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1. Borexino’s search for low-energy neutrinos associated with gravitational wave events from GWTC-3 database

Author

D. Basilico, G. Bellini, J. Benziger, R. Biondi, B. Caccianiga, F. Calaprice, A. Caminata, A. Chepurnov, D. D’Angelo, A. Derbin, A. Di Giacinto, V. Di Marcello, X. F. Ding, A. Di Ludovico, L. Di Noto, I. Drachnev, D. Franco, C. Galbiati, C. Ghiano, M. Giammarchi, A. Goretti, M. Gromov, D. Guffanti, Aldo Ianni, Andrea Ianni, A. Jany, V. Kobychev, G. Korga, S. Kumaran, M. Laubenstein, E. Litvinovich, P. Lombardi, I. Lomskaya, L. Ludhova, I. Machulin, J. Martyn, E. Meroni, L. Miramonti, M. Misiaszek, V. Muratova, R. Nugmanov, L. Oberauer, V. Orekhov, F. Ortica, M. Pallavicini, L. Pelicci, Ö. Penek, L. Pietrofaccia, N. Pilipenko, A. Pocar, G. Raikov, M. T. Ranalli, G. Ranucci, A. Re, N. Rossi, S. Schönert, D. Semenov, G. Settanta, M. Skorokhvatov, A. Singhal, O. Smirnov, A. Sotnikov, R. Tartaglia, G. Testera, E. Unzhakov, A. Vishneva, R. B. Vogelaar, F. von Feilitzsch, M. Wojcik, M. Wurm, S. Zavatarelli, K. Zuber, and G. Zuzel

Subjects
Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract

Abstract The search for neutrino events in correlation with gravitational wave (GW) events for three observing runs (O1, O2 and O3) from 09/2015 to 03/2020 has been performed using the Borexino data-set of the same period. We have searched for signals of neutrino-electron scattering and inverse beta-decay (IBD) within a time window of $$\pm \, 1000$$ ± 1000 s centered at the detection moment of a particular GW event. The search was done with three visible energy thresholds of 0.25, 0.8 and 3.0 MeV. Two types of incoming neutrino spectra were considered: the mono-energetic line and the supernova-like spectrum. GW candidates originated by merging binaries of black holes (BHBH), neutron stars (NSNS) and neutron star and black hole (NSBH) were analyzed separately. Additionally, the subset of most intensive BHBH mergers at closer distances and with larger radiative mass than the rest was considered. In total, follow-ups of 74 out of 93 gravitational waves reported in the GWTC-3 catalog were analyzed and no statistically significant excess over the background was observed. As a result, the strongest upper limits on GW-associated neutrino and antineutrino fluences for all flavors ( $$\nu _e, \nu _\mu , \nu _\tau $$ ν e , ν μ , ν τ ) at the level $$10^9{-}10^{15}~\textrm{cm}^{-2}\,\textrm{GW}^{-1}$$ 10 9 - 10 15 cm - 2 GW - 1 have been obtained in the 0.5–5 MeV neutrino energy range.

Published
2023
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2. Search for low-energy signals from fast radio bursts with the Borexino detector

Author

S. Appel, Z. Bagdasarian, D. Basilico, G. Bellini, J. Benziger, R. Biondi, B. Caccianiga, F. Calaprice, A. Caminata, A. Chepurnov, D. D’Angelo, A. Derbin, A. Di Giacinto, V. Di Marcello, X. F. Ding, A. Di Ludovico, L. Di Noto, I. Drachnev, D. Franco, C. Galbiati, C. Ghiano, M. Giammarchi, A. Goretti, A. S. Göttel, M. Gromov, D. Guffanti, Aldo Ianni, Andrea Ianni, A. Jany, V. Kobychev, G. Korga, S. Kumaran, M. Laubenstein, E. Litvinovich, P. Lombardi, I. Lomskaya, L. Ludhova, G. Lukyanchenko, I. Machulin, J. Martyn, E. Meroni, L. Miramonti, M. Misiaszek, V. Muratova, R. Nugmanov, L. Oberauer, V. Orekhov, F. Ortica, M. Pallavicini, L. Pelicci, Ö. Penek, L. Pietrofaccia, N. Pilipenko, A. Pocar, G. Raikov, M. T. Ranalli, G. Ranucci, A. Razeto, A. Re, M. Redchuk, N. Rossi, S. Schönert, D. Semenov, G. Settanta, M. Skorokhvatov, A. Singhal, O. Smirnov, A. Sotnikov, R. Tartaglia, G. Testera, E. Unzhakov, A. Vishneva, R. B. Vogelaar, F. von Feilitzsch, M. Wojcik, M. Wurm, S. Zavatarelli, I. Zhutikov, K. Zuber, G. Zuzel, and Borexino Collaboration

Subjects
Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract

Abstract The search for neutrino events in correlation with 42 most intense fast radio bursts (FRBs) has been performed using the Borexino dataset from 05/2007 to 06/2021. We have searched for signals with visible energies above 250 keV within a time window of $$\pm \, 1000$$ ± 1000 s corresponding to detection time of a particular FRB. We also applied an alternative approach based on searching for specific shapes of neutrino-electron scattering spectra in the full exposure data of the Borexino detector. In particular, two incoming neutrino spectra were considered: the monoenergetic line and the spectrum expected from supernovae. The same spectra were considered for electron antineutrinos detected through inverse beta-decay reaction. No statistically significant excess over the background was observed. As a result, the strongest upper limits on FRB-associated neutrino fluences of all flavors have been obtained in the 0.5–50 MeV neutrino energy range.

Published
2022
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3. Identification of the cosmogenic $$^{11}$$ 11 C background in large volumes of liquid scintillators with Borexino

Author

M. Agostini, K. Altenmüller, S. Appel, V. Atroshchenko, Z. Bagdasarian, D. Basilico, G. Bellini, J. Benziger, R. Biondi, D. Bravo, B. Caccianiga, F. Calaprice, A. Caminata, P. Cavalcante, A. Chepurnov, D. D’Angelo, S. Davini, A. Derbin, A. Di ZGiacintio, V. Di Marcello, X. F. Ding, A. Di Ludovico, L. Di Noto, I. Drachnev, A. Formozov, D. Franco, C. Galbiati, C. Ghiano, M. Giammarchi, A. Goretti, A. S. Göttel, M. Gromov, D. Guffanti, Aldo Ianni, Andrea Ianni, A. Jany, D. Jeschke, V. Kobychev, G. Korga, S. Kumaran, M. Laubenstein, E. Litvinovich, P. Lombardi, I. Lomskaya, L. Ludhova, G. Lukyanchenko, L. Lukyanchenko, I. Machulin, J. Martyn, E. Meroni, M. Meyer, L. Miramonti, M. Misiaszek, V. Muratova, B. Neumair, M. Nieslony, R. Nugmanov, L. Oberauer, V. Orekhov, F. Ortica, M. Pallavicini, L. Papp, L. Pelicci, Ö. Penek, L. Pietrofaccia, N. Pilipenko, A. Pocar, A. Porcelli, G. Raikov, M. T. Ranalli, G. Ranucci, A. Razeto, A. Re, M. Redchuk, A. Romani, N. Rossi, S. Schönert, D. Semenov, G. Settanta, M. Skorokhvatov, A. Singhal, O. Smirnov, A. Sotnikov, Y. Suvorov, R. Tartaglia, G. Testera, J. Thurn, E. Unzhakov, A. Vishneva, R. B. Vogelaar, F. von Feilitzsch, M. Wojcik, M. Wurm, S. Zavatarelli, K. Zuber, and G. Zuzel

Subjects
Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract

Abstract Cosmogenic radio-nuclei are an important source of background for low-energy neutrino experiments. In Borexino, cosmogenic $$^{11}$$ 11 C decays outnumber solar pep and CNO neutrino events by about ten to one. In order to extract the flux of these two neutrino species, a highly efficient identification of this background is mandatory. We present here the details of the most consolidated strategy, used throughout Borexino solar neutrino measurements. It hinges upon finding the space-time correlations between $$^{11}$$ 11 C decays, the preceding parent muons and the accompanying neutrons. This article describes the working principles and evaluates the performance of this Three-Fold Coincidence (TFC) technique in its two current implementations: a hard-cut and a likelihood-based approach. Both show stable performances throughout Borexino Phases II (2012–2016) and III (2016–2020) data sets, with a $$^{11}$$ 11 C tagging efficiency of $$\sim 90$$ ∼ 90 % and $$\sim $$ ∼ 63–66 % of the exposure surviving the tagging. We present also a novel technique that targets specifically $$^{11}$$ 11 C produced in high-multiplicity during major spallation events. Such $$^{11}$$ 11 C appear as a burst of events, whose space-time correlation can be exploited. Burst identification can be combined with the TFC to obtain about the same tagging efficiency of $$\sim 90\%$$ ∼ 90 % but with a higher fraction of the exposure surviving, in the range of $$\sim $$ ∼ 66–68 %.

Published
2021
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4. Constraints on flavor-diagonal non-standard neutrino interactions from Borexino Phase-II

Author

The Borexino collaboration, S. K. Agarwalla, M. Agostini, K. Altenmüller, S. Appel, V. Atroshchenko, Z. Bagdasarian, D. Basilico, G. Bellini, J. Benziger, D. Bick, G. Bonfini, D. Bravo, B. Caccianiga, F. Calaprice, A. Caminata, L. Cappelli, P. Cavalcante, F. Cavanna, A. Chepurnov, K. Choi, D. D’Angelo, S. Davini, A. Derbin, A. Di Giacinto, V. Di Marcello, X. F. Ding, A. Di Ludovico, L. Di Noto, I. Drachnev, K. Fomenko, A. Formozov, D. Franco, F. Gabriele, C. Galbiati, M. Gschwender, C. Ghiano, M. Giammarchi, A. Goretti, M. Gromov, D. Guffanti, C. Hagner, E. Hungerford, Aldo Ianni, Andrea Ianni, A. Jany, D. Jeschke, S. Kumaran, V. Kobychev, G. Korga, T. Lachenmaier, M. Laubenstein, E. Litvinovich, P. Lombardi, L. Ludhova, G. Lukyanchenko, L. Lukyanchenko, I. Machulin, G. Manuzio, S. Marcocci, J. Maricic, J. Martyn, E. Meroni, M. Meyer, L. Miramonti, M. Misiaszek, V. Muratova, B. Neumair, M. Nieslony, L. Oberauer, V. Orekhov, F. Ortica, M. Pallavicini, L. Papp, Ö. Penek, L. Pietrofaccia, N. Pilipenko, A. Pocar, G. Raikov, G. Ranucci, A. Razeto, A. Re, M. Redchuk, A. Romani, N. Rossi, S. Rottenanger, S. Schönert, D. Semenov, M. Skorokhvatov, O. Smirnov, A. Sotnikov, C. Sun, Y. Suvorov, T. Takeuchi, R. Tartaglia, G. Testera, J. Thurn, E. Unzhakov, A. Vishneva, R. B. Vogelaar, F. von Feilitzsch, M. Wojcik, M. Wurm, O. Zaimidoroga, S. Zavatarelli, K. Zuber, and G. Zuzel

Subjects
Neutrino Physics, Beyond Standard Model, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract

Abstract The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-ν e survival probability P ee (E), and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI’s) which modify the chiral couplings and P ee (E). In this paper, we search for such NSI’s, in particular, flavor-diagonal neutral current interactions that modify the ν e e and ν τ e couplings using Borexino Phase II data. Standard Solar Model predictions of the solar neutrino fluxes for both high- and low-metallicity assumptions are considered. No indication of new physics is found at the level of sensitivity of the detector and constraints on the parameters of the NSI’s are placed. In addition, with the same dataset the value of sin2 θ W is obtained with a precision comparable to that achieved in reactor antineutrino experiments .

Published
2020
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5. Psychological support in postoperative pain management in patients with maxillofacial fractures

Author

D. Semenov

Subjects
psychological support, postoperative pain, maxillofacial fractures, Education, Sports, GV557-1198.995, Medicine
Abstract

Relevance. Psychological distress in persons with maxillofacial area fractures are not sufficiently developed in key of their influence on postoperative pain intensity, patients interpersonal sensitivity and emotional reactions. In the context of maxillofacial reconstructive surgery the psychological support of patients is promising direction to improve the condition of patients in postoperative period. The aim: to determine the effect of psychological support on the intensity and additional characteristics of postoperative pain in patients with maxillofacial fractures. Materials and metods. 120 patients with maxillofacial area fractures, undergoing reconstructive surgery at Municipal Clinical Hospital of Emergency and Rapid Care (Zaporizhzhya, Ukraine) were examined. The study was performed on 2 parallel groups, by 60 patients in each. Patients of the main group underwent original model of psychological support and standard postoperative treatment, patients of control group underwent only standard postoperative treatment. Clinical, radiological, psychological and statistical methods were used. Results. The normalization of patient’s psychological response to postoperative pain and rational perception of physical discomfort were found. Conclusion. The original model of psychological support in the postoperative period of reconstructive surgical interventions for maxillofacial fractures reduces the subjective intensity of postoperative pain among the contingent of patients.

Published
2019

6. First results from the DarkSide-50 dark matter experiment at Laboratori Nazionali del Gran Sasso

Author

P. Agnes, T. Alexander, A. Alton, K. Arisaka, H.O. Back, B. Baldin, K. Biery, G. Bonfini, M. Bossa, A. Brigatti, J. Brodsky, F. Budano, L. Cadonati, F. Calaprice, N. Canci, A. Candela, H. Cao, M. Cariello, P. Cavalcante, A. Chavarria, A. Chepurnov, A.G. Cocco, L. Crippa, D. D'Angelo, M. D'Incecco, S. Davini, M. De Deo, A. Derbin, A. Devoto, F. Di Eusanio, G. Di Pietro, E. Edkins, A. Empl, A. Fan, G. Fiorillo, K. Fomenko, G. Forster, D. Franco, F. Gabriele, C. Galbiati, A. Goretti, L. Grandi, M. Gromov, M.Y. Guan, Y. Guardincerri, B. Hackett, K. Herner, E.V. Hungerford, Al. Ianni, An. Ianni, C. Jollet, K. Keeter, C. Kendziora, S. Kidner, V. Kobychev, G. Koh, D. Korablev, G. Korga, A. Kurlej, P.X. Li, B. Loer, P. Lombardi, C. Love, L. Ludhova, S. Luitz, Y.Q. Ma, I. Machulin, A. Mandarano, S. Mari, J. Maricic, L. Marini, C.J. Martoff, A. Meregaglia, E. Meroni, P.D. Meyers, R. Milincic, D. Montanari, A. Monte, M. Montuschi, M.E. Monzani, P. Mosteiro, B. Mount, V. Muratova, P. Musico, A. Nelson, S. Odrowski, M. Okounkova, M. Orsini, F. Ortica, L. Pagani, M. Pallavicini, E. Pantic, L. Papp, S. Parmeggiano, R. Parsells, K. Pelczar, N. Pelliccia, S. Perasso, A. Pocar, S. Pordes, D. Pugachev, H. Qian, K. Randle, G. Ranucci, A. Razeto, B. Reinhold, A. Renshaw, A. Romani, B. Rossi, N. Rossi, S.D. Rountree, D. Sablone, P. Saggese, R. Saldanha, W. Sands, S. Sangiorgio, E. Segreto, D. Semenov, E. Shields, M. Skorokhvatov, O. Smirnov, A. Sotnikov, C. Stanford, Y. Suvorov, R. Tartaglia, J. Tatarowicz, G. Testera, A. Tonazzo, E. Unzhakov, R.B. Vogelaar, M. Wada, S. Walker, H. Wang, Y. Wang, A. Watson, S. Westerdale, M. Wojcik, A. Wright, X. Xiang, J. Xu, C.G. Yang, J. Yoo, S. Zavatarelli, A. Zec, C. Zhu, and G. Zuzel

Subjects
Physics, QC1-999
Abstract

We report the first results of DarkSide-50, a direct search for dark matter operating in the underground Laboratori Nazionali del Gran Sasso (LNGS) and searching for the rare nuclear recoils possibly induced by weakly interacting massive particles (WIMPs). The dark matter detector is a Liquid Argon Time Projection Chamber with a (46.4±0.7) kg active mass, operated inside a 30 t organic liquid scintillator neutron veto, which is in turn installed at the center of a 1 kt water Cherenkov veto for the residual flux of cosmic rays. We report here the null results of a dark matter search for a (1422±67) kgd exposure with an atmospheric argon fill. This is the most sensitive dark matter search performed with an argon target, corresponding to a 90% CL upper limit on the WIMP-nucleon spin-independent cross section of 6.1×10−44 cm2 for a WIMP mass of 100 Gev/c2. Keywords: Dark matter, WIMP, Noble liquid detectors, Low-background detectors, Liquid scintillators

Published
2015
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7. The DarkSide Multiton Detector for the Direct Dark Matter Search

Author

C. E. Aalseth, P. Agnes, A. Alton, K. Arisaka, D. M. Asner, H. O. Back, B. Baldin, K. Biery, G. Bonfini, M. Bossa, A. Brigatti, J. Brodsky, F. Budano, L. Cadonati, M. Cadoni, F. Calaprice, N. Canci, A. Candela, H. Cao, M. Cariello, P. Cavalcante, A. Chepurnov, A. G. Cocco, C. Condon, L. Crippa, D. D’Angelo, M. D’Incecco, S. Davini, M. De Deo, A. Derbin, A. Devoto, F. Di Eusanio, E. Edkins, A. Empl, A. Fan, G. Fiorillo, K. Fomenko, G. Forster, M. Foxe, D. Franco, F. Gabriele, C. Galbiati, A. Goretti, L. Grandi, M. Gromov, M. Y. Guan, Y. Guardincerri, B. Hackett, K. Herner, A. Hime, P. Humble, E. Hungerford, Al. Ianni, An. Ianni, D. E. Jaffe, C. Jollet, K. Keeter, C. Kendziora, S. Kidner, V. Kobychev, G. Koh, D. Korablev, G. Korga, A. Kurlej, P. X. Li, M. Lissia, P. Lombardi, L. Ludhova, S. Luitz, G. Lukyachenko, Y. Q. Ma, I. Machulin, A. Mandarano, S. M. Mari, J. Maricic, L. Marini, D. Markov, J. Martoff, A. Meregaglia, E. Meroni, P. D. Meyers, T. Miletic, R. Milincic, M. Montuschi, M. E. Monzani, P. Mosteiro, B. Mount, V. Muratova, P. Musico, D. Montanari, A. Nelson, S. Odrowski, A. Odrzywolek, J. L. Orrell, M. Orsini, F. Ortica, L. Pagani, M. Pallavicini, E. Pantic, S. Parmeggiano, B. Parsells, K. Pelczar, N. Pelliccia, S. Perasso, L. Perasso, A. Pocar, S. Pordes, D. Pugachev, H. Qian, K. Randle, G. Ranucci, A. Razeto, K. Recine, B. Reinhold, A. Renshaw, A. Romani, N. Rossi, B. Rossi, S. D. Rountree, D. Sablone, P. Saggese, R. Saldanha, W. Sands, S. Sangiorgio, E. Segreto, D. Semenov, E. Shields, M. Skorokhvatov, M. Smallcomb, O. Smirnov, A. Sotnikov, Y. Suvurov, R. Tartaglia, J. Tatarowicz, G. Testera, A. Tonazzo, E. Unzhakov, R. B. Vogelaar, M. Wada, S. E. Walker, H. Wang, Y. Wang, A. W. Watson, S. Westerdale, R. Williams, M. Wojcik, J. Xu, C. G. Yang, J. Yoo, B. Yu, S. Zavatarelli, W. L. Zhong, and G. Zuzel

Subjects
Physics, QC1-999
Abstract

Although the existence of dark matter is supported by many evidences, based on astrophysical measurements, its nature is still completely unknown. One major candidate is represented by weakly interacting massive particles (WIMPs), which could in principle be detected through their collisions with ordinary nuclei in a sensitive target, producing observable low-energy (

Published
2015
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8. Prognosis of Alzheimer’s Disease Using Quantitative Mass Spectrometry of Human Blood Plasma Proteins and Machine Learning

Author

Alexey S. Kononikhin, Natalia V. Zakharova, Savva D. Semenov, Anna E. Bugrova, Alexander G. Brzhozovskiy, Maria I. Indeykina, Yana B. Fedorova, Igor V. Kolykhalov, Polina A. Strelnikova, Anna Yu. Ikonnikova, Dmitry A. Gryadunov, Svetlana I. Gavrilova, and Evgeny N. Nikolaev

Subjects
Proteomics, Organic Chemistry, General Medicine, Blood Proteins, Catalysis, Mass Spectrometry, Computer Science Applications, Inorganic Chemistry, Machine Learning, Alzheimer Disease, Humans, Cognitive Dysfunction, Physical and Theoretical Chemistry, Molecular Biology, targeted proteomics, mass spectrometry, Alzheimer’s disease, multiple reaction monitoring, machine learning, Spectroscopy, Biomarkers, Aged
Abstract

Early recognition of the risk of Alzheimer’s disease (AD) onset is a global challenge that requires the development of reliable and affordable screening methods for wide-scale application. Proteomic studies of blood plasma are of particular relevance; however, the currently proposed differentiating markers are poorly consistent. The targeted quantitative multiple reaction monitoring (MRM) assay of the reported candidate biomarkers (CBs) can contribute to the creation of a consistent marker panel. An MRM-MS analysis of 149 nondepleted EDTA–plasma samples (MHRC, Russia) of patients with AD (n = 47), mild cognitive impairment (MCI, n = 36), vascular dementia (n = 8), frontotemporal dementia (n = 15), and an elderly control group (n = 43) was performed using the BAK 125 kit (MRM Proteomics Inc., Canada). Statistical analysis revealed a significant decrease in the levels of afamin, apolipoprotein E, biotinidase, and serum paraoxonase/arylesterase 1 associated with AD. Different training algorithms for machine learning were performed to identify the protein panels and build corresponding classifiers for the AD prognosis. Machine learning revealed 31 proteins that are important for AD differentiation and mostly include reported earlier CBs. The best-performing classifiers reached 80% accuracy, 79.4% sensitivity and 83.6% specificity and were able to assess the risk of developing AD over the next 3 years for patients with MCI. Overall, this study demonstrates the high potential of the MRM approach combined with machine learning to confirm the significance of previously identified CBs and to propose consistent protein marker panels.

Published
2022
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9. Phonon heat capacity and self-heating normal domains in NbTiN nanostrips

Author

M Sidorova, A D Semenov, H-W Hübers, S Gyger, and S Steinhauer

Subjects
Physics - Instrumentation and Detectors, superconducting nanostrips, phonon spectrum, Condensed Matter - Superconductivity, Metals and Alloys, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), phonon heat capacity, self-heating process, 530 Physik, Condensed Matter Physics, Condensed Matter::Mesoscopic Systems and Quantum Hall Effect, Superconductivity (cond-mat.supr-con), Condensed Matter::Materials Science, granular films, Condensed Matter::Superconductivity, Materials Chemistry, Ceramics and Composites, ddc:530, Electrical and Electronic Engineering, low temperatures
Abstract

Self-heating normal domains in thin superconducting NbTiN nanostrips with the granular structure were characterized via steady-state hysteretic current–voltage characteristics measured at different substrate temperatures. The temperature dependence and the magnitude of the current, which sustains a domain in equilibrium at different voltages, can only be explained with a phonon heat capacity noticeably less than expected for 3D Debye phonons. This reduced heat capacity coincides with the value obtained earlier from magnetoconductance and photoresponse studies of the same films. The rate of heat flow from electrons at a temperature T e to phonons in the substrate at a temperature T B is proportional to ( T e p − T B p ) with the exponent p ≈ 3, which differs from the exponents for heat flows mediated by the electron–phonon interaction or by escaping of 3D Debye phonons via the film/substrate interface. We attribute both findings to the effect of grains on the phonon spectrum of thin NbTiN films. Our findings are significant for understanding the thermal transport in superconducting devices exploiting thin granular films.

Published
2022

10. Planning Simulation Experiments in the Tasks of Studying the Operational Strategies of Container Terminals

Author

Hannu Oja, Alexander Kuznetsov, Anton D. Semenov, and Alexander Kirichenko

Subjects
allocation of containers, sea cargo front (scf), container yard (cy), Computer science, stacking of containers, lcsh:TC601-791, Ocean Engineering, Transportation, Oceanography, simulation study, lcsh:HE1-9990, land cargo front (lcf), container terminal, lcsh:Canals and inland navigation. Waterways, Container (abstract data type), Systems engineering, lcsh:Transportation and communications, operational strategy
Abstract

There is a lot of scientific papers that consider the efficiency of different container yard’s handling strategies. The methods of assessment vary from abstract mathematical calculations to aposterioric collection and analyses of practical data. This article deals with a new way of stacking strategy’s estimation. It postulates that investigations based on the extrapolation of existing strategies cannot be reliable due to rapid changes in terminals’ environment and restricted amount of data that can be collected within limited periods of the strategies’ application. The hypothesis of the study is that the only method that could provide robust comparative study of container stacking strategies is the simulation modelling. In the same time, any model is only a tool of analyses. The synthesis could be provided only by massive iterations of single simulation experiments with controlled searching procedure in the space of parameters. Consequently, the stress of the simulation study should be put not on the model itself, but on the way how to use it, i.e. on the experiments planning. Only a rationally constructed machine of simulation scenario generation could provide adequate and statistically reliable results. In order to demonstrate the importance of this ‘task setting’ machine, two example strategies are selected for comparison: (1) allocation of containers to slots with the minimum height and (2) stacking of containers in accordance with expected dwell time. It also shows that the objective function has a great impact on the optimal strategy implementation. In the study described in the paper the number of moves requested to select a container is opted as an optimization criterion.

Published
2020

11. Tracing episodic accretion with NOEMA: FU Orionis-type stars and their millimeter environment

Author

O. Fehér, Á. Kóspál, F. Cruz-Saenz de Miera, P. Ábrahám, M.R. Hogerheijde, Ch. Brinch, and D. Semenov

Abstract

The earliest phases of star formation are characterised by intense mass accretion from the circumstellar disk to the central star. One group of lowmass young stellar objects, FU Orionis-type stars (FUors) exhibit accretion rate peaks accompanied by bright eruptions in the optical and infrared regime. The occurance of these outbursts might solve the luminosity problem of protostars, play a key role in accumulating the final stellar mass, and have a significant effiect on the parameters of the envelope and the disk. We are performing a systematic investigation of FUors with millimeter interferometry using NOEMA and ALMA to study the outburst events and examine whether FUors represent normal young stars in exceptional times or are unusual objects. The targeted FUors show very diverse circumstellar morphologies with envelope parameters similar to those of both Class I and Class II systems, but their disks are more massive and more compact than T Tauri disks. To shed light onto the process of disk-formation, accretion, and to what role FUors play in low-mass starformation, we require the identification and light curve monitoring of as many of these stars as possible, together with the multi-wavelength and multi-scale mapping of their circumstellar environment.

Published
2022

12. Evaluation of Sinking Effect in Container Stack

Author

Alexander Kuznetsov, Alexander Kirichenko, and Anton D. Semenov

Subjects
sinking effect, containerization, Mechanical engineering, lcsh:TC601-791, Ocean Engineering, Transportation, container cargo-handling system, Oceanography, container, lcsh:HE1-9990, container stack, container logistics, container terminal, Stack (abstract data type), lcsh:Canals and inland navigation. Waterways, Container (abstract data type), Environmental science, lcsh:Transportation and communications, teu
Abstract

The container yard is the key element of any modern container terminal. The huge amount of boxes dwelling on the operational areas of the terminals could occupy a lot of space, since one-time storage capacity of the container mega terminal handling over one million TEUs annually is something around 20 000 TEUs. The ecological pressure imposed on modern container terminal does not permit to allocate for this storage large land areas, thus forcing the box stacks grow high. The selection of the individual boxes becomes a complex and time-consuming procedure, demanding a lot of technological resources and deteriorating the service quality. The predicted combinatorial growth of redundant moves needed to clear the access to the individual container is aggravated by the well-known and widely discussed ‘sinking effect’, when containers arrived earlier are gradually covered by the ones arriving afterwards. While the random selection could be adequately assessed by combinatorial methods, the ‘sinking effect’ allows neither intuitive consideration, nor any traditional mathematical means. The only practical way to treat this problem today is in simulation, but the simulation itself causes yet another problem: the problem of model adequacy. This study deals with one possible approach to the problem designated to prove its validity and adequacy, without which the simulation has naught gnoseological value.

Published
2020

13. Box Selectivity in Different Container Cargo-handling Systems

Author

Alexander Kirichenko, Alexander Kuznetsov, and Anton D. Semenov

Subjects
business.industry, simulation model, lcsh:TC601-791, Ocean Engineering, Transportation, container cargo-handling system, Oceanography, container, artificial intelligence (ai), cargo handling system, lcsh:HE1-9990, theoretical selectivity, cargo handling, lcsh:Canals and inland navigation. Waterways, Container (abstract data type), Environmental science, box selectivity, lcsh:Transportation and communications, Selectivity, Process engineering, business
Abstract

The box selectivity in operational stack of container terminal is a quite common and long studied question. The pure random choice is governed by the theory of probability offering some combinatorial estimations. The introduction of operational rules like import/export separation, storage by shipping lines, sorting by rail or truck transportation etc., as well as the most notorious ‘sinking’ effect, i.e. covering of boxes arrived earlier by next cargo parties – all these blur the clear algebraiс picture and lead to appearance of many heuristic outlooks of the problem. A new impetus to this problem in last decades was given by the rapid development of IT, AI and simulation techniques. There are quite many examples of the models described in the scientific publication reflecting many real and arbitrary terminals, which embed very advanced and complicated mechanisms reflecting selected features and strategies. Unfortunately, these models usually are created ad hoc, with some pragmatic objectives and under the demand of closest possible proximity to the simulating objects. There are much less models designated to pure scientific study of the deep inner mechanisms responsible for the primal behavior of the operating container stack, enabling to introduce step by step new rules and restrictions, providing regular proving of every next stage’s adequacy and easy to use. This paper describes one attempt of this kind to create a new theoretical tool to put into the regular toolkit of the container terminal designer. The study starts with mathematical (combinatorial) considerations, proceeds with some restrictions caused by physical and technological characteristics, and ends up with the simulation model, which adequacy is confirmed by practical results.

Published
2019

14. Magnetodispersion of Two-Dimensional Plasmon Polaritons

Author

A. A. Zabolotnykh, I. V. Kukushkin, N. D. Semenov, V. M. Muravev, and I. V. Andreev

Subjects
Physics, Condensed matter physics, Condensed Matter - Mesoscale and Nanoscale Physics, Mesoscale and Nanoscale Physics (cond-mat.mes-hall), Polariton, FOS: Physical sciences, Physics::Optics, Plasmon
Abstract

We have investigated the spectrum of two-dimensional (2D) plasmon polaritons over the full range of magnetic fields. In our study, we investigate a disk-shaped two-dimensional electron system (2DES) with a metallic gate on the backside of the substrate. Importantly, we show that 2D plasmon polaritons hybridize with the TM$_0$ photonic mode of a dielectric waveguide formed by a sample substrate. We have developed a theory for plasmon-polaritons in an infinite 2DES. We find the experimental data to be in good agreement with the developed theory., 7 pages, 4 figures

Published
2021

15. Physical and chemical structure of high-mass star-forming regions. Unraveling chemical complexity with CORE: the NOEMA large program

Author

Friedrich Wyrowski, Timea Csengeri, Th. Henning, H. Linz, S. Leurini, Pamela Klaassen, S. N. Longmore, Roberto Galván-Madrid, S. Suri, Siyi Feng, James Urquhart, Ralph E. Pudritz, Peter Schilke, C. Gieser, Vincent Piétu, J. M. Winters, D. Semenov, A. Ahmadi, Gary A. Fuller, Luke T. Maud, Thomas Peters, Stuart Lumsden, V. de Souza Magalhães, Álvaro Sánchez-Monge, Henrik Beuther, Qizhou Zhang, M. T. Beltrán, Rolf Kuiper, Aina Palau, Karl M. Menten, Luca Moscadelli, T. Möller, and Jérôme Pety

Subjects
Physics, Astrochemistry, 010504 meteorology & atmospheric sciences, Star formation, Stars: formation, Astrophysics - astrophysics of galaxies, Core sample, Astronomy and Astrophysics, Astrophysics, Physik (inkl. Astronomie), 01 natural sciences, Spectral line, ISM: molecules, Astrophysics - solar and stellar astrophysics, Stars, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Emission spectrum, Continuum (set theory), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract

Aims. Current star formation research centers the characterization of the physical and chemical properties of massive stars, which are in the process of formation, at the spatial resolution of individual high-mass cores. Methods. We use sub-arcsecond resolution (~0.′′4) observations with the NOrthern Extended Millimeter Array at 1.37 mm to study the dust emission and molecular gas of 18 high-mass star-forming regions. With distances in the range of 0.7−5.5 kpc, this corresponds to spatial scales down to 300−2300 au that are resolved by our observations. We combined the derived physical and chemical properties of individual cores in these regions to estimate their ages. The temperature structures of these regions are determined by fitting the H2CO and CH3CN line emission. The density profiles are inferred from the 1.37 mm continuum visibilities. The column densities of 11 different species are determined by fitting the emission lines with XCLASS. Results. Within the 18 observed regions, we identified 22 individual cores with associated 1.37 mm continuum emission and with a radially decreasing temperature profile. We find an average temperature power-law index of q = 0.4 ± 0.1 and an average density power-law index of p = 2.0 ± 0.2 on scales that are on the order of several 1000 au. Comparing these results with values of p derived from the literature presumes that the density profiles remain unchanged from clump to core scales. The column densities relative to N(C18O) between pairs of dense gas tracers show tight correlations. We applied the physical-chemical model MUlti Stage ChemicaL codE to the derived column densities of each core and find a mean chemical age of ~60 000 yr and an age spread of 20 000−100 000 yr. With this paper, we release all data products of the CORE project. Conclusions. The CORE sample reveals well-constrained density and temperature power-law distributions. Furthermore, we characterized a large variety in molecular richness that can be explained by an age spread that is then confirmed by our physical-chemical modeling. The hot molecular cores show the greatest number of emission lines, but we also find evolved cores at an evolutionary stage in which most molecules are destroyed and, thus, the spectra appear line-poor once again.

Published
2021

16. The Path to Fully Representational Theory of Mind: Conceptual, Executive, and Pragmatic Challenges

Author

Annelise Pesch, Andrei D. Semenov, and Stephanie M. Carlson

Subjects
media_common.quotation_subject, lcsh:BF1-990, Context (language use), 050105 experimental psychology, working memory, 03 medical and health sciences, false belief, 0302 clinical medicine, Theory of mind, Cognitive development, Psychology, 0501 psychology and cognitive sciences, Function (engineering), Relation (history of concept), General Psychology, Original Research, media_common, theory of mind, Working memory, 05 social sciences, Pragmatics, lcsh:Psychology, executive function, Mental representation, 030217 neurology & neurosurgery, Cognitive psychology, cognitive development
Abstract

Although an explicit Theory of Mind (ToM) has been found to develop around 4 years of age in Western societies, recent work showing that 4- and 5-year-olds fail modified versions of False Belief tasks as well as seemingly easier True Belief tasks calls into question the robustness of preschoolers’ belief understanding. Some have argued these findings illustrate children’s conceptual limitations in their understanding of belief that are masked by standard False Belief tasks. However, others claim these examples of children’s failure can be explained by pragmatics of the testing situation, rather than conceptual limitations. Given the documented relation between ToM and executive function, an unexamined possibility is that children’s failure can be explained by certain executive demands. In the current study, we examined the relation between typically developing 4- (n = 43) and 5-year-olds’ (n = 42) performance on traditional and modified False Belief tasks, True Belief tasks, and one component of executive functioning - working memory. We found that children performed worse on modified False Belief tasks and True Belief tasks compared to standard 2-option False Belief tasks, and that working memory was related to modified 3-option contents False Belief performance. These results suggest that a fully representational ToM, one that is stable in the context of increased conceptual, executive, and pragmatic demands, may develop later than traditional accounts have assumed.

Published
2020

17. Multi-wavelength modelling of the circumstellar environment of the massive proto-star AFGL 2591 VLA 3

Author

Huei-Ru Chen, Álvaro Sánchez-Monge, Th. Henning, Joseph C. Mottram, Melvin Hoare, C. Gieser, Rolf Kuiper, Frédérique Motte, Thomas Peters, F. A. Olguin, Aina Palau, A. Ahmadi, Henrik Beuther, Katharine G. Johnston, Pamela Klaassen, and D. Semenov

Subjects
Young stellar object, Astrophysics::High Energy Astrophysical Phenomena, Rotational symmetry, FOS: Physical sciences, Model parameters, Kinematics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Radiative transfer, Protostar, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Physik (inkl. Astronomie), Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow, Astrophysics::Earth and Planetary Astrophysics, Dust emission
Abstract

We have studied the dust density, temperature and velocity distributions of the archetypal massive young stellar object (MYSO) AFGL 2591. Given its high luminosity ($L=2 \times 10^5$ L$_\odot$) and distance ($d=3.3$ kpc), AFGL 2591 has one of the highest $\sqrt{L}/d$ ratio, giving better resolved dust emission than any other MYSO. As such, this paper provides a template on how to use resolved multi-wavelength data and radiative transfer to obtain a well-constrained 2-D axi-symmetric analytic rotating infall model. We show for the first time that the resolved dust continuum emission from Herschel 70 $��$m observations is extended along the outflow direction, whose origin is explained in part from warm dust in the outflow cavity walls. However, the model can only explain the kinematic features from CH$_3$CN observations with unrealistically low stellar masses ($, 34 pages, 22 figures, 15 tables, 4 appendices. Accepted for publication in MNRAS

Published
2020

18. Electron energy relaxation in disordered superconducting NbN films

Author

Andreas Schilling, A. D. Semenov, Mariia Sidorova, Natalia Kaurova, Maria Moshkova, Xiaofu Zhang, Gregory Goltsman, Heinz-Wilhelm Hübers, Michael Siegel, Ilya Charaev, Konstantin Ilin, and University of Zurich

Subjects
3104 Condensed Matter Physics, Materials science, phonon softening, Phonon, Mean free path, 530 Physics, electron relaxation, FOS: Physical sciences, 02 engineering and technology, 10192 Physics Institute, 01 natural sciences, Heat capacity, Superconductivity (cond-mat.supr-con), symbols.namesake, Condensed Matter::Materials Science, Condensed Matter::Superconductivity, 0103 physical sciences, Terahertz- und Laserspektroskopie, 010306 general physics, Debye model, electron dephasing, Superconductivity, Condensed matter physics, Scattering, Condensed Matter - Superconductivity, 2504 Electronic, Optical and Magnetic Materials, Atmospheric temperature range, 021001 nanoscience & nanotechnology, superconducting nanowire, Product (mathematics), electron-phonon interaction, disordered superconductors, symbols, 0210 nano-technology
Abstract

We report on the inelastic-scattering rate of electrons on phonons and relaxation of electron energy studied by means of magnetoconductance, and photoresponse, respectively, in a series of strongly disordered superconducting NbN films. The studied films with thicknesses in the range from 3 to 33 nm are characterized by different Ioffe-Regel parameters but an almost constant product q_Tl(q_T is the wave vector of thermal phonons and l is the elastic mean free path of electrons). In the temperature range 14-30 K, the electron-phonon scattering rates obey temperature dependencies close to the power law 1/\tau_{e-ph} \sim T^n with the exponents n = 3.2-3.8. We found that in this temperature range \tau_{e-ph} and n of studied films vary weakly with the thickness and square resistance. At 10 K electron-phonon scattering times are in the range 11.9-17.5 ps. The data extracted from magnetoconductance measurements were used to describe the experimental photoresponse with the two-temperature model. For thick films, the photoresponse is reasonably well described without fitting parameters, however, for thinner films, the fit requires a smaller heat capacity of phonons. We attribute this finding to the reduced density of phonon states in thin films at low temperatures. We also show that the estimated Debye temperature in the studied NbN films is noticeably smaller than in bulk material., Comment: 23 pages, 6 figures

Published
2020

19. Sensitivity of gas-grain chemical models to surface reaction barriers: Effect from a key carbon-insertion reaction, C + H$_2$ $\rightarrow$ CH$_2$

Author

Th. Henning, D. Semenov, Cornelia Jäger, Serge A. Krasnokutski, and M. Simončič

Subjects
Astrochemistry, Analytical chemistry, FOS: Physical sciences, chemistry.chemical_element, Context (language use), 02 engineering and technology, Astrophysics, 01 natural sciences, Methane, chemistry.chemical_compound, Insertion reaction, 0103 physical sciences, Molecule, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, chemistry.chemical_classification, Physics, Astronomy and Astrophysics, 021001 nanoscience & nanotechnology, Astrophysics - Astrophysics of Galaxies, 3. Good health, Hydrocarbon, chemistry, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Atomic carbon, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics, Carbon
Abstract

The feasibility of contemporary gas-grain astrochemical models depends on the availability of accurate kinetics data, in particular, for surface processes. We study the sensitivity of gas-grain chemical models to the energy barrier Ea of the important surface reaction between some of the most abundant species: C and H2 (surface C + surface H2 = surface CH2). We used the gas-grain code ALCHEMIC to model the time-dependent chemical evolution over a 2D grid of densities (nH: 10^{3} - 10^{12}cm^{-3}) and temperatures (T: 10 - 300 K), assuming UV-dark (Av = 20 mag) and partly UV-irradiated (Av = 3 mag) conditions that are typical of the dense interstellar medium. We considered two values for the energy barrier of the surface reaction, Ea = 2500 K (as originally implemented in the networks) and Ea = 0 K (as measured in the laboratory and computed by quantum chemistry simulations). We find that if the C + H2 = CH2 surface reaction is barrierless, a more rapid conversion of the surface carbon atoms into methane ice occurs. Overproduction of the CHn hydrocarbon ices affects the surface formation of more complex hydrocarbons, cyanides and nitriles, and CS-bearing species at low temperatures < 10-15 K. The surface hydrogenation of CO and hence the synthesis of complex (organic) molecules become affected as well. As a result, important species whose abundances may change by more than a factor of two at 1 Myr include atomic carbon, small mono-carbonic (C1) and di-carbonic (C2) hydrocarbons, CO2, CN, HCN, HNC, HNCO, CS, H2CO, H2CS, CH2CO, and CH3OH (in either gas and/or ice). The abundances of key species, CO, H2O, and N2 as well as O, HCO+, N2H+, NH3, NO, and most of the S-bearing molecules, remain almost unaffected. Further accurate laboratory measurements and quantum chemical calculations of the surface reaction barriers will be crucial to improve the accuracy of astrochemical models., Submitted to Astronomy & Astrophysics (A&A), 9 pages

Published
2020

20. Neural network identification of a nonlinear model of a high-pressure sodium lamp

Author

Anatolij D. Semenov, Anton V. Volkov, and Alena Yu. Shumkina

Subjects
Materials science, Neural network identification, law, Nonlinear model, Sodium-vapor lamp, TA1-2040, Biological system, Engineering (General). Civil engineering (General), law.invention
Abstract

The article is devoted to the identification of a high-pressure sodium lamp nonlinear model parameters based on neural network technologies. Identification was carried out using a dynamic neural network. The model had 17 parameters based on second order differential equations. As a result, out of 17 parameters, four were selected that accurately reflect the real picture of the model.

Published
2020

21. Ten years of cosmic muons observation with Borexino

Author

Davide D’Angelo, M. Agostini, K. Altenmüller, S. Appel, V. Atroshchenko, Z. Bagdasarian, D. Basilico, G. Bellini, J. Benziger, D. Bick, G. Bonfini, D. Bravo, B. Caccianiga, F. Calaprice, A. Caminata, L. Cappelli, P. Cavalcante, F. Cavanna, A. Chepurnov, K. Choi, D. D’Angelo, S. Davini, A. Derbin, A. Di Giacinto, V. Di Marcello, X.F. Ding, A. Di Ludovico, L. Di Noto, I. Drachnev, K. Fomenko, A. Formozov, D. Franco, F. Gabriele, C. Galbiati, M. Gschwender, C. Ghiano, M. Giammarchi, A. Goretti, M. Gromov, D. Guffanti, C. Hagner, E. Hungerford, Aldo Ianni, Andrea Ianni, A. Jany, D. Jeschke, S. Kumaran, V. Kobychev, G. Korga, T. Lachenmaier, M. Laubenstein, E. Litvinovich, P. Lombardi, I. Lomskaya, L. Ludhova, G. Lukyanchenko, L. Lukyanchenko, I. Machulin, G. Manuzio, S. Marcocci, J. Maricic, J. Martyn, E. Meroni, M. Meyer, L. Miramonti, M. Misiaszek, V. Muratova, B. Neumair, M. Nieslony, L. Oberauer, V. Orekhov, F. Ortica, M. Pallavicini, L. Papp, O. Penek, L. Pietrofaccia, N. Pilipenko, A. Pocar, G. Raikov, M.T. Ranalli, G. Ranucci, A. Razeto, A. Re, M. Redchuk, A. Romani, N. Rossi, S. Rottenanger, S. Schönert, D. Semenov, M. Skorokhvatov, O. Smirnov, A. Sotnikov, Y. Suvorov, R. Tartaglia, G. Testera, J. Thurn, E. Unzhakov, A. Vishneva, R.B. Vogelaar, F. von Feilitzsch, M. Wojcik, M. Wurm, O. Zaimidoroga, S. Zavatarelli, K. Zuber, and G. Zuzel

Subjects
Physics, History, Physics::Instrumentation and Detectors, precision measurement, flux [muon], pi, Astronomy, model [atmosphere], solar, Computer Science Applications, Education, Gran Sasso, modulation, correlation, high [energy], High Energy Physics::Experiment, Borexino, Cosmic muons, temperature [atmosphere], Nuclear Experiment
Abstract

The Borexino detector at Gran Sasso has now accumulated over ten years of continuous data which represent a magnificent opportunity to study the cosmic muon flux at a deep underground location. We present here a precision measurement of the flux and of the expected seasonal modulation. We present the correlation with the atmospheric temperature variations from global atmospheric models. We measure the correlation parameters and infer the kaon-to-pion ratio in the production of cosmic muons from high energy primaries. We also find evidence of a long term modulation that is not present in the atmospheric data and we investigate a possible positive correlation with the solar activity. Finally we observe a seasonal modulation of the production rate of cosmogenic neutrons that is in phase with the muon modulation but shows a surprisingly larger amplitude.

Published
2020

22. Updated geoneutrino measurement with Borexino

Author

S. Rottenanger, D. Franco, A. Caminata, B. Caccianiga, E. Unzhakov, I. Lomskaya, Andrea Ianni, L. Oberauer, M. Gschwender, I. Drachnev, K. Zuber, O. Zaimidoroga, V. Atroshchenko, D. Guffanti, O. Smirnov, C. Ghiano, R.B. Vogelaar, F. von Feilitzsch, A. Re, G. Bonfini, M. Wojcik, J. Martyn, G. Zuzel, B. Neumair, X.F. Ding, A. Razeto, K. Altenmüller, G. Manuzio, V. Di Marcello, V. Strati, F. Gabriele, M. Redchuk, D. Semenov, F. Mantovani, V. Orekhov, L. Miramonti, M. Vivier, M. Gromov, M. Nieslony, D. Jeschke, N. Rossi, A. Di Ludovico, D. Bick, A. Onillon, R. Tartaglia, Ö. Penek, C. Hagner, J. Thurn, M. Meyer, L. Cappelli, B. Ricci, S. Zavatarelli, L. Pietrofaccia, M. Montuschi, A. Pocar, E. Hungerford, G. Bellini, T. Lachenmaier, A. Romani, T. Lasserre, L. Papp, A. Goretti, D. Basilico, V. Muratova, A. Sotnikov, J. Maricic, S. Kumaran, C. Galbiati, M. Giammarchi, I. Machulin, Z. Bagdasarian, G. Korga, J. Benziger, M. Agostini, S. Marcocci, A. Derbin, S. Schöinert, M. Pallavicini, Y. Suvorov, F. Ortica, Livia Ludhova, M. Skorokhvatov, M. Misiaszek, G. Ranucci, S. Davini, S. Appel, V. Kobychev, M.T. Ranalli, A. Formozov, P. Lombardi, L. Lukyanchenko, M. Laubenstein, E. Meroni, A. Chepurnov, G. Fiorentini, G. Lukyanchenko, L. Di Noto, N. Pilipenko, E. Litvinovich, A. Di Giacinto, D. D'Angelo, D. Bravo, M. Wurm, Aldo Ianni, A. Vishneva, G. Raikov, F. Calaprice, G. Testera, F. Cavanna, L. Ludhova, P. Cavalcante, A. Jany, and K. Choi

Subjects
data analysis method, History, Particle physics, liquid [scintillation counter], Geoneutrino, Computer Science Applications, Education, geophysics [neutrino], statistics, Environmental science, Borexino, low [background], activity report, experimental results
Abstract

Borexino is a 280-ton liquid scintillator detector located at the Laboratori Nazionali del Gran Sasso (LNGS), Italy and is one of the two detectors that has measured geoneutrinos so far. The unprecedented radio-purity of the scintillator, the shielding with highly purified water, and the placement of the detector at a 3800 m w.e. depth have resulted in very low background levels and has made Borexino an excellent apparatus for geoneutrino measurements. The new update of the Borexino geoneutrino measurement, using the data obtained from December 2007 to April 2019, has been presented. Enhanced analysis techniques, adopted in this measurement, have been also presented (poster presentation #39 by S. Kumaran). The updated statistics and the new elaborate analysis have led to more than a factor two increase in exposure ((1.12 ± 0.05) × 1032 protons × yr) when compared to the latest Borexino result from 2015. The resulting geoneutrino signal of 47.0 − 7.7 + 8.4 ( stat ) − 1.9 + 2.4 ( sys ) TNU has − 17.2 + 18.3 % total precision. The geological interpretations of this measurement have been discussed. In particular, the 99% C.L. observation of the mantle signal by exploiting the relatively well-known lithospheric contribution, the estimation of the radiogenic heat, as well as the comparison of these results to the predictions based on different geological models. The upper limits on the power of a hypothetical georeactor that might be present at different locations inside the Earth have been set.

Published
2020

23. Chemical complexity in high-mass star formation: An observational and modeling case study of the AFGL 2591 VLA 3 hot core

Author

H. Linz, Peter Schilke, S. L. Lumsden, S. Leurini, Steven N. Longmore, T. Möller, A. Palau, S. Suri, Luca Moscadelli, M. T. Beltrán, Timea Csengeri, A. Ahmadi, Álvaro Sánchez-Monge, Siyi Feng, Rolf Kuiper, Luke T. Maud, P. Klaassen, Qizhou Zhang, D. Semenov, Roberto Galván-Madrid, F. Bosco, Friedrich Wyrowski, Henrik Beuther, Joseph C. Mottram, R. Pudritz, James Urquhart, T. Henning, T. Peters, C. Gieser, J. M. Winters, Karl M. Menten, Katharine G. Johnston, Izaskun Jiménez-Serra, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Kuiper, R. [0000-0003-2309-8963], Sánchez Monge, A. [0000-0002-3078-9482], Galván Madrid, R. [0000-0003-1480-4643], Leurini, S. [0000-0003-1014-3390], Ahmadi, A. [0000-0003-4037-5248], Semenov, D. [0000-0002-3913-7114], Gieser, C. [0000-0002-8120-1765], Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), European Research Council (ERC), Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundations (DFG), Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica de Mexico (PAPIIT), German Research Foundation (DFG), European Commission, and IRAM NOEMA Interferometer

Subjects
individual objects: AFGL 2591 [ISM], 010504 meteorology & atmospheric sciences, Mean kinetic temperature, Chemical process modeling, Core sample, FOS: Physical sciences, Astrophysics, Spatial distribution, 01 natural sciences, Spectral line, 0103 physical sciences, massive [Stars], Protostar, Molecule, QD, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), molecules [ISM], QC, 0105 earth and related environmental sciences, Astrochemistry, QB, Physics, GE, Star formation, Astronomy and Astrophysics, Physik (inkl. Astronomie), Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We present a detailed observational and modeling study of the hot core VLA 3 in the high-mass star-forming region AFGL 2591, which is a target region of the NOrthern Extended Millimeter Array (NOEMA) large program CORE. Using NOEMA observations at 1.37 mm with an angular resolution of ~0."42 (1 400 au at 3.33 kpc), we derived the physical and chemical structure of the source. We modeled the observed molecular abundances with the chemical evolution code MUSCLE (MUlti Stage ChemicaL codE). Results. With the kinetic temperature tracers CH3CN and H2CO we observe a temperature distribution with a power-law index of q = 0.41+-0.08. Using the visibilities of the continuum emission we derive a density structure with a power-law index of p = 1.7+-0.1. The hot core spectra reveal high molecular abundances and a rich diversity in complex molecules. The majority of the molecules have an asymmetric spatial distribution around the forming protostar(s), which indicates a complex physical structure on scales < 1 400 au. Using MUSCLE, we are able to explain the observed molecular abundance of 10 out of 14 modeled species at an estimated hot core chemical age of ~21 100 years. In contrast to the observational analysis, our chemical modeling predicts a lower density power-law index of p < 1.4. Reasons for this discrepancy are discussed. Conclusions. Combining high spatial resolution observations with detailed chemical modeling allows us to derive a concise picture of the physical and chemical structure of the famous AFGL 2591 hot core. The next steps are to conduct a similar analysis for the whole CORE sample, and then use this analysis to constrain the chemical diversity in high-mass star formation to a much greater depth., 22 pages, 13 figures, accepted for publication in A&A

Published
2019

24. Russian–American Nuclear Nonproliferation Dialogue : Lessons Learned and Road Ahead

Author

Vladimir A. Orlov, Sergey D. Semenov, Vladimir A. Orlov, and Sergey D. Semenov

Subjects
Nuclear nonproliferation--United States, Nuclear nonproliferation--Russia (Federation)
Abstract

This book explores the history of the nuclear nonproliferation dialogue between Russia (USSR) and the United States. By looking into the particulars of bilateral cooperation on NPT, Cooperative Threat Reduction program, arms control, and other issues, the authors offer lessons to be learned in preventing nuclear confrontations in the future. The book has been prepared in coordination between Russian and American scholars and experts and is a result of a series of Track 2.5 events devoted to restoring the nonproliferation cooperation between Russia and the United States. Covering all the aspects of the bilateral partnership since 1960 until today, this book will interest scholars of great power conflicts and nonproliferation. The workshop and the consequent work on the monograph became possible thanks to generous organizational & financial support from Centre russe d`etudes politiques (Geneva) and the Center for Policy Studies in Russia (Monterey, USA).

Published
2022

25. Using of magnetic particles for fi xing of isolated cells in subretinal transplantation

Author

A. A. Temnov, Yu. A. Belyy, S. A. Mirgorodskaya, A. D. Semenov, A. V. Shatskikh, A. V. Revishchin, G. V. Pavlova, N. N. Kust, and A. N. Sklifas

Subjects
magnetic particles, hek-293, Medicine, equipment and supplies, pluronics, human activities
Abstract

Purpose: This study focuses on the development of the method of introduction of magnetic microparticles in the cytoplasm of HEK-293 cell line with their subsequent fixation under the retina of the eye.Materials and Methods. Magnetic particles (d = 2,8 mm) were treated with pluronic and injected into the cytoplasm of HEK-293 cell line, expressing GFP. The surgery was made under general anesthesia. HEK-293 containing magnetic particles were injected into the subretinal space of rabbit eyes (eyes 96, 48 rabbits) using original dosing device. In the experimental group (48 eyes, 24 rabbits) we fixed episcleral magnetic implant to hold cells in local place. In the control group (48 eyes, 24 rabbit) magnetic implant was not fixed. After the surgery all animals were examined using biomicroscopy, ophthalmoscopy with photographic recording, ultrasound, computed tomography and morphological study in certain terms (1, 3, 5, 7, 14, 21 day and 1 month).Results: The introduction of the magnetic particles into the cytoplasm of HEK 293 cell line has no effect on cell viability. HEK-293 containing magnetic particles remains in the place of injection during 21 days in rabbit eyes, where the magnetic implants were fixed (in control group during 3 days). Conclusions: Using of cells containing magnetic particles with fixation of the magnetic implant can be a promising method for cell therapy for the treatment of retinal diseases.

Published
2016

26. Timing jitter in photon detection by straight superconducting nanowires: Effect of magnetic field and photon flux

Author

Steffen Doerner, Ilya Charaev, Artem Kuzmin, Mariia Sidorova, Heinz-Wilhelm Hübers, Michael Siegel, A. D. Semenov, Konstantin Ilin, and Denis Yu. Vodolazov

Subjects
Superconductivity, Physics, Photon, jitter, Physics - Instrumentation and Detectors, Superconducting nanowires, Nanowire, FOS: Physical sciences, Physics::Optics, 02 engineering and technology, Electron, Instrumentation and Detectors (physics.ins-det), Photon energy, 021001 nanoscience & nanotechnology, 01 natural sciences, Computational physics, Magnetic field, Wavelength, 0103 physical sciences, 010306 general physics, 0210 nano-technology, Jitter, Optics (physics.optics), Physics - Optics
Abstract

We studied the effects of the external magnetic field and photon flux on timing jitter in photon detection by straight superconducting NbN nanowires. At two wavelengths 800 and 1560 nm, statistical distribution in the appearance times of photon counts exhibits Gaussian shape at small times and an exponential tail at large times. The characteristic exponential time is larger for photons with smaller energy and increases with external magnetic field while variations in the Gaussian part of the distribution are less pronounced. Increasing photon flux drives the nanowire from the discrete quantum detection regime to the uniform bolometric regime that averages out fluctuations of the total number of nonequilibrium electrons created by the photon and drastically reduces jitter. The difference between standard deviations of Gaussian parts of distributions for these two regimes provides the measure for the strength of electron-number fluctuations; it increases with the photon energy. We show that the two-dimensional hot-spot detection model explains qualitatively the effect of magnetic field.

Published
2018

27. Chemistry in disks. XI. Sulfur-bearing species as tracers of protoplanetary disk physics and chemistry: the DM Tau case

Author

Cécile Favre, Franck Hersant, Richard Teague, Anne Dutrey, Vincent Piétu, Th. Henning, D. Semenov, Davide Fedele, Stephane Guilloteau, Edwige Chapillon, Istituto Nazionale di Astrofisica (INAF), AMOR 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, ECLIPSE 2018, Institut de RadioAstronomie Millimétrique (IRAM), and Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrochemistry, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, FOS: Physical sciences, Context (language use), Astrophysics, Protoplanetary disk, 01 natural sciences, Oxygen, 0103 physical sciences, Radiative transfer, Molecule, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Sulfur, Astrophysics - Astrophysics of Galaxies, 3. Good health, Interstellar medium, chemistry, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Several sulfur-bearing molecules are observed in the interstellar medium and in comets, in strong contrast to protoplanetary disks where only CS, H$_2$CS and SO have been detected so far. Aims. We combine observations and chemical models to constrain the sulfur abundances and their sensitivity to physical and chemical conditions in the DM Tau protoplanetary disk. Methods. We obtained $0.5^{"}$ ALMA observations of DM Tau in Bands 4 and 6 in lines of CS, SO, SO$_2$, OCS, CCS, H$_2$CS and H$_2$S, achieving a $\sim 5$ mJy sensitivity. Using the non-LTE radiative transfer code RADEX and the forward-modeling tool DiskFit, disk-averaged CS column densities and upper limits for the other species were derived. Results. Only CS was detected with a derived column density of $\sim 2-6 \times 10^{12}$ cm$^{-2}$. We report a first tentative detection of SO$_2$ in DM Tau. The upper limits range between $\sim 10^{11}$ and $10^{14}$ cm$^{-2}$ for the other S-bearing species. The best-fit chemical model matching these values requires a gas-phase C/O ratio of > 1 at $r \sim 50-100$ au. With chemical modeling we demonstrate that sulfur-bearing species could be robust tracers of the gas-phase C/O ratio, surface reaction rates, grain size and UV intensities. Conclusions. The lack of detections of a variety of sulfur-bearing molecules in DM Tau other than CS implies a dearth of reactive sulfur in the gas phase, either through efficient freeze-out or because most of the elemental sulfur is in other large species, as found in comets. The inferred high CS/SO and CS/SO$_2$ ratios require a non-solar C/O gas-phase ratio of > 1, consistent with the recent observations of hydrocarbon rings in DM Tau. The stronger depletion of oxygen-bearing S-species compared to CS is likely linked to the low observed abundances of gaseous water in DM Tau and points to a removal mechanism of oxygen from the gas., Accepted by Astronomy & Astrophysics (15 pages, 15 figures, 8 tables)

Published
2018

28. The Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk

Author

D. Semenov, E. Di Folco, Anne Dutrey, Edwige Chapillon, Otoniel Denis-Alpizar, Thomas Henning, Uma Gorti, Thierry Stoecklin, Vincent Piétu, Stephane Guilloteau, Nicolas Grosso, Valentine Wakelam, Richard Teague, AMOR 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
010504 meteorology & atmospheric sciences, Thermal desorption, FOS: Physical sciences, Astrophysics, Protoplanetary disk, circumstellar matter, 01 natural sciences, Saucer, Planet, Coincident, 0103 physical sciences, Thermal, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Molecular cloud, protoplanetary disks, Astronomy and Astrophysics, Scale height, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], radio lines: stars, Astrophysics - Earth and Planetary Astrophysics
Abstract

Determining the gas density and temperature structures of protoplanetary disks is a fundamental task to constrain planet formation theories. This is a challenging procedure and most determinations are based on model-dependent assumptions. We attempt a direct determination of the radial and vertical temperature structure of the Flying Saucer disk, thanks to its favorable inclination of 90 degrees. We present a method based on the tomographic study of an edge-on disk. Using ALMA, we observe at 0.5$"$ resolution the Flying Saucer in CO J=2-1 and CS J=5-4. This edge-on disk appears in silhouette against the CO J=2-1 emission from background molecular clouds in $��$ Oph. The combination of velocity gradients due to the Keplerian rotation of the disk and intensity variations in the CO background as a function of velocity provide a direct measure of the gas temperature as a function of radius and height above the disk mid-plane. The overall thermal structure is consistent with model predictions, with a cold ($< 15-12 $~K), CO-depleted mid-plane, and a warmer disk atmosphere. However, we find evidence for CO gas along the mid-plane beyond a radius of about 200\,au, coincident with a change of grain properties. Such a behavior is expected in case of efficient rise of UV penetration re-heating the disk and thus allowing CO thermal desorption or favoring direct CO photo-desorption. CO is also detected up to 3-4 scale heights while CS is confined around 1 scale height above the mid-plane. The limits of the method due to finite spatial and spectral resolutions are also discussed. This method appears to be very promising to determine the gas structure of planet-forming disks, provided that the molecular data have an angular resolution which is high enough, of the order of $0.3 - 0.1"$ at the distance of the nearest star forming regions., 14 pages + 11 figures

Published
2017

29. Towards a medium-scale axion helioscope and haloscope

Author

R. Djilkibaev, F. T. Avignone, V. K. Eremin, Sergey Troitsky, Serkant Ali Cetin, A. Gardikiotis, D. Semenov, Grigory Rubtsov, M. N. Pavlinsky, V. N. Muratova, Maxim Libanov, Vassilis Anastassopoulos, Pierre Sikivie, S. Molkov, Leonid Kravchuk, V. A. Matveev, Marin Karuza, Dieter H. H. Hoffmann, N. Golubev, Giovanni Cantatore, Konstantin Zioutas, Peter Tinyakov, E. V. Unzhakov, S. N. Gninenko, Andrei M. Bykov, M. Maroudas, A. V. Derbin, H. Fischer, K. V. Ptitsyna, V. S. Pantuev, A. A. Lutovinov, I. Drachnev, A. Gangapshev, Igor Tkachev, A. Spiridonov, Anastassopoulos, V., Avignone, F., Bykov, A., Cantatore, G., Cetin, S. A., Derbin, A., Drachnev, I., Djilkibaev, R., Eremin, V., Fischer, H., Gangapshev, A., Gardikiotis, A., Gninenko, S., Golubev, N., Hoffmann, D. H. H., Karuza, M., Kravchuk, L., Libanov, M., Lutovinov, A., Maroudas, M., Matveev, V., Molkov, S., Muratova, V., Pantuev, V., Pavlinsky, M., Ptitsyna, K., Rubtsov, G., Semenov, D., Sikivie, P., Spiridonov, A., Tinyakov, P., Tkachev, I., Troitsky, S., Unzhakov, E., and Zioutas, K.

Subjects
Particle physics, solar axion, Physics::Instrumentation and Detectors, Axions, FOS: Physical sciences, 01 natural sciences, magnetic helioscope, High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics::Theory, High Energy Physics - Phenomenology (hep-ph), Axion, 0103 physical sciences, 010306 general physics, Instrumentation, Mathematical Physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Helioscope, 010308 nuclear & particles physics, solar axions, High Energy Physics::Phenomenology, Astrophysics::Instrumentation and Methods for Astrophysics, Medium scale, Solar telescope, Dark matter halo, Halo, CERN Axion Solar Telescope
Abstract

We discuss the physics case for and the concept of a medium-scale axion helioscope with sensitivities in the axion-photon coupling a few times better than CERN Axion Solar Telescope (CAST). Search for an axion-like particle with these couplings is motivated by several persistent astrophysical anomalies. We present early conceptual design, existing infrastructure, projected sensitivity and timeline of such a helioscope (Troitsk Axion Solar Telescope Experiment, TASTE) to be constructed in the Institute for Nuclear Research, Troitsk, Russia. The proposed instrument may be also used for the search of dark-matter halo axions., 38 pages, 15 figures, JINST style. V2: misprints corrected. V3: minor clarifications and detalizations, version accepted by JINST

Published
2017

30. Grain Surface Models and Data for Astrochemistry

Author

Thanja Lamberts, Robin T. Garrod, E. M. Penteado, D. Semenov, Catherine Walsh, Sergio Ioppolo, and Herma M. Cuppen

Subjects
Surface (mathematics), Physics, Astrochemistry, Field (physics), Nanotechnology, Astronomy and Astrophysics, Surface reaction, 010402 general chemistry, 01 natural sciences, 0104 chemical sciences, Space and Planetary Science, 0103 physical sciences, Statistical physics, Theoretical Chemistry, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries)
Abstract

The cross-disciplinary field of astrochemistry exists to understand the formation, destruction, and survival of molecules in astrophysical environments. Molecules in space are synthesized via a large variety of gas-phase reactions, and reactions on dust-grain surfaces, where the surface acts as a catalyst. A broad consensus has been reached in the astrochemistry community on how to suitably treat gas-phase processes in models, and also on how to present the necessary reaction data in databases; however, no such consensus has yet been reached for grain-surface processes. A team of ${\sim}25$ experts covering observational, laboratory and theoretical (astro)chemistry met in summer of 2014 at the Lorentz Center in Leiden with the aim to provide solutions for this problem and to review the current state-of-the-art of grain surface models, both in terms of technical implementation into models as well as the most up-to-date information available from experiments and chemical computations. This review builds on the results of this workshop and gives an outlook for future directions.

Published
2017

31. The DarkSide Experiment: Present Status and Future

Author

S. Odrowski, M. Gromov, E. Segreto, D. Sablone, Peter Daniel Meyers, D. Rountree, Y. Suvorov, S. Westerdale, E. V. Unzhakov, C. Stanford, J. Brodsky, S. M. Mari, P. Saggese, A. M. Goretti, A. S. Chepurnov, S. Walker, Andrea Ianni, T. N. Johnson, E. V. Hungerford, Mariano Cadoni, Hui Wang, M. Guan, L. Pagani, Q. Riffard, Thomas Alexander, Maria Rescigno, A. Devoto, A. Sotnikov, M. D. Skorokhvatov, N. Rossi, A. Navrer Agasson, L. Grandi, F. Di Eusanio, A. K. Alton, Jim Napolitano, A. Tonazzo, M. Carlini, H. O. Back, M. Orsini, I. N. Machulin, Marcello Lissia, K. Biery, Yanchu Wang, P. N. Singh, Paolo Lombardi, J. Tatarowicz, G. Fiorillo, N. Canci, Aldo Romani, G. Di Pietro, Giovanni Covone, R. Saldanha, K. Fomenko, N. Pelliccia, B. J. Mount, J. Maricic, B. Reinhold, P. Agnes, S. Pordes, Marco Pallavicini, D. Korablev, A. Zec, M. Cariello, A. V. Derbin, F. Budano, D. M. Asner, B. Baldin, D. D'Angelo, M. De Vincenzi, A. L. Renshaw, A. Brigatti, G. Testera, D. Franco, K. Randle, K. Pelczar, Cristiano Galbiati, Irina James, D. Semenov, R. Milincic, M. D'Incecco, W. Zhong, S. De Cecco, G. Forster, C. J. Martoff, D. Hughes, M. Caravati, Anselmo Meregaglia, H. Qian, C. Dionisi, C. L. Kendziora, J. Wilhelmi, Chung-Yao Yang, Monica Verducci, G. Bonfini, A. Vishneva, Ivone F. M. Albuquerque, G. K. Giovanetti, B. R. Hackett, P. Cavalcante, A. Empl, M. Wada, W. Bonivento, M. De Deo, S. Davini, Frank Calaprice, X. Xiang, Y. Guardincerri, B. Vogelaar, M. Razeti, S. Catalanotti, S. Bussino, J. D. Miller, Paul H. Humble, E. Pantic, C. Savarese, K. Keeter, C. Giganti, Laura Cadonati, A. S. Kubankin, G. Zuzel, A. G. Cocco, Stefano Giagu, Giuseppe Longo, A. Razeto, R. Tartaglia, Al. Ianni, Xiaoyuan Li, E. Edkins, D. Montanari, V. Bocci, Fausto Ortica, Cécile Jollet, A. Candela, B. Loer, B. Schlitzer, C. Zhu, F. Gabriele, G. Korga, Gioacchino Ranucci, P. Trinchese, F. Granato, E. Shields, K. Herner, M. Cadeddu, C. Cicalo, Paolo Musico, A. Fan, D. A. Pugachev, V. N. Muratova, B. Bottino, A. Monte, A. Pocar, Jilei Xu, O. Smirnov, S. Parmeggiano, Marcin Wójcik, W. Sands, Y. Q. Ma, L. Marini, M. Bossa, B. Rossi, G. Koh, Alan Watson, A. Mandarano, Xiang Xiao, Zuzel, G., Agnes, P., Albuquerque, I. F. M., Alexander, T., Alton, A. K., Asner, D. M., Back, H. O., Baldin, B., Biery, K., Bocci, V., Bonfini, G., Bonivento, W., Bossa, M., Bottino, B., Brigatti, A., Brodsky, J., Budano, F., Bussino, S., Cadeddu, M., Cadonati, L., Cadoni, M., Calaprice, F., Canci, N., Candela, A., Caravati, M., Cariello, M., Carlini, M., Catalanotti, S., Cavalcante, P., Chepurnov, A., Cicalo, C., Cocco, A. G., Covone, G., D'Angelo, D., D'Incecco, M., Davini, S., De Cecco, S., De Deo, M., De Vincenzi, M., Derbin, A., Devoto, A., Di Eusanio, F., Di Pietro, G., Dionisi, C., Edkins, E., Empl, A., Fan, A., Fiorillo, G., Fomenko, K., Forster, G., Franco, D., Gabriele, F., Galbiati, C., Giagu, S., Giganti, C., Giovanetti, G. K., Goretti, A. M., Granato, F., Grandi, L., Gromov, M., Guan, M., Guardincerri, Y., Hackett, B. R., Herner, K., Hughes, D., Humble, P., Hungerford, E. V., Ianni, A. L., Ianni, A. N., James, I., Johnson, T. N., Jollet, C., Keeter, K., Kendziora, C. L., Koh, G., Korablev, D., Korga, G., Kubankin, A., Li, X., Lissia, M., Loer, B., Lombardi, P., Longo, G., Ma, Y., Machulin, I. N., Mandarano, Marina, Mari, S. M., Maricic, J., Marini, L., Martoff, C. J., Meregaglia, A., Meyers, P. D., Milincic, R., Miller, J. D., Montanari, D., Monte, A., Mount, B. J., Muratova, V. N., Musico, P., Napolitano, J., Agasson, A. Navrer, Odrowski, S., Orsini, M., Ortica, F., Pagani, L., Pallavicini, M., Pantic, E., Parmeggiano, S., Pelczar, K., Pelliccia, N., Pocar, A., Pordes, S., Pugachev, D. A., Qian, H., Randle, K., Ranucci, G., Razeti, M., Razeto, A., Reinhold, B., Renshaw, A. L., Rescigno, M., Riffard, Q., Romani, A., Rossi, B., Rossi, N., Rountree, D., Sablone, D., Saggese, P., Saldanha, R., Sands, W., Savarese, C., Schlitzer, B., Segreto, E., Semenov, D. A., Shields, E., Singh, P. N., Skorokhvatov, M. D., Smirnov, O., Sotnikov, A., Stanford, C., Suvorov, Y., Tartaglia, R., Tatarowicz, J., Testera, G., Tonazzo, A., Trinchese, P., Unzhakov, E. V., Verducci, M., Vishneva, A., Vogelaar, B., Wada, M., Walker, S., Wang, H., Wang, Y., Watson, A. W., Westerdale, S., Wilhelmi, J., Wojcik, M. M., Xiang, X. I., Xiao, X., Xu, J., Yang, C., Zec, A., Zhong, W., Zhu, C., Budano, Federico, Bussino, Severino Angelo Maria, DE VINCENZI, Mario, Eusanio, F. Di, Pietro, G. Di, Ianni, A. l., Ianni, A. n., James, Irina, Mandarano, A., Mari, Stefano Maria, Xiang, X. i., AstroParticule et Cosmologie (APC (UMR_7164)), 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), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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 de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), 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 Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)

Subjects
WIMP nucleon: scattering, History, Physics::Instrumentation and Detectors, Dark matter, WIMP: mass, chemistry.chemical_element, talk: Moscow 2016/10/10, DarkSide, 4/3, spin: dependence, WIMP: dark matter, channel cross section: upper limit, 01 natural sciences, argon: target, dark matter, Education, Nuclear physics, Physics and Astronomy (all), WIMP, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010306 general physics, Physics, Argon, Time projection chamber, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, WIMP nucleon: cross section, time projection chamber: liquid argon, Gran Sasso, Computer Science Applications, Elementary particle physics, Double phase, chemistry, Liquid argon, High Energy Physics::Experiment, MATTER, experimental results
Abstract

International audience; DarkSide is a multi-stage program devoted to direct searches of Dark Matter particles with detectors based on double phase liquid Argon Time Projection Chamber. The DarkSide-50 setup is running underground at the Laboratori Nazionali del Gran Sasso. First it was operated with Atmospheric Argon and during that run (1422 ± 67) kg×d of truly background-free exposure has been accumulated. Obtained data made it possible to set a 90% C.L. upper limit on the WIMP-nucleon cross section of 6.1 × 10(−)(44) cm(2) (for a WIMP mass of 100 GeV/c(2)). Presently the detector is filled with Underground Argon, which is depleted in (39)Ar by a factor of (1.4 ± 0.2)×10(3) with respect to Atmospheric Argon. Acquired so far (2616 ± 43) kg×d (71 live days) in combination with the data from the Atmospheric Argon run give us the 90% C.L. upper limit on the WIMP-nucleon spin-independent cross section of 2.0×10(−)(44) cm(2) for a WIMP mass of 100 GeV/c(2). Up to date this is the best limit obtained with an argon target.

Published
2017

32. The electronics and data acquisition system for the DarkSide-50 veto detectors

Author

V. N. Muratova, B. Bottino, E. V. Unzhakov, C. Stanford, G. Koh, B. Baldin, J. Brodsky, J. Wilhelmi, S. De Cecco, P. Saggese, Chung-Yao Yang, C. Savarese, A. Tonazzo, S. D. Rountree, M. Montuschi, Paolo Lombardi, S. Davini, C. J. Martoff, M. Carlini, Peter Daniel Meyers, Yufeng Wang, M. D. Skorokhvatov, L. Grandi, P. N. Singh, M. Gromov, A. Mandarano, A. Kubankin, M. Guan, Y. Suvorov, G. Zuzel, S. Luitz, E. Segreto, A. Candela, S. Westerdale, G. Testera, A. M. Goretti, A. S. Chepurnov, F. Budano, V. V. Kobychev, Mariano Cadoni, E. Pantic, P. J. Mosteiro, A. K. Alton, A. Sotnikov, Aldo Ianni, B. Reinhold, B. R. Hackett, A. Empl, F. Gabriele, E. Edkins, B. J. Mount, A. Zec, L. Agostino, H. Cao, D. Semenov, M. Orsini, J. Maricic, Hui Wang, R. B. Vogelaar, M. De Vincenzi, N. Canci, Caoxiang Zhu, M. De Deo, R. Tartaglia, D. Montanari, Ivone F. M. Albuquerque, A. L. Renshaw, A. Devoto, Griffin Foster, P. Cavalcante, Samuele Sangiorgio, M. Cadeddu, Stefano Maria Mari, J. Tatarowicz, T. Alexander, S. Odrowski, T. Miletic, D. Franco, Sandra Zavatarelli, W. Zhong, C. Giganti, K. Arisaka, K. Herner, R. Saldanha, Fausto Ortica, G. Fiorillo, L. Crippa, K. Fomenko, M. Wada, F. Calaprice, M. D'Incecco, Stuart Derek Walker, A. Vishneva, K. Randle, Anselmo Meregaglia, X. Li, H. Qian, Irina James, Y. Guardincerri, M. E. Monzani, A. Pocar, K. Keeter, A. Monte, Jilei Xu, Q. Riffard, S. Parmeggiano, D. Korablev, A. Brigatti, Jim Napolitano, D. Sablone, N. Pelliccia, X. Xiang, E. Shields, Gioacchino Ranucci, Y. Q. Ma, L. Marini, M. Bossa, B. Rossi, Alan Watson, K. Biery, A. Fan, D. A. Pugachev, Oleg Smirnov, S. Catalanotti, A. G. Cocco, F. Di Eusanio, Aldo Romani, P. Agnes, A. Razeto, P. Musico, W. Sands, M. Cariello, Andrea Ianni, A. V. Derbin, K. Pelczar, Cristiano Galbiati, C. L. Kendziora, M. M. Wojcik, G. Korga, F. Granato, Ann E. Nelson, I. N. Machulin, N. Rossi, Marco Pallavicini, D. D'Angelo, E. Hungerford, R. Milincic, S. Pordes, Henning O. Back, G. Bonfini, Cécile Jollet, J. Yoo, G. Di Pietro, Giovanni Covone, Severino Angelo Maria Bussino, L. Pagani, Marcello Lissia, P. Trinchese, AstroParticule et Cosmologie (APC (UMR_7164)), 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département Recherches Subatomiques (DRS-IPHC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre Hospitalier Universitaire de Nice (CHU de Nice), Biomécanique et Bioingénierie (BMBI), Université de Technologie de Compiègne (UTC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Institut Pluridisciplinaire Hubert Curien (IPHC), Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University [Stanford], Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Departamento de Engenharia Elétrica [Minas Gerais] (DEE - UFMG), Universidade Federal de Minas Gerais, Rhodes University, inconnu, Inconnu, Key Lab of Computer System and Architecture, Institute of Computing Technology [Beijing] (ICT), Chinese Academy of Sciences [Beijing] (CAS), Institut Européen des membranes (IEM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Ecole Nationale Supérieure de Chimie de Montpellier (ENSCM)-Centre National de la Recherche Scientifique (CNRS), Agnes, P., Agostino, L., Albuquerque, I. F. M., Alexander, T., Alton, A. K., Arisaka, K., Back, H. O., Baldin, B., Biery, K., Bonfini, G., Bossa, M., Bottino, B., Brigatti, A., Brodsky, J., Budano, F., Bussino, S., Cadeddu, M., Cadoni, M., Calaprice, F., Canci, N., Candela, A., Cao, H., Cariello, M., Carlini, M., Catalanotti, S., Cavalcante, P., Chepurnov, A., Cocco, A. G., Covone, G., Crippa, L., D'Angelo, D., D'Incecco, M., Davini, S., Dececco, S., De Deo, M., De Vincenzi, M., Derbin, A., Devoto, A., Di Eusanio, F., Di Pietro, G., Edkins, E., Empl, A., Fan, A., Fiorillo, G., Fomenko, K., Foster, G., Franco, D., Gabriele, F., Galbiati, C., Giganti, C., Goretti, A. M., Granato, F., Grandi, L., Gromov, M., Guan, M., Guardincerri, Y., Hackett, B. R., Herner, K. R., Hungerford, E. V., Ianni, Aldo, Ianni, Andrea, James, I., Jollet, C., Keeter, K., Kendziora, C. L., Kobychev, V., Koh, G., Korablev, D., Korga, G., Kubankin, A., Li, X., Lissia, M., Lombardi, P., Luitz, S., Ma, Y., Machulin, I. N., Mandarano, A., Mari, S. M., Maricic, J., Marini, L., Martoff, C. J., Meregaglia, A., Meyers, P. D., Miletic, T., Milincic, R., Montanari, D., Monte, A., Montuschi, M., Monzani, M. E., Mosteiro, P., Mount, B. J., Muratova, V. N., Musico, P., Napolitano, J., Nelson, A., Odrowski, S., Orsini, M., Ortica, F., Pagani, L., Pallavicini, M., Pantic, E., Parmeggiano, S., Pelczar, K., Pelliccia, N., Pocar, A., Pordes, S., Pugachev, D. A., Qian, H., Randle, K., Ranucci, G., Razeto, A., Reinhold, B., Renshaw, A. L., Riffard, Q., Romani, A., Rossi, B., Rossi, N., Rountree, S. D., Sablone, D., Saggese, P., Saldanha, R., Sands, W., Sangiorgio, S., Savarese, C., Segreto, E., Semenov, D. A., Shields, E., Singh, P. N., Skorokhvatov, M. D., Smirnov, O., Sotnikov, A., Stanford, C., Suvorov, Y., Tartaglia, R., Tatarowicz, J., Testera, G., Tonazzo, A., Trinchese, P., Unzhakov, E. V., Vishneva, A., Vogelaar, R. B., Wada, M., Walker, S., Wang, H., Wang, Y., Watson, A. W., Westerdale, S., Wilhelmi, J., Wojcik, M. M., Xiang, X., Xu, J., Yang, C., Yoo, J., Zavatarelli, S., Zec, A., Zhong, W., Zhu, C., Zuzel, G., Budano, Federico, Bussino, Severino Angelo Maria, DE VINCENZI, Mario, James, Irina, and Mari, Stefano Maria

Subjects
Physics - Instrumentation and Detectors, gas and liquid scintillators), architecture, Physics::Instrumentation and Detectors, Dark matter, FOS: Physical sciences, Scintillator, algorithms, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), Data acquisition, Front-end electronics for detector readout, 0103 physical sciences, hardware, Neutron, Detector control systems (detector and experiment monitoring and slow control systems, 010306 general physics, Instrumentation, Cherenkov radiation, ComputingMilieux_MISCELLANEOUS, Mathematical Physics, Physics, [PHYS]Physics [physics], Time projection chamber, Data acquisition concepts, Scintillators, scintillation and light emission processes (solid, gas and liquid scintillators), Detector control systems (detector and experiment monitoring and slow control systems, architecture, hardware, algorithms, databases), 010308 nuclear & particles physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), scintillation and light emission processes (solid, Weakly interacting massive particles, Scintillators, High Energy Physics::Experiment, databases), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; DarkSide-50 is a detector for dark matter candidates in the form of weakly interacting massive particles. It utilizes a liquid argon time projection chamber for the inner main detector, surrounded by a liquid scintillator veto (LSV) and a water Cherenkov veto detector (WCV). The LSV and WCV act as the neutron and cosmogenic muon veto detectors for DarkSide-50. This paper describes the electronics and data acquisition system used for these two detectors. The system is made of a custom built front end electronics and commercial National Instruments high speed digitizers. The front end electronics, the DAQ, and the trigger system have been used to acquire data in the form of zero-suppressed waveform samples from the 110 PMTs of the LSV and the 80 PMTs of the WCV. The veto DAQ system has proven its performance and reliability. This electronics and DAQ system can be scaled and used as it is for the veto of the next generation DarkSide-20k detector

Published
2016

33. Importance of the H2 abundance in protoplanetary disk ices for the molecular layer chemical composition

Author

M. Ruaud, Valentine Wakelam, Franck Hersant, Anne Dutrey, Liton Majumdar, Stephane Guilloteau, D. Semenov, AMOR 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and ECLIPSE 2016

Subjects
Physics, Astrochemistry, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Binding energy, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Protoplanetary disk, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Chemical physics, Desorption, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Monolayer, Molecule, 010303 astronomy & astrophysics, Chemical composition
Abstract

Protoplanetary disks are the target of many chemical studies (both observational and theoretical) as they contain the building material for planets. Their large vertical and radial gradients in density and temperature make them challenging objects for chemical models. In the outer part of these disks, the large densities and low temperatures provide a particular environment where the binding of species onto the dust grains can be very efficient and can affect the gas-phase chemical composition. We attempt to quantify to what extent the vertical abundance profiles and the integrated column densities of molecules predicted by a detailed gas-grain code are affected by the treatment of the molecular hydrogen physisorption at the surface of the grains. We performed three different models using the Nautilus gas-grain code. One model uses a H2 binding energy on the surface of water (440 K) and produces strong sticking of H2. Another model uses a small binding energy of 23 K (as if there were already a monolayer of H2), and the sticking of H$_2$ is almost negligible. Finally, the remaining model is an intermediate solution known as the encounter desorption mechanism. We show that the efficiency of molecular hydrogen binding (and thus its abundance at the surface of the grains) can have a quantitative effect on the predicted column densities in the gas phase of major species such as CO, CS, CN, and HCN., Accepted for publication as a Research Note in A&A

Published
2016

34. DarkSide-50, a background free experiment for dark matter searches

Author

P. Agnes, 1 T. Alexander, 2 A. Alton, 3 K. Arisaka, 4 H. O. Back, 5 B. Baldin, 6 K. Biery, 6 G. Bonfini, 7 M. Bossa, 8 A. Brigatti, 9 J. Brodsky, 5 F. Budano, 10 L. Cadonati, 2 F. Calaprice, 5 N. Canci, 4 A. Candela, 7 H. Cao, 5 M. Cariello, 11 P. Cavalcante, 7 A. Chavarria, 12 A. Chepurnov, 13 A. G. Cocco, 14 L. Crippa, 9 D. D’Angelo, 9 M. D’Incecco, 7 S. Davini, 15 M. De Deo, 7 A. Derbin, 16 A. Devoto, 17 F. Di Eusanio, 5 G. Di Pietro, 9 E. Edkins, 18 A. Empl, 15 A. Fan, 4 G. Fiorillo, 14 K. Fomenko, 19 G. Forster, 2 D. Franco, 1 F. Gabriele, 7 C. Galbiati, 5 A. Goretti, 5 L. Grandi, 12 M. Gromov, 13 M. Y. Guan, 20 Y. Guardincerri, 6 B. Hackett, 18 K. Herner, 6 E. V. Hungerford, 15 A.l. Ianni, 7 A.n. Ianni, 5 C. Jollet, 21 K. Keeter, 22 C. Kendziora, 6 S. Kidner, a. V. Kobychev, 24 G. Koh, 5 D. Korablev, 19 G. Korga, 15 A. Kurlej, 2 P. X. Li, 20 B. Loer, 5 P. Lombardi, 9 C. Love, 25 L. Ludhova, 9 S. Luitz, 26 Y. Q. Ma, 20 I. Machulin, 28 A. Mandarano, 10 J. Maricic, 18 L. Marini, 10 C. J. Martoff, 25 A. Meregaglia, 21 E. Meroni, 9 P. D. Meyers, 5 R. Milincic, 18 D. Montanari, 6 M. Montuschi, 7 M. E. Monzani, 26 P. Mosteiro, 5 B. Mount, 22 V. Muratova, 16 P. Musico, 11 A. Nelson, 5 S. Odrowski, 7 M. Okounkova, 5 M. Orsini, 7 F. Ortica, 29 L. Pagani, 11 M. Pallavicini, 11 E. Pantic, 4, 30 L. Papp, 23 S. Parmeggiano, 9 R. Parsells, 5 K. Pelczar, 31 N. Pelliccia, 29 S. Perasso, 1 A. Pocar, 2 S. Pordes, 6 D. Pugachev, 27 H. Qian, 5 K. Randle, 2 G. Ranucci, 9 A. Razeto, 7 B. Reinhold, 18 A. Renshaw, 4 A. Romani, 29 B. Rossi, 5, 14 N. Rossi, 7 S. D. Rountree, 23 D. Sablone, 15 P. Saggese, 7 R. Saldanha, 12 W. Sands, 5 S. Sangiorgio, 32 E. Segreto, 7 D. Semenov, 16 E. Shields, 5 M. Skorokhvatov, 28 O. Smirnov, 19 A. Sotnikov, 19 C. Stanford, 5 Y. Suvorov, 4 R. Tartaglia, 7 J. Tatarowicz, 25 G. Testera, 11 A. Tonazzo, 1 E. Unzhakov, 16 R. B. Vogelaar, 23 M. Wada, 5 S. Walker, 14 H. Wang, 4 Y. Wang, 20 A. Watson, 25 S. Westerdale, 5 M. Wojcik, 31 A. Wright, 5 X. Xiang, 5 J. Xu, 5 C. G. Yang, 20 J. Yoo, 6 S. Zavatarelli, 11 A. Zec, 2 C. Zhu, G. Zuzel31, MARI, Stefano Maria, P., Agne, 1 T., Alexander, 2 A., Alton, 3 K., Arisaka, 4 H. O., Back, 5 B., Baldin, 6 K., Biery, 6 G., Bonfini, 7 M., Bossa, 8 A., Brigatti, 9 J., Brodsky, 5 F., Budano, 10 L., Cadonati, 2 F., Calaprice, 5 N., Canci, 4 A., Candela, 7 H., Cao, 5 M., Cariello, 11 P., Cavalcante, 7 A., Chavarria, 12 A., Chepurnov, 13 A. G., Cocco, 14 L., Crippa, 9 D., D’Angelo, 9 M., D’Incecco, 7 S., Davini, 15 M., De Deo, 7 A., Derbin, 16 A., Devoto, 17 F., Di Eusanio, 5 G., Di Pietro, 9 E., Edkin, 18 A., Empl, 15 A., Fan, 4 G., Fiorillo, 14 K., Fomenko, 19 G., Forster, 2 D., Franco, 1 F., Gabriele, 7 C., Galbiati, 5 A., Goretti, 5 L., Grandi, 12 M., Gromov, 13 M. Y., Guan, 20 Y., Guardincerri, 6 B., Hackett, 18 K., Herner, 6 E. V., Hungerford, Ianni, 15 A. l., Ianni, 7 A. n., 5 C., Jollet, 21 K., Keeter, 22 C., Kendziora, 6 S., Kidner, a. V., Kobychev, 24 G., Koh, 5 D., Korablev, 19 G., Korga, 15 A., Kurlej, 2 P. X., Li, 20 B., Loer, 5 P., Lombardi, 9 C., Love, 25 L., Ludhova, 9 S., Luitz, 26 Y. Q., Ma, 20 I., Machulin, 28 A., Mandarano, Mari, Stefano Maria, 10 J., Maricic, 18 L., Marini, 10 C. J., Martoff, 25 A., Meregaglia, 21 E., Meroni, 9 P. D., Meyer, 5 R., Milincic, 18 D., Montanari, 6 M., Montuschi, 7 M. E., Monzani, 26 P., Mosteiro, 5 B., Mount, 22 V., Muratova, 16 P., Musico, 11 A., Nelson, 5 S., Odrowski, 7 M., Okounkova, 5 M., Orsini, 7 F., Ortica, 29 L., Pagani, 11 M., Pallavicini, 11 E., Pantic, 30 L., Papp, 23 S., Parmeggiano, 9 R., Parsell, 5 K., Pelczar, 31 N., Pelliccia, 29 S., Perasso, 1 A., Pocar, 2 S., Porde, 6 D., Pugachev, 27 H., Qian, 5 K., Randle, 2 G., Ranucci, 9 A., Razeto, 7 B., Reinhold, 18 A., Renshaw, 4 A., Romani, 29 B., Rossi, 14 N., Rossi, 7 S. D., Rountree, 23 D., Sablone, 15 P., Saggese, 7 R., Saldanha, 12 W., Sand, 5 S., Sangiorgio, 32 E., Segreto, 7 D., Semenov, 16 E., Shield, 5 M., Skorokhvatov, 28 O., Smirnov, 19 A., Sotnikov, 19 C., Stanford, 5 Y., Suvorov, 4 R., Tartaglia, 7 J., Tatarowicz, 25 G., Testera, 11 A., Tonazzo, 1 E., Unzhakov, 16 R. B., Vogelaar, 23 M., Wada, 5 S., Walker, 14 H., Wang, 4 Y., Wang, 20 A., Watson, 25 S., Westerdale, 5 M., Wojcik, 31 A., Wright, 5 X., Xiang, 5 J., Xu, 5 C. G., Yang, 20 J., Yoo, 6 S., Zavatarelli, 11 A., Zec, 2 C., Zhu, and G., Zuzel31

Subjects
Physics, Large Underground Xenon experiment, Physics::Instrumentation and Detectors, Hot dark matter, Dark matter, Scalar field dark matter, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Dark matter halo, Weakly interacting massive particles, Warm dark matter, Instrumentation, Light dark matter, Mathematical Physics
Abstract

The existence of dark matter is inferred from gravitational effects, but its nature remains a deep mystery. One possibility, motivated by considerations in elementary particle physics, is that dark matter consists of elementary particles, such as the hypothesized Weakly Interacting Massive Particles (WIMPs), with mass ~ 100 GeV and cross-section ~ 10−47 cm2, that can be gravitationally trapped inside our galaxy and revealed by their scattering on nuclei. It should be possible to detect WIMPs directly, as the orbital motion of the WIMPs composing the dark matter halo pervading the galaxy should result in WIMP-nucleus collisions of sufficient energy to be observable in the laboratory. The DarkSide-50 experiment is a direct WIMP search using a Liquid Argon Time Projection Chamber (LAr-TPC) with an active mass of 50 kg with a high sensitivity and an ultra-low background detector.

Published
2014

35. First Results from the DarkSide-50 Dark Matter Experiment at Laboratori Nazionali del Gran Sasso

Author

P. Agnes, 1 T. Alexander, 2 A. Alton, 3 K. Arisaka, 4 H. O. Back, 5 B. Baldin, 6 K. Biery, 6 G. Bonfini, 7 M. Bossa, 8 A. Brigatti, 9 J. Brodsky, 5 F. Budano, 10 L. Cadonati, 2 F. Calaprice, 5 N. Canci, 4 A. Candela, 7 H. Cao, 5 M. Cariello, 11 P. Cavalcante, 7 A. Chavarria, 12 A. Chepurnov, 13 A. G. Cocco, 14 L. Crippa, 9 D. D’Angelo, 9 M. D’Incecco, 7 S. Davini, 15 M. De Deo, 7 A. Derbin, 16 A. Devoto, 17 F. Di Eusanio, 5 G. Di Pietro, 9 E. Edkins, 18 A. Empl, 15 A. Fan, 4 G. Fiorillo, 14 K. Fomenko, 19 G. Forster, 2 D. Franco, 1 F. Gabriele, 7 C. Galbiati, 5 A. Goretti, 5 L. Grandi, 12 M. Gromov, 13 M. Y. Guan, 20 Y. Guardincerri, 6 B. Hackett, 18 K. Herner, 6 E. V. Hungerford, 15 A.l. Ianni, 7 A.n. Ianni, 5 C. Jollet, 21 K. Keeter, 22 C. Kendziora, 6 S. Kidner, a. V. Kobychev, 24 G. Koh, 5 D. Korablev, 19 G. Korga, 15 A. Kurlej, 2 P. X. Li, 20 B. Loer, 5 P. Lombardi, 9 C. Love, 25 L. Ludhova, 9 S. Luitz, 26 Y. Q. Ma, 20 I. Machulin, 28 A. Mandarano, 10 J. Maricic, 18 L. Marini, 10 C. J. Martoff, 25 A. Meregaglia, 21 E. Meroni, 9 P. D. Meyers, 5 R. Milincic, 18 D. Montanari, 6 M. Montuschi, 7 M. E. Monzani, 26 P. Mosteiro, 5 B. Mount, 22 V. Muratova, 16 P. Musico, 11 A. Nelson, 5 S. Odrowski, 7 M. Okounkova, 5 M. Orsini, 7 F. Ortica, 29 L. Pagani, 11 M. Pallavicini, 11 E. Pantic, 4, 30 L. Papp, 23 S. Parmeggiano, 9 R. Parsells, 5 K. Pelczar, 31 N. Pelliccia, 29 S. Perasso, 1 A. Pocar, 2 S. Pordes, 6 D. Pugachev, 27 H. Qian, 5 K. Randle, 2 G. Ranucci, 9 A. Razeto, 7 B. Reinhold, 18 A. Renshaw, 4 A. Romani, 29 B. Rossi, 5, 14 N. Rossi, 7 S. D. Rountree, 23 D. Sablone, 15 P. Saggese, 7 R. Saldanha, 12 W. Sands, 5 S. Sangiorgio, 32 E. Segreto, 7 D. Semenov, 16 E. Shields, 5 M. Skorokhvatov, 28 O. Smirnov, 19 A. Sotnikov, 19 C. Stanford, 5 Y. Suvorov, 4 R. Tartaglia, 7 J. Tatarowicz, 25 G. Testera, 11 A. Tonazzo, 1 E. Unzhakov, 16 R. B. Vogelaar, 23 M. Wada, 5 S. Walker, 14 H. Wang, 4 Y. Wang, 20 A. Watson, 25 S. Westerdale, 5 M. Wojcik, 31 A. Wright, 5 X. Xiang, 5 J. Xu, 5 C. G. Yang, 20 J. Yoo, 6 S. Zavatarelli, 11 A. Zec, 2 C. Zhu, G. Zuzel 3, MARI, Stefano Maria, P. Agnes, P., Agne, 1 T., Alexander, 2 A., Alton, 3 K., Arisaka, 4 H. O., Back, 5 B., Baldin, 6 K., Biery, 6 G., Bonfini, 7 M., Bossa, 8 A., Brigatti, 9 J., Brodsky, 5 F., Budano, 10 L., Cadonati, 2 F., Calaprice, 5 N., Canci, 4 A., Candela, 7 H., Cao, 5 M., Cariello, 11 P., Cavalcante, 7 A., Chavarria, 12 A., Chepurnov, 13 A. G., Cocco, 14 L., Crippa, 9 D., D’Angelo, 9 M., D’Incecco, 7 S., Davini, 15 M., De Deo, 7 A., Derbin, 16 A., Devoto, 17 F., Di Eusanio, 5 G., Di Pietro, 9 E., Edkin, 18 A., Empl, 15 A., Fan, 4 G., Fiorillo, 14 K., Fomenko, 19 G., Forster, 2 D., Franco, 1 F., Gabriele, 7 C., Galbiati, 5 A., Goretti, 5 L., Grandi, 12 M., Gromov, 13 M. Y., Guan, 20 Y., Guardincerri, 6 B., Hackett, 18 K., Herner, 6 E. V., Hungerford, Ianni, 15 A. l., Ianni, 7 A. n., 5 C., Jollet, 21 K., Keeter, 22 C., Kendziora, 6 S., Kidner, a. V., Kobychev, 24 G., Koh, 5 D., Korablev, 19 G., Korga, 15 A., Kurlej, 2 P. X., Li, 20 B., Loer, 5 P., Lombardi, 9 C., Love, 25 L., Ludhova, 9 S., Luitz, 26 Y. Q., Ma, 20 I., Machulin, 28 A., Mandarano, Mari, Stefano Maria, 10 J., Maricic, 18 L., Marini, 10 C. J., Martoff, 25 A., Meregaglia, 21 E., Meroni, 9 P. D., Meyer, 5 R., Milincic, 18 D., Montanari, 6 M., Montuschi, 7 M. E., Monzani, 26 P., Mosteiro, 5 B., Mount, 22 V., Muratova, 16 P., Musico, 11 A., Nelson, 5 S., Odrowski, 7 M., Okounkova, 5 M., Orsini, 7 F., Ortica, 29 L., Pagani, 11 M., Pallavicini, 11 E., Pantic, 30 L., Papp, 23 S., Parmeggiano, 9 R., Parsell, 5 K., Pelczar, 31 N., Pelliccia, 29 S., Perasso, 1 A., Pocar, 2 S., Porde, 6 D., Pugachev, 27 H., Qian, 5 K., Randle, 2 G., Ranucci, 9 A., Razeto, 7 B., Reinhold, 18 A., Renshaw, 4 A., Romani, 29 B., Rossi, 14 N., Rossi, 7 S. D., Rountree, 23 D., Sablone, 15 P., Saggese, 7 R., Saldanha, 12 W., Sand, 5 S., Sangiorgio, 32 E., Segreto, 7 D., Semenov, 16 E., Shield, 5 M., Skorokhvatov, 28 O., Smirnov, 19 A., Sotnikov, 19 C., Stanford, 5 Y., Suvorov, 4 R., Tartaglia, 7 J., Tatarowicz, 25 G., Testera, 11 A., Tonazzo, 1 E., Unzhakov, 16 R. B., Vogelaar, 23 M., Wada, 5 S., Walker, 14 H., Wang, 4 Y., Wang, 20 A., Watson, 25 S., Westerdale, 5 M., Wojcik, 31 A., Wright, 5 X., Xiang, 5 J., Xu, 5 C. G., Yang, 20 J., Yoo, 6 S., Zavatarelli, 11 A., Zec, 2 C., Zhu, and G., Zuzel 3

Subjects
Physics::Instrumentation and Detectors, Astrophysics::Instrumentation and Methods for Astrophysics, High Energy Physics::Experiment, Astrophysics::Cosmology and Extragalactic Astrophysics, Nuclear Experiment
Abstract

We report the first results of DarkSide-50, a direct search for dark matter operating in the un- derground Laboratori Nazionali del Gran Sasso (LNGS) and searching for the rare nuclear recoils possibly induced by weakly interacting massive particles (WIMPs). The dark matter detector is a Liquid Argon Time Projection Chamber with a ( 46.4 0.7 ) kg active mass, operated inside a 30 t or- ganic liquid scintillator neutron veto, which is in turn installed at the center of a 1 kt water Cherenkov veto for the residual flux of cosmic rays. We report here the null results of a dark matter search for a ( 1422 67 ) kg d exposure with an atmospheric argon fill. This is the most sensitive dark matter search performed with an argon target, corresponding to a 90% CL upper limit on the WIMP-nucleon spin-independent cross section of 6.1 10

Published
2014

36. The Electronics and Data Acquisition System of the DarkSide Dark Matter Search

Author

The DarkSide Collaboration, P. Agnes 1, T. Alexander 2, A. Alton 3, K. Arisaka 4, H. O. Back 5, B. Baldin 6, K. Biery 6, G. Bonfini 7, M. Bossa 8, A. Brigatti 9, J. Brodsky 5, F. Budano 10, L. Cadonati 2, F. Calaprice 5, N. Canci 4, A. Candela 7, H. Cao 5, M. Cariello 11, P. Cavalcante 7, A. Chavarria 12, A. Chepurnov 13, A. G. Cocco 14, L. Crippa 9, D. D’Angelo 9, M. D’Incecco 7, S. Davini 15, M. De Deo 7, A. Derbin 16, A. Devoto 17, F. Di Eusanio 5, G. Di Pieto 9, E. Edkins 18, A. Empl 15, A. Fan 4, G. Fiorillo 14, K. Fomenko 19, G. Forster 2, D. Franco 1, F. Gabriele 7, C. Galbiati 5, A. Goretti 5, L. Grandi 12, M. Gromov 13, M. Y. Guan 20, Y. Guardincerri 6, B. Hackett 18, K. Herner 6, E. Hungerford 15, A.l. Ianni 7, A.n. Ianni 5, C. Jollet 21, K. Keeter 22, C. Kendziora 6, S. Kidner 23, V. Kobychev 24, G. Koh 5, D. Korablev 19, G. Korga 15, A. Kurlej 2, P. X. Li 20, B. Loer 5, P. Lombardi 9, C. Love 25, L. Ludhova 9, S. Luitz 26, Y. Q. Ma 20, I. Machulin 27, A. Mandarano 10, J. Maricic 18, L. Marini 10, J. Martoff 25, A. Meregaglia 21, E. Meroni 9, P. D. Meyers 5, R. Milincic 18, D. Montanari 6, M. Montuschi 7, M. E. Monzani 26, P. Mosteiro 5, B. Mount 22, V. Muratova 16, P. Musico 11, A. Nelson 5, S. Odrowski 7, M. Okounkoa 5, M. Orsini 7, F. Ortica 19, L. Pagani 11, M. Pallavicini 11, E. Pantic 4, L. Papp 23, S. Parmeggiano 9, Bob Parsells 5, K. Pelczar 31, N. Pelliccia 29, S. Perasso 1, A. Pocar 2, S. Pordes 6, D. Pugachev 27, H. Qian 5, K. Randle 2, G. Ranucci 9, A. Razeto 7, B. Reinhold 18, A. Renshaw 4, A. Romani 29, B. Rossi 5, N. Rossi 7, S. D. Rountree 23, D. Sablone 15, P. Saggese 7, R. Saldanha 12, W. Sands 5, S. Sangiorgio 30, E. Segreto 7, D. Semenov 16, E. Shields 5, M. Skorokhvatov 27, O. Smirnov 19, A. Sotnikov 19, C. Stanford 5, Suvorov 4, R. Tartaglia 17, J. Tatarowicz 25, G. Testera 11, A. Tonazzo 1, E. Unzhakov 16, R. B. Vogelaar 23, M. Wada 5, S. E. Walker 14, H. Wang 4, Y. Wang 28, A. Watson 25, S. Westerdale 5, M. Wojcik 31, A. Wright 5, X. Xiang 5, J. Xu 5, C. G. Yang 20, J. Yoo 6, S. Zavatarelli 11, A. Zec 2, C. Zhu 5, G. Zuzel 31, MARI, Stefano Maria, P. Agnes, P.Agnes, The DarkSide, Collaboration, P., Agnes 1, T., Alexander 2, A., Alton 3, K., Arisaka 4, H. O., Back 5, B., Baldin 6, K., Biery 6, G., Bonfini 7, M., Bossa 8, A., Brigatti 9, J., Brodsky 5, F., Budano 10, L., Cadonati 2, F., Calaprice 5, N., Canci 4, A., Candela 7, H., Cao 5, M., Cariello 11, P., Cavalcante 7, A., Chavarria 12, A., Chepurnov 13, A. G., Cocco 14, L., Crippa 9, D., D’Angelo 9, M., D’Incecco 7, S., Davini 15, M., De Deo 7, A., Derbin 16, A., Devoto 17, F., Di Eusanio 5, G., Di Pieto 9, E., Edkins 18, A., Empl 15, A., Fan 4, G., Fiorillo 14, K., Fomenko 19, G., Forster 2, D., Franco 1, F., Gabriele 7, C., Galbiati 5, A., Goretti 5, L., Grandi 12, M., Gromov 13, M. Y., Guan 20, Y., Guardincerri 6, B., Hackett 18, K., Herner 6, E., Hungerford 15, Ianni 7, A. l., Ianni 5, A. n., C., Jollet 21, K., Keeter 22, C., Kendziora 6, S., Kidner 23, V., Kobychev 24, G., Koh 5, D., Korablev 19, G., Korga 15, A., Kurlej 2, P. X., Li 20, B., Loer 5, P., Lombardi 9, C., Love 25, L., Ludhova 9, S., Luitz 26, Y. Q., Ma 20, I., Machulin 27, A., Mandarano 10, Mari, Stefano Maria, J., Maricic 18, L., Marini 10, J., Martoff 25, A., Meregaglia 21, E., Meroni 9, P. D., Meyers 5, R., Milincic 18, D., Montanari 6, M., Montuschi 7, M. E., Monzani 26, P., Mosteiro 5, B., Mount 22, V., Muratova 16, P., Musico 11, A., Nelson 5, S., Odrowski 7, M., Okounkoa 5, M., Orsini 7, F., Ortica 19, L., Pagani 11, M., Pallavicini 11, E., Pantic 4, L., Papp 23, S., Parmeggiano 9, Bob Parsells, 5, K., Pelczar 31, N., Pelliccia 29, S., Perasso 1, A., Pocar 2, S., Pordes 6, D., Pugachev 27, H., Qian 5, K., Randle 2, G., Ranucci 9, A., Razeto 7, B., Reinhold 18, A., Renshaw 4, A., Romani 29, B., Rossi 5, N., Rossi 7, S. D., Rountree 23, D., Sablone 15, P., Saggese 7, R., Saldanha 12, W., Sands 5, S., Sangiorgio 30, E., Segreto 7, D., Semenov 16, E., Shields 5, M., Skorokhvatov 27, O., Smirnov 19, A., Sotnikov 19, C., Stanford 5, Suvorov, 4, R., Tartaglia 17, J., Tatarowicz 25, G., Testera 11, A., Tonazzo 1, E., Unzhakov 16, R. B., Vogelaar 23, M., Wada 5, S. E., Walker 14, H., Wang 4, Y., Wang 28, A., Watson 25, S., Westerdale 5, M., Wojcik 31, A., Wright 5, X., Xiang 5, J., Xu 5, C. G., Yang 20, J., Yoo 6, S., Zavatarelli 11, A., Zec 2, C., Zhu 5, and G., Zuzel 31

Abstract

It is generally inferred from astronomical measurements th at Dark Matter (DM) comprises approximately 27% of the energy-dens ity of the universe. If DM is a subatomic particle, a possible candidate is a Weakl y Interacting Mas- sive Particle (WIMP), and the DarkSide-50 (DS) experiment i s a direct search for evidence of WIMP-nuclear collisions. DS is located undergr ound at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, and consists of thr ee active, embedded components; an outer water veto (CTF), a liquid scintillato r veto (LSV), and a liquid argon (LAr) time projection chamber (TPC). This pap er describes the data acquisition and electronic systems of the DS detectors , designed to detect the residual ionization from s

Published
2014

37. Recent results from Borexino

Author

G Testera, M Agostin, K Altenmüller, S Appel, G Bellini, J Benziger, D Bick, G Bonfini, D Bravo, B Caccianiga, F Calaprice, A Caminata, P Cavalcante, A Chepurnov, D D’Angelo, S Davini, A Derbin, L Di Noto, I Drachnev, A Etenko, K Fomenko, D Franco, F Gabriele, C Galbiati, C Ghiano, M Giammarchi, M Göger-Neff, A Goretti, M Gromov, C Hagner, E Hungerford, Aldo Ianni, Andrea Ianni, K Jedrzejczak, M Kaiser, V Kobychev, D Korablev, G Korga, D Kryn, M Laubenstein, B Lehnert, E Litvinovich, F Lombardi, P Lombardi, L Ludhova, G Lukyanchenko, I Machulin, S Manecki, W Maneschg, S Marcocci, E Meroni, M Meyer, L Miramonti, M Misiaszek, M Montuschi, P Mosteiro, V Muratova, B Neumair, L Oberauer, M Obolensky, F Ortica, M Pallavicini, L Papp, L Perasso, A Pocar, G Ranucci, A Razeto, A Re, A Romani, R Roncin, N Rossi, S Schönert, D Semenov, H Simgen, M Skorokhvatov, O Smirnov, A Sotnikov, S Sukhotin, Y Suvorov, R Tartaglia, J Thurn, M Toropova, E Unzhakov, A Vishneva, RB Vogelaar, F von Feilitzsch, H Wang, S Weinz, J Winter, M Wojcik, M Wurm, Z Yokley, O Zaimidoroga, S Zavatarelli, K Zuber, G Zuzel, AstroParticule et Cosmologie (APC (UMR_7164)), 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), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
History, neutrino: solar, 010308 nuclear & particles physics, Physics::Instrumentation and Detectors, energy spectrum, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, 7. Clean energy, Computer Science Applications, Education, Physics and Astronomy (all), 0103 physical sciences, charge: conservation law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Borexino, 010306 general physics, experimental results, energy: low
Abstract

International audience; We review the solar neutrinos results of Borexino and the limit on the charge conservation obtained in the context of the analysis of the low energy region of the energy spectrum.

Published
2016

38. The high precision measurement of the 144Ce activity in the SOX experiment

Author

M Kaiser, Lino Miramonti, A Caminata, O Zaimidoroga, E. Hungerford, M. S. Meyer, G. Korga, S Marcocci, P Mosteiro, C Hagner, F. von Feilitzsch, S Farinon, V. Fischer, M Obolensky, O. Smirnov, A. Razeto, M. Durero, K Fomenko, C Galbiati, M Cribier, E Litvinovich, J. Gaffiot, Paolo Lombardi, M Wurm, M. Vivier, C Veyssière, V. N. Muratova, D. Kryn, M Montuschi, Thierry Lasserre, Matteo Agostini, K Choi, G Bellini, E Unzhakov, N. Rossi, L Perasso, I. S. Drachnev, L Scola, A. V. Derbin, M. Goeger-Neff, R. Tartaglia, H Wang, Jay Burton Benziger, Aldo Romani, T Lachenmaier, P. Cavalcante, N Jonquères, R. Musenich, M. Misiaszek, W Maneschg, L. Di Noto, A. Pocar, K. Althenmüller, N Berton, S. Schönert, D. Bravo Berguño, F. Lombardi, A. Sotnikov, Aldo Ianni, Lothar Oberauer, S. Davini, S. Manecki, J. Thurn, R. Roncin, T. Houdy, G. Testera, T. Lehnert, Gioacchino Ranucci, D Semenov, Andrea Ianni, Matthias Laubenstein, R. Cereseto, G Mention, D DAngelo, Kai Zuber, Marcin Wójcik, Y. Suvorov, M. Skorokhvatov, S. Zavatarelli, Livia Ludhova, V. V. Kobychev, D Bick, A. S. Chepurnov, A Goretti, Marco Pallavicini, S Weinz, F. Gabriele, Denis Korablev, J Link, G. Lukyanchenko, J. Winter, A Etenko, D. Franco, C Ghiano, Marco Giammarchi, G. Zuzel, Z Yokley, J. Maricic, S. Appel, R. B. Vogelaar, L. Papp, C Rossi, B Caccianiga, S. Sukhotin, I. N. Machulin, K Jedrzejczak, Fausto Ortica, M. Gromov, B. Neumair, V.N. Kornoukhov, M Toropova, Alessandra Re, G. Bonfini, Frank Calaprice, Hardy Simgen, E Meroni, Département de Physique Nucléaire (ex SPhN) (DPHN), 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)-Université Paris-Saclay, AstroParticule et Cosmologie (APC (UMR_7164)), 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), SOX, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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 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, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Di Noto, L., Agostini, M., Althenmueller, K., Appel, S., Bellini, G., Benziger, J., Berton, N., Bick, D., Bonfini, G., Bravo-Berguno, D., Caccianiga, B., Calaprice, F., Caminata, A., Cavalcante, P., Cereseto, R., Chepurnov, A., Choi, K., Cribier, M., Dangelo, D., Davini, S., Derbin, A., Drachnev, I., Durero, M., Etenko, A., Farinon, S., Fischer, V., Fomenko, K., Franco, D., Gabriele, F., Gaffiot, J., Galbiati, C., Ghiano, C., Giammarchi, M., Goeeger-Neff, M., Goretti, A., Gromov, M., Hagner, C., Houdy, Th, Hungerford, E., Ianni, Aldo, Ianni, Andrea, Jonqueres, N., Jedrzejczak, K., Kaiser, M., Kobychev, V., Korablev, D., Korga, G., Kornoukhov, V., Kryn, D., Lachenmaier, T., Lasserre, T., Laubenstein, M., Lehnert, T., Link, J., Litvinovich, E., Lombardi, F., Lombardi, P., Ludhova, L., Lukyanchenko, G., Machulin, I., Manecki, S., Maneschg, W., Marcocci, S., Maricic, J., Mention, G., Meroni, E., Meyer, M., Miramonti, L., Misiaszek, M., Montuschi, M., Mosteiro, P., Muratova, V., Musenich, R., Neumair, B., Oberauer, L., Obolensky, M., Ortica, F., Pallavicini, M., Papp, L., Perasso, L., Pocar, A., Ranucci, G., Razeto, A., Re, A., Romani, A., Roncin, R., Rossi, C., Rossi, N., Schoenert, S., Scola, L., Semenov, D., Simgen, H., Skorokhvatov, M., Smirnov, O., Sotnikov, A., Sukhotin, S., Suvorov, Y., Tartaglia, R., Testera, G., Thurn, J., Toropova, M., Veyssiere, C., Vivier, M., Unzhakov, E., Vogelaar, R. B., von Feilitzsch, F., Wang, H., Weinz, S., Winter, J., Wojcik, M., Wurm, M., Yokley, Z., Zaimidoroga, O., Zavatarelli, S., Zuber, K., and Zuzel, G.

Subjects
History, Particle physics, Water flow, Physics::Instrumentation and Detectors, tungsten, water, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Particle detector, Education, Physics::Geophysics, thermal, Nuclear physics, Physics and Astronomy (all), alloy, 0103 physical sciences, ddc:530, 010306 general physics, Neutrino oscillation, Nuclear Experiment, background: radioactivity, Borexino, Physics, 010308 nuclear & particles physics, precision measurement, calorimeter: design, Detector, antineutrino, Computer Science Applications, Gran Sasso, cerium, flow, Measuring instrument, High Energy Physics::Experiment, neutrino: oscillation, Neutrino, Lepton
Abstract

International audience; In order to perform a resolutive measurement to clarify the neutrino anomalies and to observe possible short distance neutrino oscillations, the SOX (Short distance neutrino Oscillations with BoreXino) experiment is under construction. In the first phase, a 100 kCi (144)Ce-(144)Pr antineutrino source will be placed under the Borexino detector at the Laboratori Nazionali del Gran Sasso (LNGS), in center of Italy, and the rate measurement of the antineutrino events, observed by the very low radioactive background Borexino detector, will be compared with the high precision (< 1%) activity measurement performed by two calorimeters. The source will be embedded in a 19 mm thick tungsten alloy shield and both the calorimeters have been conceived for measuring the thermal heat absorbed by a water flow. In this report the design of the calorimeters will be described in detail and very preliminary results will be also shown.

Published
2016

39. DarkSide-50 : a WIMP search with a two-phase argon TPC

Author

P.D. Meyers, P. Agnes, D. Alton, K. Arisaka, H.O. Back, B. Baldin, K. Biery, G. Bonfini, M. Bossa, A. Brigatti, J. Brodsky, F. Budano, L. Cadonati, F. Calaprice, N. Canci, A. Candela, H. Cao, M. Cariello, P. Cavalcante, A. Chavarria, A. Chepurnov, A.G. Cocco, L. Crippa, D. DAngelo, M. D’Incecco, S. Davini, M. De Deo, A. Derbin, F. Di Eusanio, G. Di Pietro, E. Edkins, A. Empl, A. Fan, G. Fiorillo, K. Fomenko, G. Forster, D. Franco, F. Gabriele, C. Galbiati, A. Goretti, L. Grandi, M. Gromov, M. Guan, Y. Guardincerri, B. Hackett, K. Herner, P. Humble, E.V. Hungerford, Al. Ianni, An. Ianni, C. Joliet, K. Keeter, C. Kendziora, S. Kidner, V. Kobychev, G. Koh, D. Korablev, G. Korga, A. Kurlej, P. Li, B. Loer, P. Lombardi, C. Love, L. Ludhova, S. Luitz, Y. Ma, I. Machulin, A. Mandarano, S. Mari, J. Maricic, C.J. Martoff, A. Meregaglia, E. Meroni, R. Milincic, D. Montanari, M. Montuschi, M.E. Monzani, P. Mosteiro, B. Mount, V. Muratova, P. Musico, A. Nelson, M. Okounkova, M. Orsini, F. Ortica, L. Pagani, M. Pallavicini, E. Pantic, L. Papp, S. Parmeggiano, R. Parsells, K. Pelczar, N. Pelliccia, S. Perasso, F. Perfetto, A. Pocar, S. Pordes, H. Qian, K. Randle, G. Ranucci, A. Razeto, B. Reinhold, A. Romani, B. Rossi, N. Rossi, S.D. Rountree, D. Sablone, P. Saggese, R. Saldanha, W. Sands, E. Segreto, D. Semenov, E. Shields, M. Skorokhvatov, O. Smirnov, A. Sotnikov, Y. Suvarov, R. Tartaglia, J. Tatarowicz, G. Testera, A. Tonazzo, E. Unzhakov, R.B. Vogelaar, M. Wada, H. Wang, Y. Wang, A. Watson, R. Westerdale, M. Wojcik, A. Wright, J. Xu, C. Yang, J. Yoo, S. Zavatarelli, G. Zuzel, Agnes, P., Alton, D., Arisaka, K., Back, H. O., Baldin, B., Biery, K., Bonfini, G., Bossa, M., Brigatti, A., Brodsky, J., Budano, F., Cadonati, L., Calaprice, F., Canci, N., Candela, A., Cao, H., Cariello, M., Cavalcante, P., Chavarria, A., Chepurnov, A., Cocco, A. G., Crippa, L., Dangelo, D., D’Incecco, M., Davini, S., De Deo, M., Derbin, A., Di Eusanio, F., Di Pietro, G., Edkins, E., Empl, A., Fan, A., Fiorillo, Giuliana, Fomenko, K., Forster, G., Franco, D., Gabriele, F., Galbiati, C., Goretti, A., Grandi, L., Gromov, M., Guan, M., Guardincerri, Y., Hackett, B., Herner, K., Humble, P., Hungerford, E. V., Ianni, A., Joliet, C., Keeter, K., Kendziora, C., Kidner, S., Kobychev, V., Koh, G., Korablev, D., Korga, G., Kurlej, A., Li, P., Loer, B., Lombardi, P., Love, C., Ludhova, L., Luitz, S., Ma, Y., Machulin, I., Mandarano, A., Mari, S., Maricic, J., Martoff, C. J., Meregaglia, A., Meroni, E., Meyers, P. D., Milincic, R., Montanari, D., Montuschi, M., Monzani, M. E., Mosteiro, P., Mount, B., Muratova, V., Musico, P., Nelson, A., Okounkova, M., Orsini, M., Ortica, F., Pagani, L., Pallavicini, M., Pantic, E., Papp, L., Parmeggiano, S., Parsells, R., Pelczar, K., Pelliccia, N., Perasso, S., Perfetto, F., Pocar, A., Pordes, S., Qian, H., Randle, K., Ranucci, G., Razeto, A., Reinhold, B., Romani, A., Rossi, B., Rossi, N., Rountree, S. D., Sablone, D., Saggese, P., Saldanha, R., Sands, W., Segreto, E., Semenov, D., Shields, E., Skorokhvatov, M., Smirnov, O., Sotnikov, A., Suvarov, Y., Tartaglia, R., Tatarowicz, J., Testera, G., Tonazzo, A., Unzhakov, E., Vogelaar, R. B., Wada, M., Wang, H., Wang, Y., Watson, A., Westerdale, R., Wojcik, M., Wright, A., Xu, J., Yang, C., Yoo, J., Zavatarelli, S., Zuzel, G., Mari, Stefano Maria, and The Darkside, Collaboration

Subjects
Physics, Cryostat, Argon, Time projection chamber, chemistry.chemical_element, WIMP Argon Programme, Scintillator, Physics and Astronomy(all), Nuclear physics, Physics and Astronomy (all), chemistry, WIMP, pacs:95.35.+d, 29.40.Mc, Neutron, Cherenkov radiation
Abstract

DarkSide-50 is a two phase argon TPC for direct dark matter detection which is installed at the Gran Sasso underground laboratory, Italy. DarkSide-50 has a 50-kg active volume and will make use of underground argon low in 39 Ar. The TPC is installed inside an active neutron veto made with boron-loaded high radiopurity liquid scintillator. The neutron veto is installed inside a 1000 m 3 water Cherenkov muon veto. The DarkSide-50 TPC and cryostat are assembled in two radon-free clean rooms to reduce radioactive contaminants. The overall design aims for a background free exposure after selection cuts are applied. The expected sensitivity for WIMP-nucleon cross section is of the order of 10 −45 cm 2 for WIMP masses around 100 GeV/c 2 . The commissioning and performance of the detector are described. Details of the low-radioactivity underground argon and other unique features of the projects are reported.

Published
2015

40. Alignment of the ALICE Inner Tracking System with cosmic-ray tracks

Author

F. Carena, Rainer Arno Ernst Renfordt, Petr Nomokonov, Taku Gunji, Juyeon Yi, Udo Kebschull, Rashmi Raniwala, Boris Batyunya, Claude Andre Pruneau, F. Furano, S. Antinori, Roberto Barbera, H. Delagrange, T. Dobrowolski, Marian Krivda, M. Sano, Xu Cai, Zhongbao Yin, Philippe Pillot, L. Cunqueiro, E. Cattaruzza, J. Pluta, Andreas Petridis, Evgeny Ryabinkin, R. Grajcarek, Bruce Becker, L. Molnar, F. Formenti, Grzegorz Andrzej Wilk, T. Samanta, Matthias Richter, S. Huber, Raul Arteche Diaz, Hyun-Chul Kim, Konrad Tywoniuk, P. Rosinský, Fernando Scarlassara, F. Yermia, Rajeev Singh, Subhasis Chattopadhyay, Agneta Oskarsson, Sergey Nazarenko, M. Zynovyev, Krzysztof Redlich, G. Herrera Corral, D. Truesdale, J. Hamblen, Lokesh Kumar, M. Nicassio, Lawrence Pinsky, W. Sommer, X. Yuan, B. H. Han, C. Di Giglio, Jochen Klein, B. Fenton-Olsen, A. Szostak, A. Matyja, C. Bortolin, Brigitte Cheynis, C. Baumann, Janusz Oleniacz, Y. Berdnikov, Ana Vargas, T.A. Pocheptsov, Csaba Soos, I. Maldonado Cervantes, J. Gebelein, Hannes Jung, Vladislav Manko, S. Sano, Marian Putis, Bogdan Vulpescu, H. Gottschlag, Trine Spedstad Tveter, Vladimir Peskov, Sevil Salur, Sergey Kiselev, M. R. Cosentino, Hideki Hamagaki, Gunnar Løvhøiden, Elena Bruna, S. Beole, Lennart Osterman, Christian Holm Christensen, Yu.N. Pestov, F. Orsini, G. Torralba, Dayong Wang, Madan M. Aggarwal, D. Tlusty, Andreas Morsch, Alexander Mamonov, A. Pepato, Anselmo Margotti, Evgeny Kryshen, D. Perini, Klaus Johannes Reygers, C.W. Fabjan, Shih-Chang Lee, M. Fragkiadakis, T. Iwasaki, F. Lackner, R. Ichou, I. K. Yoo, N. Abel, Panagiotis Christakoglou, Dirk Hutter, M. Rodríguez Cahuantzi, S. H. Kim, Teodor Siemiarczuk, S. Rousseau, Andrei Ionut Herghelegiu, V. Kushpil, A. Palmeri, M. Bregant, A. Pesci, H. Yang, V. Grigoriev, J. W. Harris, Yu.V. Zanevsky, Mauro Gallio, Y. Corrales Morales, Hans Rudolf Schmidt, Xuan Zhang, J. Bartke, A. Raḿirez Reyes, Petra Riedler, M. Venaruzzo, Ken Oyama, L. Jirden, Rosario Nania, Roberto Preghenella, P. Crochet, Alexander Philipp Kalweit, C. Ivan, Olja Dordic, Sona Pochybova, B. S. Chang, R. Bala, G. Steyn, Satyajit Jena, Natasha Sharma, Andre Mischke, Jean-Yves Grossiord, L. K. Mangotra, H. Oeschler, I. Ilkiv, V. Altini, E. Serradilla, F. Nendaz, Cristina Terrevoli, Federico Ronchetti, V. Chambert, A. Jacholkowski, E. Nappi, I. Rashevskaya, A. Lozea Feijo Soares, Silvia Masciocchi, Z. Fodor, M. Krus, G. Sharkov, T. Sugitate, H. Taureg, S. Di Liberto, Toralf Bernhard Skaali, C. Tagridis, A. G. Agocs, Kenta Shigaki, I. Doḿinguez, Hanna Paulina Zbroszczyk, Michele Floris, C. Pastore, Laurent Ducroux, Juha Äystö, Hans Hjersing Dalsgaard, V.A. Polyakov, Marek Chojnacki, Q. Wen, G. T. Jones, Federico Carminati, Z. Buthelezi, Laurent Bernard Aphecetche, C. Nygaard, G. Martínez García, Herve Borel, J. Sarkamo, G. de Vaux, I. Sgura, V. Demanov, Michal Sumbera, A. Colla, T. Kalliokoski, Branislav Sitar, G.V. Russo, A. van den Brink, M. Boccioli, Alexey Kurepin, S. Rath, Jana Bielcikova, Cynthia Marie Hadjidakis, Vikas Singhal, Paulus Gerardus Kuijer, Kilian Eberhard Schwarz, J. Mlynarz, Catia Petta, Paolo Camerini, Sergey Voloshin, C. Lal, Gyulnara Eyyubova, A. Fernández Téllez, Wisla Carena, Martino Gagliardi, G. Luparello, Andrey Reshetin, J. Munoz, R. A. Fini, Daniela Fabris, F. Painke, Marcello Lunardon, A. K. Dutta Majumdar, E. Fragiacomo, R. Platt, A. Rachevski, H. A. Gustafsson, Y. Le Bornec, Ian Gardner Bearden, Chiara Oppedisano, B. Pastirčák, P. González-Zamora, E. Camacho, V. I. Yurevich, Natalia Kondratyeva, A. Michalon, Alberica Toia, Kjetil Ullaland, N. De Marco, Magdalena Malek, D. Di Bari, E. Belmont-Moreno, P. T. Hille, Andrei Gheata, R. Gomez, M. De Gaspari, D. Krumbhorn, V. Lafage, V. Lenti, K. Aamodt, Paolo Giubellino, B. Grinyov, Ulrich Fuchs, Francesco Riggi, O. Sokolov, Siegfried Valentin Foertsch, Panagiota Foka, V. Nikolic, Kirill Voloshin, D. Hasch, Bjarte Kileng, Bruno Alessandro, Sudhir Raniwala, M. S. Ganti, Sanjib Muhuri, P. Roy, D. Evans, L. Toscano, N. Willis, M. Szuba, V. Catanescu, H. Lee, I. Cortés Maldonado, Peter Zahariev Hristov, Y. Li, H.R. Gulkanyan, Marcel Araujo Silva Figueredo, F. Tosello, A. Marzari Chiesa, Tatiana Karavicheva, R. Gemme, H. González Santos, T. Tolyhy, A. M. Gago, Y. J. Kwon, L. Vannucci, G. Conesa Balbastre, Peter Martin Jacobs, Jon Christopher Wikne, Amalia Pop, Rachid Guernane, A. Nianine, Alexey Kuryakin, Filimon Roukoutakis, Andry Malala Rakotozafindrabe, R. Janik, Filippo Costa, M. Irfan, Martin Vala, Antonino Zichichi, M. Spyropoulou-Stassinaki, Marcelo Gameiro Munhoz, Valeria Muccifora, S. Hu, Werner Riegler, Jennifer Lynn Klay, Meidana Huang, Y. Vinogradov, L. Valencia Palomo, S. Zhou, M. Rammler, Iouri Belikov, Thomas Dietel, Oliver Busch, Chitrasen Jena, Imrich Szarka, Nicole Bastid, J. Bán, J. L. Charvet, K. Schossmaier, V. Fekete, Andrew Ivanov, E. Stan, T. Alt, Peter Graham Jones, C. Cavicchioli, Enrichetta Maria Fiore, Subrata Pal, L. Manceau, Atsushi Takahara, Giacomo Bruno, D. Hatzifotiadou, Frederick Kramer, M. Tavlet, Marian Ivanov, A. Borisov, D. Y.-U. Peressounko, Predrag Buncic, Tinku Sarkar Sinha, F. Posa, Premomoy Ghosh, Marco De Petris, A. Turvey, Gualtiero Volpe, A. Alici, Prithwish Tribedy, B. K. Srivastava, Alina Gabriela Grigoras, Livio Bianchi, Stefano Piano, Laszlo Boldizsar, J. Takahashi, E. López Torres, A. Musso, Smbat Grigoryan, A. Kolojvari, C. García Trapaga, M. Mastromarco, Leonid Vinogradov, Chiara Zampolli, Sara Vallero, A. A. Rademakers, G.F. Segato, G. de Cataldo, R. Tanabe, Vito Manzari, Johanna Stachel, Alexander Akindinov, Rainer Martin Schicker, P. Stolpovsky, Alessandro Grelli, P. Gros, Latchezar Betev, E. Crescio, Federico Cindolo, C. D. Anson, S. Jangal, D. Swoboda, B.V. Zagreev, R. Romita, Anju Bhasin, C. Lara, I. Vassiliev, G. S. Pappalardo, Peter Chochula, Mikhail Malaev, Sami Sakari Rasanen, M. Bach, G. A. Feofilov, I. Vetlitskiy, A. Baldit, E. Biolcati, A. Zepeda, M. Zhalov, J. J. Gaardhøje, Alexey Bogdanov, R. Santo, Haaland, Ajay Kumar Dash, A. Enokizono, Ewa Gladysz-dziadus, Kyong Sei Lee, Claudio Guarnaccia, Jan Rak, G. Stefanek, A. Gupta, M. E. Cotallo, Christophe Pierre Suire, Z. Conesa del Valle, Wladyslaw Henryk Trzaska, Alessandra Fantoni, E. Quercigh, Yu. V. Kharlov, Bedangadas Mohanty, Andrzej Deloff, Dominik Fehlker, R. Smakal, V. Canoa Roman, A. K. Bhati, D. Antończyk, Christoph Blume, Gergely Gábor Barnaföldi, Andrzej Rybicki, J. Dubuisson, Andrey Zarochentsev, J. F. Castillo Hernandez, Vladimir Nikulin, Maria Haiduc, Boris Hippolyte, Carlos A. Salgado, A. Punin, Christophe Furget, Jean Willy Andre Cleymans, Francesca Soramel, L. Bosisio, Radiy Ilkaev, J. Urban, A. Nyatha, S. Dash, Petr Zavada, Evgeny Zabrodin, N. Novitzky, R. P. Scharenberg, Paul Constantin, R. A. Soltz, F. Blanco, L. Šándor, A. Silenzi, E. Simili, A. Anzo, Vladimir Kaplin, R. López-Raḿirez, H. León Vargas, C. Lazzeroni, B. Polichtchouk, Massimo Masera, R. Alfaro Molina, N. Pitz, D. Felea, L. Luquin, R. Glasow, T. Aronsson, P. Ostrowski, K. Watanabe, B. S. Nilsen, Marek Kowalski, Andre Augustinus, H. Snow, Angelo Rivetti, J. P. Revol, J. Mercado Pérez, P. La Rocca, M. Meoni, A. Belogianni, M. Basile, A. Hayrapetyan, H. Caines, D. Mayani, Adela Kravcakova, Ki-Seok Choi, D. M. Madagodahettige-Don, Stefan Kirsch, W. W. Jung, A. Vacchi, I. Kraus, Henner Buesching, D. Budnikov, M. Mohisin Khan, L. Jancurová, J.A. Mares, Matevz Tadel, D. Derkach, A. Devaux, Min Jung Kweon, R. Kolevatov, I. Berceanu, Borge Svane Nielsen, Motoi Inaba, V.N. Borshchov, Xing Long Li, Tomasz Traczyk, N. van der Kolk, Ivana Hrivnacova, Volker Lindenstruth, V. Chibante Barroso, A. Charpy, Junlee Kim, T.M. Steinbeck, V. Wagner, E. G. Ferreiro, M. A. Lisa, Heng-Tong Ding, B. Hicks, Adrian Sevcenco, Nikolai Smirnov, R. Stock, Raphael Noel Tieulent, H. Ricaud, Bastian Bathen, A. De Falco, R. Salgueiro Domingues da Silva, Ciprian Mihai Mitu, G. Batigne, F. Padilla, H. K. Soltveit, M. Heide, A. Nyiri, M. Pachr, C. Pérez, Kai Schweda, Annalisa Mastroserio, Jan Fiete Grosse-Oetringhaus, Nicola Bianchi, J. Thäder, G. D'Erasmo, Mads Stormo Nilsson, Paraskevi Ganoti, Rene Brun, Raghunath Sahoo, Dagmar Adamová, M. Bogolyubsky, C. Xu, Markus Fasel, A. R. Reolon, G. Bruckner, Sedat Altinpinar, T. K. Nayak, K. Safaŕik, A. Badalà, A. Ochirov, D. De Gruttola, D. T. Larsen, H. Tydesjö, Alexander Kurepin, Sven Gotovac, Rosario Turrisi, P. R. Pujahari, A.G. Fedunov, Steffen Schreiner, P. Vande Vyvre, A. Hiei, D. Hasegan, L. Bimbot, M. van Leeuwen, Hyungsuk Son, J. Seo, I. Rusanov, Mihai Petrovici, Henning Kværnø, D. Elia, Bernd Stefan Windelband, Sangeeta Das, Vladimir Samsonov, S. Gorbunov, A. Klovning, Giacomo Ortona, Linda Vickovic, Varlen Grabski, Valerie Ramillien Barret, Néstor Armesto, F. Piuz, M. Kutouski, Eleazar Cuautle, K. Mizoguchi, Y. Hori, A. Szanto de Toledo, J. Kapitan, Diego Stocco, Y. Maruyama, Nicolas Bock, Markku Oinonen, Mikolaj Krzewicki, S. Radomski, P. Jovanovic, Luciano Musa, Oleg Karavichev, S. K. Pal, S. De Pasquale, L. Montaño Zetina, B. Boyer, A. Abrahantes Quintana, S. Kox, G. Hamar, D. Perrino, J. H. Kim, L. Leistam, Yasuo Miake, S. Evrard, I. Otterlund, L. H. González-Trueba, G. Tröger, Seyong Kim, N. Le Bris, S. Kalcher, Marie Germain, Leonid Serkin, Raffaele Grosso, H. Schindler, Pascal Dupieux, Hans Muller, M. Heinz, Lee Stuart Barnby, Andrea Dainese, A. M. Rossi, Sergey Fokin, A. J. Rubio-Montero, S. Arcelli, L. Massacrier, Anand Kumar Dubey, G. Bourdaud, Y. Kucheriaev, R. de Rooij, S. Senyukov, S. Serci, M. Morando, Bruno Espagnon, Ulrich Michael Frankenfeld, V. Paticchio, A. Blanc, F. Rettig, A. A. Vinogradov, A. G. Asryan, S. Prasad, L. Wallet, I. Martashvili, B. von Haller, C. Klein-Bösing, A. B. Kaidalov, Giuseppe Viesti, Shuaib Ahmad Khan, S. Lohn, C. Søgaard, H. León, G. Anelli, Davide Caffarri, A. Zenin, F. Bossú, Ante Bilandzic, T. Pawlak, G. O.V. de Barros, David Dobrigkeit Chinellato, E. Berdermann, David Olle Rickard Silvermyr, D. Miśkowiec, I. Makhlyueva, A. Pulvirenti, Alexandre Alarcon Do Passo Suaide, A. Konevskih, A. Peters, A. Ortiz Velasquez, Stefano Bagnasco, Airton Deppman, Giuseppe Giraudo, Barbara Guerzoni, Peter Christiansen, Marta Verweij, A. Uras, Tatjana Susa, Dai-Mei Zhou, Yves Roland Schutz, Dmitry Mal'kevich, Alexandr Tumkin, A. Nedosekin, Sang Un Ahn, J. Zhu, Alexander Kluge, F.F. Guber, Zubayer Ahammed, Giacomo Vito Margagliotti, Xavier Bernard Lopez, Jaroslav Bielcik, Marco Monteno, N. Herrmann, Kalliopi Kanaki, J. Pouthas, C. Garabatos, M. C.S. Williams, Michele Caselle, D. P. Mahapatra, P. Petrov, R. Panse, A. Wilk, Navneet Kumar, Rui Ma, D. S. Kim, Arturo Alejandro Menchaca-Rocha, Marek Bombara, Cristian Andrei, M. Kim, C.J. Oskamp, Kei Okada, A. Harutyunyan, Johan Alme, Luciano Ramello, Alla Maevskaya, H. Pereira, P. Saturnini, Mihaela Gheata, M. I. Martínez, Tatsuya Chujo, Nazeer Ahmad, Y. Okada, P. Zelnicek, Anton Andronic, J. Symons, Federico Antinori, A. Casanova Díaz, I. Kisel, M. Lenhardt, V. Angelov, O. Villalobos Baillie, R. A. Ricci, K. Polák, V. P. Kondratiev, C. Torcato de Matos, A. Soloviev, C. Pajares, J. P. Coffin, O. Vikhlyantsev, Andrey Vasiliev, Peter Strmen, S. Böttger, Gerardus Nooren, J. Peschek, Mikhail Ippolitov, M. A. Subieta Vásquez, Evgeny Karpechev, F. Chuman, M. Bondila, E. Tsilis, E. Siddi, Hiroki Yokoyama, T. Horaguchi, J. De Groot, R. Akimoto, Enrico Scomparin, A. Martínez Davalos, Ara Grigoryan, Altaf Ahmad, Bikash Sinha, Melinda Siciliano, N. Grion, Sébastien Gadrat, G. Aglieri Rinella, D. M.M. Don, Raphaelle Marie Bailhache, C.J. Schmidt, S. Schuchmann, M. Hartig, G. J. Contreras, M. Kliemant, V. Basmanov, M. Vassiliou, Y. Wang, Vladimir Vechernin, S. Sharma, Mitali Mondal, Magnus Mager, P. Mendez Lorenzo, W. J. Park, P. Mereu, Luisa Cifarelli, Jacek Tomasz Otwinowski, P. Antonioli, Ermanno Vercellin, Y. N. Gorbunov, Vladimir Ivanov, A. Frolov, W. Peryt, Eugen Mudnic, A. Mahajan, A. De Caro, Kyrre Skjerdal, A. Glenn, I. S. Zgura, Tome Anticic, V. Dobretsov, M. A. Mazzoni, Sergey Filchagin, Jorn Henning Putschke, M. Botje, An. Zalite, Stefan Rossegger, M. Dialinas, Francesco Noferini, G. L. Usai, A. Arend, Sylvain Chapeland, J. Bohm, M. Ploskon, R. Vernet, E. Dénes, R. Kamermans, Eva Sicking, A. I. Pavlinov, J. H. Kang, B. Ghidini, Gaute Øvrebekk, P. Di Nezza, G. Nazarov, A.P. de Haas, O. V. Fateev, P. G. Innocenti, J. Castillo Castellanos, A. Maŕin, Dousatsu Sakata, E. Montes, Peter Glassel, F. Prino, Y. Sibiriak, Rinaldo Rui, D. Emschermann, M. Fusco Girard, Igor Pshenichnov, K. J. Malagalage, R. W. Fearick, Francesco Barile, L. V. Bravina, Kristjan Herlache Gulbrandsen, I. Das, R. Kupczak, O.M. Listratenko, J. de Cuveland, Franco Meddi, Dmitry Aleksandrov, Franck Manso, M. Oldenburg, E. Kang, C. Yang, Claudiu Cornel Schiaua, Davide Falchieri, Sandra Moretto, Jovan Milosevic, Andrea Danu, P. Ladron de Guevara, Johannes Peter Wessels, B. Pommeresch, M. Estienne, Joakim Nystrand, J. Peyré, E. Almaráz Aviña, A. Dobrin, G. Mazza, A. Di Mauro, Dong Jo Kim, Alberto Baldisseri, A.S. Vodopianov, P.A. Polozov, M. G. Poghosyan, Boris Wagner, Chiara Bianchin, Roberta Ferretti, Benjamin Donigus, R.J.M. Snellings, Peter Braun-Munzinger, Sanjeev Singh Sambyal, F. Navach, S.A. Sadovsky, G. M. Urciuoli, M.L. Luvisetto, J. Ulery, Tiziano Virgili, G. Odyniec, Pietro Cortese, S. Bablok, R. Lietava, Philippe Rosnet, F. Staley, Ralf Keidel, Z. L. Matthews, Christian Claude Kuhn, G. P. Capitani, Peter Levai, M. A. Braun, S. Kapusta, R. Bellwied, S. Gang, H. Appelshäuser, Ketil Røed, E. S. Conner, G. Stefanini, P. Cerello, Alexandru Bercuci, A. Piccotti, T. Krawutschke, Sergey Nikolaev, M. Masetti, R. Wan, Sergey Nikulin, Eugenio Scapparone, Thomas Humanic, G. Dellacasa, E. Kornaś, Peter Kalinak, Valery Punin, F. Minafra, J. Wiechula, S.A. Zaporozhets, Adriana Telesca, Cvetan Valeriev Cheshkov, A. I. Zinchenko, S. Coli, S. Navin, Maya Hachiya Shimomura, A. Maire, M. R. Dutta Majumdar, J. S. Real, Ionut Cristian Arsene, Ivan Kralik, Miroslav Pikna, Mario Sitta, R. Arceo, Kathrin Koch, L. Riccati, Arturo Tauro, Giacomo Contin, K. Ma, G.S. Shabratova, S. Lu, S. Román López, Gennady Zinovjev, K. Antipin, H. Torii, Dieter Røhrich, K. Kozlov, K. Shtejer, Paolo Martinengo, S. Bose, Alessandro Ferretti, Adam Ryszard Kisiel, Costin Grigoras, F. Poggio, V. Zycháček, Alberto Masoni, Fiorella Fionda, Thomas Peitzmann, Y. Mao, J. S. Kim, Alexei Khanzadeev, M. Cherney, Thomas Michael Cormier, H. Bøggild, J. Kral, E. Stenlund, J. Lehnert, P. L.M. Podesta Lerma, R. Kour, D. W. Kim, Basanta Kumar Nandi, Svein Lindal, Kristin Fanebust Hetland, Svetlana Kushpil, S. Aguilar Salazar, R. De Remigis, D. Soyk, Yongsun Kim, D. S. Hwang, Sergio Vergara, Y. Zoccarato, M. Campbell, I. León Monzón, C. Cicalo, T. V. Moukhanova, Guy Paic, Roberto Divia, G. Cara Romeo, Yvonne Chiara Pachmayer, D. J. Tapia Takaki, Lamia Benhabib, Mohd Danish Azmi, Peter Malzacher, S. Kniege, Jason Newby, C. W. Son, C. Bombonati, M. López Noriega, T. S. Räihä, F. Osmic, Dmitry Blau, C. Roy, Frederic Lefevre, H. H. Gutbrod, Jean-Pierre Cussonneau, Andres Sandoval, Roberta Arnaldi, U. Abeysekara, Romualdo Santoro, Gilda Scioli, A. Palaha, Richa Gupta, L. Díaz, I. E. Yushmanov, A. Tournaire, Lijiao Liu, C. Hernández, D. Vranic, Vitaly Loginov, Pablo Saiz, Yongwook Baek, Kenneth Francis Read, Podist Kurashvili, A. Kamal, Y. P. Viyogi, A. V. Kazantsev, N. Miftakhov, Jogender Saini, Håvard Helstrup, G. Laurenti, G. Tsiledakis, T. Malkiewicz, T. C. Awes, Kyoichiro Ozawa, G. Tejeda Muñoz, G. Puddu, Ozgur Cobanoglu, A. Jusko, T. Breitner, R. Varma, Z. Vilakazi, Giuseppe Simonetti, D. P. Kikola, Ralf Peter Averbeck, Paolo Pagano, B. V.K.S. Potukuchi, E. Chiavassa, V. Petráček, Ruben Shahoyan, Janka Vrlakova, Tomoya Tsuji, A. Yasnopolsky, D. Semenov, Myunggeun Song, Jurgen Schukraft, V. Posṕisil, Christian Lippmann, Rama Narayana Singaraju, Julien Faivre, Djuvsland, J. R. Lutz, Laboratoire SUBATECH Nantes (SUBATECH), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Corpusculaire - Clermont-Ferrand (LPC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), 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), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), ALICE, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Centre de Calcul de l'IN2P3 (CC-IN2P3), 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 de Nantes (UN)-Mines Nantes (Mines Nantes), 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)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), K., Aamodt78, N., Abel43, U., Abeysekara30, A., Abrahantes Quintana42, D., Adamova ́86, M. M., Aggarwal25, G., Aglieri Rinella40, A. G., Agocs18, S., Aguilar Salazar66, Z., Ahammed55, A., Ahmad2, N., Ahmad2, S. U., Ahn50 i, R., Akimoto100, A., Akindinov68, D., Aleksandrov70, B. A. l. e. s. s. a. n. d. r. o. 1 0 2, R. . A. l. f. a. r. o. M. o. l. i. n. a. 6 6, A. . A. l. i. c. i. 1 3, E. . A. l. m. a. r. a. ́ z. A. v. i. n. ̃ a. 6 6, J. . A. l. m. e., 8, T., Alt43 ii, V., Altini5, S., Altinpinar32, C., Andrei17, A., Andronic32, G., Anelli40, V., Angelov43 ii, C., Anson27, T., Anticˇic ́113, F., Antinori40 iii, S., Antinori13, K., Antipin37, D., Anton ́czyk37, P., Antonioli14, A., Anzo66, L., Aphecetche73, H., Appelsha ̈user37, S., Arcelli13, R., Arceo66, A., Arend37, N., Armesto92, R., Arnaldi102, T., Aronsson74, I. C., Arsene78 iv, A., Asryan98, A., Augustinus40, R., Averbeck32, T. C., Awes76, J. A., ̈ysto ̈49, M. D., Azmi2, S., Bablok8, M., Bach36, A., Badala`24, Y. W., Baek50 i, S., Bagnasco102, R., Bailhache32 v, R., Bala101, A., Baldisseri89, A., Baldit26, J., Ba ́n58, R., Barbera23, G. G., Barnafo ̈ldi18, L., Barnby12, V., Barret26, J., Bartke29, F., Barile5, M., Basile13, V., Basmanov94, N., Bastid26, B., Bathen72, G., Batigne73, B., Batyunya35, C., Baumann72 v, I. G., Bearden28, B., Becker20 vi, I., Belikov99, R., Bellwied34, E., Belmont Moreno66, A., Belogianni4, L., Benhabib73, S., Beole101, I., Berceanu17, A., Bercuci32 vii, E., Berdermann32, Y., Berdnikov39, L., Betev40, A., Bhasin48, A. K., Bhati25, L., Bianchi101, N., Bianchi38, C., Bianchin79, J., Bielcˇ ́ık81, J., Bielcˇ ́ıkova ́86, A., Bilandzic3, L., Bimbot77, E., Biolcati101, A., Blanc26, F., Blanco23 viii, F., Blanco63, D., Blau70, C., Blume37, M., Boccioli40, N., Bock27, A., Bogdanov69, H., Bøggild28, M., Bogolyubsky83, J., Bohm96, L., Boldizsa ́r18, M., Bombara12 ix, C., Bombonati79 x, M., Bondila49, H., Borel89, V., Borshchov51, A., Borisov52, C., Bortolin79 xl, S., Bose54, Bosisio, Luciano, F., Bossu ́101, M., Botje3, S., Bo ̈ttger43, G., Bourdaud73, B., Boyer77, M., Braun98, P., Braun Munzinger32, 33, Ii, L., Bravina78, Bregant, Marco, T., Breitner43, G., Bruckner40, R., Brun40, E., Bruna74, G. E., Bruno5, D., Budnikov94, H., Buesching37, P., Buncic40, O., Busch44, Z., Buthelezi22, D., Caffarri79, X., Cai111, H., Caines74, E., Camacho64, Camerini, Paolo, M., Campbell40, V., Canoa Roman40, G. P., Capitani38, G., Cara Romeo14, F., Carena40, W., Carena40, F., Carminati40, A. Casanova D., ́ıaz38, M., Caselle40, J., Castillo Castellanos89, J. F., Castillo Hernandez32, V., Catanescu17, E., Cattaruzza103, C., Cavicchioli40, P., Cerello102, V., Chambert77, B., Chang96, S., Chapeland40, A., Charpy77, J. L., Charvet89, S., Chattopadhyay54, S., Chattopadhyay55, M., Cherney30, C., Cheshkov40, B., Cheynis62, E., Chiavassa101, V., Chibante Barroso40, D. D., Chinellato21, P., Chochula40, K., Choi85, M., Chojnacki106, P., Christakoglou106, C. H., Christensen28, P., Christiansen61, T., Chujo105, F., Chuman45, C., Cicalo20, L., Cifarelli13, F., Cindolo14, J., Cleymans22, O., Cobanoglu101, J. P., Coffin99, S., Coli102, A., Colla40, G., Conesa Balbastre38, Z., Conesa del Valle73 xii, E. S., Conner110, P., Constantin44, Contin, Giacomo, G. J., Contreras64, Y., Corrales Morales101, T. M., Cormier34, P., Cortese1, I. Corte ́ s., Maldonado84, M. R., Cosentino21, F., Costa40, M. E., Cotallo63, E., Crescio64, P., Crochet26, E., Cuautle65, L., Cunqueiro38, J., Cussonneau73, A., Dainese59 iii, H. H., Dalsgaard28, A., Danu16, I., Das54, S., Das54, A., Dash11, S., Dash11, G. O. V., de Barros93, A., De Caro90, G. de Cataldo6 J., de Cuveland43 ii, A., De Falco19, M., De Gaspari44, J., de Groot40, D., De Gruttola90, A. P. de Haas106 N., De Marco102, S., De Pasquale90, R., De Remigis102, R., de Rooij106, G., de Vaux22, H., Delagrange73, G., Dellacasa1, A., Deloff107, V., Demanov94, E., De ́nes18, A., Deppman93, G., D’Erasmo5, D., Derkach98, A., Devaux26, – 27 – D., Di Bari5, C., Di Giglio5 x, S., Di Liberto88, A., Di Mauro40, P., Di Nezza38, M., Dialinas73, L. D., ́ıaz65, R. D., ́ıaz49, T., Dietel72, H., Ding111, R., Divia`40, Ø., Djuvsland8, V., Dobretsov70, A., Dobrin61, T., Dobrowolski107, B., Do ̈nigus32, I., Dom ́ınguez65, D. M. M. Don46 O., Dordic78, A. K., Dubey55, J., Dubuisson40, L., Ducroux62, P., Dupieux26, A. K., Dutta Majumdar54, M. R., Dutta Majumdar55, D., Elia6, D., Emschermann44 xiv, A., Enokizono76, B., Espagnon77, M., Estienne73, D., Evans12, S., Evrard40, G., Eyyubova78, C. W., Fabjan40 xv, D., Fabris79, J., Faivre41, D., Falchieri13, A., Fantoni38, M., Fasel32, O., Fateev35, R., Fearick22, A., Fedunov35, D., Fehlker8, V., Fekete15, D., Felea16, B., Fenton Olsen28 xvi, G., Feofilov98, A., Ferna ́ndez Te ́llez84, E. G., Ferreiro92, A., Ferretti101, R., Ferretti1 xvii, M. A. S., Figueredo93, S., Filchagin94, R., Fini6, F. M., Fionda5, E. M., Fiore5, M., Floris19 x, Z., Fodor18, S., Foertsch22, P., Foka32, S., Fokin70, F., Formenti40, Fragiacomo, Enrico, M., Fragkiadakis4, U., Frankenfeld32, A., Frolov75, U., Fuchs40, F., Furano40, C., Furget41, M., Fusco Girard90, J. J., Gaardhøje28, S., Gadrat41, M., Gagliardi101, A., Gago64 xviii, M., Gallio101, S., Gang111, P., Ganoti4, M. S., Ganti55, C., Garabatos32, C., Garc ́ıa Trapaga101, J., Gebelein43, R., Gemme1, M., Germain73, A., Gheata40, M., Gheata40, B., Ghidini5, P., Ghosh55, G., Giraudo102, P., Giubellino102, E., Gladysz Dziadus29, R., Glasow72 xix, P., Gla ̈ssel44, A., Glenn60, R., Gomez31, H., Gonza ́lez Santos84, L. H., Gonza ́lez Trueba66, P., Gonza ́lez Zamora63, S., Gorbunov43 ii, Y., Gorbunov30, S., Gotovac97, H., Gottschlag72, V., Grabski66, R., Grajcarek44, A., Grelli106, A., Grigoras40, C., Grigoras40, V., Grigoriev69, A., Grigoryan112, S., Grigoryan35, B., Grinyov52, N., Grion104, P., Gros61, J. F., Grosse Oetringhaus40, J. Y., Grossiord62, Grosso, Raffaele, C., Guarnaccia90, F., Guber67, R., Guernane41, B., Guerzoni13, K., Gulbrandsen28, H., Gulkanyan112, T., Gunji100, A., Gupta48, R., Gupta48, H. A., Gustafsson61, H., Gutbrod32, Ø., Haaland8, C., Hadjidakis77, M., Haiduc16, H., Hamagaki100, G., Hamar18, J., Hamblen53, B. H., Han95, J. 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Subjects
Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, perspective, High Energy Phisics, Detector alignment and calibration methods (lasers, sources, particle-beams), Particle tracking detectors (Solid-state detectors), Instrumentation, Mathematical Physics, 01 natural sciences, 7. Clean energy, law.invention, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), law, Particle tracking detectors, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Tracking detectors, Heavy Ion Physics, Detectors and Experimental Techniques, Detector alignment and calibration methods, Nuclear Experiment, physics.ins-det, detectors, Physics, Large Hadron Collider, Solenoidal vector field, Detector, Instrumentation and Detectors (physics.ins-det), particle-beams), collisions, Detector alignment and calibration methods (lasers, sources, collaboration, detector alignment and calibration methods (lasers, particle tracking detectors (solid-state detectors), performance, quark-gluon plasma, Colliding beam accelerators, collisions, Pb-Pb collisions, QUARK-GLUON PLASMA, Detector alignment and calibration method, FOS: Physical sciences, Cosmic ray, 114 Physical sciences, Nuclear physics, Optics, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Collider, Pixel, 010308 nuclear & particles physics, business.industry, hep-ex, Quark–gluon plasma, ALICE (propellant), business
Abstract

ALICE (A Large Ion Collider Experiment) is the LHC (Large Hadron Collider) experiment devoted to investigating the strongly interacting matter created in nucleus-nucleus collisions at the LHC energies. The ALICE ITS, Inner Tracking System, consists of six cylindrical layers of silicon detectors with three different technologies; in the outward direction: two layers of pixel detectors, two layers each of drift, and strip detectors. The number of parameters to be determined in the spatial alignment of the 2198 sensor modules of the ITS is about 13,000. The target alignment precision is well below 10 micron in some cases (pixels). The sources of alignment information include survey measurements, and the reconstructed tracks from cosmic rays and from proton-proton collisions. The main track-based alignment method uses the Millepede global approach. An iterative local method was developed and used as well. We present the results obtained for the ITS alignment using about 10^5 charged tracks from cosmic rays that have been collected during summer 2008, with the ALICE solenoidal magnet switched off., 37 pages, 15 captioned figures, 1 table, published version, figures at http://aliceinfo.cern.ch/ArtSubmission/node/3907

Published
2010

41. Two-pion Bose-Einstein correlations in pp collitions at sqrt(s)=900 GeV

Author

K. AAMODT, N. ABEL, U. ABEYSEKARA, A. ABRAHANTES QUINTANA, A. ACERO, D. ADAMOVA, M. M. AGGARWAL, G. AGLIERI RINELLA, A. G. AGOCS, S. AGUILAR SALAZAR, Z. AHAMMED, A. AHMAD, N. AHMAD, S. U. AHN, R. AKIMOTO, A. AKINDINOV, D. ALEKSANDROV, B. ALESSANDRO, R. ALFARO MOLINA, A. ALICI, E. ALMARAZ AVINA, J. ALME, T. ALT, V. ALTINI, S. ALTINPINAR, C. ANDREI, A. ANDRONIC, G. ANELLI, V. ANGELOV, C. ANSON, T. ANTICIC, F. ANTINORI, S. ANTINORI, K. ANTIPIN, D. ANTONCZYK, P. ANTONIOLI, A. ANZO, L. APHECETCHE, H. APPELSHAUSER, R. ARCEO, A. AREND, N. ARMESTO, R. ARNALDI, T. ARONSSON, I. C. ARSENE, A. ASRYAN, A. AUGUSTINUS, R. AVERBECK, T. C. AWES, J. AYSTO, M. D. AZMI, S. BABLOK, M. BACH, A. BADALA, Y. W. BAEK, S. BAGNASCO, R. BAILHACHE, R. BALA, A. BALDISSERI, A. BALDIT, J. BAN, R. BARBERA, G. G. BARNAFOLDI, L. BARNBY, V. BARRET, J. BARTKE, F. BARILE, V. BASMANOV, N. BASTID, B. BATHEN, G. BATIGNE, B. BATYUNYA, C. BAUMANN, I. G. BEARDEN, B. BECKER, I. BELIKOV, R. BELLWIED, E. BELMONT MORENO, A. BELOGIANNI, L. BENHABIB, S. BEOLE, I. BERCEANU, A. BERCUCI, E. BERDERMANN, Y. BERDNIKOV, L. BETEV, A. BHASIN, A. K. BHATI, L. BIANCHI, N. BIANCHI, C. BIANCHIN, J. BIELCIK, J. BIELCIKOVA, A. BILANDZIC, L. BIMBOT, E. BIOLCATI, A. BLANC, F. BLANCO, D. BLAU, C. BLUME, M. BOCCIOLI, N. BOCK, A. BOGDANOV, H. BOGGILD, M. BOGOLYUBSKY, J. BOHM, L. BOLDIZSAR, M. BOMBARA, C. BOMBONATI, M. BONDILA, H. BOREL, V. BORSHCHOV, C. BORTOLIN, S. BOSE, L. BOSISIO, F. BOSSU, M. BOTJE, S. BOTTGER, G. BOURDAUD, B. BOYER, M. BRAUN, P. BRAUN MUNZINGER, L. BRAVINA, M. BREGANT, T. BREITNER, G. BRUCKNER, R. BRUN, E. BRUNA, G. E. BRUNO, D. BUDNIKOV, H. BUESCHING, K. BUGAEV, P. BUNCIC, O. BUSCH, Z. BUTHELEZI, D. CAFFARRI, X. CAI, H. CAINES, E. CAMACHO, P. CAMERINI, M. CAMPBELL, V. CANOA ROMAN, G. P. CAPITANI, G. CARA ROMEO, F. CARENA, W. CARENA, F. CARMINATI, A. CASANOVA DIAZ, M. CASELLE, J. CASTILLO CASTELLANOS, J. F. CASTILLO HERNANDEZ, V. CATANESCU, E. CATTARUZZA, C. CAVICCHIOLI, P. CERELLO, V. CHAMBERT, B. 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KAZANTSEV, U. KEBSCHULL, R. KEIDEL, M. M. KHAN, S. A. KHAN, A. KHANZADEEV, Y. KHARLOV, D. KIKOLA, B. KILENG, D. J KIM, D. S. KIM, D. W. KIM, H. N. KIM, J. KIM, J. H. KIM, J. S. KIM, M. KIM, S. H. KIM, S. KIM, Y. KIM, S. KIRSCH, I. KISEL, S. KISELEV, A. KISIEL, J. L. KLAY, J. KLEIN, C. KLEIN, M. KLIEMANT, A. KLOVNING, A. KLUGE, S. KNIEGE, K. KOCH, R. KOLEVATOV, A. KOLOJVARI, V. KONDRATIEV, N. KONDRATYEVA, A. KONEVSKIH, E. KORNAS, R. KOUR, M. KOWALSKI, S. KOX, K. KOZLOV, J. KRAL, I. KRALIK, F. KRAMER, I. KRAUS, A. KRAVCAKOVA, T. KRAWUTSCHKE, M. KRIVDA, D. KRUMBHORN, M. KRUS, E. KRYSHEN, M. KRZEWICKI, Y. KUCHERIAEV, C. KUHN, P. G. KUIJER, L. KUMAR, N. KUMAR, R. KUPCZAK, P. KURASHVILI, A. KUREPIN, A. N. KUREPIN, A. KURYAKIN, S. KUSHPIL, V. KUSHPIL, M. KUTOUSKI, H. KVAERNO, M. J. KWEON, Y. KWON, P. LA ROCCA, F. LACKNER, P. LADRON DE GUEVARA, V. LAFAGE, C. LAL, C. LARA, D. T. LARSEN, G. LAURENTI, C. LAZZERONI, Y. LE BORNEC, N. LE BRIS, H. LEE, K. S. LEE, S. C. LEE, F. LEFEVRE, M. LENHARDT, L. LEISTAM, J. LEHNERT, V. LENTI, H. LEON, I. LEON MONZON, H. LEON VARGAS, P. LEVAI, Y. LI, R. LIETAVA, S. LINDAL, V. LINDENSTRUTH, C. LIPPMANN, M. A. LISA, O. LISTRATENKO, L. LIU, V. LOGINOV, S. LOHN, X. LOPEZ, M. LOPEZ NORIEGA, R. LOPEZ-RAMIREZ, E. LOPEZ TORRES, G. LOVHOIDEN, A. LOZEA FEIJO SOARES, S. LU, M. LUNARDON, G. LUPARELLO, L. LUQUIN, J. -R. LUTZ, M. LUVISETTO, K. MA, R. MA, D. M. MADAGODAHETTIGE-DON, A. MAEVSKAYA, M. MAGER, A. MAHAJAN, D. P. MAHAPATRA, A. MAIRE, I. MAKHLYUEVA, D. MAL~RKEVICH, M. MALAEV, I. MALDONADO CERVANTES, M. MALEK, T. MALKIEWICZ, P. MALZACHER, A. MAMONOV, L. MANCEAU, L. MANGOTRA, V. MANKO, F. MANSO, V. MANZARI, Y. MAO, J. MARES, G. V. MARGAGLIOTTI, A. MARGOTTI, A. MARIN, I. MARTASHVILI, P. MARTINENGO, M. I. MARTINEZ, A. MARTINEZ DAVALOS, G. MARTINEZ GARCIA, Y. MARUYAMA, A. MARZARI CHIESA, S. MASCIOCCHI, M. MASERA, M. MASETTI, A. MASONI, L. MASSACRIER, M. MASTROMARCO, A. MASTROSERIO, Z. L. MATTHEWS, B. MATTOS TAVARES, A. MATYJA, D. MAYANI, G. MAZZA, M. A. MAZZONI, F. MEDDI, A. MENCHACA-ROCHA, P. MENDEZ LORENZO, M. MEONI, J. MERCADO PEREZ, P. MEREU, Y. MIAKE, A. MICHALON, N. MIFTAKHOV, J. MILOSEVIC, F. MINAFRA, A. MISCHKE, D. MISKOWIEC, C. MITU, K. MIZOGUCHI, J. MLYNARZ, B. MOHANTY, L. MOLNAR, M. M. MONDAL, L. MONTANO ZETINA, M. MONTENO, E. MONTES, M. MORANDO, S. MORETTO, A. MORSCH, T. MOUKHANOVA, V. MUCCIFORA, E. MUDNIC, S. MUHURI, H. MULLER, M. G. MUNHOZ, J. MUNOZ, L. MUSA, A. MUSSO, B. K. NANDI, R. NANIA, E. NAPPI, F. NAVACH, S. NAVIN, T. K. NAYAK, S. NAZARENKO, G. NAZAROV, A. NEDOSEKIN, F. NENDAZ, J. NEWBY, A. NIANINE, M. NICASSIO, B. S. NIELSEN, S. NIKOLAEV, V. NIKOLIC, S. NIKULIN, V. NIKULIN, B. S. NILSEN, M. S. NILSSON, F. NOFERINI, P. NOMOKONOV, G. NOOREN, N. NOVITZKY, A. NYATHA, C. NYGAARD, A. NYIRI, J. NYSTRAND, A. OCHIROV, G. ODYNIEC, H. OESCHLER, M. OINONEN, K. OKADA, Y. OKADA, M. OLDENBURG, J. OLENIACZ, C. OPPEDISANO, F. ORSINI, A. ORTIZ VELAZQUEZ, G. ORTONA, C. OSKAMP, A. OSKARSSON, F. OSMIC, L. OSTERMAN, P. OSTROWSKI, I. OTTERLUND, J. OTWINOWSKI, G. OVREBEKK, K. OYAMA, K. OZAWA, Y. PACHMAYER, M. PACHR, F. PADILLA, P. PAGANO, G. PAIC, F. PAINKE, C. PAJARES, S. PAL, S. K. PAL, A. PALAHA, A. PALMERI, R. PANSE, G. S. PAPPALARDO, W. J. PARK, B. PASTIRCAK, C. PASTORE, V. PATICCHIO, A. PAVLINOV, T. PAWLAK, T. PEITZMANN, A. PEPATO, H. PEREIRA, D. PERESSOUNKO, C. PEREZ, D. PERINI, D. PERRINO, W. PERYT, J. PESCHEK, A. PESCI, V. PESKOV, Y. PESTOV, A. J. PETERS, V. PETRACEK, A. PETRIDIS, M. PETRIS, P. PETROV, M. PETROVICI, C. PETTA, J. PEYRE, S. PIANO, A. PICCOTTI, M. PIKNA, P. PILLOT, L. PINSKY, N. PITZ, F. PIUZ, R. PLATT, M. PLOSKON, J. PLUTA, T. POCHEPTSOV, S. POCHYBOVA, P. L. M. PODESTA LERMA, F. POGGIO, M. G. POGHOSYAN, K. POLAK, B. POLICHTCHOUK, P. POLOZOV, V. POLYAKOV, B. POMMERESCH, A. POP, F. POSA, V. POSPISIL, B. POTUKUCHI, J. POUTHAS, S. K. PRASAD, R. PREGHENELLA, F. PRINO, C. A. PRUNEAU, I. PSHENICHNOV, G. PUDDU, P. PUJAHARI, A. PULVIRENTI, A. PUNIN, V. PUNIN, M. PUTIS, J. PUTSCHKE, E. QUERCIGH, A. RACHEVSKI, A. RADEMAKERS, S. RADOMSKI, T. S. RAIHA, J. RAK, A. RAKOTOZAFINDRABE, L. RAMELLO, A. RAMIREZ REYES, M. RAMMLER, R. RANIWALA, S. RANIWALA, S. RASANEN, I. RASHEVSKAYA, S. RATH, K. F. READ, J. REAL, K. REDLICH, R. RENFORDT, A. R. REOLON, A. RESHETIN, F. RETTIG, J. -P. REVOL, K. REYGERS, H. RICAUD, L. RICCATI, R. A. RICCI, M. RICHTER, P. RIEDLER, W. RIEGLER, F. RIGGI, A. RIVETTI, M. RODRIGUEZ CAHUANTZI, K. ROED, D. ROHRICH, S. ROMAN LOPEZ, R. ROMITA, F. RONCHETTI, P. ROSINSKY, P. ROSNET, S. ROSSEGGER, A. ROSSI, F. ROUKOUTAKIS, S. ROUSSEAU, C. ROY, P. ROY, A. J. RUBIO-MONTERO, R. RUI, I. RUSANOV, G. RUSSO, E. RYABINKIN, A. RYBICKI, S. SADOVSKY, K. SAFARIK, R. SAHOO, J. SAINI, P. SAIZ, D. SAKATA, C. A. SALGADO, R. SALGUEIRO DOMINQUES DA SILVA, S. SALUR, T. SAMANTA, S. SAMBYAL, V. SAMSONOV, L. SANDOR, A. SANDOVAL, M. SANO, S. SANO, R. SANTO, R. SANTORO, J. SARKAMO, P. SATURNINI, E. SCAPPARONE, F. SCARLASSARA, R. P. SCHARENBERG, C. SCHIAUA, R. SCHICKER, H. SCHINDLER, C. SCHMIDT, H. R. SCHMIDT, S. SCHREINER, S. SCHUCHMANN, J. SCHUKRAFT, Y. SCHUTZ, K. SCHWARZ, K. SCHWEDA, G. SCIOLI, E. SCOMPARIN, G. SEGATO, D. SEMENOV, S. SENYUKOV, J. SEO, S. SERCI, L. SERKIN, E. SERRADILLA, A. SEVCENCO, I. SGURA, G. SHABRATOVA, R. SHAHOYAN, G. SHARKOV, N. SHARMA, S. SHARMA, K. SHIGAKI, M. SHIMOMURA, K. SHTEJER, Y. SIBIRIAK, M. SICILIANO, E. SICKING, E. SIDDI, T. SIEMIARCZUK, A. SILENZI, D. SILVERMYR, E. SIMILI, G. SIMONETTI, R. SINGARAJU, R. SINGH, V. SINGHAL, B. C. SINHA, T. SINHA, B. SITAR, M. SITTA, T. B. SKAALI, K. SKJERDAL, R. SMAKAL, N. SMIRNOV, R. SNELLINGS, H. SNOW, C. SOGAARD, O. SOKOLOV, A. SOLOVIEV, H. K. SOLTVEIT, R. SOLTZ, W. SOMMER, C. W. SON, H. S. SON, M. SONG, C. SOOS, F. SORAMEL, D. SOYK, M. SPYROPOULOU-STASSINAKI, B. K. SRIVASTAVA, J. STACHEL, F. STALEY, I. STAN, G. STEFANEK, G. STEFANINI, T. STEINBECK, E. STENLUND, G. STEYN, D. STOCCO, R. STOCK, P. STOLPOVSKY, P. STRMEN, A. A. P. SUAIDE, M. A. SUBIETA VASQUEZ, T. SUGITATE, C. SUIRE, M. SUMBERA, T. SUSA, D. SWOBODA, T. J. M. SYMONS, A. SZANTO DE TOLEDO, I. SZARKA, A. SZOSTAK, M. SZUBA, M. TADEL, C. TAGRIDIS, A. TAKAHARA, J. TAKAHASHI, R. TANABE, J. D. TAPIA TAKAKI, H. TAUREG, A. TAURO, M. TAVLET, G. TEJEDA MUNOZ, A. TELESCA, C. TERREVOLI, J. THADER, R. TIEULENT, D. TLUSTY, A. TOIA, T. TOLYHY, C. TORCATO DE MATOS, H. TORII, G. TORRALBA, L. TOSCANO, F. TOSELLO, A. TOURNAIRE, T. TRACZYK, P. TRIBEDY, G. TROGER, D. TRUESDALE, W. H. TRZASKA, G. TSILEDAKIS, E. TSILIS, T. TSUJI, A. TUMKIN, R. TURRISI, A. TURVEY, T. S. TVETER, H. TYDESJO, K. TYWONIUK, J. ULERY, K. ULLALAND, A. URAS, J. URBAN, G. M. URCIUOLI, G. L. USAI, A. VACCHI, M. VALA, L. VALENCIA PALOMO, S. VALLERO, A. VAN DEN BRINK, N. VAN DER KOLK, P. VANDE VYVRE, M. VAN LEEUWEN, L. VANNUCCI, A. VARGAS, R. VARMA, A. VASILIEV, I. VASSILIEV, M. VASSILIOU, V. VECHERNIN, M. VENARUZZO, E. VERCELLIN, S. VERGARA, R. VERNET, M. VERWEIJ, I. VETLITSKIY, L. VICKOVIC, G. VIESTI, O. VIKHLYANTSEV, Z. VILAKAZI, O. VILLALOBOS BAILLIE, A. VINOGRADOV, L. VINOGRADOV, Y. VINOGRADOV, T. VIRGILI, Y. P. VIYOGI, A. VODOPIANOV, K. VOLOSHIN, S. VOLOSHIN, G. VOLPE, B. VON HALLER, D. VRANIC, J. VRLAKOVA, B. VULPESCU, B. WAGNER, V. WAGNER, L. WALLET, R. WAN, D. WANG, Y. WANG, K. WATANABE, Q. WEN, J. WESSELS, J. WIECHULA, J. WIKNE, A. WILK, G. WILK, M. C. S. WILLIAMS, N. WILLIS, B. WINDELBAND, C. XU, C. YANG, H. YANG, A. YASNOPOLSKY, F. YERMIA, J. YI, Z. YIN, H. YOKOYAMA, I. -K. YOO, X. YUAN, I. YUSHMANOV, E. ZABRODIN, B. ZAGREEV, A. ZALITE, C. ZAMPOLLI, YU. ZANEVSKY, S. ZAPOROZHETS, A. ZAROCHENTSEV, P. ZAVADA, H. ZBROSZCZYK, P. ZELNICEK, A. ZENIN, A. ZEPEDA, I. ZGURA, M. ZHALOV, X. ZHANG, D. ZHOU, S. ZHOU, J. ZHU, A. ZICHICHI, A. ZINCHENKO, G. ZINOVJEV, M. ZINOVJEV, Y. ZOCCARATO, and V. ZYCHACEK

Published
2010

42. Less-structured time in children’s daily lives predicts self-directed executive functioning

Author

Jane E. Barker, Lindsay S. Provan, Laura Michaelson, Hannah R. Snyder, Andrei D. Semenov, and Yuko Munakata

Subjects
unstructured activities, Pediatric Research Initiative, Leisure time, lcsh:BF1-990, Psychological intervention, 050105 experimental psychology, Developmental psychology, Task (project management), 03 medical and health sciences, 0302 clinical medicine, Behavioral and Social Science, Cognitive development, Verbal fluency test, Psychology, 0501 psychology and cognitive sciences, Original Research Article, self-directed executive function, General Psychology, Pediatric, 4. Education, 05 social sciences, verbal fluency, Executive functions, leisure time, Mental Health, lcsh:Psychology, Categorization, Cognitive Sciences, 030217 neurology & neurosurgery, cognitive development
Abstract

Executive functions in childhood predict important life outcomes. Thus, there is great interest in attempts to improve executive functions early in life. Many interventions are led by trained adults, including structured training activities in the lab, and less-structured activities implemented in schools. Such programs have yielded gains in children’s externally-driven executive functioning, where they are instructed on what goal-directed actions to carry out and when. However, it is less clear how children’s experiences relate to their development of self-directed executive functioning, where they must determine on their own what goal-directed actions to carry out and when. We hypothesized that time spent in less-structured activities would give children opportunities to practice self-directed executive functioning, and lead to benefits. To investigate this possibility, we collected information from parents about their 6-7 year-old children’s daily, annual, and typical schedules. We categorized children’s activities as structured or less-structured based on categorization schemes from prior studies on child leisure time use. We assessed children’s self-directed executive functioning using a well-established verbal fluency task, in which children generate members of a category and can decide on their own when to switch from one subcategory to another. The more time that children spent in less-structured activities, the better their self-directed executive functioning. The opposite was true of structured activities, which predicted poorer self-directed executive functioning. These relationships were robust (holding across increasingly strict classifications of structured and less-structured time) and specific (time use did not predict externally-driven executive functioning). We discuss implications, caveats, and ways in which potential interpretations can be distinguished in future work, to advance an understanding of this fundamental aspect of growing up.

Published
2014

43. Heterodyne receiver at 2.5 THz with quantum cascade laser and hot electron bolometric mixer

Author

Lukas Mahler, A. D. Semenov, H. Richter, S.G. Pavlov, Alessandro Tredicucci, Harvey E. Beere, David A. Ritchie, Heinz-Wilhelm Hübers, Jonas Zmuidzinas Wayne S. Holland Stafford Withington William D. Duncan, H. W., Hüber, S. G., Pavlov, H., Richter, A. D., Semenov, L., Mahler, Tredicucci, Alessandro, H. E., Beere, and D. A., Ritchie

Subjects
spectroscopy, heterodyne, Gas laser, Physics::Instrumentation and Detectors, Local oscillator, Superheterodyne receiver, Terahertz, heterodyne receiver, local oscillator, Physics::Optics, quantum cascade laser, law.invention, Laser linewidth, Resonator, Optics, law, Physics::Atomic Physics, Terahertz, quantum cascade lasers, spectroscopy, heterodyne, Astrophysics::Galaxy Astrophysics, Physics, Noise temperature, quantum cascade lasers, business.industry, hot electron bolometer, Laser, business, Quantum cascade laser
Abstract

Quantum cascade lasers (QCLs) operating at 2.5 THz have been used for gas phase spectroscopy and as local oscillator in a heterodyne receiver. One QCL has a Fabry-Perot resonator while the other has a distributed feedback resonator. The linewidth and frequency tunability of both QCLs have been investigated by either mixing two modes of the QCL or by mixing the emission from the QCL with the emission from a 2.5 THz gas laser. The frequency tunability as well as the linewidth is sufficient for Doppler limited spectroscopy of methanol gas. The QCLs have been used successfully as local oscillators in a heterodyne receiver. Noise temperature measurements with a hot electron bolometer and a QCL yielded the same result as with a gas laser as local oscillator.

Published
2006

44. Effect of the wire width on the intrinsic detection efficiency of superconducting-nanowire single-photon detectors

Author

Alexander Korneev, Y. Korneeva, Denis Yu. Vodolazov, Michael Siegel, Konstantin Ilin, Andrey Trifonov, R. Lusche, A. D. Semenov, H.-W. Huebers, and Gregory Goltsman

Subjects
Superconductivity, Materials science, Condensed matter physics, business.industry, Condensed Matter - Superconductivity, Photon detector, Nanowire, General Physics and Astronomy, FOS: Physical sciences, Supraleiter, Superconductivity (cond-mat.supr-con), Quanteneffizienz, Wavelength, Wire width, NbN, Optoelectronics, Cooper pair, business, Photonenzähler
Abstract

Thorough spectral study of the intrinsic single-photon detection efficiency in superconducting TaN and NbN nanowires with different widths shows that the experimental cut-off in the efficiency at near-infrared wavelengths is most likely caused by the local deficiency of Cooper pairs available for current transport. For both materials the reciprocal cut-off wavelength scales with the wire width whereas the scaling factor quantitatively agrees with the hot-spot detection models. Comparison of the experimental data with vortex-assisted detection scenarios shows that these models predict a stronger dependence of the cut-off wavelength on the wire width., 16 pages, 6 figures

Published
2013

45. Light yield in DarkSide-10 : a prototype two-phase argon TPC for dark matter searches

Author

M. D. Skorokhvatov, L. Grandi, Marc S. Seigar, A. G. Cocco, A. Fan, Aldo Romani, S. Kidner, I. N. Machulin, C. Salvo, E. de Haas, D. Semenov, A. Nelson, N. Rossi, Marco Pallavicini, K. Arisaka, D. D'Angelo, E. V. Hungerford, E. V. Unzhakov, G. Fiorillo, Y. Meng, C. Ghag, G. Guray, A. Sotnikov, J. Thompson, G. Bonfini, C. L. Kendziora, W. Sands, F. Gabriele, R. B. Vogelaar, J. Brodsky, P. Saggese, C. Condon, P. Beltrame, S. Davini, B. J. Mount, C. Ghiano, M. Guan, A. Candela, P. J. Mosteiro, David B. Cline, R. Tartaglia, E. Meroni, H. O. Back, K. Keeter, S. Gazzana, M. Zehfus, Peter Daniel Meyers, An. Ianni, Laura Cadonati, F. Perfetto, A. Nemtzow, D. Korablev, Y. Suvorov, S. Westerdale, Hui Wang, A. V. Derbin, A. Brigatti, G. Koh, M. Montuschi, Livia Ludhova, V. N. Muratova, Thomas Alexander, I. Dratchnev, Y. Q. Ma, A. M. Goretti, A. Razeto, N. N. Nurakhov, R. Saldanha, A. S. Chepurnov, C. J. Martoff, J. Tatarowicz, G. Testera, Frank Calaprice, A. E. Chavarria, Cristiano Galbiati, L. Lukyanchenko, G. Zuzel, Fausto Ortica, M. Orsini, C. Guo, Al. Ianni, A. Teymourian, L. Perasso, H. Cao, Gioacchino Ranucci, W. Zhong, Sandra Zavatarelli, G. Korga, P. X. Li, D. Alton, A.V. Etenko, E. Pantic, Austin P. Lund, M. Gromov, R. Parsells, P. Cavalcante, G. Di Pietro, A. Empl, N. Pelliccia, J. Maricic, E. Shields, C. Love, T. Mohayai, Paolo Lombardi, S. V. Sukhotin, A. Wright, V. V. Kobychev, K. Lung, B. Loer, Jay Burton Benziger, Chung-Yao Yang, Lawrence Pinsky, A. Kayunov, D. Montanari, D. Durben, A. Pocar, Jilei Xu, O. Smirnov, S. Parmeggiano, Marcin Wójcik, S. Pordes, K. Fomenko, Alexander, T., Alton, D., Arisaka, K., Back, H. O., Beltrame, P., Benziger, J., Bonfini, G., Brigatti, A., Brodsky, J., Cadonati, L., Calaprice, F., Candela, A., Cao, H., Cavalcante, P., Chavarria, A., Chepurnov, A., Cline, D., Cocco, A. G., Condon, C., D'Angelo, D., Davini, S., Haas, E. D., Derbin, A., Pietro, G. D., Dratchnev, I., Durben, D., Empl, A., Etenko, A., Fan, A., Fiorillo, Giuliana, Fomenko, K., Gabriele, F., Galbiati, C., Gazzana, S., Ghag, C., Ghiano, C., Goretti, A., Grandi, L., Gromov, M., Guan, M., Guo, C., Guray, G., Hungerford, E. V., Ianni, A., Kayunov, A., Keeter, K., Kendziora, C., Kidner, S., Kobychev, V., Koh, G., Korablev, D., Korga, G., Shields, E., Li, P., Loer, B., Lombardi, P., Love, C., Ludhova, L., Lukyanchenko, L., Lund, A., Lung, K., Ma, Y., Machulin, I., Maricic, J., Martoff, C. J., Meng, Y., Meroni, E., Meyers, P. D., Mohayai, T., Montanari, D., Montuschi, M., Mosteiro, P., Mount, B., Muratova, V., Nelson, A., Nemtzow, A., Nurakhov, N., Orsini, M., Ortica, F., Pallavicini, M., Pantic, E., Parmeggiano, S., Parsells, R., Pelliccia, N., Perasso, L., Perfetto, F., Pinsky, L., Pocar, A., Pordes, S., Ranucci, G., Razeto, A., Romani, A., Rossi, N., Saggese, P., Saldanha, R., Salvo, C., Sands, W., Seigar, M., Semenov, D., Skorokhvatov, M., Smirnov, O., Sotnikov, A., Sukhotin, S., Suvorov, Y., Tartaglia, R., Tatarowicz, J., Testera, G., Teymourian, A., Thompson, J., Unzhakov, E., Vogelaar, R. B., Wang, H., Westerdale, S., Wojcik, M., Wright, A., Xu, J., Yang, C., Zavatarelli, S., Zehfus, M., Zhong, W., and Zuzel, G.

Subjects
Physics::Instrumentation and Detectors, Dark matter, light yield, FOS: Physical sciences, chemistry.chemical_element, dark matter, law.invention, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), XENON, law, DEPENDENCE, LIQUID ARGON, PARTICLES, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Scintillation, Time projection chamber, Argon, Gamma ray, Astronomy and Astrophysics, Laser, time projection chamber, chemistry, Yield (chemistry), Scintillation counter, argon, High Energy Physics::Experiment, Astrophysics - Instrumentation and Methods for Astrophysics, photoelectron yield
Abstract

As part of the DarkSide program of direct dark matter searches using liquid argon TPCs, a prototype detector with an active volume containing 10 kg of liquid argon, DarkSide-10, was built and operated underground in the Gran Sasso National Laboratory in Italy. A critically important parameter for such devices is the scintillation light yield, as photon statistics limits the rejection of electron-recoil backgrounds by pulse shape discrimination. We have measured the light yield of DarkSide-10 using the readily-identifiable full-absorption peaks from gamma ray sources combined with single-photoelectron calibrations using low-occupancy laser pulses. For gamma lines of energies in the range 122-1275 keV, we get consistent light yields averaging 8.887+-0.003(stat)+-0.444(sys) p.e./keVee. With additional purification, the light yield measured at 511 keV increased to 9.142+-0.006(stat) p.e./keVee., 10 pages, 7 figures, Accepted for publication in Astroparticle Physics

Published
2013

46. Unconventional superconductivity in ultrathin superconducting NbN films studied by scanning tunneling spectroscopy

Author

Dimitri Roditchev, Christophe Brun, V. Cherkez, C. Carbillet, François Debontridder, Tristan Cren, A. D. Semenov, Y. Noat, Heinz-Wilhelm Hübers, Michael Siegel, Konstantin Ilin, Institut des Nanosciences de Paris (INSP), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Superconductivity, Physics, Phase transition, sacnning tunneling, Condensed matter physics, superconductivity, Scanning tunneling spectroscopy, 02 engineering and technology, 021001 nanoscience & nanotechnology, Condensed Matter Physics, 01 natural sciences, Electronic, Optical and Magnetic Materials, Magnetic field, Vortex, Homogeneous, Lattice (order), magnic vortex, Condensed Matter::Superconductivity, 0103 physical sciences, microscopy, [PHYS.COND]Physics [physics]/Condensed Matter [cond-mat], 010306 general physics, 0210 nano-technology, Coherence (physics)
Abstract

International audience; Using scanning tunneling spectroscopy, we address the problem of the superconductor-insulator phase transition in homogeneously disordered ultrathin (2-15 nm) films of NbN. Samples thicker than 8 nm, for which the Ioffe-Regel parameter k(F)l >= 5.6, manifest a conventional superconductivity: a spatially homogeneous BCS-like gap, vanishing at the critical temperature, and a disordered vortex lattice in magnetic field. Upon thickness reduction, however, while k(F)l lowers, the STS reveals striking deviations from the BCS scenario, among which a progressive decrease of the coherence peak height and small spatial inhomogeneities. In addition, the gap below T-C develops on a spectral background, which becomes more and more ``V-shaped'' approaching the localization. The thinnest film (2.16 nm), while not being exactly at the superconductor-insulator transition (SIT) (T-C approximate to 0.4T(C)(bulk)), showed unconventional signatures such as the vanishing of the coherence peaks and the absence of vortices. This behavior suggests a weakening of long-range phase coherence, when approaching the SIT in this quasi-2D limit.

Published
2013

47. Frontend for a 2.5-THz heterodyne spectrometer without liquid cryogen

Author

Harvey E. Beere, David A. Ritchie, Michael Siegel, S.G. Pavlov, Lukas Mahler, A. D. Semenov, Heiko Richter, Konstantin Ilin, Alessandro Tredicucci, H.-W. Hübers, Richter, H., Semenov, A. D., Pavlov, S. G., Mahler, L., Tredicucci, Alessandro, Beere, H. E., Ritchie, D. A., Il'In, K., Siegel, M., and Hubers, H. W.

Subjects
Heterodyne, Physics, Spectrometer, business.industry, Terahertz radiation, Terahertz- und Infrarotsensorik, Local oscillator, Bolometer, pulse tube cooler, Laser, law.invention, Terahertz spectroscopy and technology, Full width at half maximum, Optics, law, QCL, HEB, business, SOFIA
Abstract

As part of a study for a second generation heterodyne spectrometer on SOFIA we are developing a 2.5-THz frontend which is implemented in a pulse-tube cooler . It consists of a quantum-cascade laser as local oscillator and a phonon-cooled NbN hot electron bolometric mixer. Frequency stabilization to below 300 kHz full width at half maximum is achieved by locking to a molecular absorption line. We will present the design and performance of the frontend and discuss the prospects for an application on board of SOFIA.

Published
2011

48. Molecular spectroscopy with a multimode THz quantum-cascade laser

Author

Rudolf Hey, Heiko Richter, Martin Wienold, M. Giehler, H.-W. Hübers, René Eichholz, S.G. Pavlov, Lutz Schrottke, Holger T. Grahn, and A. D. Semenov

Subjects
spectroscopy, Materials science, Spectrometer, Terahertz radiation, business.industry, Physics::Instrumentation and Detectors, Terahertz- und Infrarotsensorik, Far-infrared laser, Physics::Optics, multimode QCL, Laser, law.invention, Terahertz spectroscopy and technology, Photomixing, terahertz, Optics, law, Optoelectronics, THz, spectrometer, Quantum cascade laser, business, Terahertz time-domain spectroscopy, Nuclear Experiment
Abstract

A terahertz absorption spectrometer for high-resolution molecular spectroscopy is realized. The spectrometer is based on a multimode quantum-cascade laser. The design and performance of the spectrometer are presented. Three aspects are discussed: sensitivity, frequency calibration, and frequency multiplexing.

Published
2011

49. Chemistry in Disks. III. -- Photochemistry and X-ray driven chemistry probed by the ethynyl radical (CCH) in DM Tau, LkCa 15, and MWC 480

Author

Vincent Piétu, Stéphane Guilloteau, Anne Dutrey, Th. Henning, Franck Hersant, E. Chapillon, Katharina Schreyer, Ralf Launhardt, D. Semenov, Valentine Wakelam, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, AMOR 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), and FORMATION STELLAIRE 2010

Subjects
Ethynyl radical, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Photochemistry, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], chemistry.chemical_compound, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, X-ray, Plateau de Bure Interferometer, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 3. Good health, T Tauri star, Wavelength, Temperature gradient, chemistry, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Excitation
Abstract

We studied several representative circumstellar disks surrounding the Herbig Ae star MWC 480 and the T Tauri stars LkCa 15 and DM Tau at (sub-)millimeter wavelengths in lines of CCH. Our aim is to characterize photochemistry in the heavily UV-irradiated MWC 480 disk and compare the results to the disks around cooler T Tauri stars. We detected and mapped CCH in these disks with the IRAM Plateau de Bure Interferome- ter in the C- and D-configurations in the (1-0) and (2-1) transitions. Using an iterative minimization technique, the CCH column densities and excitation conditions are con- strained. Very low excitation temperatures are derived for the T Tauri stars. These values are compared with the results of advanced chemical modeling, which is based on a steady-state flared disk structure with a vertical temperature gradient, and a gas- grain chemical network with surface reactions. Both model and observations suggest that CCH is a sensitive tracer of the X-ray and UV irradiation. The predicted radial dependency and source to source variations of CCH column densities qualitatively agree with the observed values, but the predicted column densities are too low by a factor of several. The chemical model fails to reproduce high concentrations of CCH in very cold disk midplane as derived from the observed low excitation condition for both the (1-0) and (2-1) transitions., 23 pages, 9 figures, 3 tables, accepted for publication in ApJ

Published
2010

50. Development of a THz heterodyne receiver with quantum cascade laser and hot electron bolometer mixer for standoff detection of explosive material

Author

Heiko Richter, L. Mahler, H.-W. Hübers, A. Tredicucci, Michael Siegel, S.G. Pavlov, Ulrich Schade, David A. Ritchie, Konstantin Ilin, A. D. Semenov, Michele Ortolani, Harvey E. Beere, Richter, H., Semenov, A. D., Pavlov, S. G., Mahler, L., Tredicucci, Alessandro, Beere, H. E., Ritchie, D. A., Ortolani, M., Schade, U., Il'In, K. S., Siegel, M., and Hubers, H. W.

Subjects
Physics, Explosive material, business.industry, Terahertz radiation, Local oscillator, Superheterodyne receiver, Bolometer, pulse tube cooler, Physics::Optics, Laser, law.invention, Optics, law, QCL, HEB, Optoelectronics, Explosive detection, THz, Quantum cascade laser, business, radar
Abstract

The terahertz (THz) portion of the electromagnetic spectrum provides specific spectroscopic information for substance identification. It has been shown that the spectral features of explosive materials might be used for detection and identification at stand-off distances. We report on the development of a THz spectrometer for explosive detection and identification. The system is based on THz quantum cascade lasers working at different frequencies. These are used for illumination of the object under test. The reflected and backscattered radiation from the object under test is detected with a sensitive heterodyne receiver. As a first step a single frequency, liquid-cryogen free heterodyne receiver operating at 2.5 THz has been developed. In order to realize maximum sensitivity a phonon-cooled NbN hot electron bolometric mixer with a quantum cascade laser as local oscillator were chosen. The concept of the system and first results will be presented.

Published
2009

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