exotic nuclei structure and reaction noyaux exotiques ... - IPN - IN2P3

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An infill array of 400 additional SD stations will be placed on the empty positions of the 1-mile grid. This denser array will allow extending to lower energies and to a detector density similar to Auger South. Almost full coverage of the SD array will be achieved with 39 fluorescence telescopes arranged in five stations, anticipating a usable viewing distance of 40 kilometers. A layout of the site is shown in fig. 1. Auger North Detectors The SD consists of Water Cherenkov Detectors similar to those of Auger South. However, due to low winter temperatures (-35 ◦ C) expected in Colorado, the tanks will require additional thermal insulation. This can be done by integrating a polyethylene foam insulation on the inside surface of the tank during the rotomolding process. In case of Auger South, the Cherenkov light produced in the water tanks is detected by 3 large 9” viewing the water from the top. Only one PMT, placed in the middle of the tank will be used for Auger North. The Auger South dynamic range of 15 bits will be increased to about 22 bits by reading the signals from an intermediate dynode. This will allow to keep the signal saturation in an acceptable level even for the very high energy showers. The research and development for the increased dynamic range has been done by the IPN-Orsay (SEP and RDD, see contribution to this annual report). The FD design is based upon the well proven principles implemented in Auger South. Individual telescopes are installed in buildings holding six telescopes. The transmitted light is collected by spherical mirrors with 3.4 m radius. The camera in the focal surface of the optical system includes a photomultiplier array of 440 PMTs. The read-out electronics of the camera is similar to that of Auger South. The communication system The biggest modifications compared to the Auger South concerns the communication system. Auger North communication system makes use of Wireless Sensor Nets (WSNs). It is configured as a WSN with heavy reliance on local station-to-station communication using the Wireless Architecture for Hard Real-time Embedded Networks (WAHREN) sensor nets paradigm. Unlike an ad hoc WSN, WAHREN provides a base infrastructure of fixed nodes suitable for fixed installations such as the SD array. Each message is multicast to its nearest neighbors, all of whom can then forward the message. The SD communications system is interfaced to optical fibers for transmission of the data to the observatory central campus at Concentrator Stations (CSs). Each FD site provides convenient place to install a CS, as they will have a connection to fiber. Performance It is important that the trigger efficiency or aperture is well understood as a function of energy, in particular when the spectral index changes in the energy range concerned. The aperture has been studied using Monte Carlo simulations of the Auger North detector configuration. The simulations were verified using real data from Auger South, in which only sub-sets of SD stations were used such that the spacing resembled the sparser array projected for Auger North.The 1-mile square array becomes fully efficient at an energy close to that of Auger South, with more than 90% efficiency down to 4 EeV. Therefore, the denser infill array allows efficiently to compare data from Auger North to the data from Auger South. In the case of the √2-miles square array about 90% efficiency is reached around 30 EeV for proton primaries, and 20 EeV for Fe primaries. The √2-miles square array becomes fully efficient slightly below the energy where the Auger South data show evidence for anisotropy in cosmic ray arrival direction and allows efficiently to accumulate statistics above this crucial energy. Using a Monte-Carlo simulation and comparing the reconstructed arrival direction with the simulated one, the accuracy in the determination of the arrival direction of the cosmic rays was estimated. For a fixed energy of 50 EeV the resolutions are 2.2 ◦, 1.2 ◦ and better than 1◦ for zenith angles of 25 ◦ , 45 ◦ and 60 ◦ , respectively. Three components dominate the energy determination based on the FD: the fluorescence yield, the light transmission properties of the atmosphere, and the absolute calibration of the photometric response of the telescopes. The global systematic uncertainty of the FD energy measurement is expected to be below 15%, similarly to Auger South. The expected resolution for shower maximum X max is below 20 gcm −2 . Although the acceptance is increased by about a factor of 7 compared to Auger South, Auger North conserves the performances and resolutions that are important for reliable physics results. The hybrid concept allows to use the nearly calorimetric energy determination of the FD, the angular resolution of the SD is sufficient to determine arrival directions, and the X max resolution of the FD to identify the masses of the primary cosmics rays. The prototype R&D Array (RDA) A prototype array RDA of 10 SD stations and 10 additional stations for communication system will be installed on site in Colorado during 2010. The aim of the RDA is to test the surface detector with the new electronics and communication system. IPNO is strongly involved in the construction of this array (see corresponding technical contribution to this annual report). The PMT bases and the front– end electronic have been designed and produced at IPN-Orsay, they will be shipped together with the PMTs for tests to be performed at fall 2010. References: [1] T. Suomijärvi for the Pierre Auger Collaboration, 1rst International Conference of Technology ans Instrumentation in Particle Physics (TIPP’09), Tsukuba, Japan, 12-17 march 2009, to be published in NIM. 55
The Pierre Auger southern Observatory: Results on Ultra-High Energy Cosmic Rays IPNO Participation: O. Deligny , P.N. Dong, P. Ghia, A. Lemière, I. Lhenry-Yvon, H. Lyberis, T. Suomijärvi Collaboration : Pierre Auger Collaboration Le site sud de l’Observatoire Pierre Auger: résultats sur les rayons cosmiques d’ultra-haute énergie. Les premiers résultats publiés par la collaboration Pierre Auger ont apporté des informations fondamentales sur l’énergie, la masse et les directions d’arrivée des rayons cosmiques aux énergies les plus hautes. L’extinction du flux au-delà de 50 EeV est en accord avec la coupure prévue par Greisen-Zatsepin- Kuzmin (GZK). Cette hypothèse est renforcée par la mesure d’une corrélation des rayons cosmiques audelà de 55 EeV avec des AGN proches (d
Page 1 and 2: EXOTIC NUCLEI STRUCTURE AND REACTIO
Page 3 and 4: in the spectra by analyzing their t
Page 5 and 6: were taken from ref. [5]. Concernin
Page 7 and 8: keV -ray with the particles and the
Page 9 and 10: the 605.9 keV line of the 74 Zn 2+
Page 11 and 12: Figure 2 a n d analysis. Figure 2 s
Page 13 and 14: ing particles was thus obtained by
Page 15 and 16: First p-p p collisions in the ALICE
Page 17 and 18: Quarkonia physics with ALICE IPNO P
Page 19 and 20: NA50 updated puzzle IPNO Participat
Page 21 and 22: Status of the HADES experiment (I):
Page 23 and 24: Status of the HADES experiments (II
Page 25 and 26: Status of the HADES experiment (III
Page 27 and 28: Hadron physics in pbar-p p annihila
Page 29 and 30: Hadron Electrodynamics IPNO Partici
Page 31 and 32: G0 experiment at Jefferson Lab. IPN
Page 33 and 34: GEp-III and GEp-2 at Jefferson Lab
Page 35 and 36: Exotic low mass narrow baryons from
Page 37 and 38: The PVA4 parity violation experimen
Page 39 and 40: Etude des Distributions de Partons
Page 41 and 42: Latest Results from GRAAL IPNO Part
Page 43 and 44: Persistence of the Polarization in
Page 45: The northern site of the Pierre Aug
Page 49 and 50: In figure 4 we plot the differentia
Page 51 and 52: THEORETICAL PHYSICS Research in the
Page 53 and 54: transfer reaction, the 34 Si(d, 3 H
Page 55 and 56: Collective excitations with SKYRME
Page 57 and 58: Pairing and nuclear incompressibili
Page 59 and 60: Pairing properties in nuclei and in
Page 61 and 62: Evaporation-residue residue cross s
Page 63 and 64: Extending the VMI model: normal and
Page 65 and 66: Alpha particle condensation in nucl
Page 67 and 68: Collective Modes in Ultracold Trapp
Page 69 and 70: Exploring key unknown neutrino prop
Page 71 and 72: Relic astrophysical and cosmologica
Page 73 and 74: After a term by term Borel resummat
Page 75 and 76: Chiral expansions of the π 0 lifet
Page 77 and 78: IPNO Participation: H. Sazdjian Eff
Page 79 and 80: fer is used to extract f + (0). We
Page 81 and 82: cleon. The spectrum becomes strongl
Page 83 and 84: A pseudo Coulombian potential in D=
Page 85 and 86: The many-body problem with an energ
Page 87 and 88: The rotational spectrum and the att
Page 89 and 90: Z-identification of very heavy nucl
Page 91 and 92: The Pegase project, a new solid sur
Page 93 and 94: But at 80 keV total energy ( 200 eV
Page 95 and 96: Isospin effects on fragment and par
Page 97 and 98:
Radial collective energy and fragme
Page 99 and 100:
Latent heat of the phase transition
Page 101 and 102:
Alpha-particle particle condensatio
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Fluo X: Deexcitation time measureme
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ENERGY AND ENVIRONMENT The increasi
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toe/cap/y which energy access inequ
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nides. A global comparison can be p
Page 111 and 112:
3D coupling of Monte-Carlo neutroni
Page 113 and 114:
Fission cross sections of actinides
Page 115 and 116:
Studies and synthesis of specific m
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Chemistry and Electrochemistry of T
Page 119 and 120:
function of temperature. The recent
Page 121 and 122:
global electron number of the redox
Page 123:
(D 0 /D)-1 ln complexes of Pa(V). I
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exotic nuclei structure and reaction noyaux exotiques ... - IPN - IN2P3

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