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Performances of photodiode detectors for top and bottom counting detectors of ISS-CREAM experiment
Hyun, H.J.,Anderson, T.,Angelaszek, D.,Baek, S.J.,Copley, M.,Coutu, S.,Han, J.H.,Huh, H.G.,Hwang, Y.S.,Im, S.,Jeon, H.B.,Kah, D.H.,Kang, K.H.,Kim, H.J.,Kim, K.C.,Kwashnak, K.,Lee, J.,Lee, M.H.,Link, J Elsevier 2015 Nuclear Instruments & Methods in Physics Research. Vol.787 No.-
<P><B>Abstract</B></P> <P>The Cosmic Ray Energetics and Mass (CREAM) experiment at the International Space Station (ISS) aims to elucidate the source and acceleration mechanisms of high-energy cosmic rays by measuring the energy spectra from protons to iron. The instrument is planned for launch in 2015 at the ISS, and it comprises a silicon charge detector, a carbon target, top and bottom counting detectors, a calorimeter, and a boronated scintillator detector. The top and bottom counting detectors are developed for separating the electrons from the protons, and each of them comprises a plastic scintillator and a 20×20 silicon photodiode array. Each photodiode is 2.3cm×2.3cm in size and exhibits good electrical characteristics. The leakage current is measured to be less than 20nA/cm<SUP>2</SUP> at an operating voltage. The signal-to-noise ratio is measured to be better than 70 using commercial electronics, and the radiation hardness is tested using a proton beam. A signal from the photodiode is amplified by VLSI (very-large-scale integration) charge amp/hold circuits, the VA-TA viking chip. Environmental tests are performed using whole assembled photodiode detectors of a flight version. Herein, we present the characteristics of the developed photodiode along with the results of the environmental tests.</P>
Jiang, Z,Pá,linká,š,, V,Arias, F E,Liard, J,Merlet, S,Wilmes, H,Vitushkin, L,Robertsson, L,Tisserand, L,Pereira Dos Santos, F,Bodart, Q,Falk, R,Baumann, H,Mizushima, S,Mä,kinen, J Springer-Verlag 2012 METROLOGIA -BERLIN- Vol.49 No.6
<P>The 8th International Comparison of Absolute Gravimeters (ICAG2009) took place at the headquarters of the International Bureau of Weights and Measures (BIPM) from September to October 2009. It was the first ICAG organized as a key comparison in the framework of the CIPM Mutual Recognition Arrangement of the International Committee for Weights and Measures (CIPM MRA) (CIPM 1999). ICAG2009 was composed of a Key Comparison (KC) as defined by the CIPM MRA, organized by the Consultative Committee for Mass and Related Quantities (CCM) and designated as CCM.G-K1. Participating gravimeters and their operators came from national metrology institutes (NMIs) or their designated institutes (DIs) as defined by the CIPM MRA. A Pilot Study (PS) was run in parallel in order to include gravimeters and their operators from other institutes which, while not signatories of the CIPM MRA, nevertheless play important roles in international gravimetry measurements. The aim of the CIPM MRA is to have international acceptance of the measurement capabilities of the participating institutes in various fields of metrology. The results of CCM.G-K1 thus constitute an accurate and consistent gravity reference traceable to the SI (International System of Units), which can be used as the global basis for geodetic, geophysical and metrological observations of gravity. The measurements performed afterwards by the KC participants can be referred to the international metrological reference, i.e. they are SI-traceable.</P><P>The ICAG2009 was complemented by a number of associated measurements: the Relative Gravity Campaign (RGC2009), high-precision levelling and an accurate gravity survey in support of the BIPM watt balance project. The major measurements took place at the BIPM between July and October 2009. Altogether 24 institutes with 22 absolute gravimeters (one of the 22 AGs was ultimately withdrawn) and nine relative gravimeters participated in the ICAG/RGC campaign.</P><P>This paper is focused on the absolute gravity campaign. We review the history of the ICAGs and present the organization, data processing and the final results of the ICAG2009.</P><P>After almost thirty years of hosting eight successive ICAGs, the CIPM decided to transfer the responsibility for piloting the future ICAGs to NMIs, although maintaining a supervisory role through its Consultative Committee for Mass and Related Quantities.</P>
Hough, L. E.,Jung, H. T.,Krü,erke, D.,Heberling, M. S.,Nakata, M.,Jones, C. D.,Chen, D.,Link, D. R.,Zasadzinski, J.,Heppke, G.,Rabe, J. P.,Stocker, W.,Kö,rblova, E.,Walba, D. M.,Glaser, M. A. American Association for the Advancement of Scienc 2009 Science Vol.325 No.5939
<P>In the formation of chiral crystals, the tendency for twist in the orientation of neighboring molecules is incompatible with ordering into a lattice: Twist is expelled from planar layers at the expense of local strain. We report the ordered state of a neat material in which a local chiral structure is expressed as twisted layers, a state made possible by spatial limitation of layering to a periodic array of nanoscale filaments. Although made of achiral molecules, the layers in these filaments are twisted and rigorously homochiral--a broken symmetry. The precise structural definition achieved in filament self-assembly enables collective organization into arrays in which an additional broken symmetry--the appearance of macroscopic coherence of the filament twist--produces a liquid crystal phase of helically precessing layers.</P>
A novel quantum interference probe of the energy spectrum of coupled nanodevices
T.P. Martin,R.P. Taylor,H. Linke,B. Murray,N. Aoki,D. Oonishi,Y. Iwase,Y. OchiaI 한국물리학회 2006 Current Applied Physics Vol.6 No.3
Quantum transport of an array of quantum billiards is investigated as a function of the coupling strength of the quantum point con-invasive probe of two characteristic energy scales of the energy level spectrumthe average energy level spacing and average energy levelbroadening. This analysis reveals a marked transition in the coherent area of the array as the coupling between the billiards is increasedand the array evolves into a combined quantum system.
Quantum conductance fluctuations in semiconductor devices
B.C. Scannell,T.P. Martin,M.S. Fairbanks,H. Linke,C.A. Marlow,T.M. Fromhold,C.V. Brown,K. Ishibashi,R.P. Taylor 한국물리학회 2008 Current Applied Physics Vol.8 No.3,4
Magneto-conductance uctuations serve as the traditional method for investigating the dynamics of electrons as they ow throughsolid-state materials. Generated by electron wave interference, their spectral content is critically sensitive to the precise scattering con-gurations in the material. In this paper, we exploit this sensitivity to study the electron dynamics in the diusive regime of semiconduc-tors where the dynamics are determined by material-induced scattering. We show that the spectral content of the uctuations measuredon diusive n+GaAs wires and quasi-ballistic AlGaAs/GaAs wires follow a fractal scaling behaviour similar to that previously observed.
Proton and Helium Spectra from the CREAM-III Flight
Yoon, Y. S.,Anderson, T.,Barrau, A.,Conklin, N. B.,Coutu, S.,Derome, L.,Han, J. H.,Jeon, J. A.,Kim, K. C.,Kim, M. H.,Lee, H. Y.,Lee, J.,Lee, M. H.,Lee, S. E.,Link, J. T.,Menchaca-Rocha, A.,Mitchell, J American Astronomical Society 2017 The Astrophysical journal Vol.839 No.1
<P>Primary cosmic-ray elemental spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass (CREAM) experiment since 2004. The third CREAM payload (CREAM-III) flew for 29 days during the 2007-2008 Antarctic season. Energies of incident particles above 1 TeV are measured with a calorimeter. Individual elements are clearly separated with a charge resolution of similar to 0.12 e (in charge units) and similar to 0.14 e for protons and helium nuclei, respectively, using two layers of silicon charge detectors. The measured proton and helium energy spectra at the top of the atmosphere are harder than other existing measurements at a few tens of GeV. The relative abundance of protons to helium nuclei is 9.53 +/- 0.03 for the range of 1 TeV/n. to 63 TeV/n. This ratio is considerably smaller than other measurements at a few tens of GeV/n. The spectra become softer above similar to 20 TeV. However, our statistical uncertainties are large at these energies and more data are needed.</P>