Aubert7, J. Aublin8, B. Baret8, S. Basa9, B. Belhorma10, V. Bertin7, S. Biagi11, M. Bissinger5, J. Boumaaza12, S. Bourret8, M. Bouta13, M. C. Bouwhuis14, H. Brânzaş15, R. Bruijn14,16, J. Brunner7, J. Busto7, A. Capone17,18, L. Caramete15, J. Carr7, S. Celli17,18,19, M. Chabab20, T. N. Chau8, R. Cherkaoui El Moursli12, T. Chiarusi21, M. Circella22, A. Coleiro8, M. Colomer8,23, R. Coniglione11, H. Costantini7, P. Coyle7, A. Creusot8, A. F. Díaz24, G. de Wasseige8, A. Deschamps25, C. Distefano11, I. Karlsruhe Institute of Technology, Institut für Kernphysik, D-76021 Karlsruhe, Germany, 60 ben laser. 29 Dipartimento di Fisica e Astronomia dell'Università, Viale Berti Pichat 6/2, I-40127 Bologna, Italy INFN—Sezione di Bologna, Viale Berti-Pichat 6/2, I-40127 Bologna, Italy, 22 Nikhef, Science Park, Amsterdam, The Netherlands, 15 -enedithiolate complexes – a look at both ends of the catalytic transformation. Synthesis and characterization of cyano and isocyano complexes of bis(dithiolato) molybdenum using Me For each model, the values of the neutrino spectrum parameters, Φ0, Γ, Ecut, and β entering Equation (5) are provided. Discovery flux (red dots), median sensitivity (blue dots) and 90% C.L. Neutrinos are expected to be produced through the decay of charged mesons, a result of hadronic interactions of accelerated protons with matter or radiation in the surroundings of the acceleration sites. Both the ANTARES and the IceCube event selection criteria were optimized to minimize the neutrino flux needed for a 5σ discovery of a point-like source emitting with a {E}_{\nu }^{-2.0} spectrum. 2018a). Alle Informationen zu den Sportstars, Vereinen und Nationalteams wurden nach bestem Wissen und Gewissen zusammengetragen - sollten Sie aber trotzdem einen Fehler bemerkt haben, dann können Sie sich gern per E-Mail (info@trikotshop.net) mit uns in Verbindung setzen und wir werden den Fehler umgehend korrigieren. Searches for pair-produced scalar leptoquarks are performed using 20 fb of proton–proton collision data provided by the LHC and recorded by the ATLAS detector at TeV. Polymer-Supported Dioxido-MoVI Complexes as Truly Functional Molybdenum Oxotransferase Model Systems. 2019) and based on the methods described by Vissani et al. Shower-like events are induced by neutral current (NC) interactions, as well as by CC interactions of electron and tau neutrinos and antineutrinos, and are characterized by an almost spherically symmetric light emission around the shower maximum. of Physics and Astronomy, University of Gent, B-9000 Gent, Belgium, 81 Common backgrounds in both detectors are atmospheric muons and neutrinos originating from cosmic-ray interactions in Earth's atmosphere. A new series of molybdenum-(iv), -(v), and -(vi) dithiolate compounds as active site models of molybdoenzymes: preparation, crystal structures, spectroscopic/electrochemical properties and reactivity in oxygen atom transfer. Figure 1. For an {E}_{\nu }^{-2.0} spectrum, the largest improvement is achieved in a region of the sky that is centered approximately at the decl. of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand, 49 iv Some of the observed γ-ray spectra extend up to tens of TeV, suggesting that these objects are accelerators of high-energy particles. of Physics, University of Oxford, Parks Road, Oxford OX1 3PU, UK, 100 7, D-96049 Bamberg, Germany, 37 Institute of Basic Science, Sungkyunkwan University, Suwon 16419, Republic of Korea, 101 Dept. School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332, USA, 75 All‐electron The most significant source candidate is HESSJ1023-575, with a posttrial significance of 42%. The largest excess above the background is found for a point-like source hypothesis, with best-fit {\hat{n}}_{{\rm{s}}}=2.9 and \hat{\gamma }=2.1, and a significance of 6% (1.6σ in the one-sided sigma convention). INFN—Sezione di Bari, Via E. Orabona 4, I-70126 Bari, Italy, 23 Reported are the source extension σs, the best-fit parameters (number of signal events, {\hat{n}}_{{\rm{s}}}, spectral index, \hat{\gamma }, decl., \hat{\delta }, R.A., \hat{\alpha }), and the pretrial and posttrial p-values. This result is consistent with the findings of the previous combined analysis (Adrian-Martinez et al. Comparative molecular chemistry of molybdenum and tungsten and its relation to hydroxylase and oxotransferase enzymes. 1,-40\buildrel{\circ}\over{.} A three-dimensional array of photomultiplier tubes (PMTs) inside a transparent medium—water or ice, respectively—collects the Cerenkov photons induced by the passage of relativistic charged particles. When searching for spatially extended sources, the value of σi is replaced with {\sigma }_{\mathrm{eff},i}=\sqrt{{\sigma }_{i}^{2}+{\sigma }_{{\rm{s}}}^{2}}, where {\sigma }_{{\rm{s}}} is the extension of the source assuming a Gaussian profile. Google has many special features to help you find exactly what you're looking for. The American Astronomical Society. Receive alerts on all new research papers in American Astronomical Society Upper limits on the neutrino flux from 57 astrophysical candidate sources were presented. A Gaussian extension with σs = 06 is assumed for the source as reported by the γ-ray analysis performed by the H.E.S.S. 2014) and the IceCube (Aartsen et al. Dept. Und dann wären da noch die beiden Transfers von Manuel Schäffler und Pascal Köpke. Note. The most significant clustering with respect to the expected background is searched for at any position in a predefined region of the sky. In each box, the unbinned likelihood maximization is performed, with the source position being an additional parameter that is free to vary inside the 1° × 1° boundaries. The expected mean number of signal events for each IceCube sample j ∈ [3, 7] given in Table 1 is calculated using Equation (1), including only the contribution of the muon flavor. A combined search for neutrino sources in the Southern Sky using data from the ANTARES and IceCube telescopes was presented. of Astronomy, University of Wisconsin, Madison, WI 53706, USA, 85 SNRs are the prime candidates for the acceleration of Galactic cosmic rays, and hence are potential sources of astrophysical neutrinos. This makes it possible to properly calculate the median of the background Q-distribution. Baran, Dominika M. 2018. Dept. 717, Oujda 6000, Morocco, 14 The complementarity of the two detectors is mostly effective for a harder spectral index, as all the samples provide a significant contribution. Carbon dioxide would be an ideal carbon source for these production systems, but efficient production of long carbon chains from CO2 is difficult to achieve in a single organism. By Pascal Chevalier, ... By Eojin Kim, Jong-Kyun Chung, Yong Ha Kim, Geonhwa Jee, Sun-hak Hong and Jeong-ho Cho ... Wissenskommunikation und Transfer für die Landschaftsentwicklung. )O- and Mo( Sein aktueller Verein ist 1.FC Nürnberg, er spielt dort im Sturm - Mittelstürmer. For an {E}_{\nu }^{-2.0} spectrum, all samples contribute significantly to most of the Southern Sky. of Physics, Sungkyunkwan University, Suwon 16419, Republic of Korea, 76 The results are shown in Figure 2 in comparison to the discovery potentials from the individual IceCube and ANTARES analyses (sensitivities are shown in Figure 6). In this study, the location of 57 astrophysical objects is investigated to look for point-like emission of high-energy neutrinos. 3124/2004, Springer Berlin / Heidelberg, August 2004, pp. upper limits on the one-flavor neutrino flux normalization of the Galactic Center region search, assuming an {E}_{\nu }^{-2.0} spectrum for different source extensions σs. Microbial biosynthesis of alkanes is considered a promising method for the sustainable production of drop-in fuels and chemicals. The mission of the AAS is to enhance and share humanity's scientific understanding of the universe. Jongoh Shin, Seulgi Kang, Yoseb Song, Sangrak Jin, Jin Soo Lee, Jung-Kul Lee, Dong Rip Kim, Sun Chang Kim, Suhyung Cho, Byung-Kwan Cho, Genome engineering of Eubacterium limosum using expanded genetic tools and CRISPR-Cas9 system , ACS Synthetic Biology, 10.1021/acssynbio.9b00150, (2019). Physics Department, South Dakota School of Mines and Technology, Rapid City, SD 57701, USA, 59 Dept. It has a worldwide membership of around 50 000 comprising physicists from all sectors, as well as those with an interest in physics. The direction with the smallest p-value identifies the most significant cluster of each search. Institut d'Investigació per a la Gestió Integrada de les Zones Costaneres (IGIC)—Universitat Politècnica de València. Der FCN hat jede Menge nominelle Mittelstürmer und hat trotzdem noch zwei weitere hinzugefügt. Here, we present an untargeted search, to allow for the greatest range of possibilities. By continuing to use this site you agree to our use of cookies. Table 6. 2,-40\buildrel{\circ}\over{.} of Physics, Pennsylvania State University, University Park, PA 16802, USA, 55 2017a)). Synthesis, Structure and a DFT/TDDFT Study of a Diimido-Bridged Asymmetric Dimolybdenum Complex. 2390, Marrakech, Morocco, 21 The PMTs are distributed over 12 vertical lines with a length of 350 m, and with an interline separation between 60 and 75 m, instrumenting a total volume of ~0.01 km3. This Letter reports on a first measurement of the inclusive W+ jets cross section in proton–proton collisions at a centre-of-mass energy of 7 TeV at the LHC, with the ATLAS detector. 2018). 2016; Kopper 2017, and Aartsen et al. Figure 6 shows the 90% C.L. The first molybdenum dioxo compounds with η Project Leader(s): Köpke, Prof.Dr. The IceCube telescope (Achterberg et al. The green line indicates the sensitivity of the combined analysis. A. Aguilar49, M. Ahlers50, M. Ahrens51, C. Alispach52, K. Andeen53, T. Anderson54, I. Ansseau49, G. Anton55, C. Argüelles56, J. Auffenberg57, S. Axani56, P. Backes57, H. Bagherpour47, X. Bai58, A. Balagopal V.59, A. Barbano52, S. W. Barwick60, B. Bastian48, V. Baum61, S. Baur49, R. Bay62, J. J. Beatty63,64, K.-H. Becker65, J. Becker Tjus66, S. BenZvi67, D. Berley68, E. Bernardini102,48, D. Z. Besson103,69, G. Binder62,70, D. Bindig65, E. Blaufuss68, S. Blot48, C. Bohm51, S. Böser61, O. Botner71, J. Böttcher57, E. Bourbeau50, J. Bourbeau72, F. Bradascio48, J. Braun72, S. Bron52, J. Brostean-Kaiser48, A. Burgman71, J. Buscher57, R. S. Busse73, T. Carver52, C. Chen74, E. Cheung68, D. Chirkin72, S. Choi75, K. Clark76, L. Classen73, A. Coleman77, G. H. Collin56, J. M. Conrad56, P. Coppin78, P. Correa78, D. F. Cowen54,79, R. Cross67, P. Dave74, C. De Clercq78, J. J. DeLaunay54, H. Dembinski77, K. Deoskar51, S. De Ridder80, P. Desiati72, K. D. de Vries78, G. de Wasseige78, M. de With81, T. DeYoung82, A. Diaz56, J. C. Díaz-Vélez72, H. Dujmovic59, M. Dunkman54, E. Dvorak58, B. Eberhardt72, T. Ehrhardt61, P. Eller54, R. Engel59, P. A. Evenson77, S. Fahey72, A. R. Fazely83, J. Felde68, K. Filimonov62, C. Finley51, D. Fox79, A. Franckowiak48, E. Friedman68, A. Fritz61, T. K. Gaisser77, J. Gallagher84, E. Ganster57, S. Garrappa48, L. Gerhardt70, K. Ghorbani72, T. Glauch85, T. Glüsenkamp55, A. Goldschmidt70, J. G. Gonzalez77, D. Grant82, T. Grégoire54, Z. Griffith72, S. Griswold67, M. Günder57, M. Gündüz66, C. Haack57, A. Hallgren71, R. Halliday82, L. Halve57, F. Halzen72, K. Hanson72, A. Haungs59, D. Hebecker81, D. Heereman49, P. Heix57, K. Helbing65, R. Hellauer68, F. Henningsen85, S. Hickford65, J. Hignight86, G. C. Hill87, K. D. Hoffman68, R. Hoffmann65, T. Hoinka88, B. Hokanson-Fasig72, K. Hoshina104,72, F. Huang54, M. Huber85, T. Huber48,59, K. Hultqvist51, M. Hünnefeld88, R. Hussain72, S. In75, N. Iovine49, A. Ishihara89, M. Jansson51, G. S. Japaridze90, M. Jeong75, K. Jero72, B. J. P. Jones91, F. Jonske57, R. Joppe57, D. Kang59, W. Kang75, A. Kappes73, D. Kappesser61, T. Karg48, M. Karl85, A. Karle72, U. Katz55, M. Kauer72, J. L. Kelley72, A. Kheirandish72, J. Kim75, T. Kintscher48, J. Kiryluk92, T. Kittler55, S. R. Klein62,70, R. Koirala77, H. Kolanoski81, L. Köpke61, C. Kopper82, S. Kopper93, D. J. Koskinen50, M. Kowalski48,81, K. Krings85, G. Krückl61, N. Kulacz86, N. Kurahashi94, A. Kyriacou87, J. L. Lanfranchi54, M. J. Larson68, F. Lauber65, J. P. Lazar72, K. Leonard72, A. Leszczyńska59, M. Leuermann57, Q. R. Liu72, E. Lohfink61, C. J. Lozano Mariscal73, L. Lu89, F. Lucarelli52, J. Lünemann78, W. Luszczak72, Y. Lyu62,70, W. Y. Ma48, J. Madsen95, G. Maggi78, K. B. M. Mahn82, Y. Makino89, P. Mallik57, K. Mallot72, S. Mancina72, I. C. Mariş49, R. Maruyama96, K. Mase89, R. Maunu68, F. McNally97, K. Meagher72, M. Medici50, A. Medina64, M. Meier88, S. Meighen-Berger85, G. Merino72, T. Meures49, J. Micallef82, D. Mockler49, G. Momenté61, T. Montaruli52, R. W. Moore86, R. Morse72, M. Moulai56, P. Muth57, R. Nagai89, U. Naumann65, G. Neer82, H. Niederhausen85, M. U. Nisa82, S. C. Nowicki82, D. R. Nygren70, A. Obertacke Pollmann65, M. Oehler59, A. Olivas68, A. O'Murchadha49, E. O'Sullivan51, T. Palczewski62,70, H. Pandya77, D. V. Pankova54, N. Park72, P. Peiffer61, C. Pérez de los Heros71, S. Philippen57, D. Pieloth88, S. Pieper65, E. Pinat49, A. Pizzuto72, M. Plum53, A. Porcelli80, P. B. Price62, G. T. Przybylski70, C. Raab49, A. Raissi47, M. Rameez50, L. Rauch48, K. Rawlins98, I. C. Rea85, R. Reimann57, B. Relethford94, M. Renschler59, G. Renzi49, E. Resconi85, W. Rhode88, M. Richman94, S. Robertson70, M. Rongen57, C. Rott75, T. Ruhe88, D. Ryckbosch80, D. Rysewyk82, I. Safa72, S. E. Sanchez Herrera82, A. Sandrock88, J. Sandroos61, M. Santander93, S. Sarkar99, S. Sarkar86, K. Satalecka48, M. Schaufel57, H. Schieler59, P. Schlunder88, T. Schmidt68, A. Schneider72, J. Schneider55, F. G. Schröder59,77, L. Schumacher57, S. Sclafani94, D. Seckel77, S. Seunarine95, S. Shefali57, M. Silva72, R. Snihur72, J. Soedingrekso88, D. Soldin77, M. Song68, G. M. Spiczak95, C. Spiering48, J. Stachurska48, M. Stamatikos64, T. Stanev77, R. Stein48, J. Stettner57, A. Steuer61, T. Stezelberger70, R. G. Stokstad70, A. Stößl89, N. L. Strotjohann48, T. Stürwald57, T. Stuttard50, G. W. Sullivan68, I. Taboada74, F. Tenholt66, S. Ter-Antonyan83, A. Terliuk48, S. Tilav77, K. Tollefson82, L. Tomankova66, C. Tönnis100, S. Toscano49, D. Tosi72, A. Trettin48, M. Tselengidou55, C. F. Tung74, A. Turcati85, R. Turcotte59, C. F. Turley54, B. Ty72, E. Unger71, M. A. Unland Elorrieta73, M. Usner48, J. Vandenbroucke72, W. Van Driessche80, D. van Eijk72, N. van Eijndhoven78, J. van Santen48, S. Verpoest80, M. Vraeghe80, C. Walck51, A. Wallace87, M. Wallraff57, N. Wandkowsky72, T. B. Watson91, C. Weaver86, A. Weindl59, M. J. Weiss54, J. Weldert61, C. Wendt72, J. Werthebach72, B. J. Whelan87, N. Whitehorn101, K. Wiebe61, C. H. Wiebusch57, L. Wille72, D. R. Williams93, L. Wills94, M. Wolf85, J. Wood72, T. R. Wood86, K. Woschnagg62, G. Wrede55, D. L. Xu72, X. W. Xu83, Y. Xu92, J. P. Yanez86, G. Yodh60, S. Yoshida89, T. Yuan72, M. Zöcklein57, and (IceCube Collaboration), Published 2020 April 1 • The relative contribution Cj(δ, Φ) for each sample j, defined as the ratio of the expected mean number of signal events for the given sample to that for all samples, {C}^{j}={N}^{j}/{\sum }_{i=1}^{7}{N}^{i}, depends on the expected flux from the source Φ and decl. Indeed, the surroundings of this kind of black hole are highly plausible acceleration sites of very-high-energy cosmic rays, and therefore are possible sources of cosmic neutrinos (Bai et al. An Asymmetrically Substituted Aliphatic Bis-Dithiolene Mono-Oxido Molybdenum(IV) Complex With Ester and Alcohol Functions as Structural and Functional Active Site Model of Molybdoenzymes. CN Salt. In addition, special focus is given to the region around the Galactic Center, whereby a dedicated search at the location of SgrA* is performed, and to the location of the supernova remnant RXJ 1713.7-3946. Mediterranean Institute of Oceanography (MIO), Aix-Marseille University, F-13288, Marseille, Cedex 9, France, 39 Neutrinos are stable, neutral, and weakly interacting particles and, in contrast to cosmic rays, they are not deflected by magnetic fields. δ. Synthesis, characterization, and spectroscopy of model molybdopterin complexes. INFN—Laboratori Nazionali del Sud (LNS), Via S. Sofia 62, I-95123 Catania, Italy, 12 Notes. The most significant source of the list is HESSJ1023-575, a TeV γ-ray source coincident with the young stellar cluster Westerlund 2 (Aharonian 2007), with a pretrial p-value of 0.79%. 2006; Aartsen et al. PGC2018-096663-B-C41, -A-C42, -B-C43, -B-C44) (MCIU/FEDER), Severo Ochoa Centre of Excellence and MultiDark Consolider (MCIU), Junta de Andalucía (ref. In Section 3, the samples employed in the searches are described. As no significant evidence of cosmic neutrinos was observed, upper limits were derived. 7,-11\buildrel{\circ}\over{.} of Physics and Astronomy, Uppsala University, Box 516, SE-75120 Uppsala, Sweden, 72 Dioxidomolybdenum(VI) complexes chelated with N4-(3-methoxyphenyl)thiosemicarbazone as molybdenum(IV) precursors in oxygen atom transfer process and oxidation of styrene. 2017b) neutrino telescopes collected during nine (Adrian-Martinez et al. Structural, electrochemical and oxygen atom transfer properties of a molybdenum selenoether complex [Mo2O4(OC3H6SeC3H6O)2] and its thioether analogue [Mo2O4(OC3H6SC3H6O)2]. Necessity of fine tuning in Mo(iv) bis(dithiolene) complexes to warrant nitrate reduction. Dept. Dots (...) in the fitted number of source events, spectral index and pretrial p-value indicate sources with null observations ({\hat{n}}_{{\rm{s}}}=0.001). of Physics and Astronomy, University of Alaska Anchorage, 3211 Providence Dr., Anchorage, AK 99508, USA, 99 }/{{\rm{\Phi }}}_{0}, and ratio of the upper limit to the assumed source flux, {{\rm{\Phi }}}_{\mathrm{UL}}^{90 \% {\rm{C}}.{\rm{L}}. In the third one, the directions of a predefined list of known sources that are potential neutrino emitters are investigated. Dept. Generation of bis(dithiolene)dioxomolybdenum(vi) complexes from bis(dithiolene)monooxomolybdenum(iv) complexes by proton-coupled electron transfer in aqueous media. Proceedings, José Neuman de Souza, Petre Dini, Pascal Lorenz (Eds. ), Lecture Notes in Computer Science, Vol. The charged particles are produced in neutrino interactions with the target medium, inside or near the instrumented volume.
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