF) S(r) is fitted to the signals recorded by the water tanks and used to quantify S(1000). Therefore, knowledge of the LDF is a fundamental requirement for determining the energy of the primary particle. The Engineering Array (EA), a prototype facility consisting of 32 tanks, has taken data continuously since late 2001. On the basis of selected experimental data and Monte Carlo simulations various preliminary LDFs are examined., To appear in the proceedings of the 28th ICRC (Tsukuba, Japan), 4 pages, 2 figures

15. TeV gamma-ray observations of southern BL lacs with the CANGAROO 3.8m Imaging telescope

Author

Roberts, M. D., Dazeley, S. A., Edwards, P. G., Hara, T., Hayami, Y., Holder, J., Kakimoto, F., Kamei, S., Kawachi, A., Kifune, T., Kita, R., Konishi, T., Masaike, A., Matsubara, Y., Matsuoka, T., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Nishijima, K., Oda, S., Ogio, S., Patterson, J. R., Gavin Rowell, Sako, T., Sakurazawa, K., Susukita, R., Suzuki, A., Suzuki, R., Tamura, T., Tanimori, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

Observational and theoretical results indicate that low-redshift BL Lacertae objects are the most likely extragalactic sources to be detectable at TeV energies. In this paper we present the results of observations of 4 BL Lacertae objects (PKS0521-365, EXO0423.4-0840, PKS2005-489 and PKS2316-423) made between 1993 and 1996 with the CANGAROO 3.8m imaging Cherenkov telescope. During the period of these observations the gamma-ray energy threshold of the 3.8m telescope was ~2TeV. Searches for steady long-term emission have been made, and, inspired by the TeV flares detected from Mkn421 and Mkn501, a search on a night-by-night timescale has also been performed for each source. Comprehensive Monte Carlo simulations are used to estimate upper limits for both steady and short timescale emission., 6 pages including 2 figures

16. Performance of the Pierre Auger Fluorescence Detector and Analysis of well recontructed events

Author

Argiro, S., Clay, W., Ave, M., Letessier, A., Bertou, X., Deligny, O., Lachaud, C., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., Brunet, J. M., Capdevielle, J. N., Cohen, F., Courty, B., Guglielmi, L., Jaeger, J. J., Benoît Revenu, Tristram, G., Waisbard, J., Billoir, P., Boratav, M., Castera, A., Sylvie DAGORET, Genolini, B., Lefebvre, F., Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, D., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Roberts, M., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Fick, B., Sommers, P., Luis. Anchordoqui, Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Kajita T. Asaoka Y. Kawachi A. Matsubara M. Sasaki M, PIERRE AUGER, and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics
Abstract

The Pierre Auger Observatory is designed to elucidate the origin and nature of Ultra High Energy Cosmic Rays using a hybrid detection technique. A first run of data taking with a prototype version of both detectors (the so called Engineering Array) took place in 2001-2002, allowing the Collaboration to evaluate the performance of the two detector systems and to approach an analysis strategy. In this contribution, after a brief description of the system, we will report some results on the behavior of the Fluorescence Detector (FD) Prototype. Performance studies, such as measurements of noise, sensitivity and duty cycle, will be presented. We will illustrate a preliminary analysis of selected air showers. This analysis is performed using exclusively the information from the FD, and includes reconstruction of the shower geometry and of the longitudinal profile, Presented at the 28th International Cosmic Ray Conferences (ICRC 2003), Tsukuba, Japan, 31 Jul - 7 Aug 2003

17. Observations of the supernova remnant W28 at TeV energies

Author

Gavin Rowell, Naito, T., Dazeley, S. A., Edwards, P. G., Gunji, S., Hara, T., Holder, J., Kawachi, A., Kifune, T., Matsubara, Y., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Nishijima, K., Ogio, S., Patterson, J. R., Roberts, M. D., Sako, T., Sakurazawa, K., Susukita, R., Tamura, T., Tanimori, T., Thornton, G. J., Yanagita, S., Yoshida, T., and Yoshikoshi, T.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The atmospheric Cerenkov imaging technique has been used to search for point-like and diffuse TeV gamma-ray emission from the southern supernova remnant, W28, and surrounding region. The search, made with the CANGAROO 3.8m telescope, encompasses a number of interesting features, the supernova remnant itself, the EGRET source 3EG J1800-2338, the pulsar PSR J1801-23, strong 1720 MHz OH masers and molecular clouds on the north and east boundaries of the remnant. An analysis tailored to extended and off-axis point sources was used, and no evidence for TeV gamma-ray emission from any of the features described above was found in data taken over the 1994 and 1995 seasons. Our upper limit (E>1.5 TeV) for a diffuse source of radius 0.25deg encompassing both molecular clouds was calculated at 6.64e-12 photons cm^-2 s^-1 (from 1994 data), and interpreted within the framework of a model predicting TeV gamma-rays from shocked-accelerated hadrons. Our upper limit suggests the need for some cutoff in the parent spectrum of accelerated hadrons and/or slightly steeper parent spectra than that used here (-2.1). As to the nature of 3EG J1800-2338, it possibly does not result entirely from pi-zero decay, a conclusion also consistent with its location in relation to W28., 11 pages, 5 figures. Accepted for publication in Astronomy and Astrophysics

18. Processing of the Signals from the Surface Detectors of the Pierre - Auger Observatory

Author

Roberts, M., Ave, M., Letessier, A., Bertou, X., Deligny, O., Lachaud, C., Altmann, E., Alvarez, P., Bauleo, P., Bonifazi, C., Etchegoyen, A., Eusebi, R., Fazzini, N., Ferrero, A., Filevich, A., Reguera, A., Cillis, A., Dova, M. T., Epele, L. N., Grunfeld, C., Mariazzi, A., Martinez, N., Roulet, E., Sciutto, S. J., Veiga, A., Allekotte, I., Avila, G., Masperi, L., Orsaria, M., Rovero, A., Clay, R. W., Dawson, B. R., Pace, R., Riordan, D., Thornton, G. J., Wild, N. R., Boutonnet, C., Brunet, J. M., Capdevielle, J. N., Cohen, F., Courty, B., Guglielmi, L., Jaeger, J. J., Benoît Revenu, Tristram, G., Waisbard, J., Billoir, P., Boratav, M., Castera, A., Sylvie DAGORET, Genolini, B., Lefebvre, F., Lhenry-Yvon, I., Trung, T. N., Parizot, E., Pouthas, J., Suomijarvi, T., Albert, J. N., Arnault, C., Bilhaut, R., Cordier, A., Cormier, E., Eschstruth, P., Jouniaux, O., Lavigne, B., Oleg Lodygensky, Rypko, J., Martin Urban, Bluemer, H., Bollmann, E., Csabo, T., Grindler, A., Gumbsheimer, R., Heck, D., Hucker, H., Kern, H., Klages, H. O., Kleinfeller, J., Mathes, H. J., Matussek, P., Michel-Piper, I., Risse, M., Schleif, G., Thouw, T., Balzer, M., Berg, R., Bormann, D., Gemmeke, H., Giraud, H., Kleifges, M., Kopmann, A., Kunka, N., Menchikov, A., Osswald, B., Remmel, U., Tscherniakhovski, D., Barenthien, N., Kampert, K. H., Keilhauer, B., Argiro, S., Camin, D. V., Guerard, C., Ambrosio, M., Bernardini, C., Facal, P., Filosofi, R., Fois, M., Matthiae, G., Privitera, P., Salina, G., Borreani, G., Cester, R., Menichetti, E., Pastrone, N., Aramo, C., Cangiano, E., Fonte, R., Insolia, A., Raia, G., Gora, D., Homola, P., Kutschera, M., Ostrowski, M., Wilczynska, B., Wilczynski, H., Arcon, I., Filipcic, A., Zavrtanik, D., Zavrtanik, M., Clark, P., Bruijn, L., Knapp, J., Lloyd-Evans, J., Patel, M., Tunnicliffe, V., Walker, P., Watson, A., Arisaka, K., Bonushkin, Y., Kubic, J., Slater, W., Tripathi, A., Brack, J., Hofman, G., Ristinen, R., Harton, J., Sites, J., Warner, D., Wilson, R., Cronin, J. W., Gibbs, K., Albrow, M., Andrews, R., Berman, E., Hoffer, D., Glass, H., Hojvat, C., Mantsch, P., Mazur, P., Spinka, H., Voyvodic, L., Matthews, J. M., Mcewen, M., Meyhandan, R., Darling, J., Dorofeev, A., Nemiroff, B., Nitz, D., Rafert, B., Ruotsala, S., Szadkowski, Z., Trombley, M., Dieterle, B., Matthews, J., Riley, S., Allison, P., Beatty, J., Coutu, S., Duvernois, M., Cassiday, G., Fick, B., Sommers, P., Luis. Anchordoqui, Machacek, M., Paul, T., Swain, J., Taylor, L., Akhperjanian, A., Chilingarian, A., Hovsepian, G., Mnatzakanian, E., Sahakian, V., Ter-Antonian, S., Aguirre, C., Bustos, R., Choque, K., Ticona, A., Ticona, R., Velarde, A., Thieu, D. Q., Darriulat, P., Chung, N., Dzung, N. T., Dinh, P. N., Phuong, P. T., Thuan, V. V., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Kajita T. Asaoka Y. Kawachi A. Matsubara M. Sasaki M., PIERRE AUGER, Lantz, Simone, and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics
Abstract

The detectors of the surface array of the Pierre Auger Observatory are water Cherenkov tanks. The signals from each tank are read out using three photomultipliers. The energy of the primary particle is inferred from signal densities and requires good linearity of the PMTs and a large dynamic range. The absolute time of arrival of the shower front at each tank is obtained from the Global Positioning System (GPS) with a resolution of about 10 ns, ensuring an accurate primary angular reconstruction. Additionally, it is intended to use the rise time and shape of the signals to constrain the nature of the primary particle: this sets further requirements on the signal processing. In this paper, the main features of the signal processing associated with the surface detector will be presented and its performance will be discussed in the context of the extraction of shower parameters., Comment: Submitted to 28th International Cosmic Ray Conferences (ICRC 2003), Tsukuba, Japan, 31 Jul - 7 Aug 2003

Catalog

Books, media, physical & digital resources
See catalog results