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MEASUREMENTS OF THE RELATIVE ABUNDANCES OF HIGH-ENERGY COSMIC-RAY NUCLEI IN THE TeV/NUCLEON REGION
Ahn, H. S.,Allison, P. S.,Bagliesi, M. G.,Barbier, L.,Beatty, J. J.,Bigongiari, G.,Brandt, T. J.,Childers, J. T.,Conklin, N. B.,Coutu, S.,DuVernois, M. A.,Ganel, O.,Han, J. H.,Jeon, J. A.,Kim, K. C.,L IOP Publishing 2010 The Astrophysical journal Vol.715 No.2
<P>We present measurements of the relative abundances of cosmic-ray nuclei in the energy range of 500-3980 GeV/nucleon from the second flight of the Cosmic Ray Energetics And Mass balloon-borne experiment. Particle energy was determined using a sampling tungsten/scintillating-fiber calorimeter, while particle charge was identified precisely with a dual-layer silicon charge detector installed for this flight. The resulting element ratios C/O, N/O, Ne/O, Mg/O, Si/O, and Fe/O at the top of atmosphere are 0.919 +/- 0.123(stat) +/- 0.030(syst), 0.076 +/- 0.019(stat) +/- 0.013(syst), 0.115 +/- 0.031(stat) +/- 0.004(syst), 0.153 +/- 0.039(stat) +/- 0.005(syst), 0.180 +/- 0.045(stat) +/- 0.006(syst), and 0.139 +/- 0.043(stat) +/- 0.005(syst), respectively, which agree with measurements at lower energies. The source abundance of N/O is found to be 0.054 +/- 0.013(stat) +/- 0.009(-0.017)(syst+0.010esc). The cosmic-ray source abundances are compared to local Galactic (LG) abundances as a function of first ionization potential and as a function of condensation temperature. At high energies the trend that the cosmic-ray source abundances at large ionization potential or low condensation temperature are suppressed compared to their LG abundances continues. Therefore, the injection mechanism must be the same at TeV/nucleon energies as at the lower energies measured by HEAO-3, CRN, and TRACER. Furthermore, the cosmic-ray source abundances are compared to a mixture of 80% solar system abundances and 20% massive stellar outflow (MSO) as a function of atomic mass. The good agreement with TIGER measurements at lower energies confirms the existence of a substantial fraction of MSO material required in the similar to TeV per nucleon region.</P>
SEARCHES FOR EXTENDED AND POINT-LIKE NEUTRINO SOURCES WITH FOUR YEARS OF ICECUBE DATA
Aartsen, M. G.,Ackermann, M.,Adams, J.,Aguilar, J. A.,Ahlers, M.,Ahrens, M.,Altmann, D.,Anderson, T.,Arguelles, C.,Arlen, T. C.,Auffenberg, J.,Bai, X.,Barwick, S. W.,Baum, V.,Beatty, J. J.,Tjus, J. Be IOP Publishing 2014 The Astrophysical journal Vol.796 No.2
<P>We present results on searches for point-like sources of neutrinos using four years of IceCube data, including the first year of data from the completed 86 string detector. The total livetime of the combined data set is 1373 days. For an E-2 spectrum, the observed 90% C. L. flux upper limits are similar to 10(-12) TeV-1 cm(-2) s(-1) for energies between 1 TeV and 1 PeV in the northern sky and similar to 10(-11) TeV-1 cm(-2) s(-1) for energies between 100 TeV and 100 PeV in the southern sky. This represents a 40% improvement compared to previous publications, resulting from both the additional year of data and the introduction of improved reconstructions. In addition, we present the first results from an all-sky search for extended sources of neutrinos. We update the results of searches for neutrino emission from stacked catalogs of sources and test five new catalogs; two of Galactic supernova remnants and three of active galactic nuclei. In all cases, the data are compatible with the background-only hypothesis, and upper limits on the flux of muon neutrinos are reported for the sources considered.</P>
The IceProd framework: Distributed data processing for the IceCube neutrino observatory
Aartsen, M.G.,Abbasi, R.,Ackermann, M.,Adams, J.,Aguilar, J.A.,Ahlers, M.,Altmann, D.,Arguelles, C.,Auffenberg, J.,Bai, X.,Baker, M.,Barwick, S.W.,Baum, V.,Bay, R.,Beatty, J.J.,Becker Tjus, J.,Becker, Elsevier 2015 Journal of parallel and distributed computing Vol.75 No.-
<P><B>Abstract</B></P> <P>IceCube is a one-gigaton instrument located at the geographic South Pole, designed to detect cosmic neutrinos, identify the particle nature of dark matter, and study high-energy neutrinos themselves. Simulation of the IceCube detector and processing of data require a significant amount of computational resources. This paper presents the first detailed description of IceProd, a lightweight distributed management system designed to meet these requirements. It is driven by a central database in order to manage mass production of simulations and analysis of data produced by the IceCube detector. IceProd runs as a separate layer on top of other middleware and can take advantage of a variety of computing resources, including grids and batch systems such as CREAM, HTCondor, and PBS. This is accomplished by a set of dedicated daemons that process job submission in a coordinated fashion through the use of middleware plugins that serve to abstract the details of job submission and job management from the framework.</P> <P><B>Highlights</B></P> <P> <UL> <LI> IceProd is a lightweight distributed workflow management framework. </LI> <LI> Uses existing middleware and protocols. </LI> <LI> Runs at user-level and is easily adaptable to other applications. </LI> <LI> It has been successful in managing 450k cores across 25 computing centers. </LI> <LI> Identified areas of improvement including scalability and load balancing. </LI> </UL> </P>
Song, J.H.,Meats, A.W.,Riu, K.Z.,Beattie, G.A.C. Korean Society of Applied Entomology 2006 Journal of Asia-Pacific Entomology Vol.9 No.1
Two-stage sampling and geostatistical techniques for cost-effective and precise sampling were examined using red scale data that were collected from a commercial orange orchard in Kulnura, Australia in mid-summer, 2004 and 2005. The distribution pattern of red scale on a twig and a fruit well followed the negative binomial, and the degree of aggregation was higher on a fruit than a twig. The analysis of variance and two-stage sampling were used to obtain the suitable sample unit (a leaf, a twig including 2 leaves and 15 em branch and a fruit in this study) and optimum sample size. A fruit was the most suitable than any other sample units, and a twig was better than a leaf. The optimum sample size for twigs and fruits per tree was 4 twigs (2 leaves and 15 cm branch) and 4 fruits (2 directions), respectively. The variance of primary sample unit for fruits was higher than that of secondary sample unit, but that was reversed for twigs. There was a non-linear relationship between 2 years for the density on 40 fruits of the same tree, because the Spearman rank correlation coefficient (0.84) was much higher than the Pearson's (0.29). The spatial continuity for directions of $0^{\circ},\;45^{\circ},\;90^{\circ},\;135^{\circ}$, and omni-direction was similar except $90^{\circ}$ in which trees were touched with together. The autocorrelation analysis showed that omnidirectional 10m apart from each sampled tree was needed to obtain the independent data.
J.H. Song,A.W. Meats,K.Z. Riu,G.A.C. Beattie 한국응용곤충학회 2006 Journal of Asia-Pacific Entomology Vol.9 No.1
sampling and geostatistical tech-niques for cost-effective and precise sampling wereexamined using red scale data that were collectedfrom a commercial orange orchard in Kulnura, Aus-tralia in mid-summer, 2004 and 2005. The distri-bution pattern of red scale on a twig and a fruit wellfollowed the negative binomial, and the degree ofanalysis of variance and two-stage sampling wereused to obtain the suitable sample unit (a leaf, atwig including 2 leaves and 15 cm branch and afruit in this study) and optimum sample size. A fruitwas the most suitable than any other sample units,and a twig was better than a leaf. The optimumsample size for twigs and fruits per tree was 4 twigs( 2 l e a v e s a n d 1 5 c m b r a n c h ) a n d 4 f r u i t s ( 2 d i r e c -tions), respectively. The variance of primary sampleunit for fruits was higher than that of secondarysample unit, but that was reversed for twigs. Therewas a non-linear elationship between 2 years forthe Spearman rank correlation coefficient (0.84) wasmuch higher than the Pearsons (0.29). The spatialcontinuity for directions of 0, 45, 90, 135, andomni-direction was similar except 90 in which treeswere touched with together. The autocorrelation ana-lysis howed that omnidirectional 10m apart fromeach sampled tree was needed to obtain the inde-pendent data.Key words Aonidiella aurantii, Sample size, Auto-corelation, Semivariogram, MoransI
Namgay Om,Zoya A. Yefremova,Ekaterina N. Yegorenkova,G. Andrew C. Beattie,Nerida J. Donovan,Paul Holford 한국응용곤충학회 2017 Journal of Asia-Pacific Entomology Vol.20 No.2
Parasitised nymphs of Diaphorina communis, a host of ‘Candidatus Liberibacter asiaticus’, were observed on Bergera koenigii in the Wangdue Phodrang Dzongkhag, Bhutan, and parasitised nymphs of Diaphorina citri were found on Murraya paniculata in the Chukhha Dzongkhag. The nymphs of both hosts were collected along with leaf tissue and placed individually in gelatine capsules. Emerging parasitoids were preserved in ethanol and used either for DNA extraction or morphological examination. Molecular and phylogenetic analyses of the sequence data of the COI, ITS1 and ITS2 regions showed that the parasitoids from the two hosts belonged to two different clades. Morphological examination confirmed that the parasitoids belong to two separate species of Tamarixia, and that the parasitoid from Diaphorina communis is a new species. This is the first record of an ectoparasitoid of Diaphorina communis, and the parasitoid has been named Tamarixia drukyulensis sp. n. The molecular and phylogenetic studies also suggest the occurrence of a eulophid parasitoid or hyperparasitoid of Diaphorina communis belonging to the genus, Aprostocetus.
Search for non-relativistic magnetic monopoles with IceCube
Aartsen, M. G.,Abbasi, R.,Ackermann, M.,Adams, J.,Aguilar, J. A.,Ahlers, M.,Altmann, D.,Arguelles, C.,Arlen, T. C.,Auffenberg, J.,Bai, X.,Baker, M.,Barwick, S. W.,Baum, V.,Bay, R.,Beatty, J. J.,Becker Springer-Verlag 2014 European Physical Journal C Vol.74 No.7
Search for neutrino-induced particle showers with IceCube-40
Aartsen, M. G.,Abbasi, R.,Ackermann, M.,Adams, J.,Aguilar, J. A.,Ahlers, M.,Altmann, D.,Arguelles, C.,Arlen, T. C.,Auffenberg, J.,Bai, X.,Baker, M.,Barwick, S. W.,Baum, V.,Bay, R.,Beatty, J. J.,Becker American Physical Society 2014 PHYSICAL REVIEW D - Vol.89 No.10
Searches for small-scale anisotropies from neutrino point sources with three years of IceCube data
Aartsen, M.G.,Ackermann, M.,Adams, J.,Aguilar, J.A.,Ahlers, M.,Ahrens, M.,Altmann, D.,Anderson, T.,Arguelles, C.,Arlen, T.C.,Auffenberg, J.,Bai, X.,Barwick, S.W.,Baum, V.,Beatty, J.J.,Becker Tjus, J. North-Holland 2015 Astroparticle physics Vol.66 No.-
<P><B>Abstract</B></P> <P>Recently, IceCube found evidence for a diffuse signal of astrophysical neutrinos in an energy range of ∼ 60 TeV to the PeV-scale [1]. The origin of those events, being a key to understanding the origin of cosmic rays, is still an unsolved question. So far, analyses have not succeeded to resolve the diffuse signal into point-like sources. Searches including a maximum-likelihood-ratio test, based on the reconstructed directions and energies of the detected down- and up-going neutrino candidates, were also performed on IceCube data leading to the exclusion of bright point sources. In this paper, we present two methods to search for faint neutrino point sources in three years of IceCube data, taken between 2008 and 2011. The first method is an autocorrelation test, applied separately to the northern and southern sky. The second method is a multipole analysis, which expands the measured data in the northern hemisphere into spherical harmonics and uses the resulting expansion coefficients to separate signal from background. With both methods, the results are consistent with the background expectation with a slightly more sparse spatial distribution, corresponding to an underfluctuation. Depending on the assumed number of sources, the resulting upper limit on the flux per source in the northern hemisphere for an <SUP> E - 2 </SUP> energy spectrum ranges from ∼ 1.5 · <SUP> 10 - 8 </SUP> GeV/cm<SUP>2</SUP> s<SUP>−1</SUP>, in the case of one assumed source, to ∼ 4 · <SUP> 10 - 10 </SUP> GeV/cm<SUP>2</SUP> s<SUP>−1</SUP>, in the case of 3500 assumed sources.</P> <P><B>Highlights</B></P> <P> <UL> <LI> We applied two methods to search for clusters of astrophysical neutrinos on background. </LI> <LI> Investigated both hemispheres separately and three different energy spectra. </LI> <LI> Saw underfluctuation consistent with background and set limits on astrophysical flux. </LI> <LI> Compared limits to recently found astrophysical flux to constrain number of sources. </LI> <LI> Excluded few sources of very hard energy spectra for seen astrophysical flux. </LI> </UL> </P>