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1. Combined spatial and retrospective analysis of fluoroalkyl chemicals in fluvial sediments reveal changes in levels and patterns over the last 40 years

Author: J. Raux, Pierre Labadie, Marc Desmet, Marc Babut, Hélène Budzinski, Cécile Grosbois, Yoann Copard, Patrick Pardon, Brice Mourier, Maxime Debret, Impacts des Polluants sur les Écosystèmes, Laboratoire d'Ecologie des Hydrosystèmes Naturels et Anthropisés (LEHNA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physico -& Toxico Chimie des systèmes naturels (LPTC), Université Sciences et Technologies - Bordeaux 1-Centre National de la Recherche Scientifique (CNRS), GéoHydrosystèmes COntinentaux (GéHCO EA6293), Université de Tours, Morphodynamique Continentale et Côtière (M2C), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires (ISM), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Agence de l'Eau Rhin-Meuse, Rhone-Mediterranean and Corsica Water Agency, Region Auvergne-Rhone-Alpes, Region Nouvelle-Aquitaine, European Union (EU), French National Research Agency (ANR) ANR-10-LABX-45, Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE), Centre National de la Recherche Scientifique (CNRS)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Caen Normandie (UNICAEN), Normandie Université (NU), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS), and Université de Tours (UT)
Subjects: Geologic Sediments, 010504 meteorology & atmospheric sciences, Health, Toxicology and Mutagenesis, Carboxylic Acids, Drainage basin, Fluvial, 010501 environmental sciences, Toxicology, 01 natural sciences, chemistry.chemical_compound, Manufacturing and Industrial Facilities, Rivers, Dry weight, Water Pollution, Chemical, Retrospective analysis, Sediment core, Retrospective Studies, 0105 earth and related environmental sciences, Spatial trend, Fluorocarbons, geography, geography.geographical_feature_category, Rhône river, General Medicine, Contamination, Pollution, 6. Clean water, Bed sediment, Perfluorooctane, Alkanesulfonic Acids, chemistry, 13. Climate action, Environmental chemistry, [SDE]Environmental Sciences, Environmental science, Per- and polyfluoroalkyl substances, France, Temporal trend, Sulfonic Acids, Long chain, Water Pollutants, Chemical, Environmental Monitoring
Abstract: International audience; Bed sediments and a dated sediment core were collected upstream and downstream from the city of Lyon (France) to assess the spatial and temporal trends of contamination by per- and polyfluoroalkyl substances (PFASs) in this section of the Rhône River. Upstream from Lyon, concentrations of total PFASs (ΣPFASs) in sediments are low (between 0.19 and 2.6 ng g−1 dry weight - dw), being characterized by a high proportion of perfluorooctane sulfonate (PFOS). Downstream from Lyon, and also from a fluoropolymer manufacturing plant, ΣPFASs concentrations reach 48.7 ng g−1 dw. A gradual decrease of concentrations is reported at the coring site further downstream (38 km). Based on a dated sediment core, the temporal evolution of PFASs is reconstructed from 1984 to 2013. Prior to 1987, ΣPFASs concentrations were low (≤2 ng g−1 dw), increasing to a maximum of 51 ng g−1 dw in the 1990s and then decreasing from 2002 to the present day (∼10 ng g−1 dw). In terms of the PFAS pattern, the proportion of perfluoroalkyl sulfonic acids (PFSAs) has remained stable since the 1980s (∼10%), whereas large variations are reported for carboxylic acids (PFCAs). Long chain- (C > 8) PFCAs characterized by an even number of perfluorinated carbons represent about 74% of the total PFAS load until 2005. However, from 2005 to 2013, the relative contribution of long chain- (C > 8) PFCAs with an odd number of perfluorinated carbons reaches 80%. Such changes in the PFAS pattern likely highlight a major shift in the industrial production process. This spatial and retrospective study provides valuable insights into the long-term contamination patterns of PFAS chemicals in river basins impacted by both urban and industrial activities.
Published: 2019
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2. RestframeI-band Hubble diagram for type Ia supernovae up to redshiftz$\mathsf{\sim}$ 0.5

Author: Supernova Cosmology, I. M. Hook, Vitaliy Fadeyev, Vallery Stanishev, Saul Perlmutter, G. Sainton, Ling-Jun Wang, A. L. Spadafora, P. Antilogus, D. E. Groom, D. A. Howell, Sebastien Fabbro, J. Raux, S. Nobili, Chris Lidman, Ariel Goobar, S. E. Deustua, Alex Conley, P. Ruiz-Lapuente, R. A. Knop, A. G. Kim, G. Garavini, R. Gibbons, Richard Ellis, G. Folatelli, Rahman Amanullah, M. S. Burns, Nicolas Regnault, Eric P. Smith, R. C. Thomas, R. M. Quimby, Peter Nugent, Greg Aldering, G. Goldhaber, Pierre Astier, K. Schahmaneche, and R. Pain
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Diagram, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Intergalactic dust, Light curve, Lambda, 01 natural sciences, Omega, Redshift, Universe, Supernova, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We present a novel technique for fitting restframe I-band light curves on a data set of 42 Type Ia supernovae (SNe Ia). Using the result of the fit, we construct a Hubble diagram with 26 SNe from the subset at 0.01< z
Published: 2005
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3. Supernova photometric data analysis and reduction details

Author: J. Raux
Subjects: Reduction (complexity), Physics, Supernova, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Reduction methods, Astrophysics::Galaxy Astrophysics
Abstract: This paper presents reduction methods in photometric analysis, currently used for type Ia supernova surveys.
Published: 2004
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4. Spectroscopic observations of eight supernovae at intermediate redshift

Author: Mike Irwin, J. Raux, K. Schahmaneche, Sebastien Fabbro, G. Garavini, R. Pascoal, Christophe Balland, Nicholas A. Walton, S. Nobili, Reynald Pain, Pierre Astier, Rahman Amanullah, Richard G. McMahon, Ariel Goobar, Gastón Folatelli, A. Mourao, D. Hardin, M. Mouchet, G. Sainton, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris
Subjects: Physics, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, Space and Planetary Science, Homogeneous, 0103 physical sciences, William Herschel Telescope, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We present spectra of six Type Ia and two Type II supernovae obtained in June 2002 at the William Herschel Telescope during a search for Type Ia supernovae (SNIa) at intermediate redshift. Supernova type identification and phase determination are performed using a fitting technique based on a Xi2 minimization against a series of model templates. The spectra range from z=0.033 to z=0.328, including one spectroscopically underluminous SNIa at z=0.033. This set of spectra significantly increases the sample of well-observed type SNIa supernovae available in the range 0.15< z, 30 pages, 15 figures. Published in A&A
Published: 2007
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5. Discovery of Very-High-Energy Gamma-Rays from the Galactic Centre Ridge

Author: V. Sahakian, Conor Masterson, Michael Punch, D. Hauser, M. Beilicke, A. Djannati-Ataï, C. Stegmann, Stefan Gillessen, G. Fontaine, Christo Venter, B. Degrange, Wystan Benbow, J. L. Osborne, F. Feinstein, Luigi Costamante, L. O'c. Drury, F. Breitling, Dieter Horns, M. Lemoine-Goumard, M. Tluczykont, A. M. Brown, Helene Sol, P. Espigat, N. Leroy, Gavin Rowell, Konrad Bernlöhr, R. Le Gallou, J.-P. Tavernet, P. M. Chadwick, M. Panter, L. Rolland, G. Pühlhofer, G. Heinzelmann, I. J. Latham, A. Reimer, Olaf Reimer, A. Lemiere, M. de Naurois, Nu. Komin, R. Cornils, S. J. Nolan, Martin Raue, M. Hauser, Ullrich Schwanke, P. Goret, A. G. Akhperjanian, S. M. Rayner, R. Steenkamp, C. G. Théoret, Jim Hinton, Guy Pelletier, Ilana M. Braun, Sven Klages, J. Raux, K. J. Orford, M. Siewert, C. van Eldik, O. Bolz, M. Holleran, A. Noutsos, P. Vincent, S. Schlenker, Werner Hofmann, Y. Fuchs, Felix Aharonian, T. J. L. McComb, A. Jacholkowska, A. Konopelko, Heinrich J. Völk, Gilles Henri, Reinhard Schlickeiser, Dimitrios Emmanoulopoulos, V. Borrel, Hugh Dickinson, A. R. Bazer-Bachi, B. Giebels, O. C. de Jager, Stefan Wagner, J. Ripken, L. Saugé, Stefan Funk, Jean Michel Martin, David Berge, Thomas Lohse, D. Spangler, Catherine Boisson, S. Pita, B. Khélifi, G. Hermann, Regis Terrier, Y. A. Gallant, C. Schuster, B. C. Raubenheimer, J. F. Glicenstein, O. Martineau-Huynh, L. Rob, M. Ouchrif, G. Vasileiadis, C. Hadjichristidis, Guillaume Dubus, L.-M. Chounet, A. Marcowith, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), HESS, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, and Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Acceleration, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sagittarius-A, 01 natural sciences, Emission, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova remnant, 0103 physical sciences, Molecular clouds, Center region, Shell, High Energy Stereoscopic System, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Sagittarius A, Physics, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Molecular cloud, Astrophysics (astro-ph), Astronomy, Mass, Galaxy, Supernova, Direction, 13. Climate action
Abstract: The origin of Galactic cosmic rays (with energies up to 10^15 eV) remains unclear, though it is widely believed that they originate in the shock waves of expanding supernova remnants. Currently the best way to investigate their acceleration and propagation is by observing the gamma-rays produced when cosmic rays interact with interstellar gas. Here we report observations of an extended region of very high energy (VHE, >100 GeV) gamma-ray emission correlated spatially with a complex of giant molecular clouds in the central 200 pc of the Milky Way. The hardness of the gamma-ray spectrum and the conditions in those molecular clouds indicate that the cosmic rays giving rise to the gamma-rays are likely to be protons and nuclei rather than electrons. The energy associated with the cosmic rays could have come from a single supernova explosion around 10,000 years ago., 8 pages, 3 figures, published in Nature
Published: 2006
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6. A low level of extragalactic background light as revealed by gamma-rays from blazars

Author: P. Espigat, Michael Punch, Olaf Reimer, D. Hauser, M. Beilicke, O. C. de Jager, F. Breitling, Dieter Horns, Wystan Benbow, Stefan Wagner, C. van Eldik, Y. Fuchs, M. Holleran, S. Schlenker, Felix Aharonian, J. Raux, Nu. Komin, Werner Hofmann, P. Goret, Jim Hinton, Gilles Henri, J.-P. Tavernet, Sven Klages, K. J. Orford, C. Hadjichristidis, Guillaume Dubus, V. Borrel, M. Panter, L. Rob, M. Ouchrif, M. de Naurois, M. Hauser, G. Vasileiadis, D. Spangler, A. Djannati-Ataï, B. Giebels, Christo Venter, A. Noutsos, V. Sahakian, T. J. L. McComb, P. M. Chadwick, A. Jacholkowska, Conor Masterson, Martin Raue, G. Fontaine, R. Le Gallou, N. Leroy, M. Siewert, C. Stegmann, Stefan Gillessen, B. C. Raubenheimer, R. Cornils, J. L. Osborne, L. Rolland, S. Pita, F. Feinstein, A. M. Brown, I. J. Latham, B. Degrange, P. Vincent, M. Lemoine-Goumard, B. Khélifi, G. Hermann, Regis Terrier, S. M. Rayner, S. J. Nolan, J. F. Glicenstein, O. Martineau-Huynh, Guy Pelletier, Dimitrios Emmanoulopoulos, G. Heinzelmann, M. Tluczykont, A. R. Bazer-Bachi, Konrad Bernlöhr, Heinrich J. Völk, G. Pühlhofer, A. Reimer, Ilana M. Braun, Luigi Costamante, A. Konopelko, L. O'c. Drury, Reinhard Schlickeiser, O. Bolz, Hugh Dickinson, Jean Michel Martin, Anne Lemiere, Gavin Rowell, David Berge, L.-M. Chounet, A. Marcowith, C. Schuster, Thomas Lohse, J. Ripken, L. Saugé, Stefan Funk, Y. A. Gallant, Catherine Boisson, C. G. Théoret, Helene Sol, Ullrich Schwanke, A. G. Akhperjanian, and R. Steenkamp
Subjects: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Space, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Absorption, Universe, Spectrum, 0103 physical sciences, Galaxy formation and evolution, H1426+428, Blazar, 010303 astronomy & astrophysics, Telescope, Astrophysics::Galaxy Astrophysics, media_common, Physics, Multidisciplinary, 010308 nuclear & particles physics, 2Mass, Astrophysics (astro-ph), Astronomy, Stars, Redshift, Galaxy, Extragalactic background light, High-energy photons, Intergalactic travel, MKN 501
Abstract: The diffuse extragalactic background light consists of the sum of the starlight emitted by galaxies through the history of the Universe, and it could also have an important contribution from the first stars, which may have formed before galaxy formation began. Direct measurements are difficult and not yet conclusive, owing to the large uncertainties caused by the bright foreground emission associated with zodiacal light. An alternative approach is to study the absorption features imprinted on the gamma-ray spectra of distant extragalactic objects by interactions of those photons with the background light photons. Here we report the discovery of gamma-ray emission from the blazars H 2356-309 and 1ES 1101-232, at redshifts z=0.165 and z=0.186, respectively. Their unexpectedly hard spectra provide an upper limit on the background light at optical/near-infrared wavelengths that appears to be very close to the lower limit given by the integrated light of resolved galaxies. The background flux at these wavelengths accordingly seems to be strongly dominated by the direct starlight from galaxies, thus excluding a large contribution from other sources -- in particular from the first stars formed. This result also indicates that intergalactic space is more transparent to gamma-rays than previously thought., 15 pages, 7 figures. Accepted by Nature, in press (April 20 issue). Replaced with published version. Title changed, text and figures rearranged with addition of Supplementary Information
Published: 2005

7. Spectroscopic confirmation of high-redshift supernovae with the ESO VLT ***

Author: Vallery Stanishev, Peter Nugent, Nobunari Kashikawa, Alex Conley, Chris Lidman, A. G. Kim, Mamoru Doi, Bradley E. Schaefer, D. A. Howell, Vitaliy Fadeyev, W. M. Wood-Vasey, A. L. Spadafora, J. Raux, Tomoki Morokuma, Nicholas A. Walton, I. M. Hook, Naoki Yasuda, K. Schahmaneche, P. Antilogus, Greg Aldering, G. Goldhaber, V. Prasad, Robert Quimby, Kentaro Motohara, R. A. Knop, R. Gibbons, S. Nobili, Reynald Pain, Pierre Astier, Brian C. Lee, Guillermo A. Blanc, M. S. Burns, Saul Perlmutter, Eric P. Smith, Sebastien Fabbro, Nicolas Regnault, Ariel Goobar, G. Sainton, Lifan Wang, S. E. Deustua, Gastón Folatelli, Richard S. Ellis, Javier Méndez, Rahman Amanullah, Donald E. Groom, G. Garavini, Pilar Ruiz-Lapuente, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), SUPERNOVAE, and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Physics, supernovae : general [stars], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Light curve, Redshift, Spectral line, observations [cosmology], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, Space and Planetary Science, astro-ph, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences
Abstract: We present VLT FORS1 and FORS2 spectra of 39 candidate high-redshift supernovae that were discovered as part of a cosmological study using Type Ia supernovae (SNe Ia) over a wide range of redshifts. From the spectra alone, 20 candidates are spectrally classified as SNe Ia with redshifts ranging from z=0.212 to z=1.181. Of the remaining 19 candidates, 1 might be a Type II supernova and 11 exhibit broad supernova-like spectral features and/or have supernova-like light curves. The candidates were discovered in 8 separate ground-based searches. In those searches in which SNe Ia at z ~ 0.5 were targeted, over 80% of the observed candidates were spectrally classified as SNe Ia. In those searches in which SNe Ia with z > 1 were targeted, 4 candidates with z > 1 were spectrally classified as SNe Ia and later followed with ground and space based observatories. We present the spectra of all candidates, including those that could not be spectrally classified as supernova., 30 pages, 43 figures. Accepted by A&A. A version with higher resolution finding charts is available at http://supernova.lbl.gov/
Published: 2005
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8. Multi-wavelength observations of PKS 2155-304 with H.E.S.S

Author: F. Aharonian, A. G. Akhperjanian, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, K. Bernlöhr, C. Boisson, O. Bolz, V. Borrel, I. Braun, F. Breitling, A. M. Brown, P. M. Chadwick, L.-M. Chounet, R. Cornils, L. Costamante, B. Degrange, H. J. Dickinson, A. Djannati-Ataï, null L. O'C. Drury, G. Dubus, D. Emmanoulopoulos, P. Espigat, F. Feinstein, G. Fontaine, Y. Fuchs, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, J. F. Glicenstein, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, A. Jacholkowska, O. C. de Jager, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, A. Lemière, M. Lemoine-Goumard, N. Leroy, T. Lohse, J. M. Martin, O. Martineau-Huynh, A. Marcowith, C. Masterson, T. J. L. McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, D. Spangler, R. Steenkamp, C. Stegmann, J.-P. Tavernet, R. Terrier, C. G. Théoret, M. Tluczykont, G. Vasileiadis, C. Venter, P. Vincent, null H. J . Völk, S. J. Wagner, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), HESS, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Energy gamma Rays, Photon, Astrophysics::High Energy Astrophysical Phenomena, Hadron, Proportional counter, FOS: Physical sciences, radiation mechanisms: non thermal, Astrophysics, Synchrotron-proton blazar, 01 natural sciences, galaxie: active, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Tev blazars, Atmospheric Cherenkov telescopes, 0103 physical sciences, X-rays, Radiation mechanisms, High Energy Stereoscopic System, Spectral variability, 010303 astronomy & astrophysics, Observations, BL Lacertae objects: Individual: PKS 2155-304, PKS 2155-304, Physics, Active galactic nuclei, Non thermal, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, BL-LAC objects, Astrophysics (astro-ph), X-rays:galaxies, Astronomy and Astrophysics, 13. Climate action, Space and Planetary Science, Active galaxies, Satellite, Simultaneous x-ray, Kilosecond, gamma rays: observations, BL Lac object
Abstract: The High Energy Stereoscopic System (H.E.S.S.) has observed the high-frequency peaked BL Lac object PKS2155-304 in 2003 between October 19 and November 26 in Very High Energy (VHE) gamma-rays (E>160 GeV for these observations). Observations were carried out simultaneously with the Proportional Counter Array (PCA) on board the Rossi X-ray Timing Explorer satellite (RXTE), the Robotic Optical Transient Search Experiment (ROTSE) and the Nancay decimetric radiotelescope (NRT). Intra-night variability is seen in the VHE band, the source being detected with a high significance on each night it was observed. Variability is also found in the X-ray and optical bands on kilosecond timescales, along with flux-dependent spectral changes in the X-rays. The average H.E.S.S. spectrum shows a very soft power law shape with a photon index of 3.37+/-0.07(stat)+/-0.10(sys). The energy outputs in the 2-10 keV and in the VHE gamma-ray range are found to be similar, with the X-rays and the optical fluxes at a level comparable to some of the lowest historical measurements, indicating that PKS2155-304 was in a low or quiescent state during the observations. Both a leptonic and a hadronic model are used to derive source parameters from these observations., 16 pages, 13 figures, Accepted (June 22) for publication in A&A
Published: 2005
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9. Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations

Author: F. Aharonian, A. G. Akhperjanian, K.-M. Aye, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus, K. Bernlöhr, C. Boisson, O. Bolz, C. Borgmeier, F. Breitling, A. M. Brown, J. Bussons Gordo, P. M. Chadwick, L.-M. Chounet, R. Cornils, L. Costamante, B. Degrange, A. Djannati-Ataï, null L. O'C. Drury, G. Dubus, T. Ergin, P. Espigat, F. Feinstein, P. Fleury, G. Fontaine, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, O. C. de Jager, I. Jung, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, A. Lemière, M. Lemoine, N. Leroy, T. Lohse, A. Marcowith, C. Masterson, T. J. L. McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, I. Redondo, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. P. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J.-P. Tavernet, C. G. Théoret, M. Tluczykont, D. J. van der Walt, G. Vasileiadis, P. Vincent, B. Visser, H. J. Völk, S. J. Wagner, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), HESS, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Epoch (astronomy), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Flux (metallurgy), law, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Gamma ray, Astronomy and Astrophysics, Synchrotron, 13. Climate action, Space and Planetary Science, gamma rays: observations
Abstract: Observations of the shell-type supernova remnant SN1006 have been carried out with the H.E.S.S. system of Cherenkov telescopes during 2003 (18.2h with two operating telescopes) and 2004 (6.3h with all four telescopes). No evidence for TeV gamma-ray emission from any compact or extended region associated with the remnant is seen and resulting upper limits at the 99.9% confidence level are up to a factor 10 lower than previously-published fluxes from CANGAROO. For SN1006 at its current epoch of evolution we give limits for a number of important global parameters. Upper limits on the gamma-ray luminosity (for E=0.26 to 10 TeV, distance d=2 kpc) of L_gamma < 1.7x10^{33} erg s^{-1}, and the total energy in corresponding accelerated protons, W_p25microG results when considering the synchrotron/inverse-Compton framework for the observed X-ray flux and gamma-ray upper limits., 6 pages, 2 figures. Accepted in Astronomy and Astrophysics
Published: 2005
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10. A search for very high energy gamma-ray emission from the starburst galaxy NGC 253 with H.E.S.S

Author: F. Aharonian, A. G. Akhperjanian, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, K. Bernlöhr, C. Boisson, O. Bolz, V. Borrel, I. Braun, F. Breitling, A. M. Brown, P. M. Chadwick, L.-M. Chounet, R. Cornils, L. Costamante, B. Degrange, H. J. Dickinson, A. Djannati-Ataï, null L. O'C. Drury, G. Dubus, D. Emmanoulopoulos, P. Espigat, F. Feinstein, G. Fontaine, Y. Fuchs, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, J. F. Glicenstein, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, A. Jacholkowska, O. C. de Jager, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, A. Lemière, M. Lemoine-Goumard, N. Leroy, T. Lohse, J. M. Martin, O. Martineau-Huynh, A. Marcowith, C. Masterson, T. J. L. McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, D. Spangler, R. Steenkamp, C. Stegmann, J.-P. Tavernet, R. Terrier, C. G. Théoret, M. Tluczykont, G. Vasileiadis, C. Venter, P. Vincent, H. J. Völk, S. J. Wagner, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), HESS, Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: High energy, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, HESS - Abteilung Hofmann, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Gamma ray, Galaxies: individual objects: NGC253, gamma-rays: observations, Astronomy and Astrophysics, Radius, Galaxy, Space and Planetary Science, Galaxies: starburst
Abstract: We present the result of 28 hours of observations of the nearby starburst galaxy NGC 253 with the H.E.S.S. detector in 2003. We find no evidence for very high energy gamma-ray emission from this object. Gamma-ray emission above 400 GeV from NGC 253 had been reported by the CANGAROO collaboration in 2002. From the H.E.S.S. data we derive upper limits on the flux above 300 GeV of 1.9 * 10^-12 photons cm^-2 s^-1 for a point-like source and 6.3 * 10^-12 photons cm^-2 s^-1 for a source of radius 0.5 degrees as reported by CANGAROO, both at a confidence level of 99%. These upper limits are inconsistent with the spectrum reported by CANGAROO. The expected very high energy gamma-ray emission from this object is discussed in the framework of a galactic wind propagation model., 7 pages, 3 figures
Published: 2005
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11. Search for TeV emission from the region around PSR B1706-44 with the H.E.S.S. experiment

Author: F. Aharonian, A. G. Akhperjanian, K.-M. Aye, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus, K. Bernlöhr, C. Boisson, O. Bolz, C. Borgmeier, I. Braun, F. Breitling, A. M. Brown, J. Bussons Gordo, P. M. Chadwick, L.-M. Chounet, R. Cornils, L. Costamante, B. Degrange, A. Djannati-Ataï, null L. O'C. Drury, G. Dubus, T. Ergin, P. Espigat, F. Feinstein, P. Fleury, G. Fontaine, Y. Fuchs, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, O. C. de Jager, I. Jung, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, A. Lemière, M. Lemoine, N. Leroy, T. Lohse, A. Marcowith, C. Masterson, T. J. L. McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, I. Redondo, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J.-P. Tavernet, R. Terrier, C. G. Théoret, M. Tluczykont, G. Vasileiadis, C. Venter, P. Vincent, B. Visser, H. J. Völk, S. J. Wagner, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), HESS, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Spectral shape analysis, Photon, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Gamma rays: observations, 7. Clean energy, 01 natural sciences, Power law, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Pulsar, Position (vector), 0103 physical sciences, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, Cherenkov radiation, ISM: supernova remnants, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Astronomy and Astrophysics, ISM: individual objects: G 343.1-2.3, Space and Planetary Science, ISM: individual objects: PSR B1706-44
Abstract: The region around PSR B1706-44 has been observed with the H.E.S.S. imaging atmospheric Cherenkov telescopes in 2003. No evidence for gamma-ray emission in the TeV range was found at the pulsar position or at the radio arc which corresponds to the supernova remnant G 343.1-2.3. The 99% confidence level flux upper limit at the pulsar position is Ful(E > 350GeV) = 1.4e-12 /cm^2/s assuming a power law with photon index of 2.5 and Ful(E > 500GeV) = 1.3e-12 /cm^2/s without an assumption on the spectral shape. The reported upper limits correspond to 8% of the flux from an earlier detection by the CANGAROO experiment., 5 pages, 3 figures, accepted by A&A letters
Published: 2005
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12. Serendipitous discovery of the unidentified extended TeV gamma-ray source HESS J1303-631

Author: F. Aharonian, A. G. Akhperjanian, K.-M. Aye, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus, K. Bernlöhr, C. Boisson, O. Bolz, I. Braun, F. Breitling, A. M. Brown, J. Bussons Gordo, P. M. Chadwick, L.-M. Chounet, R. Cornils, L. Costamante, B. Degrange, A. Djannati-Ataï, null L. O'C. Drury, G. Dubus, D. Emmanoulopoulos, P. Espigat, F. Feinstein, P. Fleury, G. Fontaine, Y. Fuchs, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, J. F. Glicenstein, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, O. C. de Jager, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, A. Lemière, M. Lemoine-Goumard, N. Leroy, T. Lohse, O. Martineau-Huynh, A. Marcowith, C. Masterson, T. J. L. McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, I. Redondo, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J.-P. Tavernet, R. Terrier, C. G. Théoret, M. Tluczykont, D. J. van der Walt, G. Vasileiadis, C. Venter, P. Vincent, H. J. Völk, S. J. Wagner, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), HESS, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Field of view, Astrophysics, Gamma rays: observations, 01 natural sciences, Galaxy: disk, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, HESS - Abteilung Hofmann, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Gamma ray, Astronomy and Astrophysics, Galactic plane, Wavelength, Crab Nebula, Space and Planetary Science, High Energy Physics::Experiment
Abstract: The serendipitous discovery of an unidentified extended TeVgamma-ray source close to the galactic plane named HESS J1303-631 at a significance of 21 standard deviations is reported. The observations were performed between February and June 2004 with the H.E.S.S. stereoscopic system of Cherenkov telescopes in Namibia. HESS J1303-631 was discovered roughly 0.6 deg north of the binary system PSR B1259-63/SS 2883, the target object of the initial observation campaign which was also detected at TeV energies in the same field of view. HESS J1303-631 is extended with a width of an assumed intrinsic Gaussian emission profile of sigma = (0.16 +- 0.02) deg and the integral flux above 380 GeV is compatible with constant emission over the entire observational period of (17 +- 3)% of the Crab Nebula flux. The measured energy spectrum can be described by a power-law dN/dE ~ E^-Gamma with a photon index of Gamma = 2.44 +- 0.05_stat +- 0.2_syst. Up to now, no counterpart at other wavelengths is identified. Various possible TeV production scenarios are discussed., 9 pages, 8 figures, accepted in Astronomy and Astrophysics
Published: 2005
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13. Discovery of VHE Gamma Rays from PKS 2005-489

Author: F. Aharonian, A. G. Akhperjanian, K.-M. Aye, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus, K. Bernlöhr, C. Boisson, O. Bolz, I. Braun, F. Breitling, A. M. Brown, J. Bussons Gordo, P. M. Chadwick, L.-M. Chounet, R. Cornils, L. Costamante, B. Degrange, A. Djannati-Ataï, null L. O'C. Drury, G. Dubus, D. Emmanoulopoulos, P. Espigat, F. Feinstein, P. Fleury, G. Fontaine, Y. Fuchs, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, J. F. Glicenstein, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, O. C. de Jager, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, A. Lemière, M. Lemoine-Goumard, N. Leroy, T. Lohse, O. Martineau-Huynh, A. Marcowith, C. Masterson, T. J. L. McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, I. Redondo, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J.-P. Tavernet, R. Terrier, C. G. Théoret, M. Tluczykont, G. Vasileiadis, C. Venter, P. Vincent, H. J. Völk, S. J. Wagner, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), HESS, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Physics, Photon, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, galaxies: active, Astrophysics (astro-ph), Gamma ray, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Crab Nebula, Space and Planetary Science, 0103 physical sciences, Energy spectrum, BL Lacertae objects: individual: PKS 2005-489, Blazar, 010303 astronomy & astrophysics, gamma rays: observations
Abstract: The high-frequency peaked BL Lac PKS 2005-489 (z=0.071) was observed in 2003 and 2004 with the H.E.S.S. stereoscopic array of imaging atmospheric-Cherenkov telescopes in Namibia. A signal was detected at the 6.7 sigma level in the 2004 observations (24.2 hrs live time), but not in the 2003 data set (27.3 hrs live time). PKS 2005-489 is the first blazar independently discovered by H.E.S.S. to be an emitter of VHE photons, and only the second such blazar in the Southern Hemisphere. The integral flux above 200 GeV observed in 2004 is (6.9 +/- 1.0 +/- 1.4) x 10$^{-12}$ cm$^{-2}$ s$^{-1}$, corresponding to ~2.5% of the flux observed from the Crab Nebula. The 99% upper limit on the flux in 2003, I(>200 GeV) < 5.2 x 10$^{-12}$ cm$^{-2}$ s$^{-1}$, is smaller than the flux measured in 2004, suggesting an increased level of activity in 2004. However, the data show no evidence for significant variability on any time scale less than a year. An energy spectrum is measured and is characterized by a very soft power law (photon index = 4.0 +/- 0.4)., 5 pages, 2 figures, Accepted (April 20, 2005) for Publication in A&A Letters
Published: 2005
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14. A new population of very high energy gamma-ray sources in the Milky Way

Author: G. Fontaine, R. Le Gallou, O. Bolz, M. Panter, Tulun Ergin, P. M. Chadwick, M. Hauser, O. C. de Jager, R. Cornils, I. J. Latham, P. Berghaus, U. Schwanke, J. Raux, G. Pühlhofer, P. Fleury, Michael Punch, L. O'c. Drury, I. Redondo, C. Stegmann, Stefan Gillessen, David Berge, Stefan Wagner, B. C. Raubenheimer, Klaus-Michael Aye, I. Jung, R. Steenkamp, M. Beilicke, C. G. Théoret, M. Raue, B. Degrange, L. Rob, A. R. Bazer-Bachi, Werner Hofmann, Thomas Lohse, M. Ouchrif, B. Khélifi, Wystan Benbow, S. M. Rayner, German Hermann, Catherine Boisson, P. Vincent, Helene Sol, Y. A. Gallant, J. L. Osborne, R. Terrier, F. Feinstein, A. Konopelko, Guy Pelletier, F. Breitling, Dieter Horns, A. Lemière, J. Ripken, A. Noutsos, B. Giebels, K. J. Orford, A. Djannati-Ataï, M. Holleran, Stefan Funk, S. Schlenker, S. Pita, C. Borgmeier, C. Hadjichristidis, P. Espigat, D. J. van der Walt, Christo Venter, Guillaume Dubus, A. G. Akhperjanian, Felix Aharonian, M. Tluczykont, T. J. L. McComb, Konrad Bernlöhr, Luigi Costamante, Olaf Reimer, Nu. Komin, M. de Naurois, J.-P. Tavernet, L. Saugé, A. Reimer, P. Goret, M. Lemoine, Jim Hinton, B. Visser, Reinhard Schlickeiser, A. Marcowith, Gavin Rowell, C. Schuster, V. Sahakian, Conor Masterson, G. Heinzelmann, L.-M. Chounet, G. Vasileiadis, N. Leroy, L. Rolland, S. J. Nolan, M. Siewert, J. Bussons Gordo, Heinrich J. Völk, Ilana M. Braun, Gilles Henri, A. M. Brown, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), HESS, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, education.field_of_study, Multidisciplinary, COSMIC cancer database, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics (astro-ph), Gamma ray, Astronomy, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Pulsar, 0103 physical sciences, High Energy Stereoscopic System, education, 010303 astronomy & astrophysics
Abstract: Very high energy γ-rays probe the long-standing mystery of the origin of cosmic rays. Produced in the interactions of accelerated particles in astrophysical objects, they can be used to image cosmic particle accelerators. A first sensitive survey of the inner part of the Milky Way with the High Energy Stereoscopic System (HESS) reveals a population of eight previously unknown firmly detected sources of very high energy γ-rays. At least two have no known radio or x-ray counterpart and may be representative of a new class of “dark” nucleonic cosmic ray sources.
Published: 2005
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15. Very high energy gamma rays from the direction of Sagittarius A*

Author: F. Aharonian, A. G. Akhperjanian, K.-M. Aye, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus, K. Bernlöhr, O. Bolz, C. Boisson, C. Borgmeier, F. Breitling, A. M. Brown, J. Bussons Gordo, P. M. Chadwick, V. R. Chitnis, L.-M. Chounet, R. Cornils, L. Costamante, B. Degrange, A. Djannati-Ataï, null L. O'C. Drury, T. Ergin, P. Espigat, F. Feinstein, P. Fleury, G. Fontaine, S. Funk, Y. Gallant, B. Giebels, S. Gillessen, P. Goret, J. Guy, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, O. C. de Jager, I. Jung, B. Khélifi, Nu. Komin, A. Konopelko, I. J. Latham, R. Le Gallou, M. Lemoine, A. Lemière, N. Leroy, T. Lohse, A. Marcowith, C. Masterson, T. J. L. McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, M. Pohl, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, I. Redondo, A. Reimer, O. Reimer, J. Ripken, M. Rivoal, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J.-P. Tavernet, C. G. Théoret, M. Tluczykont, D. J. van der Walt, G. Vasileiadis, P. Vincent, B. Visser, H. J. Völk, S. J. Wagner, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), HESS, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Groupe d'Astroparticules de Montpellier (GAM), Université Montpellier 2 - Sciences et Techniques (UM2), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Photomultiplier, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, Stability (probability), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, 0103 physical sciences, Calibration, High Energy Stereoscopic System, 010303 astronomy & astrophysics, Cherenkov radiation, Observations, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Astrophysics (astro-ph), Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy centre, Space and Planetary Science, business, Gamma-rays
Abstract: We report the detection of a point-like source of very high energy (VHE) gamma-rays coincident within 1' of Sgr A*, obtained with the H.E.S.S. array of Cherenkov telescopes. The gamma-rays exhibit a power-law energy spectrum with a spectral index of -2.2 +/- 0.09 +/- 0.15 and a flux above the 165 GeV threshold of (1.82 +/- 0.22) * 10^-7 m^-2 s^-1. The measured flux and spectrum differ substantially from recent results reported in particular by the CANGAROO collaboration., 5 pages, 4 figures, replacement with corrected EGRET points in Fig.4
Published: 2004
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16. A new camera for the HESS phase II experiment

Author: E. Delagnes, F. Toussenel, J. Raux, M. Tluczykont, M. De Naurois, P. Corona, F. Voisin, P. Manigot, A. R. Bazer-Bachi, J. P. Tavernet, A. Karar, J.-F. Huppert, Michael Punch, Y. Degerly, M. Ouchrif, F. Feinstein, Gilles Fontaine, Pascal Vincent, B. Degrange, L.-M. Chounet, P. Goret, P. Nayman, S. Pita, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), A. Aharonian, Heinz J. Völk, and Dieter Horns, HESS, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: gamma-ray sources (astronomical), Astrophysics::High Energy Astrophysical Phenomena, quasars, 98.70.Rz, 95.55.Ka, Astrophysics, 7. Clean energy, Particle identification, Coincidence, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 03 medical and health sciences, Pulsar, law, cameras, gamma-ray detection, 030304 developmental biology, Physics, 0303 health sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Quasar, astronomical telescopes, pulsars, Satellite, High Energy Physics::Experiment, Gamma-ray burst
Abstract: The HESS experiment is now fully operational with the four telescopes installed by the end of December, 2003. Many galactic and extragalactic objects have been observed since operation began and the detection of various sources has proven the performance of the detector and validated the technical options chosen. The collaboration is currently studying the next phase of the HESS project. The detector system currently in operation has a threshold around 100 GeV. Many sources such as pulsars, micro-quasars, or neutralino annihilation are expected to emit gamma radiation at lower energy. The second phase of the HESS experiment consists of an additional larger telescope positioned in the centre of the existing four-telescope array. The new system may reach a threshold as low as 10–20 GeV in single telescope mode and about 50 GeV in coincidence with the four other telescopes. It will also improve the sensitivity of the existing system above 100 GeV. The construction should start next year and the installation is expected to take place in 2008, less than one year after the launch of the GLAST satellite. After a brief overview of the HESS phase I experiment, we will describe the upgraded parameters of the HESS camera. Then the set-up and expected performance are presented.
Published: 2004
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17. Calibration of cameras of the H.E.S.S. detector

Author: M. Panter, Wystan Benbow, Gilles Henri, J. Raux, G. Fontaine, David Berge, B. Khélifi, C. Borgmeier, G. Hermann, A. Djannati-Ataï, L-M. Chounet, Catherine Boisson, Nu. Komin, Felix Aharonian, Thomas Lohse, C. G. Théoret, P. Goret, I. Redondo, T. J. L. McComb, O. C. de Jager, B. Degrange, Y. A. Gallant, R. Le Gallou, C. Hadjichristidis, M. Siewert, V. Sahakian, S. M. Rayner, Martin Raue, M. de Naurois, O. Bolz, J. Ripken, L. Saugé, Michael Punch, B. C. Raubenheimer, Guy Pelletier, B. Giebels, A. Lemière, Stefan Wagner, Tulun Ergin, D. J. van der Walt, Stefan Funk, A. R. Bazer-Bachi, Conor Masterson, J.-P. Tavernet, P. Vincent, M. Beilicke, Jim Hinton, Helene Sol, I. J. Latham, S. Pita, J. L. Osborne, F. Feinstein, B. Visser, K. J. Orford, M. Lemoine, L. Rob, M. Ouchrif, Martin Pohl, P. M. Chadwick, Werner Hofmann, P. Espigat, Heinrich J. Völk, Luigi Costamante, Julien Guy, M. Rivoal, F. Breitling, Dieter Horns, Gerd Pühlhofer, Olaf Reimer, G. Heinzelmann, G. Vasileiadis, L. O'c. Drury, Klaus-Michael Aye, A. Konopelko, Ullrich Schwanke, Reinhard Schlickeiser, A. G. Akhperjanian, R. Steenkamp, A. Marcowith, P. Berghaus, Gavin Rowell, C. Schuster, A. M. Brown, M. Holleran, S. Schlenker, V. R. Chitnis, C. Stegmann, Stefan Gillessen, I. Jung, N. Leroy, L. Rolland, S. J. Nolan, M. Hauser, R. Cornils, P. Fleury, M. Tluczykont, Konrad Bernlöhr, A. Reimer, A. Noutsos, 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), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), HESS, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)
Subjects: High energy, Photomultiplier, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Optical-system, FOS: Physical sciences, Stereoscopy, Astrophysics, 01 natural sciences, Stability (probability), law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, Atmospheric Cherenkov telescopes, law, 0103 physical sciences, Calibration, High Energy Stereoscopic System, Performance, 010303 astronomy & astrophysics, Cherenkov radiation, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Detector, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, business
Abstract: H.E.S.S. - the High Energy Stereoscopic System- is a new system of large atmospheric Cherenkov telescopes for GeV/TeV astronomy. Each of the four telescopes of 107 m^2 mirror area is equipped with a 960-pixel photomulitiplier-tube camera. This paper describes the methods used to convert the photomultiplier signals into the quantities needed for Cherenkov image analysis. Two independent calibration techniques have been applied in parallel to provide an estimation of uncertainties. Results on the long-term stability of the H.E.S.S. cameras are also presented., Comment: 29 pages, 13 figures, accepted by Astroparticle Physics
Published: 2004
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18. High-energy particle acceleration in the shell of a supernova remnant

Author: V. Sahakian, Conor Masterson, B. Khélifi, C. Stegmann, Stefan Gillessen, R. Steenkamp, O. C. de Jager, U. Schwanke, R. Cornils, I. Redondo, M. de Naurois, I. J. Latham, D. J. van der Walt, J. L. Osborne, F. Feinstein, Stefan Wagner, S. Pita, O. Bolz, L. O'c. Drury, G. Heinzelmann, J. Ripken, L. Saugé, Y. A. Gallant, Tulun Ergin, Klaus-Michael Aye, P. Berghaus, N. Leroy, Jim Hinton, Gilles Henri, P. Espigat, G. Pühlhofer, Stefan Funk, B. Visser, K. J. Orford, M. Panter, M. Ouchrif, C. Schuster, David Berge, Nu. Komin, M. Holleran, Julien Guy, A. Djannati-Ataï, P. Goret, Michael Punch, S. Schlenker, A. Noutsos, L-M. Chounet, Catherine Boisson, Gavin Rowell, Thomas Lohse, V. R. Chitnis, P. Fleury, M. Beilicke, S. J. Nolan, A. Lemière, L. Rob, I. Jung, Olaf Reimer, Wystan Benbow, J. Raux, F. Breitling, Dieter Horns, Werner Hofmann, M. Tluczykont, Konrad Bernlöhr, A. Konopelko, A. R. Bazer-Bachi, M. Siewert, A. Marcowith, Reinhard Schlickeiser, A. Reimer, Luigi Costamante, M. Hauser, G. Vasileiadis, P. Vincent, B. Degrange, J. Bussons Gordo, C. Hadjichristidis, M. Lemoine, M. Rivoal, L. Rolland, Heinrich J. Völk, C. Borgmeier, Felix Aharonian, T. J. L. McComb, B. C. Raubenheimer, German Hermann, Martin Pohl, G. Fontaine, R. Le Gallou, M. Raue, S. M. Rayner, Guy Pelletier, B. Giebels, P. M. Chadwick, A. M. Brown, C. G. Théoret, Helene Sol, J.-P. Tavernet, A. G. Akhperjanian, 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), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), HESS, OpenMETU, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: System, High energy particle, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics, Discovery, Cassiopeia-A, 01 natural sciences, Gamma-ray emission, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spectrum, G347.3-0.5, 0103 physical sciences, origin, Cosmic-rays, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Origin, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], SNR RX-J1713.7-3946, Astrophysics (astro-ph), Astronomy, Charged particle, Particle acceleration, Cassiopeia A, Interstellar medium, Supernova
Abstract: A significant fraction of the energy density of the interstellar medium is in the form of high-energy charged particles (cosmic rays). The origin of these particles remains uncertain. Although it is generally accepted that the only sources capable of supplying the energy required to accelerate the bulk of Galactic cosmic rays are supernova explosions, and even though the mechanism of particle acceleration in expanding supernova remnant (SNR) shocks is thought to be well understood theoretically, unequivocal evidence for the production of high-energy particles in supernova shells has proven remarkably hard to find. Here we report on observations of the SNR RX J1713.7-3946 (G347.3-0.5), which was discovered by ROSAT in the X-ray spectrum and later claimed as a source of high-energy \gamma-rays of TeV energies (1 TeV=10^{12} eV). We present a TeV \gamma-ray image of the SNR: the spatially resolved remnant has a shell morphology similar to that seen in X-rays, which demonstrates that very-high-energy particles are accelerated there. The energy spectrum indicates efficient acceleration of charged particles to energies beyond 100 TeV, consistent with current ideas of particle acceleration in young SNR shocks., Comment: 9 pages, 3 figures, published in Nature
Published: 2004
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19. New Constraints on ΩM, ΩΛ, and w from an Independent Set of 11 High-Redshift Supernovae Observed with the Hubble Space Telescope

Author: Peter Nugent, Dale Andrew Howell, Gerson Goldhaber, Rahman Amanullah, K. Schahmaneche, M. S. Burns, Donald E. Groom, G. Garavini, Nino Panagia, Vallery Stanishev, Naoki Yasuda, A. G. Kim, K. Garton, Reynald Pain, J. Raux, A. S. Fruchter, Saul Perlmutter, Gastón Folatelli, Robert Quimby, Nicholas A. Walton, E. Smith, G. Sainton, Christopher Lidman, Lifan Wang, Sebastien Fabbro, R. A. Knop, Pilar Ruiz-Lapuente, A. Conley, G. Blanc, Ariel Goobar, Mark Sullivan, D. Hardin, Susana E. Deustua, N. Regnault, Richard S. Ellis, Pierre Astier, Bradley E. Schaefer, W. M. Wood-Vasey, Brian C. Lee, Javier Méndez, Mamoru Doi, A. L. Spadafora, R. Gibbons, S. Garmond, Greg Aldering, C. R. Pennypacker, S. Nobili, I. M. Hook, National Science Foundation (US), University of California, Knut and Alice Wallenberg Foundation, National Aeronautics and Space Administration (US), and Department of Energy (US)
Subjects: Deceleration parameter, Astrophysics::High Energy Astrophysical Phenomena, Cosmological parameters, general [Supernovae], Supernovae: general, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmological constant, Astrophysics, Astronomy & Astrophysics, Atomic, 01 natural sciences, Omega, Cosmology, Particle and Plasma Physics, astro-ph, 0103 physical sciences, Nuclear, observations [Cosmology], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Cosmology: observations, Molecular, Astronomy and Astrophysics, Redshift, Supernova, 13. Climate action, Space and Planetary Science, Dark energy, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Supernova Legacy Survey, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract: 36 pags., 13 figs., 31 tabs., 1 app., We report measurements of ΩM, ΩΛ w from 11 supernovae (SNe) at z ¼ 0:36 0:86 with high-quality light curves measured using WFPC2 on the Hubble Space Telescope (HST). This is an independent set of high-redshift SNe that confirms previous SN evidence for an accelerating universe. The high-quality light curves available from photometry on WFPC2 make it possible for these 11 SNe alone to provide measurements of the cosmological parameters comparable in statistical weight to the previous results. Combined with earlier Supernova Cosmology Project data, the new SNe yield a measurement of the mass density ΩM ¼ 0:25þ0:07 Ω0:06 ðstatisticalÞ Λ 0:04 (identified systematics), or equivalently, a cosmological constant of ΩΛ ¼ 0:75þ0:06 Ω0:07 ðstatisticalÞ Λ 0:04 (identified systematics), under the assumptions of a flat universe and that the dark energy equation-of-state parameter has a constant value w ¼ Ω1.When the SN results are combined with independent flat-universe measurements of ΩM from cosmic microwave background and galaxy redshift distortion data, they provide a measurement of w ¼ Ω1:05þ0:15 Ω0:20 ðstatisticalÞ Λ 0:09 (identified systematic), if w is assumed to be constant in time. In addition to high-precision light-curve measurements, the new data offer greatly improved color measurements of the high-redshift SNe and hence improved host galaxy extinction estimates. These extinction measurements show no anomalous negative E(BΩ) at high redshift. The precision of the measurements is such that it is possible to perform a host galaxy extinction correction directly for individual SNe without any assumptions or priors on the parent E(BΩV) distribution. Our cosmological fits using full extinction corrections confirm that dark energy is required with PðΩΛ > 0Þ > 0:99, a result consistent with previous and current SN analyses that rely on the identification of a low-extinction subset or prior assumptions concerning the intrinsic extinction distribution., Support for this work was provided by NASA through grants HST-GO-07336.01-A and HST-GO-08346.01-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This work was supported in part by the Director, Office of Science,Office of High Energy and Nuclear Physics, of the US Department of Energy under Contract DE-AC03- 76SF000098, by the Center for Particle Astrophysics, an NSF Science and Technology Center operated by the University of California, Berkeley, under Cooperative Agreement AST 91-20005. This work was supported in part by a NASA LTSA grant to P. E. N., G. A., S. P., and S. E. D., and W. M. W.-V. was supported in part by a National Science Foundation Graduate Research Fellowship. A.G. is a Royal Swedish Academy Research Fellow supported by a grant from the Knut and Alice Wallenberg Foundation.
Published: 2003

20. The Hubble diagram of type Ia supernovae as a function of host galaxy morphology

Author: D. Hardin, Javier Méndez, Christopher Lidman, Saul Perlmutter, Nicholas A. Walton, Mamoru Doi, Rahman Amanullah, Gerson Goldhaber, Nicolas Regnault, Peter Nugent, S. Nobili, R. Gibbons, A. L. Spadafora, Pilar Ruiz-Lapuente, Donald E. Groom, Naoki Yasuda, J. Raux, M. S. Burns, K. Schahmaneche, Pierre Astier, Mike Irwin, Alex Conley, R. A. Knop, Greg Aldering, Dale Andrew Howell, Guillermo A. Blanc, G. Garavini, Robert Quimby, Gastón Folatelli, Richard G. McMahon, A. G. Kim, C. R. Pennypacker, Nino Panagia, I. M. Hook, Reynald Pain, Sebastien Fabbro, Bradley E. Schaefer, W. M. Wood-Vasey, Richard S. Ellis, Lifan Wang, Susana E. Deustua, A. S. Fruchter, Ariel Goobar, Mark Sullivan, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), SUPERNOVAE, and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Cosmological constant, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, distance scale, 01 natural sciences, Cosmology, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], astro-ph, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, cosmological parameters, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Sigma, Astronomy and Astrophysics, Galaxy, observations [cosmology], Supernova, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, general [supernovae], Astronomical and Space Sciences
Abstract: (Abridged) We present new results on the Hubble diagram of distant type Ia supernovae (SNe Ia) segregated according to the type of host galaxy. This makes it possible to check earlier evidence for a cosmological constant by explicitly comparing SNe residing in galaxies likely to contain negligible dust with the larger sample. The cosmological parameters derived from these SNe Ia hosted by presumed dust-free early-type galaxies supports earlier claims for a cosmological constant, which we demonstrate at 5 sigma significance, and the internal extinction implied is small even for late-type systems (A_B, MNRAS; post-referee version. 21 pages, 10 figures including 4 colour figures. Preprint also available at http://supernova.lbl.gov/
Published: 2003
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21. Combined spatial and retrospective analysis of fluoroalkyl chemicals in fluvial sediments reveal changes in levels and patterns over the last 40 years.

Author: Mourier B, Labadie P, Desmet M, Grosbois C, Raux J, Debret M, Copard Y, Pardon P, Budzinski H, and Babut M
Subjects: Alkanesulfonic Acids, Carboxylic Acids, France, Manufacturing and Industrial Facilities, Retrospective Studies, Rivers chemistry, Sulfonic Acids analysis, Environmental Monitoring, Fluorocarbons analysis, Geologic Sediments chemistry, Water Pollutants, Chemical analysis, Water Pollution, Chemical statistics & numerical data
Abstract: Bed sediments and a dated sediment core were collected upstream and downstream from the city of Lyon (France) to assess the spatial and temporal trends of contamination by per- and polyfluoroalkyl substances (PFASs) in this section of the Rhône River. Upstream from Lyon, concentrations of total PFASs (ΣPFASs) in sediments are low (between 0.19 and 2.6 ng g -1 dry weight - dw), being characterized by a high proportion of perfluorooctane sulfonate (PFOS). Downstream from Lyon, and also from a fluoropolymer manufacturing plant, ΣPFASs concentrations reach 48.7 ng g -1 dw. A gradual decrease of concentrations is reported at the coring site further downstream (38 km). Based on a dated sediment core, the temporal evolution of PFASs is reconstructed from 1984 to 2013. Prior to 1987, ΣPFASs concentrations were low (≤2 ng g -1 dw), increasing to a maximum of 51 ng g -1 dw in the 1990s and then decreasing from 2002 to the present day (∼10 ng g -1 dw). In terms of the PFAS pattern, the proportion of perfluoroalkyl sulfonic acids (PFSAs) has remained stable since the 1980s (∼10%), whereas large variations are reported for carboxylic acids (PFCAs). Long chain- (C > 8) PFCAs characterized by an even number of perfluorinated carbons represent about 74% of the total PFAS load until 2005. However, from 2005 to 2013, the relative contribution of long chain- (C > 8) PFCAs with an odd number of perfluorinated carbons reaches 80%. Such changes in the PFAS pattern likely highlight a major shift in the industrial production process. This spatial and retrospective study provides valuable insights into the long-term contamination patterns of PFAS chemicals in river basins impacted by both urban and industrial activities., (Copyright © 2019. Published by Elsevier Ltd.)
Published: 2019
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22. Occurrence of 1,1'-dimethyl-4,4'-bipyridinium (Paraquat) in irrigated soil of the Lake Chad Basin, Niger.

Author: Crampon M, Copard Y, Favreau G, Raux J, Merlet-Machour N, Le Coz M, Ibrahim M, Peulon-Agasse V, and Portet-Koltalo F
Subjects: Agricultural Irrigation, Crops, Agricultural growth & development, Groundwater analysis, Niger, Lakes analysis, Paraquat analysis, Pesticides analysis, Soil Pollutants analysis, Water Pollutants, Chemical analysis
Abstract: Increased use of agrochemical products to improve yields for irrigated crops in sub-Saharan Africa has been accompanied by a significant increase in the risk of environmental contamination. Detailed examples of the fate of pesticides after initial spreading on crop fields are scarce in tropical regions, where safe practices and related health risks are poorly understood by smallholder farmers. In the semi-arid environment of the Lake Chad Basin, SE Niger, both intrinsic properties of pesticides and extrinsic factors such as soil and climate helped to characterize processes leading to an accumulation of pesticides in soils. Analysis by HPLC-UV of a 6 m deep soil profile showed the presence of Paraquat at concentrations from 953 ± 102 μg kg(-1) to 3083 ± 175 μg kg(-1) at depths between 0.80 and 2.75 m below the land surface. Soil analysis revealed that up to approximately 15 % of the total soil matrix consists of smectites, a clay mineral capable of retaining cationic pesticides such as Paraquat, and a very low content of organic matter (<0.15 wt.% TOC). Paraquat could be stored and not bioavailable in a clayey barrier at approximately 2-m depth and therefore does not represent an immediate risk for populations or environment in this form. However, if the Paraquat application rate remains constant, the clayey barrier could reach a saturation limit within 150-200 years and 180-220 years if we consider a DT50 in soil of ~1,000 days (FAO). Consequently, it could lead to a deeper infiltration and so a pollution of groundwater. Such a scenario can represent a health risk for drinking water and for the Lake Chad, which is a major resource for this densely populated region of semi-arid Africa. Further analyses should focus on deeper layers and groundwater Paraquat contents to validate or invalidate the hypothesis of storage in this clay-rich layer.
Published: 2014
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23. A low level of extragalactic background light as revealed by gamma-rays from blazars.

Author: Aharonian F, Akhperjanian AG, Bazer-Bachi AR, Beilicke M, Benbow W, Berge D, Bernlöhr K, Boisson C, Bolz O, Borrel V, Braun I, Breitling F, Brown AM, Chadwick PM, Chounet LM, Cornils R, Costamante L, Degrange B, Dickinson HJ, Djannati-Ataï A, Drury LO, Dubus G, Emmanoulopoulos D, Espigat P, Feinstein F, Fontaine G, Fuchs Y, Funk S, Gallant YA, Giebels B, Gillessen S, Glicenstein JF, Goret P, Hadjichristidis C, Hauser D, Hauser M, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hofmann W, Holleran M, Horns D, Jacholkowska A, de Jager OC, Khélifi B, Klages S, Komin N, Konopelko A, Latham IJ, Le Gallou R, Lemière A, Lemoine-Goumard M, Leroy N, Lohse T, Martin JM, Martineau-Huynh O, Marcowith A, Masterson C, McComb TJ, de Naurois M, Nolan SJ, Noutsos A, Orford KJ, Osborne JL, Ouchrif M, Panter M, Pelletier G, Pita S, Pühlhofer G, Punch M, Raubenheimer BC, Raue M, Raux J, Rayner SM, Reimer A, Reimer O, Ripken J, Rob L, Rolland L, Rowell G, Sahakian V, Saugé L, Schlenker S, Schlickeiser R, Schuster C, Schwanke U, Siewert M, Sol H, Spangler D, Steenkamp R, Stegmann C, Tavernet JP, Terrier R, Théoret CG, Tluczykont M, van Eldik C, Vasileiadis G, Venter C, Vincent P, Völk HJ, and Wagner SJ
Abstract: The diffuse extragalactic background light consists of the sum of the starlight emitted by galaxies through the history of the Universe, and it could also have an important contribution from the 'first stars', which may have formed before galaxy formation began. Direct measurements are difficult and not yet conclusive, owing to the large uncertainties caused by the bright foreground emission associated with zodiacal light. An alternative approach is to study the absorption features imprinted on the gamma-ray spectra of distant extragalactic objects by interactions of those photons with the background light photons. Here we report the discovery of gamma-ray emission from the blazars H 2356 - 309 and 1ES 1101 - 232, at redshifts z = 0.165 and z = 0.186, respectively. Their unexpectedly hard spectra provide an upper limit on the background light at optical/near-infrared wavelengths that appears to be very close to the lower limit given by the integrated light of resolved galaxies. The background flux at these wavelengths accordingly seems to be strongly dominated by the direct starlight from galaxies, thus excluding a large contribution from other sources-in particular from the first stars formed. This result also indicates that intergalactic space is more transparent to gamma-rays than previously thought.
Published: 2006
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24. Discovery of very-high-energy gamma-rays from the Galactic Centre ridge.

Author: Aharonian F, Akhperjanian AG, Bazer-Bachi AR, Beilicke M, Benbow W, Berge D, Bernlöhr K, Boisson C, Bolz O, Borrel V, Braun I, Breitling F, Brown AM, Chadwick PM, Chounet LM, Cornils R, Costamante L, Degrange B, Dickinson HJ, Djannati-Ataï A, Drury LO, Dubus G, Emmanoulopoulos D, Espigat P, Feinstein F, Fontaine G, Fuchs Y, Funk S, Gallant YA, Giebels B, Gillessen S, Glicenstein JF, Goret P, Hadjichristidis C, Hauser D, Hauser M, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hofmann W, Holleran M, Horns D, Jacholkowska A, de Jager OC, Khélifi B, Klages S, Komin N, Konopelko A, Latham IJ, Le Gallou R, Lemière A, Lemoine-Goumard M, Leroy N, Lohse T, Marcowith A, Martin JM, Martineau-Huynh O, Masterson C, McComb TJ, de Naurois M, Nolan SJ, Noutsos A, Orford KJ, Osborne JL, Ouchrif M, Panter M, Pelletier G, Pita S, Pühlhofer G, Punch M, Raubenheimer BC, Raue M, Raux J, Rayner SM, Reimer A, Reimer O, Ripken J, Rob L, Rolland L, Rowell G, Sahakian V, Saugé L, Schlenker S, Schlickeiser R, Schuster C, Schwanke U, Siewert M, Sol H, Spangler D, Steenkamp R, Stegmann C, Tavernet JP, Terrier R, Théoret CG, Tluczykont M, van Eldik C, Vasileiadis G, Venter C, Vincent P, Völk HJ, and Wagner SJ
Abstract: The source of Galactic cosmic rays (with energies up to 10(15) eV) remains unclear, although it is widely believed that they originate in the shock waves of expanding supernova remnants. At present the best way to investigate their acceleration and propagation is by observing the gamma-rays produced when cosmic rays interact with interstellar gas. Here we report observations of an extended region of very-high-energy (> 10(11) eV) gamma-ray emission correlated spatially with a complex of giant molecular clouds in the central 200 parsecs of the Milky Way. The hardness of the gamma-ray spectrum and the conditions in those molecular clouds indicate that the cosmic rays giving rise to the gamma-rays are likely to be protons and nuclei rather than electrons. The energy associated with the cosmic rays could have come from a single supernova explosion around 10(4) years ago.
Published: 2006
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25. Discovery of very high energy gamma rays associated with an x-ray binary.

Author: Aharonian F, Akhperjanian AG, Aye KM, Bazer-Bachi AR, Beilicke M, Benbow W, Berge D, Berghaus P, Bernlöhr K, Boisson C, Bolz O, Borrel V, Braun I, Breitling F, Brown AM, Bussons Gordo J, Chadwick PM, Chounet LM, Cornils R, Costamante L, Degrange B, Dickinson HJ, Djannati-Ataï A, Drury LO, Dubus G, Emmanoulopoulos D, Espigat P, Feinstein F, Fleury P, Fontaine G, Fuchs Y, Funk S, Gallant YA, Giebels B, Gillessen S, Glicenstein JF, Goret P, Hadjichristidis C, Hauser M, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hofmann W, Holleran M, Horns D, Jacholkowska A, de Jager OC, Khélifi B, Komin N, Konopelko A, Latham IJ, Le Gallou R, Lemière A, Lemoine-Goumard M, Leroy N, Lohse T, Marcowith A, Martin JM, Martineau-Huynh O, Masterson C, McComb TJ, de Naurois M, Nolan SJ, Noutsos A, Orford KJ, Osborne JL, Ouchrif M, Panter M, Pelletier G, Pita S, Pühlhofer G, Punch M, Raubenheimer BC, Raue M, Raux J, Rayner SM, Reimer A, Reimer O, Ripken J, Rob L, Rolland L, Rowell G, Sahakian V, Saugé L, Schlenker S, Schlickeiser R, Schuster C, Schwanke U, Siewert M, Sol H, Spangler D, Steenkamp R, Stegmann C, Tavernet JP, Terrier R, Théoret CG, Tluczykont M, Vasileiadis G, Venter C, Vincent P, Völk HJ, and Wagner SJ
Abstract: X-ray binaries are composed of a normal star in orbit around a neutron star or stellar-mass black hole. Radio and x-ray observations have led to the presumption that some x-ray binaries called microquasars behave as scaled-down active galactic nuclei. Microquasars have resolved radio emission that is thought to arise from a relativistic outflow akin to active galactic nuclei jets, in which particles can be accelerated to large energies. Very high energy gamma-rays produced by the interactions of these particles have been observed from several active galactic nuclei. Using the High Energy Stereoscopic System, we find evidence for gamma-ray emission of >100 gigaelectron volts from a candidate microquasar, LS 5039, showing that particles are also accelerated to very high energies in these systems.
Published: 2005
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26. A new population of very high energy gamma-ray sources in the Milky Way.

Author: Aharonian F, Akhperjanian AG, Aye KM, Bazer-Bachi AR, Beilicke M, Benbow W, Berge D, Berghaus P, Bernlöhr K, Boisson C, Bolz O, Borgmeier C, Braun I, Breitling F, Brown AM, Gordo JB, Chadwick PM, Chounet LM, Cornils R, Costamante L, Degrange B, Djannati-Ataï A, Drury LO, Dubus G, Ergin T, Espigat P, Feinstein F, Fleury P, Fontaine G, Funk S, Gallant YA, Giebels B, Gillessen S, Goret P, Hadjichristidis C, Hauser M, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hofmann W, Holleran M, Horns D, de Jager OC, Jung I, Khélifi B, Komin N, Konopelko A, Latham IJ, Le Gallou R, Lemière A, Lemoine M, Leroy N, Lohse T, Marcowith A, Masterson C, McComb TJ, de Naurois M, Nolan SJ, Noutsos A, Orford KJ, Osborne JL, Ouchrif M, Panter M, Pelletier G, Pita S, Pühlhofer G, Punch M, Raubenheimer BC, Raue M, Raux J, Rayner SM, Redondo I, Reimer A, Reimer O, Ripken J, Rob L, Rolland L, Rowell G, Sahakian V, Saugé L, Schlenker S, Schlickeiser R, Schuster C, Schwanke U, Siewert M, Sol H, Steenkamp R, Stegmann C, Tavernet JP, Terrier R, Théoret CG, Tluczykont M, van der Walt DJ, Vasileiadis G, Venter C, Vincent P, Visser B, Völk HJ, and Wagner SJ
Abstract: Very high energy gamma-rays probe the long-standing mystery of the origin of cosmic rays. Produced in the interactions of accelerated particles in astrophysical objects, they can be used to image cosmic particle accelerators. A first sensitive survey of the inner part of the Milky Way with the High Energy Stereoscopic System (HESS) reveals a population of eight previously unknown firmly detected sources of very high energy gamma-rays. At least two have no known radio or x-ray counterpart and may be representative of a new class of "dark" nucleonic cosmic ray sources.
Published: 2005
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27. High-energy particle acceleration in the shell of a supernova remnant.

Author: Aharonian FA, Akhperjanian AG, Aye KM, Bazer-Bachi AR, Beilicke M, Benbow W, Berge D, Berghaus P, Bernlöhr K, Bolz O, Boisson C, Borgmeier C, Breitling F, Brown AM, Gordo JB, Chadwick PM, Chitnis VR, Chounet LM, Cornils R, Costamante L, Degrange B, Djannati-Ataï A, Drury LO, Ergin T, Espigat P, Feinstein F, Fleury P, Fontaine G, Funk S, Gallant YA, Giebels B, Gillessen S, Goret P, Guy J, Hadjichristidis C, Hauser M, Heinzelmann G, Henri G, Hermann G, Hinton JA, Hofmann W, Holleran M, Horns D, De Jager OC, Jung I, Khélifi B, Komin N, Konopelko A, Latham IJ, Le Gallou R, Lemoine M, Lemière A, Leroy N, Lohse T, Marcowith A, Masterson C, McComb TJ, De Naurois M, Nolan SJ, Noutsos A, Orford KJ, Osborne JL, Ouchrif M, Panter M, Pelletier G, Pita S, Pohl M, Pühlhofer G, Punch M, Raubenheimer BC, Raue M, Raux J, Rayner SM, Redondo I, Reimer A, Reimer O, Ripken J, Rivoal M, Rob L, Rolland L, Rowell G, Sahakian V, Saugé L, Schlenker S, Schlickeiser R, Schuster C, Schwanke U, Siewert M, Sol H, Steenkamp R, Stegmann C, Tavernet JP, Théoret CG, Tluczykont M, Van Der Walt DJ, Vasileiadis G, Vincent P, Visser B, Völk HJ, and Wagner SJ
Abstract: A significant fraction of the energy density of the interstellar medium is in the form of high-energy charged particles (cosmic rays). The origin of these particles remains uncertain. Although it is generally accepted that the only sources capable of supplying the energy required to accelerate the bulk of Galactic cosmic rays are supernova explosions, and even though the mechanism of particle acceleration in expanding supernova remnant (SNR) shocks is thought to be well understood theoretically, unequivocal evidence for the production of high-energy particles in supernova shells has proven remarkably hard to find. Here we report on observations of the SNR RX J1713.7 - 3946 (G347.3 - 0.5), which was discovered by ROSAT in the X-ray spectrum and later claimed as a source of high-energy gamma-rays of TeV energies (1 TeV = 10(12) eV). We present a TeV gamma-ray image of the SNR: the spatially resolved remnant has a shell morphology similar to that seen in X-rays, which demonstrates that very-high-energy particles are accelerated there. The energy spectrum indicates efficient acceleration of charged particles to energies beyond 100 TeV, consistent with current ideas of particle acceleration in young SNR shocks.
Published: 2004
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27 results on '"J. Raux"'

1. Combined spatial and retrospective analysis of fluoroalkyl chemicals in fluvial sediments reveal changes in levels and patterns over the last 40 years

2. RestframeI-band Hubble diagram for type Ia supernovae up to redshiftz$\mathsf{\sim}$ 0.5

3. Supernova photometric data analysis and reduction details

4. Spectroscopic observations of eight supernovae at intermediate redshift

5. Discovery of Very-High-Energy Gamma-Rays from the Galactic Centre Ridge

6. A low level of extragalactic background light as revealed by gamma-rays from blazars

7. Spectroscopic confirmation of high-redshift supernovae with the ESO VLT ***

8. Multi-wavelength observations of PKS 2155-304 with H.E.S.S

9. Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations

10. A search for very high energy gamma-ray emission from the starburst galaxy NGC 253 with H.E.S.S

11. Search for TeV emission from the region around PSR B1706-44 with the H.E.S.S. experiment

12. Serendipitous discovery of the unidentified extended TeV gamma-ray source HESS J1303-631

13. Discovery of VHE Gamma Rays from PKS 2005-489

14. A new population of very high energy gamma-ray sources in the Milky Way

15. Very high energy gamma rays from the direction of Sagittarius A*

16. A new camera for the HESS phase II experiment

17. Calibration of cameras of the H.E.S.S. detector

18. High-energy particle acceleration in the shell of a supernova remnant

19. New Constraints on ΩM, ΩΛ, and w from an Independent Set of 11 High-Redshift Supernovae Observed with the Hubble Space Telescope

20. The Hubble diagram of type Ia supernovae as a function of host galaxy morphology

21. Combined spatial and retrospective analysis of fluoroalkyl chemicals in fluvial sediments reveal changes in levels and patterns over the last 40 years.

22. Occurrence of 1,1'-dimethyl-4,4'-bipyridinium (Paraquat) in irrigated soil of the Lake Chad Basin, Niger.

23. A low level of extragalactic background light as revealed by gamma-rays from blazars.

24. Discovery of very-high-energy gamma-rays from the Galactic Centre ridge.

25. Discovery of very high energy gamma rays associated with an x-ray binary.

26. A new population of very high energy gamma-ray sources in the Milky Way.

27. High-energy particle acceleration in the shell of a supernova remnant.

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27 results on '"J. Raux"'

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