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1. Charged-particle branching ratios above the neutron threshold in F19 : Constraining N15 production in core-collapse supernovae

Author: I. Matea, A. Gottardo, I. Sivacek, Mahmoud Mahgoub, M. Assié, S. Gillespie, L. Olivier, F. Hammache, M. Degerlier, V. Alcindor, I. Stefan, C. Delafosse, Didier Beaumel, A. Georgiadou, Jérôme Guillot, R. Garg, Marin Chabot, J. Riley, T. Faestermann, Alison Laird, L. Perrot, Valdir Guimaraes, F. Flavigny, Ralf Hertenberger, J. Kiener, P. Adsley, A. Lefebvre-Schuhl, N. de Sereville, Vincent Tatischeff, H.-F. Wirth, Arnd Meyer, and S. P. Fox
Subjects: Physics, 010308 nuclear & particles physics, Inelastic scattering, Branching (polymer chemistry), 01 natural sciences, Charged particle, Nuclear physics, Supernova, Nucleosynthesis, Excited state, 0103 physical sciences, Neutron, Nuclear Experiment, 010306 general physics, Ground state
Abstract: Spatially-correlated overabundances of $^{15}$N and $^{18}$O observed in some low-density graphite meteoritic grains have been connected to nucleosynthesis taking place in the helium-burning shell during core-collapse supernovae. Two of the reactions which have been identified as important to the final abundances of $^{15}$N and $^{18}$O are $^{18}$F($n,\alpha$)$^{15}$N and $^{18}$F($n,p$)$^{18}$O. The relative strengths of the $^{18}$F($n,\alpha$)$^{15}$N and $^{18}$F($n,p$)$^{18}$O reactions depend on the relative $\alpha_0$ and $p_0$ decays from states above the neutron threshold in $^{19}$F in addition to other properties. Experimental data on the charged-particle decays from these highly excited states are lacking or inconsistent. Two experiments were performed using proton inelastic scattering from LiF targets and magnetic spectrographs. The first experiment used the high-resolution Q3D spectrograph at Munich to constrain properties of levels in $^{19}$F. A second experiment using the Orsay Split-Pole spectrograph and an array of silicon detectors was performed in order to measure the charged-particle decays of neutron-unbound levels in $^{19}$F. A number of levels in $^{19}$F have been identified along with their corresponding charged-particle decays. The first state above the neutron threshold which has an observed proton-decay branch to the ground state of $^{18}$O lies 68 keV above the neutron threshold while the $\alpha$-particle decays from the neutron-unbound levels are generally observed to be much stronger than the proton decays. Neutron-unbound levels in $^{19}$F are observed to decay predominantly by $\alpha$-particle emission, supporting the role of $^{18}$F($n,\alpha$)$^{15}$N in the production of $^{15}$N in the helium-burning shell of supernovae. Improved resonant-scattering reaction data are required in order to be able to determine the reaction rates accurately.
Published: 2021
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2. Sub-threshold states in Ne19 relevant to F18(p,α)O15

Author: Giuseppe Verde, Mark A. Williams, Alison Laird, M. Assié, R. Garg, S. Gillespie, Vincent Tatischeff, Anuj Parikh, A. Lefebvre-Schuhl, J. Riley, N. de Sereville, A. Remadi, S. Franchoo, N. J. Hubbard, C. Hamadache, I. Stefan, J. Kiener, F. Hammache, L. Perrot, B. Bastin, F. de Oliveira Santos, S. P. Fox, F. Boulay, Daisuke Suzuki, Valdir Guimaraes, P. Adsley, and A. Coc
Subjects: Physics, Thermonuclear fusion, Spin states, Proton, 010308 nuclear & particles physics, Parity (physics), 01 natural sciences, 7. Clean energy, Coincidence, Nuclear physics, Reaction rate, 0103 physical sciences, Sub threshold, Nuclear Experiment, 010306 general physics, Charge exchange
Abstract: Classical novae result from thermonuclear explosions producing several $\gamma$-ray emitters which are prime targets for satellites observing in the MeV range. The early 511 keV gamma-ray emission depends critically on the $^{18}$F(p,$\alpha$)$^{15}$O reaction rate which, despite many experimental and theoretical efforts, still remains uncertain. One of the main uncertainties in the $^{18}$F(p,$\alpha$)$^{15}$O reaction rate is the contribution in the Gamow window of interference between sub-threshold $^{19}$Ne states and known broad states at higher energies. Therefore the goal of this work is to clarify the existence and the nature of these sub-threshold states. States in the $^{19}$Ne compound nucleus were studied at the Tandem-ALTO facility using the $^{19}$F($^3$He,t)$^{19}$Ne charge exchange reaction. Tritons were detected with an Enge Split-pole spectrometer while decaying protons or $\alpha$-particles from unbound $^{19}$Ne states were collected, in coincidence, with a double-sided silicon strip detector array. Angular correlations were extracted and constraints on the spin and parity of decaying states established. The coincidence yield at $E_x$ = 6.29 MeV was observed to be high spin, supporting the conclusion that it is indeed a doublet consisting of high spin and low spin components. Evidence for a broad, low spin state was observed around 6 MeV. Branching ratios were extracted for several states above the proton threshold and were found to be consistent with the literature. R-matrix calculations show the relative contribution of sub-threshold states to the astrophysically important energy region above the proton threshold. The levels schemes of $^{19}$Ne and $^{19}$F are still not sufficiently well known and further studies of the analogue assignments are needed. The tentative broad state at 6 MeV may only play a role if the reduced proton width is large.
Published: 2021
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3. Probing nuclear forces beyond the nuclear drip line: the cases of $^{16}$F and $^{15}$F: A Tribute to Mahir Hussein

Author: L. Caceres, A.M. Sánchez Benítez, Igor T. Čeliković, A. Matta, D. Verney, F. Rotaru, Valdir Guimaraes, P. Adsley, O. Sorlin, J. Guillot, T. Roger, C. Portail, V. Girard-Alcindor, I. Matea, A. Georgiadou, C. Petrone, D. Pantelica, R. Borcea, D. Suzuki, O. Kamalou, V. Lapoux, Megumi Niikura, I. Stefan, J. Piot, F. Flavigny, G. D’Agata, F. de Oliveira Santos, M. Ciemala, V. Tatischeff, V. Chudoba, L. Lalanne, C. Stodel, J. C. Thomas, N. Goyal, M. Stanoiu, C. Fougeres, S. Grévy, F. Negoita, N. de Séréville, L. Perrot, G. Dumitru, M. Assie, A. Meyer, J. C. Angelique, Marlete Assunção, Nicolas Michel, F. Hammache, D. Beaumel, S. Franchoo, Predrag Ujić, Dieter Ackermann, Shoko Koyama, F. de Grancey, J. Kiener, E. Berthoumieux, P. Morfouace, J. Mrazek, K. Subotic, Grand Accélérateur National d'Ions Lourds (GANIL), 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), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Elastic scattering, Physics, Nuclear and High Energy Physics, Proton, 010308 nuclear & particles physics, media_common.quotation_subject, Hadron, Nuclear Theory, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Asymmetry, Excited state, 0103 physical sciences, Nuclear force, Mirror nuclei, Atomic physics, 010306 general physics, Wave function, Nuclear Experiment, media_common
Abstract: The unbound proton-rich nuclei $$^{16}$$ F and $$^{15}$$ F are investigated experimentally and theoretically. Several experiments using the resonant elastic scattering method were performed at GANIL with radioactive beams to determine the properties of the low lying states of these nuclei. Strong asymmetry between $$^{16}$$ F– $$^{16}$$ N and $$^{15}$$ F– $$^{15}$$ C mirror nuclei is observed. The strength of the $$nucleon-nucleon$$ effective interaction involving the loosely bound proton in the $$s_{1/2}$$ orbit is significantly modified with respect to their mirror nuclei $$^{16}$$ N and $$^{15}$$ C. The reduction of the effective interaction is estimated by calculating the interaction energies with a schematic zero-range force. It is found that, after correcting for the effects due to changes in the radial distribution of the single-particle wave functions, the mirror symmetry of the $$n-p$$ interaction is preserved between $$^{16}$$ F and $$^{16}$$ N, while a difference of 63% is measured between the $$p-p$$ versus $$n-n$$ interactions in the second excited state of $$^{15}$$ F and $$^{15}$$ C nuclei. Several explanations are proposed.
Published: 2021
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4. Measurement and analysis of nuclear γ -ray production cross sections in proton interactions with Mg, Si, and Fe nuclei abundant in astrophysical sites over the incident energy range E=30–66 MeV

Author: S. P. Noncolela, P. Papka, J. Kiener, J. L. Conradie, A. Belhout, D. Moussa, S. Damache, W. Yahia-Chérif, J. L. Easton, E. A. Lawrie, Vincent Tatischeff, A. Chafa, J. J. Lawrie, Dinesh Negi, T. Lamula, S. N. T. Majola, N. de Sereville, F. Hammache, J. Ndayishimye, M. Wiedeking, M. Debabi, N. A. Khumalo, C. Hamadache, T. D. Bucher, J.F. Sharpey-Schafer, B. V. Kheswa, O. Shirinda, H. Benhabiles-Mezhoud, S. M. Wyngaardt, I. Deloncle, Peter B. Jones, and S. Ouichaoui
Subjects: Nuclear reaction, Physics, Range (particle radiation), Proton, 010308 nuclear & particles physics, Scattering, Cyclotron, 01 natural sciences, law.invention, Semiconductor detector, Nuclear physics, law, 0103 physical sciences, Nuclear Experiment, Nucleon, 010303 astronomy & astrophysics, Excitation
Abstract: Gamma-ray production cross section excitation functions have been measured for $30$, $42$, $54$ and $66$ MeV proton beams accelerated onto targets of astrophysical interest, $^{nat}$C, C + O (Mylar), $^{nat}$Mg, $^{nat}$Si and $^{56}$Fe, at the Sector Separated Cyclotron (SSC) of iThemba LABS (near Cape Town, South Africa). The AFRODITE array equipped with 8 Compton suppressed HPGe clover detectors was used to record $\gamma$-ray data. For known, intense $\gamma$-ray lines the previously reported experimental data measured up to $E_{p}\simeq$ $25$ MeV at the Washington and Orsay tandem accelerators were extended to higher proton energies. Our experimental data for the last 3 targets are reported here and discussed with respect to previous data and the Murphy \textit{et al.} compilation [ApJS 183, 142 (2009)], as well as to predictions of the nuclear reaction code TALYS. The overall agreement between theory and experiment obtained in first-approach calculations using default input parameters of TALYS has been appreciably improved by using modified optical model potential (OMP), deformation, and level density parameters. The OMP parameters have been extracted from theoretical fits to available experimental elastic/inelastic nucleon scattering angular distribution data by means of the coupled-channels reaction code OPTMAN. Experimental data for several new $\gamma$-ray lines are also reported and discussed. The astrophysical implications of our results are emphasised.
Published: 2020
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5. Gamma ray emission in alpha particle reactions with C, Mg, Si, Fe

Author: Jörg Röhrich, H. Benhabiles, Andrea Denker, I. Deloncle, Jürgen Bundesmann, J. Kiener, R. Mezhoud, C. Hamadache, V. Tatischeff, I. Bourgaoub, A. Gostojic, J. Peyré, F. Hammache, A. Coc, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Institut de Physique Nucléaire d'Orsay (IPNO)
Subjects: Nuclear reaction, History, Materials science, Astrophysics::High Energy Astrophysical Phenomena, Analytical chemistry, FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 7. Clean energy, 01 natural sciences, Education, Cross section (physics), 0103 physical sciences, Emission spectrum, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), Solar flare, 010308 nuclear & particles physics, Accelerator research and development, Gamma ray, Alpha particle, Computer Science Applications, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Cross sections for the strongest gamma-ray emission lines produced in alpha-particle reactions with C, Mg, Si, Fe have been measured in the range E_alpha = 50 - 90 MeV at the center for proton therapy at the Helmholtz-Zentrum Berlin. Data for more than 60 different gamma-ray lines were determined, with particular efforts for lines that are in cross section compilations/evaluations with astrophysical purpose, and where data exist at lower projectile energies. The data are compared with predictions of a modern nuclear reaction code and cross-section curves of the latest evaluation for gamma-ray line emission in accelerated-particle interactions in solar flares., Comment: 5 pages, 5 figures, contribution to the XXIII International School on Nuclear Physics, Neutron Physics and Applications, Varna, Bulgaria, September 22-28, 2019
Published: 2020
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6. Shape and angular distribution of the 4.439-MeV γ -ray line from proton inelastic scattering off C12

Author: J. Kiener
Subjects: Physics, Nuclear reaction, 010308 nuclear & particles physics, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Resonance, Parity (physics), Inelastic scattering, 01 natural sciences, Inelastic neutron scattering, Superposition principle, 0103 physical sciences, Angular momentum coupling, Atomic physics, 010306 general physics
Abstract: The emission of the 4.439-MeV $\ensuremath{\gamma}$ ray in proton inelastic scattering off $^{12}\mathrm{C}$ has been investigated in detail. For this, two independent descriptions of the correlated scattering and emission process have been used: one for the direct reaction mechanism and the other for the compound-nucleus (CN) component. Direct reactions were calculated in the framework of the coupled-channels formalism, while the CN component was described as a superposition of separate resonances with definite spin and parity, treated with the angular momentum coupling theory. Both components were incoherently added and compared to a comprehensive data set on measured $\ensuremath{\gamma}$-ray line shapes and angular distributions in the proton energy range ${E}_{p}=5.44--25.0$ MeV. In the range ${E}_{p}\ensuremath{\approx}14--25$ MeV, good agreement with data was obtained with a dominating direct reaction component. At lower energy, an important CN component was required to describe line shape and angular distribution data. In general, a good description of the data could be found for a CN component with spin and parity corresponding to a known nearby resonance. The new calculation was found to improve significantly the agreement with line shape data in particular in the region of dominating CN resonances compared to previous calculations. Based on these results, predictions for $\ensuremath{\gamma}$-ray line shapes and angular distributions up to ${E}_{p}=100$ MeV were made and applied to $\ensuremath{\gamma}$-ray emissions in solar flares and proton radiotherapy.
Published: 2019
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7. Experimental Study of the ${^{30}}{\text {P}({\text {p}}}{,}{\gamma })^{31}\text {S}$ Reaction in Classical Novae

Author: A. Georgiadou, A. Gottardo, Alison Laird, N. Oulebsir, Á. M. Sánchez Benítez, F. Flavigny, J. Kiener, A. Coc, F. de Oliveira, J. Riley, D. Beaumel, M. MacCormick, L. Olivier, J. Guillot, L. Grassi, I. Matea, N. Hubbard, Giuseppe D’Agata, C. Delafosse, K. Béroff, Valdir Guimaraes, L. Perrot, S. P. Fox, P. Adsley, N. de Séréville, C. Portail, F. Hammache, A. Meyer, Anuj Parikh, Alessandro Luiz Lara, V. Tatischeff, M. Assié, T. Id Barkach, Marlete Assunção, I. Stefan, B. Bastin, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Physics, Reaction rate, Particle physics, 010308 nuclear & particles physics, 0103 physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 010306 general physics, 01 natural sciences, 7. Clean energy
Abstract: International audience; The$^{30}$ P(p, $\gamma $ )$^{31}$ S reaction is one of the few remaining reactions whose rate uncertainty has a strong impact on classical novae model predictions. To reduce the nuclear uncertainties associated to this reaction, we measured the$^{31}$ P($^{3}$ He,t)$^{31}$ S reaction at the ALTO facility. Simultaneous detection of the triton and proton decays from the populated resonances will provide the proton branching ratios. The astrophysical context of this work, the current situation of the$^{30}$ P(p, $\gamma $ )$^{31}$ S reaction rate, the experimental set-up and the analysis of the single and coincidence events will be presented.
Published: 2018
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8. Application of artificial neural network in 3D imaging with lanthanum bromide calorimeter

Author: S. Blin, B. Travers, Vincent Tatischeff, L. Gibelin, C. Hamadache, N. Karkour, X. Grave, A. Gostojic, Pierre Barrillon, D. Linget, J. Kiener, CSNSM AN, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), CSNSM ELEC, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CSNSM INFOR, Laboratoire de l'Accélérateur Linéaire (LAL), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Artificial neural network, Nuclear and High Energy Physics, Photomultiplier, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Compton telescope, [INFO.INFO-NE]Computer Science [cs]/Neural and Evolutionary Computing [cs.NE], Scintillator, 7. Clean energy, 01 natural sciences, law.invention, Telescope, Optics, Position reconstruction, law, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation, GEANT4, Physics, Gamma-ray astronomy, Calorimeter (particle physics), 010308 nuclear & particles physics, business.industry, Detector, Gamma ray, Space instrumentation, LaBr3:Ce, business
Abstract: Gamma-ray astronomy in the energy range from 0.1 up to 100 MeV holds many understudied questions connected with e.g. stellar nucleosynthesis, the active Sun, neutron stars and black holes. To access the physics behind, a significant improvement in detection sensitivity is needed compared to previous missions, e.g. CGRO and INTEGRAL. One of the promising concepts for a future gamma-ray mission is an Advanced Compton Telescope. Under the project of creating a prototype of such instrument, we study the perspectives of using a novel inorganic scintillator as a calorimeter part. Modern inorganic crystal or ceramics scintillators are constantly improving on qualities such as energy resolution and radiation hardness, and this makes them a smart choice for a new space-borne telescope. At CSNSM Orsay, we have assembled a detection module from a 5 × 5 cm 2 area and 1 cm thick, cerium-doped lanthanum (III) bromide (LaBr 3 :Ce) inorganic scintillator coupled to a 64 channel multi-anode photomultiplier. The readout of the PMT signals is carried out with the ASIC MAROC, used previously for the luminometer of the ATLAS detector (CERN). Characterization, thorough measurements with various radioactive sources, as well as, single photoelectron detection have been done. Furthermore, we made a comparison of measurements with a detailed GEANT4-based simulation which includes tracking of the optical photons. Finally, we have studied the 3D reconstruction of the first interaction point of incident gamma rays, utilizing a neural network algorithm. This spatial position resolution plays a crucial part in the future implementations and, together with the other measured properties, it makes our detector module very interesting for the next generation of space telescopes operating in the MeV range.
Published: 2015
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9. The e-ASTROGAM gamma-ray space observatory for the multimessenger astronomy of the 2030s

Author: Koji Nakazawa, F. Longo, A. Brogna, Andrei M. Bykov, J. Peyré, J. M. Paredes, A. A. Zdziarski, M. Hernanz, D. de Martino, Paolo De Coppi, Irfan Kuvvetli, M. Roncadelli, I. Donnarumma, A. De Angelis, I. Grenier, B. Patricelli, Vincent Tatischeff, G. Piano, Marco Tavani, Elisa Bernardini, M. Pohl, S. Ciprini, Carl Budtz-Jørgensen, Marco Ajello, P. von Ballmoos, J. Kiener, D. J. Thompson, Philippe Laurent, A. Aboudan, Jürgen Knödlseder, P. Cumani, Miriam Lucio Martinez, Lorraine Hanlon, Stefan Funk, Michele Doro, Martino Marisaldi, J. E. Grove, R. Rando, Gabriele Ghisellini, R. M. Curado da Silva, A. A. Moiseev, V. Bonvicini, Fabrizio Tavecchio, Julie McEnery, Gottfried Kanbach, A. Argan, Mark D. Leising, Roland Diehl, O. Limousin, Andrea Bulgarelli, Manuela Mallamaci, M. Cardillo, M. Branchesi, Xin Wu, A. Morselli, Sandro Mereghetti, Mark Pearce, R. Turolla, G. Minervini, R. Walter, C. Hamadache, Dieter H. Hartmann, Valentina Fioretti, Piotr Orleanski, A. Vacchi, A. Ulyanov, G. Ambrosi, Karl Mannheim, Ferdinando Giordano, D. Bernard, N. M. Mazziotta, Riccardo Campana, Uwe Oberlack, Jordi Isern, M. Hayashida, Andreas Zoglauer, Claudio Labanti, den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, e-ASTROGAM, FRA, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Jan-Willem A. den Herder, Shouleh Nikzad, Kazuhiro Nakazawa, Tatischeff, V., De Angelis, A., Tavani, M., Grenier, I., Oberlack, U., Hanlon, L., Walter, R., Argan, A., Von Ballmoos, P., Bulgarelli, A., Donnarumma, I., Hernanz, M., Kuvvetli, I., Mallamaci, M., Pearce, M., Zdziarski, A., Aboudan, A., Ajello, M., Ambrosi, G., Bernard, D., Bernardini, E., Bonvicini, V., Brogna, A., Branchesi, M., Budtz-Jorgensen, C., Bykov, A., Campana, R., Cardillo, M., Ciprini, S., Coppi, P., Cumani, P., Curado Da Silva, R. M., De Martino, D., Diehl, R., Doro, M., Fioretti, V., Funk, S., Ghisellini, G., Grove, J. E., Giordano, F., Hamadache, C., Hartmann, D. H., Hayashida, M., Isern, J., Kanbach, G., Kiener, J., Knodlseder, J., Labanti, C., Laurent, P., Leising, M., Limousin, O., Longo, F., Mannheim, K., Marisaldi, M., Martinez, M., Mazziotta, N. M., Mcenery, J. E., Mereghetti, S., Minervini, G., Moiseev, A., Morselli, A., Nakazawa, K., Orleanski, P., Paredes, J. M., Patricelli, B., Peyre, J., Piano, G., Pohl, M., Rando, R., Roncadelli, M., Tavecchio, F., Thompson, D. J., Turolla, R., Ulyanov, A., Vacchi, A., Wu, X., Zoglauer, A., 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: Cherenkov Telescope Array, High-energy astrophysical phenomena, Compton and pair creation telescope, Gamma-ray astronomy, gamma-ray polarization, high-energy astrophysical phenomena, space mission, time-domain astronomy, energy resolution, 7. Clean energy, 01 natural sciences, Space mission, law.invention, IceCube, Einstein Telescope, law, Observatory, LIGO, 010303 astronomy & astrophysics, KM3NeT, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Applied Mathematics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Gamma-ray polarization, Condensed Matter Physics, photon: energy, observatory, Nuclear astrophysics, Apace mission, Astrophysics - High Energy Astrophysical Phenomena, performance, detector: technology, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, Telescope, 0103 physical sciences, supernova, Electronic, calorimeter, gamma ray: detector, Optical and Magnetic Materials, KAGRA, Electrical and Electronic Engineering, 010306 general physics, Time domain astronomy, LISA, Astronomy, Institut für Physik und Astronomie, Time-domain astronomy, sensitivity, messenger, VIRGO, 13. Climate action, Electronic, Optical and Magnetic Materials, ddc:520, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: e-ASTROGAM is a concept for a breakthrough observatory space mission carrying a gamma-ray telescope dedicated to the study of the non-thermal Universe in the photon energy range from 0.15 MeV to 3 GeV. The lower energy limit can be pushed down to energies as low as 30 keV for gamma-ray burst detection with the calorimeter. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with remarkable polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous and current generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will be a major player of the multiwavelength, multimessenger time-domain astronomy of the 2030s, and provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LISA, LIGO, Virgo, KAGRA, the Einstein Telescope and the Cosmic Explorer, IceCube-Gen2 and KM3NeT, SKA, ALMA, JWST, E-ELT, LSST, Athena, and the Cherenkov Telescope Array., Comment: 15 pages, 7 figures. Submitted to the proceedings of the conference SPIE Astronomical Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray. v2: corrections of authors' affiliations
Published: 2018
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10. New determination of proton spectroscopic factors and reduced widths forBe8states in the 16.5–18.0 MeV excitation energy region via the study of theLi7(He3,d)Be8transfer reaction atElab=20MeV: Implication for theLi7(p,α)He4hydrogen burning reaction

Author: H. Beaumevieille, A. Bouchemha, S. Ouichaoui, S. Fortier, L. Rosier, J. Kiener, J. M. Maison, J. Vernotte, A. Belhout, J. P. Thibaud, J. Rotbard, V. Tatischeff, A. Lefebvre-Schuhl, and G. Bogaert
Subjects: Physics, Proton, 010308 nuclear & particles physics, 01 natural sciences, Spectral line, Ion, Deuterium, 0103 physical sciences, Bound state, Atomic physics, Born approximation, Nuclear Experiment, 010306 general physics, Energy (signal processing), Excitation
Abstract: The angular distributions of $^{8}\mathrm{Be}$ states in the excitation energy region ${E}_{x}\ensuremath{\sim}(16.5\text{--}18.2)$ MeV produced in the $^{7}\mathrm{Li}(^{3}\mathrm{He},d)^{8}\mathrm{Be}$ proton transfer reaction have been measured at the Orsay $14.8\ensuremath{-}\mathrm{MV}$ tandem accelerator for $^{3}\mathrm{He}^{2+}$ ion bombarding energy, ${E}_{\text{lab}}\phantom{\rule{4pt}{0ex}}=20$ MeV, and forward angular range, ${\ensuremath{\theta}}_{\text{lab}}=5{}^{\ensuremath{\circ}}\text{--}50{}^{\ensuremath{\circ}}$. A high energy resolution detection system composed of a split-pole magnetic spectrometer and a $\mathrm{\ensuremath{\Delta}}E\ensuremath{-}E$, position-sensitive drift chamber was used to record the energy spectra of outgoing deuterons. The measured cross section data for the direct reaction component have been separated from the compound nucleus one, then analyzed in the framework of the nonlocal, finite-range (FR)--distorted-wave Born approximation (DWBA) theory. New values of the ${C}^{2}S$ and (${S}_{p1/2},\phantom{\rule{4pt}{0ex}}{S}_{p3/2})$ proton absolute and partial spectroscopic factors and related ${\ensuremath{\gamma}}_{p}^{2}(a)$ proton reduced widths versus the $p+^{7}\mathrm{Li}$ channel radius have been extracted for the ${2}^{+}(16.626)$ and ${2}^{+}(16.922),T=0+1$ isospin-mixed loosely bound states of astrophysical interest and the ${1}^{+}(17.640)$, $T=1$ unbound state of $^{8}\mathrm{Be}$. They are compared to sparse earlier experimental values and to shell-model-predicted ones from the literature, and are discussed. In particular, the status of the spectroscopic information on the ${2}^{+}$ isospin-mixed doublet is reviewed and updated. The application in nuclear astrophysics of the DWBA derived results is emphasized.
Published: 2017
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11. Study of key resonances in the $^{30}$P(p,γ)$^{31}$S reaction in classical novae

Author: F. Flavigny, L. Olivier, A. Alellara, B. Bastin, L. Perrot, J. Riley, L. Grassi, F. de Oliveira, T. Id Barkach, J. Guillot, Alison Laird, J. Kiener, Á. M. Sánchez Benítez, D. Beaumel, V. Tatischeff, Marlete Assunção, Anuj Parikh, S. P. Fox, A. Meyer, P. Adsley, Giuseppe D’Agata, C. Portail, A. Gottardo, F. Hammache, I. Matea, M. Assié, N. Oulebsir, A. Georgiadou, C. Delafosse, M. MacCormick, N. Hubbard, Valdir Guimaraes, A. Coc, N. de Séréville, I. Stefan, K. Béroff, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Physics, Proton, 010308 nuclear & particles physics, QC1-999, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Coincidence, Nuclear physics, Reaction rate, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, Excited state, 0103 physical sciences, 010303 astronomy & astrophysics
Abstract: Among reactions with strong impact on classical novae model predictions, 30P(p,γ)31S is one of the few remained that are worthy to be measured accurately, because of their rate uncertainty, as like as 18F(p,α)15O and 25Al(pγ)26Si. To reduce the nuclear uncertainties associated to this reaction, we performed an experiment at ALTO facility of Orsay using the 31P(3He,t)31S reaction to populate 31S excited states of astrophysical interest and detect in coincidence the protons coming from the decay of the populated states in order to extract the proton branching ratios. After a presentation of the astrophysical context of this work, the current situation of the 30P(p,γ)31S reaction rate will be discussed. Then the experiment set-up of this work and the analysis of the single events will be presented.
Published: 2017
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12. Spectroscopy of Fe61 via the neutron transfer reaction H2(Fe60,p)Fe*61

Author: S. Giron, F. Hammache, N. de Séréville, P. Roussel, J. Burgunder, M. Moukaddam, D. Beaumel, L. Caceres, G. Duchêne, E. Clément, B. Fernandez-Dominguez, F. Flavigny, G. de France, S. Franchoo, D. Galaviz-Redondo, L. Gasques, J. Gibelin, A. Gillibert, S. Grevy, J. Guillot, M. Heil, J. Kiener, V. Lapoux, F. Maréchal, A. Matta, I. Matea, L. Nalpas, J. Pancin, L. Perrot, A. Obertelli, R. Raabe, J. A. Scarpaci, K. Sieja, O. Sorlin, I. Stefan, C. Stodel, M. Takechi, J. C. Thomas, and Y. Togano
Subjects: Physics, Photon, Silicon, 010308 nuclear & particles physics, chemistry.chemical_element, 01 natural sciences, 7. Clean energy, Charged particle, Cross section (physics), chemistry, 0103 physical sciences, Bound state, Neutron, Atomic physics, 010306 general physics, Adiabatic process, Spectroscopy
Abstract: The direct component of the 60Fe(n,γ)61Fe cross section was investigated by populating the bound states of the 61Fe nucleus through the (d,pγ) transfer reaction in inverse kinematics using a radioactive beam of 60Fe at 27A MeV. The experiment was performed at GANIL using the MUST2 array and an annular double-sided silicon strip detector for the detection of the light charged particle in coincidence with the photons measured in the EXOGAM γ-ray detectors. For the first time, the spectroscopic factors of the first 3/2−, 5/2−, 1/2−, and 9/2+ states of 61Fe were deduced experimentally from an adiabatic distorted wave approximation analysis of the data. The obtained results show a very good agreement with the shell-model predictions. The calculated direct component of the (n,γ) cross section was found negligible and of about 2% of the total, indicating a dominant resonant component.
Published: 2017
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13. The e-ASTROGAM mission: Exploring the extreme Universe with gamma rays in the MeV â GeV range

Author: Barbara Patricelli, V. Bonvicini, Riccardo Rando, Sandro Mereghetti, Andrea Vacchi, Kazuhiro Nakazawa, Claudio Labanti, Jordi Isern, M. Hayashida, Josep M. Paredes, J. Eric Grove, C. Hamadache, Andreas Zoglauer, Olivier Limousin, Julie McEnery, Andrei M. Bykov, G. Ambrosi, D. de Martino, Francesco Longo, Irfan Kuvvetli, Alexander Moiseev, Xin Wu, Fabrizio Tavecchio, I. Donnarumma, M. I. Martínez, Marco Tavani, J. Peyré, Elisa Bernardini, A. Argan, Roland Walter, J. Kiener, Piotr Orleanski, Mark Pearce, Ignasi Reichardt, A. Morselli, Andrzej A. Zdziarski, Martino Marisaldi, Vincent Tatischeff, Andrea Bulgarelli, Marica Branchesi, Uwe Oberlack, Rui Curado da Silva, Dieter H. Hartmann, Lorraine Hanlon, Philippe Laurent, Marco Ajello, D. Bernard, Valentina Fioretti, Martin Pohl, Alessio Aboudan, Gottfried Kanbach, Alessandro De Angelis, Gabriele Ghisellini, Stefan Funk, Peter von Ballmoos, Michele Doro, M. N. Mazziotta, Marco Roncadelli, Harald Ramarijaona, Roland Diehl, Margarita Hernanz, Alexei Ulyanov, G. Minervini, G. Piano, Riccardo Campana, Carl Budtz-Jørgensen, D. J. Thompson, M. Cardillo, Paolo De Coppi, Karl Mannheim, Roberto Turolla, Jürgen Knödlseder, Isabelle Grenier, A. Brogna, De Angelis, A., Tatischeff, V., Tavani, M., Oberlack, U., Grenier, I., Hanlon, L., Walter, R., Argan, A., von Ballmoos, P., Bulgarelli, A., Donnarumma, I., Hernanz, M., Kuvvetli, I., Pearce, M., Zdziarski, A., Aboudan, A., Ajello, M., Ambrosi, G., Bernard, D., Bernardini, E., Bonvicini, V., Brogna, A., Branchesi, M., Budtz-Jorgensen, C., Bykov, A., Campana, R., Cardillo, M., Coppi, P., De Martino, D., Diehl, R., Doro, M., Fioretti, V., Funk, S., Ghisellini, G., Grove, E., Hamadache, C., Hartmann, D. H., Hayashida, M., Isern, J., Kanbach, G., Kiener, J., Knödlseder, J., Labanti, C., Laurent, P., Limousin, O., Longo, F., Mannheim, K., Marisaldi, M., Martinez, M., Mazziotta, M. N., Mcenery, J., Mereghetti, S., Minervini, G., Moiseev, A., Morselli, A., Nakazawa, K., Orleanski, P., Paredes, J. M., Patricelli, B., Peyré, J., Piano, G., Pohl, M., Ramarijaona, H., Rando, R., Reichardt, I., Roncadelli, M., Silva, R., Tavecchio, F., Thompson, D. J., Turolla, R., Ulyanov, A., Vacchi, A., Wu, X., Zoglauer, A., and ITA
Subjects: Counterparts of gravitational wave, Multiwavelength Observations of the Universe, 01 natural sciences, Early Universe, Observatory, Jets, Nuclear Astrophysics, Nuclear astrophysics, Dark Matter, Nuclear Experiment (nucl-ex), Nuclear Astrophysic, Nuclear Experiment, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::Instrumentation and Methods for Astrophysics, Counterparts of gravitational waves, Gamma-Ray Burst, Cosmic Rays, Compton and Pair Creation Telescope, Supernovae, Astrophysics - Solar and Stellar Astrophysics, High-Energy Astrophysics, Active Galactic Nuclei, Cosmic Antimatter, Fermi, Gamma-Ray Bursts, High-Energy Gamma-Ray Astronomy, Nucleosynthesis, Outflows, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Active galactic nucleus, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmic Ray, High-Energy Astrophysic, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Nucleosynthesi, 010308 nuclear & particles physics, Institut für Physik und Astronomie, Astronomy, Outflow, Astronomy and Astrophysic, Universe, Galaxy, Jet, Fermi Gamma-ray Space Telescope
Abstract: e-ASTROGAM (`enhanced ASTROGAM') is a breakthrough Observatory mission dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. In the largely unexplored MeV-GeV domain, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on Galactic ecosystems. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA. Keywords: High-energy gamma-ray astronomy, High-energy astrophysics, Nuclear Astrophysics, Compton and Pair creation telescope, Gamma-ray bursts, Active Galactic Nuclei, Jets, Outflows, Multiwavelength observations of the Universe, Counterparts of gravitational waves, Fermi, Dark Matter, Nucleosynthesis, Early Universe, Supernovae, Cosmic Rays, Cosmic antimatter., Comment: Exp Astron (2017)
Published: 2017

14. Characterization of LaBr3:Ce and CeBr3 calorimeter modules for 3D imaging in gamma-ray astronomy

Author: N. Karkour, C. Hamadache, D. Linget, N. Dosme, L. Gibelin, X. Lafay, A. Gostojić, S. Blin, J. Kiener, E. Legay, X. Grave, V. Tatischeff, Jean Peyré, P. Barrillon, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM AN), Université Paris-Saclay-Univ. Paris-Sud-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), CSNSM INSTRU, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CSNSM ELEC, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), CSNSM INFOR, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Laboratoire de l'Accélérateur Linéaire (LAL)
Subjects: Artificial neural network, Nuclear and High Energy Physics, Test bench, Anger logic, Instrumentation, Compton telescope, Astrophysics::High Energy Astrophysical Phenomena, 01 natural sciences, law.invention, Telescope, Data acquisition, Optics, law, CeBr3, 0103 physical sciences, Energy resolution, 010303 astronomy & astrophysics, Physics, [PHYS]Physics [physics], Gamma-ray astronomy, Calorimeter (particle physics), 010308 nuclear & particles physics, business.industry, Geant4 Position reconstruction, Detector, PERFORMANCE, 3. Good health, ARRAYS, CRYSTALS, Space instrumentation, LaBr3:Ce, business, SCINTILLATION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; For the purpose of future space instrumentation for gamma-ray astronomy, we developed a small prototype of a Compton telescope and studied novel detector modules aimed for Compton imaging. We assembled and tested 2 modules, one with a cerium-doped lanthanum(111) bromide (LaBr3:Ce) crystal and the other with cerium(111) bromide (CeBr3). Both crystals measure 5 x 5 cm(2) in area and are 1 cm thick. They are coupled to and read out by 64-channel multi-anode PMTS. Our goals are to obtain the best possible energy resolution and position resolution in 3D on the first impact of an incident gamma-ray within the detector. Both information are vital for successful reconstruction of a Compton image with the telescope prototype. We developed a test bench to experimentally study both modules and have utilized a customized readout electronics and data acquisition system. Furthermore, we have written a detailed Geant4 simulation of the experiment, and utilize simulated data to train an Artificial Neural Network (ANN) algorithm to create a simplified 3D impact position reconstruction method. We give experimental test results obtained by both modules and present detailed parametrization and results from the Geant4 simulation and from the ANN. We compare and discuss the performance of the modules and conclude by giving a brief overview of the future prospects for using such modules in gamma-ray astronomy. (C) 2016 Elsevier B.V. All rights reserved.
Published: 2016
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15. GAMCOTE: a prototype for an advanced Compton Telescope

Author: N. de Séréville, A.-S. Torrentó, J.-J. Dormard, C. Santos, E. Legay, W. Bertoli, N. Karkour, J. Peyré, J. Kiener, V. Le Ven, C. Hamadache, X. Lafay, O. Limousin, E. Wanlin, E. Rauly, Vincent Tatischeff, N. Dosme, A. Gostojic, D. Linget, R. Oger, B. Genolini, Ph. Rosier, L. Gibelin, Ph. Laurent, G. Brulin, T. Faul, X. Grave, and D. Maier
Subjects: Physics, Photomultiplier, Photon, Calorimeter (particle physics), Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Compton telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Compton scattering, Astronomy, Gamma-ray astronomy, 01 natural sciences, law.invention, Telescope, Optics, law, 0103 physical sciences, business, 010303 astronomy & astrophysics
Abstract: Astronomy in the MeV gamma-ray band (0.1 - 100 MeV) holds a rich promise for elucidating many fundamental questions concerning the most violent cosmic phenomena. The next generation of gamma-ray space instrument could be a Compton and pair-creation telescope made of two main parts: a silicon tracker optimized for Compton scattering of cosmic gamma rays and a calorimeter that absorbs the scattered photons. We present here the first results of GAMCOTE, a GAMma-ray COmpton TElescope prototype which includes thick double sided silicon strip detectors coupled to a LaBr3:Ce crystal read by a 64 multi-anode photomultiplier tube.
Published: 2016
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16. The e-ASTROGAM gamma-ray space mission

Author: Andrei M. Bykov, A. De Angelis, Dieter H. Hartmann, Sheila McBreen, Uwe Oberlack, M. Cardillo, C. Pittori, D. Bernard, Sandro Mereghetti, Francesco Longo, Philippe Laurent, Jürgen Knödlseder, R. Walter, Andreas Zoglauer, Valentina Fioretti, Marco Tavani, S. Sabatini, A. Brogna, Martino Marisaldi, C. Labanti, Jordi Isern, Kazuhiro Nakazawa, J. Peyré, Paolo Coppi, Julie McEnery, A. Morselli, J. Kiener, Lorraine Hanlon, G. Piano, Andrzej A. Zdziarski, Xin Wu, A. Argan, Andrea Bulgarelli, Riccardo Campana, D. J. Thompson, P. A. Caraveo, Margarita Hernanz, Alessio Aboudan, P. von Ballmoos, F. Mirabel, I. Donnarumma, V. Tatischeff, I. A. Grenier, Olivier Limousin, G. Kanbach, Roland Diehl, Alexei Ulyanov, J. E. Grove, L. Stawarz, A. Giuliani, C. Hamadache, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre de Sciences Nucléaires et de Sciences de la Matière ( CSNSM ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -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 ), AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Tatischeff, V., Tavani, M., Von Ballmoos, P., Hanlon, L., Oberlack, U., Aboudan, A., Argan, A., Bernard, D., Brogna, A., Bulgarelli, A., Bykov, A., Campana, R., Caraveo, P., Cardillo, M., Coppi, P., De Angelis, A., Diehl, R., Donnarumma, I., Fioretti, V., Giuliani, A., Grenier, I., Grove, J. E., Hamadache, C., Hartmann, D., Hernanz, M., Isern, J., Kanbach, G., Kiener, J., Knodlseder, J., Labanti, C., Laurent, P., Limousin, O., Longo, F., Marisaldi, M., Mcbreen, S., Mcenery, J. E., Mereghetti, S., Mirabel, F., Morselli, A., Nakazawa, K., Peyre, J., Piano, G., Pittori, C., Sabatini, S., Stawarz, L., Thompson, D. J., Ulyanov, A., Walter, R., Wu, X., Zdziarski, A., Zoglauer, A., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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: Compton and pair creation telescope, Gamma-ray astronomy, gamma-ray polarization, high-energy astrophysical phenomena, space mission, time-domain astronomy, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Dark matter, Observatories, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Polarization, 0103 physical sciences, Galaxy groups and clusters, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, Active galactic nuclei, 010308 nuclear & particles physics, Sensors, Galactic Center, Galaxy, Particle accelerators, Neutron star, Gamma radiation, Chemicals, Electronics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope, Telescopes
Abstract: The e-ASTROGAM is a gamma-ray space mission to be proposed as the M5 Medium-size mission of the European Space Agency. It is dedicated to the observation of the Universe with unprecedented sensitivity in the energy range 0.2 - 100 MeV, extending up to GeV energies, together with a groundbreaking polarization capability. It is designed to substantially improve the COMPTEL and Fermi sensitivities in the MeV-GeV energy range and to open new windows of opportunity for astrophysical and fundamental physics space research. e-ASTROGAM will operate as an open astronomical observatory, with a core science focused on (1) the activity from extreme particle accelerators, including gamma-ray bursts and active galactic nuclei and the link of jet astrophysics to the new astronomy of gravitational waves, neutrinos, ultra-high energy cosmic rays, (2) the high-energy mysteries of the Galactic center and inner Galaxy, including the activity of the supermassive black hole, the Fermi Bubbles, the origin of the Galactic positrons, and the search for dark matter signatures in a new energy window; (3) nucleosynthesis and chemical evolution, including the life cycle of elements produced by supernovae in the Milky Way and the Local Group of galaxies. e-ASTROGAM will be ideal for the study of high-energy sources in general, including pulsars and pulsar wind nebulae, accreting neutron stars and black holes, novae, supernova remnants, and magnetars. And it will also provide important contributions to solar and terrestrial physics. The e-ASTROGAM telescope is optimized for the simultaneous detection of Compton and pair-producing gamma-ray events over a large spectral band. It is based on a very high technology readiness level for all subsystems and includes many innovative features for the detectors and associated electronics., 11 pages, 5 figures, published in the proceedings of SPIE Astronomical Telescopes and Instrumentation: Ultraviolet to Gamma Ray conference, Edinburgh 2016. Addition of an acknowledgment statement in version 2
Published: 2016
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17. NUCLEAR GAMMA-RAY DE-EXCITATION LINES AND CONTINUUM FROM ACCELERATED-PARTICLE INTERACTIONS IN SOLAR FLARES

Author: Gerald H. Share, Benzion Kozlovsky, J. Kiener, R. J. Murphy, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Sun: flares, Physics, Solar flare, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Projectile, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Spectral line, Computational physics, Ion, law.invention, Space and Planetary Science, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Chromosphere, Excitation, Flare
Abstract: Analyses of gamma-ray line emission in solar flares have provided information about conditions in flaring magnetic loops, the abundances of the chromosphere where the gamma rays are produced, and the composition and spectrum of the flare-accelerated ions. While laboratory measurements of the cross sections for production of the strongest lines seen in flare spectra are available, these measurements often only cover a limited range of projectile energies. In addition, the bulk of the gamma-ray emission arises from the numerous weaker lines for which there are no measurements. The gamma-ray de-excitation-line production code, developed originally by Ramaty, Kozlovsky, and Lingenfelter, has been and continues to be the primary theoretical tool used for analyses of solar-flare gamma-ray data. The code uses both measured cross sections and estimated cross sections where measurements are inadequate. We have improved the completeness and accuracy of this code in three ways. (1) We use recent cross section measurements to improve cross sections for those lines already explicitly included in the code and to provide cross sections for new explicit lines. (2) For the first time, we give a detailed evaluation of the unresolved-line "continuum" (i.e., all line emission not accounted for by the explicit lines in the code). Because adequate laboratory measurements for this emission are not available, the primary tool for this evaluation was the theoretical nuclear program TALYS. We explore how this unresolved-line continuum depends on parameters relevant for solar flares. (3) We use TALYS to improve those line cross sections where available laboratory measurements are inadequate and to provide cross sections for new explicit lines for which no measurements exist. Numerical cross section values for all lines explicitly addressed by the code and for the unresolved-line continua are given in the Appendix.
Published: 2009
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18. Search for resonant states in $^{10}$C and $^{11}$C and their impact on the primordial $^{7}$Li abundance

Author: L. Lefebvre, Predrag Ujić, J. Kiener, J. Mrazek, André Palma da Cunha Matta, B. Fernández-Domínguez, A. Coc, A. M. Sánchez-Benítez, I. Stefan, P. Morfouace, Didier Beaumel, Daisuke Suzuki, I. Matea, S. Franchoo, B. Le Crom, M. Assié, A. Lefebvre-Schuhl, N. de Sereville, F. Hammache, F. de Oliveira Santos, L. Audouin, G. Mavilla, Vincent Tatischeff, Anuj Parikh, C. Hamadache, Marine Vandebrouck, L. Perrot, Alison Laird, S. P. Fox, P. Roussel, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Grand Accélérateur National d'Ions Lourds (GANIL), 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), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear reaction, Physics, History, 010308 nuclear & particles physics, Primordial 7Li, Resonant states, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 7. Clean energy, 01 natural sciences, Cosmology, Computer Science Applications, Education, Nuclear physics, Helium-4, Nucleosynthesis, Helium-3, 0103 physical sciences, Isotopes of beryllium, 010303 astronomy & astrophysics, Isotopes of helium, Radioactive decay, 7Li abundance
Abstract: The cosmological 7Li problem arises from the signi cant discrepancy of about a factor 3 between the predicted primordial 7Li abundance and the observed one. The main process for the production of 7Li during Big-Bang nucleosynthesis is the decay of 7Be. Many key nuclear reactions involved in the production and destruction of 7Be were investigated in attempt to explain the 7Li de cit but none of them led to successful conclusions. However, some authors suggested recently the possibility that the destruction of 7Be by 3He and 4He may reconcile the predictions and observations if missing resonant states in the compound nuclei 10C and 11C exist. Hence, a search of these missing resonant states in 10C and 11C was investigated at the Orsay Tandem-Alto facility through 10B(3He,t)10C and 11B(3He,t)11C charge-exchange reactions respectively. After a short overview of the cosmological 7Li problem from a nuclear physics point of view, a description of the Orsay experiment will be given as well as the obtained results and their impact on the 7Li problem.
Published: 2015
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19. The 7 Be( d , p )2α Cross Section at Big Bang Energies and the Primordial 7 Li Abundance

Author: Pierre Leleux, I. Mukha, Vincent Tatischeff, P. Figuera, Manoel Couder, A.S. Murphy, B.R. Fulton, F. Vanderbist, T. Davinson, Elisabeth Vangioni, P. Demaret, A. Coc, E. Casarejos, J. Kiener, N. A. Orr, Carmen Angulo, N. L. Achouri, and D. Cortina-Gil
Subjects: Physics, Big Bang, 010308 nuclear & particles physics, Cosmic microwave background, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, CMB cold spot, Galactic halo, Baryon, Stars, Big Bang nucleosynthesis, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Anisotropy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The WMAP satellite, devoted to the observations of the anisotropies of the Cosmic Microwave Background (CMB) radiation, has recently provided a determination of the baryonic density of the Universe with unprecedented precision. Using this, Big Bang Nucleosynthesis (BBN) calculations predict a primordial 7Li abundance which is a factor 2-3 higher than that observed in galactic halo dwarf stars. It has been argued that this discrepancy could be resolved if the 7Be(d,p)2alpha reaction rate is around a factor of 100 larger than has previously been considered. We have now studied this reaction, for the first time at energies appropriate to the Big Bang environment, at the CYCLONE radioactive beam facility at Louvain-la-Neuve. The cross section was found to be a factor of 10 smaller than derived from earlier measurements. It is concluded therefore that nuclear uncertainties cannot explain the discrepancy between observed and predicted primordial 7Li abundances, and an alternative astrophysical solution must be investigated.
Published: 2005
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20. Study of 7Be+d reactions for Standard Big Bang Nucleosynthesis

Author: Pierre Leleux, D. Cortina-Gil, Vincent Tatischeff, A.S. Murphy, Carmen Angulo, Alain Ninane, B. R. Fulton, N. A. Orr, J. Kiener, T. Davinson, Ivan Mukha, P. Figuera, E. Casarejos, A. Coc, F. Vanderbist, Manoel Couder, N. L. Achouri, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), and Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)
Subjects: Physics, Nuclear and High Energy Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, 7. Clean energy, 01 natural sciences, CMB cold spot, Abundance of the chemical elements, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear physics, Big Bang nucleosynthesis, Baryon density, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: The recent WMAP results tightly constrain the baryon density in the universe, which in turn constrains the light element abundance predicted in Standard Big Bang Nucleosynthesis (SBBN). There is a discrepance in the $^7$Li abundance which cannot be explained by uncertainties in the main reactions included in the SBBN. Up to now, the influence of the reaction $^7Be(d,p)2\alpha$ has been neglected. We have investigated this reaction at SBBN energies using a radioactive $^7$Be beam and a $(CD_2)_n$ self-supporting target at the CYCLONE RIB facility at Louvain-la-Neuve. The experimental method is briefly described. Preliminary results and consequences for primordial nucleosynthesis are discussed.
Published: 2005
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21. New determination of the 12C(α, γ)16O reaction rate from γ-ray angular distribution measurements

Author: Neil Rowley, F. Fleurot, A. Lopez-Martens, J. Kiener, A. Korichi, D. Le Du, J. W. Hammer, C. Beck, F. Haas, S. Courtin, Alain Coc, Suzana Szilner, G. Staudt, J.J. Correia, C. Boukari-Pelissie, E. Galanopoulos, M. Rousseau, J.L. Weil, C. Grama, R. Kunz, D. Malcherek, P. Papka, R. Meunier, T. Paradellis, Vincent Tatischeff, M. Fey, Sotirios Harissopulos, E. Krmpotic, F. Hammache, and M. Assunção
Subjects: Physics, Reaction rate, Nuclear and High Energy Physics, Angular distribution, 010308 nuclear & particles physics, Nucleosynthesis, 0103 physical sciences, Gamma ray, Alpha (ethology), Atomic physics, 010306 general physics, 01 natural sciences
Published: 2005
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22. SPI instrumental background characteristics

Author: Bonnard J. Teegarden, Pierre Leleux, Bertrand Cordier, G. Vedrenne, P. A. Caraveo, P. Mandrou, Pierre Jean, Georg Weidenspointner, G. G. Lichti, Emrah Kalemci, P. von Ballmoos, M. Gros, Cornelia B. Wunderer, Jean-Pierre Roques, Stéphane Schanne, Gerald K. Skinner, S. E. Boggs, Roland Diehl, V. Lonjou, Jürgen Knödlseder, A. von Kienlin, David Attié, J. Kiener, V. Schönfelder, P. Paul, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), 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), 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), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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, and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, 01 natural sciences, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Telescope, Optics, Observatory, law, 0103 physical sciences, Sensitivity (control systems), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Range (particle radiation), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Spectrometer, Spacecraft, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, gamma-ray: instruments, 13. Climate action, Space and Planetary Science, business, Energy (signal processing), Space environment
Abstract: In its space environment the INTEGRAL observatory is subject to an intense irradiation by energetic cosmic-ray particles that leads, via nuclear interactions with the telescope and spacecraft materials, to an important background of false events. In this paper we present the characteristics of the instrumental background that is observed in the spectrometer SPI (SPectrometer of INTEGRAL). We explain the tuning that has been performed on the parameters of the anticoincidence system in order to optimise the telescope sensitivity over the full energy range. Temporal variations of the instrumental background are discussed and methods are proposed that allow for their modelling in first order.
Published: 2003
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23. Low-Energy Measurement of theB7e(p,γ)B8Cross Section

Author: L. Brillard, G. Bogaert, M. Jacotin, J. P. Thibaud, C. Le Naour, J. N. Scheurer, A. Coc, Carmen Angulo, V. Tatischeff, M. Hussonnois, A. Lefebvre, F. Hammache, S. Ouichaoui, J.F. Chemin, E. Virassamynaiken, G. Claverie, J. Kiener, P. Aguer, and S. Barhoumi
Subjects: Physics, Spectrometer, 010308 nuclear & particles physics, S-factor, General Physics and Astronomy, Zero-point energy, Alpha particle, 01 natural sciences, Coincidence, Spectral line, Cross section (physics), Low energy, 0103 physical sciences, Atomic physics, 010306 general physics
Abstract: We have measured the cross section of the 7Be(p,gamma)8B reaction for E_cm = 185.8 keV, 134.7 keV and 111.7 keV using a radioactive 7Be target (132 mCi). Single and coincidence spectra of beta^+ and alpha particles from 8B and 8Be^* decay, respectively, were measured using a large acceptance spectrometer. The zero energy S factor inferred from these data is 18.5 +/- 2.4 eV b and a weighted mean value of 18.8 +/- 1.7 eV b (theoretical uncertainty included) is deduced when combining this value with our previous results at higher energies. Comment: Accepted for publication in Phys. Rev. Lett
Published: 2001
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24. New Measurement and Analysis of theB7e(p,γ)B8Cross Section

Author: M. Hussonnois, C. Angulo, J. P. Thibaud, J. Kiener, L. Brillard, A. Coc, M. Jacotin, S. Barhoumi, G. Claverie, A. Lefebvre, P. Aguer, E. Virassamynaiken, J. N. Scheurer, J.F. Chemin, G. Bogaert, and F. Hammache
Subjects: Physics, Cross section (physics), 010308 nuclear & particles physics, 0103 physical sciences, General Physics and Astronomy, Atomic physics, 010306 general physics, 7. Clean energy, 01 natural sciences
Abstract: Cross sections for the ${}^{7}\mathrm{Be}(p,\ensuremath{\gamma}{)}^{8}\mathrm{B}$ reaction have been measured for ${E}_{\mathrm{c}.\mathrm{m}.}\phantom{\rule{0ex}{0ex}}=\phantom{\rule{0ex}{0ex}}0.35--1.4\mathrm{MeV}$ using radioactive ${}^{7}\mathrm{Be}$ targets. Two independent measurements carried out with different beam conditions, different targets, and detectors are in excellent agreement. A statistical comparison of these measurements with previous results leads to a restricted set of consistent data. The deduced zero-energy $S$ factor $S(0)$ is found to be 15%--20% smaller than the previously recommended value. This implies a ${}^{8}\mathrm{B}$ solar neutrino flux lower than previously predicted in various standard solar models.
Published: 1998
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25. Ionic charge dependence of the internal conversion coefficient and nuclear lifetime of the first excited state in125Te

Author: G. Bogaert, C. Grunberg, J. P. Thibaud, J.F. Chemin, A. Lefebvre, F. Attallah, W. E. Meyerhof, J. N. Scheurer, J. Kiener, M. Aiche, J. R. Grandin, P. Aguer, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and 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)
Subjects: Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Electron, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, 7. Clean energy, Ion, Excited state, 0103 physical sciences, State dependence, Atomic physics, 010306 general physics, Internal conversion coefficient
Abstract: We have studied the ionic charge state dependence of the nuclear lifetime of the 35.5-keV first excited state of {sup 125}Te. We found for the 47{sup +} and 48{sup +} ions, 400 and 670{percent} variations with respect to the neutral-atom half-life (1.49 ns). These unusually large effects are due to the energetic blocking of the K-shell internal conversion as the charge state increases past 47{sup +}. For the 46{sup +}, we suggest a new internal conversion mode without any electron emission into the energy continuum. {copyright} {ital 1997} {ital The American Physical Society}
Published: 1997
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26. Search for new resonant states in10C and11C and their impact on the cosmological lithium problem

Author: Daisuke Suzuki, P. Morfouace, B. Fernández-Domínguez, A. M. Sánchez-Benítez, I. Matea, S. Franchoo, A. Lefebvre-Schuhl, N. de Sereville, J. Kiener, P. Roussel, Marine Vandebrouck, I. Stefan, B. Le Crom, Predrag Ujić, A. Coc, S. P. Fox, J. Mrazek, Alison Laird, C. Hamadache, L. Audouin, S. Ancelin, F. Hammache, G. Mavilla, Anuj Parikh, L. Lefebvre, M. Assié, Fdo Santos, André Palma da Cunha Matta, L. Perrot, Didier Beaumel, and Tatischeff
Subjects: Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, chemistry.chemical_element, 01 natural sciences, chemistry, Big Bang nucleosynthesis, Nucleosynthesis, 0103 physical sciences, Incident energy, Lithium, Atomic physics, 010303 astronomy & astrophysics, Energy (signal processing), Excitation
Abstract: The observed primordial ${}^{7}$Li abundance in metal-poor halo stars is found to be lower than its Big-Bang nucleosynthesis (BBN) calculated value by a factor of approximately three. Some recent works suggested the possibility that this discrepancy originates from missing resonant reactions which would destroy ${}^{7}$Be, parent of ${}^{7}$Li. The most promising candidate resonances which were found include a possibly missed 1${}^{\ensuremath{-}}$ or 2${}^{\ensuremath{-}}$ narrow state around 15 MeV in the compound nucleus ${}^{10}$C formed by ${}^{7}$Be+${}^{3}$He and a state close to 7.8 MeV in the compound nucleus ${}^{11}$C formed by ${}^{7}$Be+${}^{4}$He. In this work, we studied the high excitation energy region of ${}^{10}$C and the low excitation energy region in ${}^{11}$C via the reactions ${}^{10}$B(${}^{3}$He,$t$)${}^{10}$C and ${}^{11}$B(${}^{3}$He,$t$)${}^{11}$C, respectively, at the incident energy of 35 MeV. Our results for ${}^{10}$C do not support ${}^{7}$Be+${}^{3}$He as a possible solution for the ${}^{7}$Li problem. Concerning ${}^{11}$C results, the data show no new resonances in the excitation energy region of interest and this excludes the ${}^{7}$Be+${}^{4}$He reaction channel as an explanation for the ${}^{7}$Li deficit.
Published: 2013
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27. Charge State Blocking ofK-Shell Internal Conversion in125Te

Author: J. Kiener, J. P. Grandin, M. Aiche, C. Grunberg, A. Lefebvre, W. E. Meyerhof, F. Attallah, J. F. Chemin, J. N. Scheurer, G. Bogaert, P. Aguer, and J. P. Thibaud
Subjects: Materials science, 010308 nuclear & particles physics, Blocking (radio), Electron shell, General Physics and Astronomy, Charge (physics), State (functional analysis), 01 natural sciences, Ion, Internal conversion, Excited state, 0103 physical sciences, State dependence, Atomic physics, 010306 general physics
Abstract: We have studied the atomic charge state dependence of the nuclear lifetime of the 35.5-keV first excited state of {sup 125}Te. For the 47{sup +} and 48{sup +} ions, 300% and 640% increases, respectively, of the half-life were found with respect to the neutral-atom value (1.49 ns). These unusually large effects are due to the energetic blocking of {ital K}-shell internal conversion as the charge state increases past 47{sup +}.
Published: 1995
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28. Scientific Analysis within SEPServer – New Perspectives in Solar Energetic Particle Research: The Case Study of the 13 July 2005 Event

Author: Bernd Heber, C. Hamadache, Nicole Vilmer, E. Riihonen, Panagiota Preka-Papadema, Athanasios Papaioannou, Vincent Tatischeff, Kostas Tziotziou, J. Kiener, Yulia Kartavykh, Henry Aurass, Blai Sanahuja, S. Braune, Eino Valtonen, Karl-Ludwig Klein, Olga Malandraki, Alexander Nindos, W. Dröge, A. Kouloumvakos, Neus Agueda, Rami Vainio, R. Rodríguez-Gasén, Democritus University of Thrace (DUTH), National Observatory of Athens, ISARS, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Institut für Experimentelle und Angewandte Physik [Kiel] (IEAP), Christian-Albrechts-Universität zu Kiel (CAU), Dept. Astronomica i Meteorologia, Universitat de Barcelona (UB), Department of Astrophysics, Astronomy and Mechanics [Kapodistrian Univ], National and Kapodistrian University of Athens (NKUA), CSNSM AN, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM)
Subjects: Solar energetic particles, 010504 meteorology & atmospheric sciences, Meteorology, Space weather, Radio signatures, 01 natural sciences, Acceleration, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Instrumentation (computer programming), Aerospace engineering, 010303 astronomy & astrophysics, Monte Carlo simulation, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Physics, Spacecraft, business.industry, Astronomy and Astrophysics, Interplanetary propagation, Space and Planetary Science, Physics::Space Physics, Coronal mass ejections, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, Interplanetary spaceflight, Event (particle physics)
Abstract: Solar energetic particle (SEP) events are a key ingredient of solar-terrestrial physics both for fundamental research and space weather applications. Multi-satellite observations are an important and incompletely exploited tool for studying the acceleration and the coronal and interplanetary propagation of the particles. While STEREO uses for this diagnostic two identical sets of instrumentation, there are many earlier observations carried out with different spacecraft. It is the aim of the SEPServer project to make these data and analysis tools available to a broad user community. The consortium will carry out data-driven analysis and simulation-based data analysis capable of deconvolving the effects of interplanetary transport and solar injection from SEP observations, and will compare the results with the electromagnetic signatures. The tools and results will be provided on the web server of the project in order to facilitate further analysis by the research community. This paper describes the data products and analysis strategies with one specific event, the case study of 13 July 2005. The release time of protons and electrons are derived using data-driven and simulation-based analyses, and compared with hard X-ray and radio signatures. The interconnection of the experimental and the simulation-based results are discussed in detail.
Published: 2012
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29. Spectroscopy of the Unbound Nucleus Na-18

Author: J. Kiener, J. Mrazek, M. Stanoiu, Muriel Fallot, M. Assié, Philip Woods, J. C. Angelique, Predrag Ujić, C. Borcea, L. Achouri, F. de Oliveira Santos, F. de Grancey, D.Y. Pang, I. Stefan, F. Rotaru, A. Lefebvre-Schuhl, Igor T. Čeliković, Thomas Davinson, G. L. Lotay, L. Caceres, C. Ducoin, A. M. Sánchez-Benítez, R. Stanoiu, M. G. Saint-Laurent, K. Subotic, Yu. Sobolev, V. Chudoba, R. Wolski, J. Alcantara-Nunez, L. Perrot, Grand Accélérateur National d'Ions Lourds (GANIL), 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), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Physique théorique, 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)-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), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), CSNSM AN, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), SPIRAL, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Normandie Université (NU)-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)-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)-Centre National de la Recherche Scientifique (CNRS), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM)
Subjects: Physics, Elastic scattering, Nuclear and High Energy Physics, Isotope, 010308 nuclear & particles physics, Scattering, General Physics and Astronomy, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Isotopes of sodium, 01 natural sciences, medicine.anatomical_structure, Isotopes of neon, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, Excited state, 0103 physical sciences, medicine, Atomic physics, 010306 general physics, Spectroscopy, Nucleus
Abstract: The unbound nucleus 18 Na , the intermediate nucleus in the two-proton radioactivity of 19 Mg , is studied through the resonant elastic scattering 17 Ne ( p ,17 Ne ) p . The spectroscopic information obtained in this experiment is discussed and put in perspective with previous measurements and the structure of the mirror nucleus 18 N .
Published: 2011
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30. High-energy breakup ofLi6as a tool to study the Big Bang nucleosynthesis reactionH2(α,γ)Li6

Author: F. Schümann, F. Hammache, Andreas Wagner, J. Kiener, Naohito Iwasa, Kilian Eberhard Schwarz, D. Galaviz, Peter Mohr, Stefan Typel, B. Kohlmeyer, M. Caamaño, Vincent Tatischeff, P. Senger, F. Uhlig, O. Sorlin, W. Walus, Michael Heil, D. Cortina, E. Schwab, K. Sümmerer, F. Attallah, Elisabeth Vangioni, J. P. Thibaud, Hans Geissel, Margareta Hellström, A. Coc, and P. Koczon
Subjects: Physics, Nuclear reaction, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Scattering, Isotopes of lithium, Coulomb excitation, 01 natural sciences, Nuclear physics, Big Bang nucleosynthesis, Nucleosynthesis, 0103 physical sciences, Coulomb, 010306 general physics, Radioactive decay
Abstract: The recently claimed observations of non-negligible amounts of $^{6}\mathrm{Li}$ in old halo stars have renewed interest in the Big Bang nucleosynthesis (BBN) of $^{6}\mathrm{Li}$. One important ingredient in the predicted BBN abundance of $^{6}\mathrm{Li}$ is the low-energy $^{2}\mathrm{H}$($\ensuremath{\alpha}$,$\ensuremath{\gamma}$)$^{6}\mathrm{Li}$ cross section. Up to now, the only available experimental result for this cross section showed an almost constant astrophysical $S$ factor below $400$ keV, contrary to theoretical expectations. We report on a new measurement of the $^{2}\mathrm{H}$($\ensuremath{\alpha}$,$\ensuremath{\gamma}$)$^{6}\mathrm{Li}$ reaction using the breakup of $^{6}\mathrm{Li}$ at 150 $A $ MeV. Even though we cannot separate experimentally the Coulomb contribution from the nuclear one, we find clear evidence for Coulomb-nuclear interference by analyzing the scattering angular distributions. This is in line with our theoretical description, which indicates a drop of the ${S}_{24}$ factor at low energies as predicted also by most other models. Consequently, we find even lower upper limits for the calculated primordial $^{6}\mathrm{Li}$ abundance than before.
Published: 2010
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31. Development of an Anger camera in Lanthanum Bromide for gamma-ray space astronomy in the MeV range

Author: A. T. Astorino, D. Linget, S. Blin, D. C. Bardalez Gagliuffi, N. Karkour, C. Hamadache, V. Tatischeff, J. Kiener, G. Sedes, P. Barrillon, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de l'Accélérateur Linéaire (LAL), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Photomultiplier, Scintillation, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Photon, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Calorimeter (particle physics), 010308 nuclear & particles physics, business.industry, Physics::Instrumentation and Detectors, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Detector, Gamma ray, Scintillator, 01 natural sciences, Anger Camera, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Optics, 0103 physical sciences, [SPI.NANO]Engineering Sciences [physics]/Micro and nanotechnologies/Microelectronics, 010306 general physics, business
Abstract: International audience; Lanthanum bromide is a very promising scintillator material for the next generation of g-ray telescopes. We present in this paper first g-ray imaging results obtained by coupling a LaBr3 crystal with a position-sensitive 8×8 multianode photomultiplier tube to form a simple Anger camera module. The readout of the 64 signals is carried out with the most recent evolution of the MultiAnode ReadOut Chip (MAROC) which was initially designed for the luminometer of the ATLAS detector. Measured charge distributions are compared with detailed GEANT4 simulations that include the tracking of the optical photons produced in the scintillation crystal. The depth of interaction (d.o.i.) of 662-keV g-rays inside the crystal is derived from the charge distributions using an artificial neural network. We obtain for an irradiation at detector centre a mean standard deviation of the d.o.i. of 1.69 mm. Such a position-sensitive g-ray detector can form an innovative building block for a future space calorimeter
Published: 2010

32. Study of [sup 60]Fe(n,γ)[sup 61]Fe reaction of astrophysical interest via d([sup 60]Fe,pγ) indirect reaction

Author: S. Giron, F. Hammache, N. de Séréville, D. Beaumel, J. Burgunder, L. Caceres, E. Clement, G. Duchene, F. Flavigny, G. De France, S. Franchoo, B. Fernandez, D. Galaviz-Redondo, L. Gasques, J. Gibelin, A. Gillibert, S. Grevy, J. Guillot, M. Heil, J. Kiener, V. Lapoux, F. Maréchal, A. Matta, Y. Matea, M. Moukaddam, L. Nalpas, A. Obertelli, L. Perrot, R. Raabe, J. A. Scarpaci, O. Sorlin, I. Stefan, C. Stoedel, M. Takechi, J. C. Thomas, Y. Togano, Claudi Spitaleri, Claus Rolfs, and Rosario G. Pizzone
Subjects: Nuclear reaction, Physics, Angular momentum, 010308 nuclear & particles physics, Context (language use), 7. Clean energy, 01 natural sciences, Nuclear physics, Supernova, Nucleosynthesis, Excited state, 0103 physical sciences, Atomic physics, Radioactive decay, Excitation
Abstract: INTEGRAL and RHESSI spacecrafts recently detected the 1.173 and 1.333 MeV γ‐ray lines coming from the 60Fe—60Co—60Ni radioactive decay chain. The long lived isotope 60Fe (T1/2 = 1.5 106y) is believed to be primarily produced in core‐collapse supernovae. However the interpretation of the observations is difficult because of the large uncertainties concerning 59Fe(n,γ)60Fe and 60Fe(n,γ)61Fe cross sections, involved in 60Fe nucleosynthesis.The direct component of the 60Fe(n,γ)61Fe reaction was studied indirectly via the d(60Fe,pγ)61Fe transfer reaction. The experiment performed in GANIL in spring 2009 will allow to determine the excitation energies of the populated excited states of 61Fe and for the first time their spectroscopic factors as well as their transfer angular momentum.I will first give an overview of the astrophysical context, then I will describe the experimental setup and finally present some preliminary results of the ongoing analysis.
Published: 2010
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33. Gamma-ray burst investigation via polarimetry and spectroscopy (GRIPS)

Author: R. Bellazini, Andreas Zoglauer, M. I. Panasyuk, René Hudec, L. G. Balasz, R. Marcinkowski, V. M. Lipunov, Mark Pearce, Felix Ryde, Andrei M. Bykov, Elena Pian, D. Hartmann, Guido Barbiellini, Andrew W. Strong, A. Majczyna, Zsolt Bagoly, Sandra Savaglio, J. Kiener, István T. Horváth, B. K. Lubsandorgiev, R. V. Poleschuk, Sheila McBreen, Vincent Tatischeff, Karl Mannheim, G. Wrochna, A. M. Chernenko, Martino Marisaldi, G. Bisnovaty-Kogan, A. Pollo, Attila Mészáros, A. F. Iyudin, A. G. Zabrodskij, J. Uvarov, S. Larsson, W. Dröge, S. E. Boggs, A. M. Cherepashuk, Gottfried Kanbach, Andreas von Kienlin, Norbert Langer, S. I. Svertilov, Dmitry Bisikalo, L. M. Zeleny, G. Dicocco, Jochen Greiner, Werner Collmar, Roland Diehl, B. McBreen, Lorraine Hanlon, Claudio Labanti, Cornelia B. Wunderer, Boris Shustov, E. Orlando, Marco Ajello, M. Gierlik, D. A. Varshalovich, Alexei Pozanenko, G. G. Lichti, L. B. Bezrukov, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Greiner, J., Iyudin, A., Kanbach, G., Zoglauer, A., Diehl, R., Ryde, F., Hartmann, D., v. Kienlin, A., Mcbreen, S., Ajello, M., Bagoly, Z., Balasz, L. G., Barbiellini, G., Bellazini, R., Bezrukov, L., Bisikalo, D. V., Bisnovaty-Kogan, G., Boggs, S., Bykov, A., Cherepashuk, A. M., Chernenko, A., Collmar, W., Dicocco, G., Droege, W., Gierlik, M., Hanlon, L., Horvath, I., Hudec, R., Kiener, J., Labanti, C., Langer, N., Larsson, S., Lichti, G., Lipunov, V. M., Lubsandorgiev, B. K., Majczyna, A., Mannheim, K., Marcinkowski, R., Marisaldi, M., Mcbreen, B., Meszaros, A., Orlando, E, Panasyuk, M. I., Pearce, M., Pian, E., Poleschuk, R. V., Pollo, A., Pozanenko, A., Savaglio, S., Shustov, B., Strong, A., Svertilov, S., Tatischeff, V., Uvarov, J., Varshalovich, D. A., Wunderer, C. B., Wrochna, G., Zabrodskij, A. G., and Zeleny, L. M.
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, education, Early universe, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Polarimetry, Astrophysics, Compton and pair creation telescope, 7. Clean energy, 01 natural sciences, Primary (astronomy), Nucleosynthesis, Observatory, 0103 physical sciences, Nuclear astrophysics, Hardware_ARITHMETICANDLOGICSTRUCTURES, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, health care economics and organizations, ComputingMethodologies_COMPUTERGRAPHICS, media_common, Physics, 010308 nuclear & particles physics, gamma-ray bursts, Astrophysics::Instrumentation and Methods for Astrophysics, nucleosynthesis, Astronomy, Astronomy and Astrophysics, social sciences, early universe, Universe, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 95.55.Ka * 98.70.Rz * 26.30.-k, Space and Planetary Science, Compton and Pair creation telescope, Gamma-ray bursts, Gamma-ray burst
Abstract: The primary scientific goal of the GRIPS mission is to revolutionize our understanding of the early universe using gamma-ray bursts. We propose a new generation gamma-ray observatory capable of unprecedented spectroscopy over a wide range of gamma-ray energies (200 keV-50 MeV) and of polarimetry (200-1000 keV). The gamma-ray sensitivity to nuclear absorption features enables the measurement of column densities as high as 10(28)cm (-aEuro parts per thousand 2). Secondary goals achievable by this mission include direct measurements of all types of supernova interiors through gamma-rays from radioactive decays, nuclear astrophysics with massive stars and novae, and studies of particle acceleration near compact stars, interstellar shocks, and clusters of galaxies.
Published: 2009
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34. Indirect study of theC13(α,n)O16reaction via theC13(Li7,t)O17transfer reaction

Author: Pierre Descouvemont, V. Tatischeff, P. Roussel, S. Fortier, D. Beaumel, L. Audouin, M. Vilmay, J. Kiener, M. G. Pellegriti, F. Hammache, L. Gaudefroy, M. Stanoiu, and A. Lefebvre-Schuhl
Subjects: Physics, Nuclear reaction, Oxygen-17, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Neutron emission, Isotopes of lithium, Alpha particle, 01 natural sciences, 7. Clean energy, Reaction rate, 0103 physical sciences, Atomic physics, Nuclear Experiment, 010306 general physics, s-process, Oxygen-16
Abstract: The $^{13}\mathrm{C}$($\ensuremath{\alpha},n$)$^{16}\mathrm{O}$ reaction is considered the main neutron source for the s process in low mass asymptotic giant branch (AGB) stars. In the Gamow peak, the cross section sensitively depends on the $1/{2}^{+}$ subthreshold state of $^{17}\mathrm{O}$ (${E}_{x}=6.356$ MeV). In this work, we determined the astrophysical $S$ factor through an evaluation of the \ensuremath{\alpha} spectroscopic factor and the corresponding asymptotic normalization factor (ANC) of the 6.356 MeV state using the transfer reaction $^{13}\mathrm{C}$($^{7}\mathrm{Li}$,$t$)$^{17}\mathrm{O}$ at two different incident energies. Our result confirms that the contribution of the $1/{2}^{+}$ state is dominant at astrophysical energies. Our reaction rate at $T=0.09$ GK is slightly lower than the value adopted in the Nuclear Astrophysics Compilation of REaction rates (NACRE), but two times larger than the one obtained in a recent ANC measurement.
Published: 2008
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35. Quasi-bound low energy tail of resonance

Author: I. Stefan, F. de Oliveira Santos, M. G. Pellegriti, M. Angélique, J. C. Dalouzy, F. de Grancey, M. Fadil, S. Grévy, M. Lenhardt, M. Lewitowicz, A. Navin, L. Perrot, M. G. Saint Laurent, I. Ray, O. Sorlin, C. Stodel, J. C. Thomas, G. Dumitru, A. Buta, R. Borcea, F. Negoita, D. Pantelica, J. C. Angélique, E. Berthoumieux, A. Coc, J. Kiener, A. Lefebvre-Schuhl, V. Tatischeff, J. M. Daugas, O. Roig, T. Davinson, M. Stanoiu, Lídia S. Ferreira, Paramasivan Arumugan, Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Horia Hulubei National Institute of Physics and Nuclear Engineering (NIPNE), IFIN-HH, Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), 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), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Physics, Mass number, Proton, 010308 nuclear & particles physics, Proton decay, Resonance, Coulomb barrier, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Charged particle, 0103 physical sciences, Atomic physics, 010306 general physics, Ground state, Oxygen-16
Abstract: The ground state of particle‐unbound nuclei is observed as a resonance. According to the Heisenberg's uncertainty principle, the shorter is the lifetime of the state the broader is the resonance. The Breit‐Wigner formalism describes perfectly the shape of the resonance when energy‐dependent partial‐widths are used. In the low energy tail of a ground state resonance near the particle‐emission threshold, the partial‐width for the emission of a charged particle through the Coulomb barrier is drastically reduced. The fact that the proton decay is strongly hindered seems to be equivalent to the assertion that the decay of the proton is strongly delayed. In this interpretation and as an example, possible consequences are discussed in astrophysical context. Two reactions 15O(p,β+)16O and 15O(p,γ)(β+)16O are proposed as new pathways to bypass the 15O waiting point. Cross‐sections were calculated after precise measurements of energies and widths of the proton‐unbound 16F low lying states, obtained using the H(15O,...
Published: 2007
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36. Experimental determination of theO17(p,α)N14andO17(p,γ)F18reaction rates

Author: J. Kiener, S. Barhoumi, A. Lefebvre-Schuhl, N. de Sereville, S. Ouichaoui, Vincent Tatischeff, F. Garrido, Jordi José, Margarita Hernanz, J. P. Thibaud, A. Coc, A. Chafa, and P. Aguer
Subjects: Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Resonance, Atmospheric temperature range, 7. Clean energy, 01 natural sciences, Omega, Reaction rate, Chemical kinetics, Crystallography, 13. Climate action, Nucleosynthesis, 0103 physical sciences, Activation method, 010306 general physics, Energy (signal processing)
Abstract: The {sup 17}O(p,{alpha}){sup 14}N and {sup 17}O(p,{gamma}){sup 18}F reactions are of major importance to hydrogen-burning nucleosynthesis in a number of different stellar sites. In particular, {sup 17}O and {sup 18}F nucleosynthesis in classical novae is strongly dependent on the thermonuclear rates of these two reactions. The previously estimated rate for {sup 17}O(p,{alpha}){sup 14}N carries very large uncertainties in the temperature range of classical novae (T=0.01-0.4 GK), whereas a recent measurement has reduced the uncertainty of the {sup 17}O(p,{gamma}){sup 18}F rate. We report on the observation of a previously undiscovered resonance at E{sub c.m.}=183.3 keV in the {sup 17}O(p,{alpha}){sup 14}N reaction, with a measured resonance strength {omega}{gamma}{sub p{alpha}}=(1.6{+-}0.2)x10{sup -3} eV. We studied in the same experiment the {sup 17}O(p,{gamma}){sup 18}F reaction by an activation method, and the resonance strength was found to amount to {omega}{gamma}{sub p{gamma}}=(2.2{+-}0.4)x10{sup -6} eV. The excitation energy of the corresponding level in {sup 18}F was determined to be 5789.8{+-}0.3 keV in a Doppler shift attenuation method measurement, which yielded a value of {tau}
Published: 2007
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37. Measurement and DWBA analysis of the $^{12}C(^6Li, d)^{16}O \alpha$-transfer reaction cross sections at 48.2 MeV. R-matrix analysis of $^{12}C(\alpha,\gamma)^{16}$O direct capture reaction data

Author: A. Boughrara, S.K. Mehdi, J. P. Thibaud, A. Trabelsi, J. Vernotte, J. Kiener, H. Beaumevieille, J.M. Maison, S. Ouichaoui, L. H. Rosier, S. Fortier, A. Belhout, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Nuclear reaction, Nuclear and High Energy Physics, 16O, Deduced S-factor, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], E (c.m.), 01 natural sciences, level parameters using DWBA analysis, deduced, 0103 physical sciences, A value, Analysed existing data using R-matrix formalism, E=48.2 MeV, 12C(α, 010306 general physics, R-matrix, Physics, Range (particle radiation), 5 MeV, 010308 nuclear & particles physics, Resolution (electron density), γ)16O, State (functional analysis), Radius, Measured differential cross sections and angular distributions, 25.70.Hi, 24.10.Eq, 27.20.+n, 26.20.+f, Deduced spectroscopic factors, Atomic physics, 12C(6Li, Excitation, d)16O
Abstract: The angular distributions for low lying states of 16O produced in the 12C(6Li, d)16O α-transfer reaction at E Li 6 ( lab ) = 48.2 MeV have been measured using a high energy resolution position sensitive detection system. The measured cross section data have been analyzed by the FRDWBA theory with a particular emphasis put on the states of astrophysical interest mainly the 1 − (7.12 MeV) state. Extracted values of nuclear level parameters (excitation energy, E x , line width, Γ c . m . , α-spectroscopic factor, S α , and reduced α-width, γ α 2 or θ α 2 ) are reported and discussed in comparison to previous ones. The used binding potential corresponds to a long nuclear interaction range (up to a channel radius a = 7.7 fm ), suggesting that the channel radius a = 6.5 fm is likely suitable for the calculations of reduced α-widths near the nuclear surface. However, given that previous DWBA results are available for comparison only near the channel radius a = 5.5 fm , calculations have been carried out here for both three preceding a values. Formal values, 0.0036 ⩽ θ α 2 ( 7.12 ) ⩽ 0.152 and 0.019 ⩽ θ α 2 ( 6.92 ) ⩽ 0.096 of the reduced α-widths ( a = 6.5 fm ) of the 1 − (7.12 MeV) and 2 + (6.92 MeV) states have thus been derived. Furthermore, the R-matrix analysis of various data sets of importance to the 12C( α , γ )16O direct capture reaction has been carried out, leading to the range of values for the 1 − (7.12 MeV) state, 0.0096 ⩽ θ α 2 ( 7.12 ) ⩽ 0.0166 , which is consistent with the preceding DWBA interval, and to a result for the E1 component of the reaction astrophysical factor, S E 1 ( 0.3 ) = 80.6 −16 +17 keV b , very consistent with most constrained values previously reported in the literature.
Published: 2007
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38. New pathway to bypass the $^{15}$O waiting point

Author: I. Stefan, F. de Oliveira Santos, M. G. Pellegriti, M. Angélique, J. C. Dalouzy, F. de Grancey, M. Fadil, S. Grévy, M. Lenhardt, M. Lewitowicz, A. Navin, L. Perrot, M. G. Saint Laurent, I. Ray, O. Sorlin, C. Stodel, J. C. Thomas, G. Dumitru, A. Buta, R. Borcea, F. Negoita, D. Pantelica, J. C. Angélique, E. Berthoumieux, A. Coc, J. Kiener, A. Lefebvre-Schuhl, V. Tatischeff, J. M. Daugas, O. Roig, T. Davinson, M. Stanoiu, Grand Accélérateur National d'Ions Lourds (GANIL), 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), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), A. Arnould, M. Lewitowicz, H. Emling, H. Akimune, M. Ohta, H. Utsunomiya, T. Wada, T. Yamagata, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Particle physics, 010308 nuclear & particles physics, Gamma ray, FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Resonance (particle physics), Low energy, 0103 physical sciences, Point (geometry), Nuclear Experiment (nucl-ex), 010306 general physics, Ground state, Nuclear Experiment
Abstract: We propose the sequential reaction process $^{15}$O($p$,$\gamma)(\beta^{+}$)$^{16}$O as a new pathway to bypass of the $^{15}$O waiting point. This exotic reaction is found to have a surprisingly high cross section, approximately 10$^{10}$ times higher than the $^{15}$O($p$,$\beta^{+}$)$^{16}$O. These cross sections were calculated after precise measurements of energies and widths of the proton-unbound $^{16}$F low lying states, obtained using the H($^{15}$O,p)$^{15}$O reaction. The large $(p,\gamma)(\beta^{+})$ cross section can be understood to arise from the more efficient feeding of the low energy wing of the ground state resonance by the gamma decay. The implications of the new reaction in novae explosions and X-ray bursts are discussed., Comment: submitted
Published: 2006
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39. New low-energy measurement of the 18F(p,α)15O reaction

Author: Enrique Casarejos, Pierre Descouvemont, P. Mumby-Croft, N. de Sereville, Donald Robertson, Alain Coc, Pierre Leleux, S. P. Fox, Alison Laird, F. Hammache, Vincent Tatischeff, N. L. Achouri, A. Lefebvre, N. A. Orr, Thomas Davinson, J. Kiener, K. Vaughan, Carmen Angulo, P. Figuera, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and Institut de Physique Nucléaire d'Orsay (IPNO)
Subjects: Physics, 010308 nuclear & particles physics, Extrapolation, General Physics and Astronomy, Nova (laser), [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Interference (wave propagation), 01 natural sciences, Intensity (physics), Nuclear physics, Cross section (physics), 0103 physical sciences, General Materials Science, Satellite, Physical and Theoretical Chemistry, Atomic physics, 010306 general physics, computer, Beam (structure), Leda, computer.programming_language
Abstract: The F-18, produced during nova explosions, is the main responsible for the 511 keV gamma-ray emitted during the outburst that could be detected with satellite missions or future gamma-ray telescopes. In spite of many experimental efforts, the amount of F-18 synthesized still suffers from large uncertainties concerning mainly the F-18(p, alpha)O-15 reaction. We report here on a new direct measurement of the F-18(p, alpha)O-15 cross section recently carried out at the RIB facility at Louvain-la-Neuve. Cross section data down to a center-of-mass energy of 400 keV have been obtained using an isobarically pure F-18 beam ( averaged intensity of the order of 10(6) pps) and a thin polyethylene target. The reaction products were detected using the multi-strip detector array LEDA. The cross section data are analysed in the framework of the R-matrix model. Our main aim is to determine the interference sign between three 3/2(+) resonances above threshold that can significantly affect the extrapolation of the F-18(p, alpha)O-15 cross section to the energies relevant for novae, and thus, the modeling of nova explosions.
Published: 2006
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40. E1andE2Sfactors ofC12(α,γ0)O16fromγ-ray angular distributions with a 4π-detector array

Author: E. Galanopoulos, A. Korichi, J.L. Weil, R. Meunier, A. Coc, D. Malcherek, T. Paradellis, Neil Rowley, C. Boukari-Pelissie, D. Ledu, J.J. Correia, Marlete Assunção, A. Lopez-Martens, J. Kiener, Vincent Tatischeff, C. Grama, R. Kunz, F. Hammache, A. Lefebvre-Schuhl, G. Staudt, F. Haas, F. Hannachi, J. W. Hammer, Suzana Szilner, C. Beck, S. Courtin, Marc Rousseau, J. P. Thibaud, F. Fleurot, M. Fey, and Sotirios Harissopulos
Subjects: Physics, Nuclear and High Energy Physics, Range (particle radiation), 010308 nuclear & particles physics, Scattering, Gamma ray, Carbon-12, Alpha particle, 7. Clean energy, 01 natural sciences, Bismuth germanate, Nuclear physics, chemistry.chemical_compound, chemistry, 0103 physical sciences, Nuclear astrophysics, Atomic physics, 010306 general physics, Ground state
Abstract: A new experiment to determine the thermonuclear cross section of the C-12(alpha,gamma)O-16 reaction has been performed in regular kinematics using an intense alpha-particle beam of up to 340 mu A from the Stuttgart DYNAMITRON. For the first time, a 4 pi-germanium-detector setup has been used to measure the angular distribution of the gamma rays at all angles simultaneously. It consisted of an array of nine EUROGAM high-purity Ge detectors in close geometry, actively shielded individually with bismuth germanate crystals. The C-12 targets were isotopically enriched by magnetic separation during implantation. The depth profiles of the implanted carbon in the C-12 targets were determined by Rutherford backscattering for purposes of cross-section normalization and absolute determination of the E1 and E2 S factors. Angular distributions of the gamma decay to the O-16 ground state were measured in the energy range E-c.m.=1.30-2.78 MeV and in the angular range (lab.) 30 degrees-130 degrees. From these distributions, astrophysical E1 and E2 S-factor functions vs energy were calculated, both of which are indispensable to the modeling of this reaction and the extrapolation toward lower energies. The separation of the E1 and E2 capture channels was done both by taking the phase value phi(12) as a free parameter and by fixing it using the results of elastic alpha-particle scattering on C-12 in the same energy range.
Published: 2006
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41. High resolution gamma ray spectroscopy of flares on the east and west limbs of the Sun

Author: Michael J. Harris, Vincent Tatischeff, G. Weidenspointner, M. Gros, J. Kiener, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Centre d'étude spatiale des rayonnements (CESR), 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)-Centre National de la Recherche Scientifique (CNRS)-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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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, 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), and 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)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Recoil, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Gamma spectroscopy, 010303 astronomy & astrophysics, Line (formation), Physics, Solar flare, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Magnetic field, Space and Planetary Science, Physics::Space Physics, symbols, Doppler effect, Flare
Abstract: A new generation of Ge-based high-resolution gamma-ray spectrometers has allowed accurate measurements to be made of the profiles, widths and energies of the gamma-ray lines emitted in the impulsive phases of solar flares. Here we present measurements in two flares of the energies of the de-excitation lines of 12C and 16O at 4.4 and 6.1 MeV respectively by the Ge spectrometer SPI on board INTEGRAL, from which Doppler shifts are derived and compared with those expected from the recoil of 12C and 16O nuclei which were excited by the impacts of flare-accelerated ions. An anomalous Doppler measurement (in terms of recoil theory) has been reported by the Ge spectrometer RHESSI in a flare near the east limb, and explained by a tilt of the magnetic field lines at the footpoint of a magnetic loop away from the vertical, and towards the observer. This might be interpreted to imply a significant difference between the Doppler shifts on the east and west limbs, if it is a general phenomenon. SPI observed both east and west limb flares and found no significant difference in Doppler shifts. We also measured the shapes and fluences of these lines, and their fluence ratio to the 2.2 MeV line from the capture of flare-generated neutrons. Analyses of both quantities using thick-target models parametrized by solar physical and geometric quantities suggest that the two flares studied here also have magnetic fields tilted towards the observer, though the significance of the measurements is not high., 9 pp., 7 figs., accepted by A&A
Published: 2006
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42. Comparison of low-energy resonances in15N(α,γ)19F and15O(α,γ)19Ne and related uncertainties

Author: J. Kiener, Peter J. Mohr, G. Rotbard, P. Aguer, G. Staudt, Vincent Tatischeff, V. Kölle, J. Vernotte, J. P. Thibaud, G. Bogaert, F. de Oliveira, S. Wilmes, S. Fortier, A. Coc, A. Lefebvre, L. H. Rosier, and J.M. Maison
Subjects: Physics, Nuclear and High Energy Physics, Theoretical physics, Crystallography, Low energy, 010308 nuclear & particles physics, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, 0103 physical sciences, Resonance, Mirror nuclei, 010306 general physics, 01 natural sciences
Abstract: A disagreement between two determinations of {Gamma}{sub {alpha}} of the astrophysically relevant level at E{sub x}=4.378 MeV in {sup 19}F has been stated in two recent papers by Wilmes {ital et al.} and de Oliveira {ital et al.} In this work the uncertainties of both papers are discussed in detail, and we adopt the value {Gamma}{sub {alpha}} = (1.5{sub {minus}0.8}{sup +1.5}){times}10{sup {minus}9} eV for the 4.378 MeV state. In addition, the validity and the uncertainties of the usual approximations for mirror nuclei {Gamma}{sub {gamma}}({sup 19}F){approx}{Gamma}{sub {gamma}}({sup 19}Ne), {theta}{sub {alpha}}{sup 2}({sup 19}F){approx}{theta}{sub {alpha}}{sup 2}({sup 19}Ne) are discussed, together with the resulting uncertainties on the resonance strengths in {sup 19}Ne and on the {sup 15}O({alpha},{gamma}){sup 19}Ne rate. {copyright} {ital 1997} {ital The American Physical Society}
Published: 1997
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43. Hydrogen Burning ofO17in Classical Novae

Author: A. Chafa, N. de Séréville, Vincent Tatischeff, F. Garrido, A. Lefebvre-Schuhl, P. Aguer, S. Barhoumi, S. Ouichaoui, J. Kiener, A. Coc, Margarita Hernanz, Jordi José, J. P. Thibaud, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and UCL
Subjects: Hydrogen, nuclear energy level transitions, FOS: Physical sciences, General Physics and Astronomy, Alpha (ethology), chemistry.chemical_element, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Astrophysics, proton radiative capture, 7. Clean energy, 01 natural sciences, Omega, alpha particle-nucleus reactions, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear physics, Nucleosynthesis, proton-nucleus reactions, 0103 physical sciences, Nuclear Experiment (nucl-ex), Nuclear Experiment, 010303 astronomy & astrophysics, novae, Physics, Oxygen-17, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), nucleosynthesis, Resonance, Alpha particle, 26.30.+k, 25.40.Lw, 25.40.Ny, 27.20.+n, chemistry, Excitation
Abstract: We report on the observation of a previously unknown resonance at E=194.1+/-0.6 keV (lab) in the 17-O(p,alpha)14-N reaction, with a measured resonance strength omega_gamma(p,alpha)=1.6+/-0.2 meV. We studied in the same experiment the 17-O(p,gamma)18-F reaction by an activation method and the resonance-strength ratio was found to be omega_gamma(p,alpha)/omega_gamma(p,gamma)=470+/-50. The corresponding excitation energy in the 18-F compound nucleus was determined to be 5789.8+/-0.3 keV by gamma-ray measurements using the 14-N(alpha,gamma)18-F reaction. These new resonance properties have important consequences for 17-O nucleosynthesis and gamma-ray astronomy of classical novae., 4 pages, 4 figures. Accepted for publication in Physical Review Letters
Published: 2005
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44. E1 and E2 capture cross section and astrophysical reaction rate of the key reaction $^{12}C$($\alpha$,$\gamma$)$^{16}O$

Author: D. Le Du, M. Rousseau, J Kiener, A Coc, J.L. Weil, E. Galanopoulos, R. Meunier, F. Fleurot, Neil Rowley, E Krmpotic, C. Grama, D. Malcherek, M. Fey, G. Staudt, Tatischeff, C. Beck, J. W. Hammer, A Korichi, R. Kunz, M Assuncao, F Hammache, F Haas, J.J. Correia, Sotirios Harissopulos, S Courtin, Suzana Szilner, A. Lopez-Martens, P. Papka, T. Paradellis, C. Boukari-Pelissie, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Nuclear physics, Reaction rate, Nuclear and High Energy Physics, Cross section (physics), Nucleosynthesis, 0103 physical sciences, Key (cryptography), Alpha (navigation), [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 010306 general physics, 010303 astronomy & astrophysics, 01 natural sciences
Published: 2004
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45. Gamma-ray lines from cosmic-ray interactions with interstellar dust grains

Author: J. Kiener, V. Tatischeff, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics, 01 natural sciences, Galaxy, Interstellar medium, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Excited state, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation), Cosmic dust
Abstract: As pointed out by Lingenfelter and Ramaty (1977), the shapes of some gamma-ray lines produced by cosmic-ray interactions with the interstellar medium potentially contain valuable information on the physical properties of dust grains, including their compositions and size distributions. The most promising of such lines are at 847, 1369, 1779 and 6129 keV, from 56-Fe*, 24-Mg*, 28-Si* and 16-O*, respectively. We performed detailed calculations of their profiles using, in particular, available laboratory measurements combined with optical model calculations to evaluate the energy distributions of the recoiling excited nuclei. We show that the line shapes are mainly sensitive to relatively large interstellar grains, with radii greater than 0.25 microns. Line fluxes from the inner Galaxy are then predicted., 7 pages, 4 figures, to be published in New Astronomy Reviews (proceedings of the Workshop "Astronomy with Radioactivities IV and Filling the Sensitivity Gap in MeV Astronomy", Seeon, Germany, May 26-30, 2003)
Published: 2003
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46. Cross sections relevant toγ-ray line emission in solar flares:3He-induced reactions on16Onuclei

Author: J. Kiener, Vincent Tatischeff, J. A. Scarpaci, F. Hammache, J. P. Thibaud, Ch. Bourgeois, Josette Duprat, Cécile Engrand, M. G. Porquet, A. Coc, Marlete Assunção, Marin Chabot, A. Lefebvre, N. de Sereville, and M. Gounelle
Subjects: Physics, Nuclear and High Energy Physics, Solar flare, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, 01 natural sciences, Nuclear physics, 0103 physical sciences, Electromagnetic shielding, Electronic anticoincidence, Atomic physics, Nuclear Experiment, 010303 astronomy & astrophysics, Excitation, Line (formation)
Abstract: Gamma-ray production cross sections have been measured for gamma-ray lines copiously emitted in the $^3$He bombardment of $^{16}$O nuclei: the 937, 1042 and 1081 keV lines of $^{18}$F and the 1887 keV line of $^{18}$Ne. Four Ge detectors with BGO shielding for Compton suppression were used to measure the angular distributions of the gamma-rays. The excitation functions have been obtained for $^3$He bombarding energies from 3.7 to 36 MeV. Total cross sections are tabulated for calculations relevant to gamma-ray astronomy. The importance of these lines as diagnosis for the presence and properties of accelerated $^3$He in solar flares is discussed in light of the measured cross sections.
Published: 2003
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47. 2H(18F,pα)15Nreaction applied to nova γ-ray emission

Author: Marlete Assunção, N. A. Smirnova, Marc Loiselet, F. de Oliveira Santos, P. Figuera, N. de Sereville, Alain Ninane, J. Kiener, Guido Ryckewaert, Manoel Couder, B. Bouzid, A. Coc, Michel Gaelens, A. Lefebvre, Pierre Leleux, C. Angulo, J. P. Thibaud, P. Demaret, S. Ouichaoui, Daniel Labar, S. Fortier, S. Cherubini, Vincent Tatischeff, F. Hammache, and Didier Beaumel
Subjects: Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, 0103 physical sciences, Astrophysics, Nova (laser), 010306 general physics, 01 natural sciences
Published: 2003
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48. INTEGRAL/SPI ground calibration

Author: J. Kiener, Steven J. Sturner, P. von Ballmoos, V. Schönfelder, Jürgen Knödlseder, S. Crespin, Bonnard J. Teegarden, David Attié, Georg Weidenspointner, Pierre Leleux, Marie-Geneviève Porquet, G. Vedrenne, Bertrand Cordier, V. Tatischeff, Chris Shrader, F. Sanchez, A. von Kienlin, Ph. Paul, C. B. Wunderer, Philippe Laurent, M. Gros, Andrew W. Strong, Jean-Pierre Roques, P. Jean, G. Tauzin, Robert Georgii, S. Joly, Laurent Bouchet, P. Mandrou, G. G. Lichti, Y. André, Gerald K. Skinner, S. Schanne, 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), Centre d'étude spatiale des rayonnements (CESR), 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)-Centre National de la Recherche Scientifique (CNRS)-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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), INTEGRAL, 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, 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-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Point source, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Instrumentation, Detectors, Spectrographs, Space vehicles, Gamma rays, Observations, Astrophysics, UNESCO::ASTRONOMÍA Y ASTROFÍSICA, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, 0103 physical sciences, Calibration, Source separation, Angular resolution, Spectral resolution, space vehicles: instruments, 010303 astronomy & astrophysics, ASTRONOMÍA Y ASTROFÍSICA::Astronomía óptica [UNESCO], instrumentation: spectrographs, Physics, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, instrumentation: detectors, UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Astronomía óptica, Antenna aperture, Astrophysics (astro-ph), Astronomy and Astrophysics, Optical axis, Space and Planetary Science, business, ASTRONOMÍA Y ASTROFÍSICA [UNESCO], gamma rays: observations
Abstract: Three calibration campaigns of the spectrometer SPI have been performed before launch in order to determine the instrument characteristics, such as the effective detection area, the spectral resolution and the angular resolution. Absolute determination of the effective area has been obtained from simulations and measurements. At 1 MeV, the effective area is 65 cm^2 for a point source on the optical axis, the spectral resolution ~2.3 keV. The angular resolution is better than 2.5 deg and the source separation capability about 1 deg. Some temperature dependant parameters will require permanent in-flight calibration., Comment: 9 pages, 12 figures, 2 tables. Accepted for publication in A&AL (INTEGRAL Special issue)
Published: 2003
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49. Calibration of the spectrometer aboard the INTEGRAL satellite

Author: Roland Diehl, Stéphane Schanne, Gerald K. Skinner, David Attié, R. Carli, G. Vedrenne, J. P. Roques, Filomeno Sanchez, M. Gros, Andrew W. Strong, Philippe Laurent, Bonnard J. Teegarden, G. G. Lichti, P. Paul, Bertrand Cordier, Vincent Tatischeff, Chris Shrader, Steven J. Sturner, J. A. Paul, Peter von Ballmoos, P. H. Connell, P. Jean, Cornelia B. Wunderer, L. Bouchet, J. Kiener, V. Schönfelder, Jürgen Knödlseder, Andreas von Kienlin, G. Weidenspointner, P. Mandrou, 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), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Toulouse III - Paul Sabatier (UT3), 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-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Photon, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, media_common.quotation_subject, Astrophysics (astro-ph), Detector, FOS: Physical sciences, Field of view, Astrophysics, 7. Clean energy, 01 natural sciences, On board, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, Sky, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Spectral resolution, 010303 astronomy & astrophysics, Mutual influence, Remote sensing, media_common
Abstract: SPI, the Spectrometer on board the ESA INTEGRAL satellite, to be launched in October 2002, will study the gamma-ray sky in the 20 keV to 8 MeV energy band with a spectral resolution of 2 keV for photons of 1 MeV, thanks to its 19 germanium detectors spanning an active area of 500 cm2. A coded mask imaging technique provides a 2 deg angular resolution. The 16 deg field of view is defined by an active BGO veto shield, furthermore used for background rejection. In April 2001 the flight model of SPI underwent a one-month calibration campaign at CEA in Bruy\`eres le Ch\^atel using low intensity radioactive sources and the CEA accelerator for homogeneity measurements and high intensity radioactive sources for imaging performance measurements. After integration of all scientific payloads (the spectrometer SPI, the imager IBIS and the monitors JEM-X and OMC) on the INTEGRAL satellite, a cross-calibration campaign has been performed at the ESA center in Noordwijk. A set of sources has been placed in the field of view of the different instruments in order to compare their performances and determine their mutual influence. Some of those sources had already been used in Bruy\`eres during the SPI standalone test. For the lowest energy band calibration an X-ray generator has been used. We report on the scientific goals of this calibration activity, and present the measurements performed as well as some preliminary results., Comment: 12 pages, 19 figures, Published in Proceedings of SPIE conference, 24-28 August 2002, Waikoloa, Hawaii, USA
Published: 2002

50. Study of the $^{18}$F(p,$\alpha$)$^{15}$O reaction for application to nova $\gamma$-ray emission

Author: C. Angulo, Daniel Labar, Michel Gaelens, J. Kiener, N. de Sereville, Alain Ninane, N. A. Smirnova, J. P. Thibaud, F. Hammache, P. Demaret, Marc Loiselet, A. Coc, Didier Beaumel, A. Lefebvre, Manoel Couder, S. Ouichaoui, F. de Oliveira Santos, P. Figuera, Guido Ryckewaert, Marlete Assunção, B. Bouzid, S. Cherubini, S. Fortier, Pierre Leleux, Vincent Tatischeff, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and 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)
Subjects: Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Gamma ray, Alpha (ethology), Resonance, FOS: Physical sciences, Astrophysics, Nova (laser), [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 7. Clean energy, 01 natural sciences, Reaction rate, Louvain la neuve, 0103 physical sciences, Nuclear Experiment (nucl-ex), Nuclear Experiment, 010303 astronomy & astrophysics
Abstract: The ^18F(p, alpha)^15O reaction is recognized as one of the most important reaction for nova gamma-ray astronomy as it governs the early =< 511 keV emission. However, its rate remains largely uncertain at nova temperatures due to unknown low-energy resonance strengths. In order to better constrain this reaction rate, we have studied the one-nucleon transfer reaction, D(^18F,p alpha)^15N, at the CRC-RIB facility at Louvain La Neuve., Contribution to The Seventh International Symposium on Nuclei in the Cosmos
Published: 2002

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