80 research outputs found
Feasibility study for the measurement of transition distribution amplitudes at ANDA in
No full textInternational audienceThe exclusive charmonium production process in p¯p annihilation with an associated π0 meson p¯p→J/ψπ0 is studied in the framework of QCD collinear factorization. The feasibility of measuring this reaction through the J/ψ→e+e- decay channel with the AntiProton ANnihilation at DArmstadt (P¯ANDA) experiment is investigated. Simulations on signal reconstruction efficiency as well as the background rejection from various sources including the p¯p→π+π-π0 and p¯p→J/ψπ0π0 reactions are performed with PandaRoot, the simulation and analysis software framework of the P¯ANDA experiment. It is shown that the measurement can be done at P¯ANDA with significant constraining power under the assumption of an integrated luminosity attainable in four to five months of data taking at the maximum design luminosity
Feasibility studies for the measurement of time-like proton electromagnetic form factors from p ̄ p→ μ+μ- at P ̄ ANDA at FAIR
No full textThis paper reports on Monte Carlo simulation results for future measurements of the moduli of time-like proton electromagnetic form factors, | GE| and | GM| , using the p ̄ p→ μ+μ- reaction at P ̄ ANDA (FAIR). The electromagnetic form factors are fundamental quantities parameterizing the electric and magnetic structure of hadrons. This work estimates the statistical and total accuracy with which the form factors can be measured at P ̄ ANDA , using an analysis of simulated data within the PandaRoot software framework. The most crucial background channel is p ̄ p→ π+π-, due to the very similar behavior of muons and pions in the detector. The suppression factors are evaluated for this and all other relevant background channels at different values of antiproton beam momentum. The signal/background separation is based on a multivariate analysis, using the Boosted Decision Trees method. An expected background subtraction is included in this study, based on realistic angular distributions of the background contribution. Systematic uncertainties are considered and the relative total uncertainties of the form factor measurements are presented
Study of excited Ξ baryons with the P ̄ ANDA detector
No full textThe study of baryon excitation spectra provides insight into the inner structure of baryons. So far, most of the world-wide efforts have been directed towards N∗ and Δ spectroscopy. Nevertheless, the study of the double and triple strange baryon spectrum provides independent information to the N∗ and Δ spectra. The future antiproton experiment P ̄ANDA will provide direct access to final states containing a Ξ ̄ Ξ pair, for which production cross sections up to μb are expected in p ̄p reactions. With a luminosity of L= 10 31 cm- 2 s- 1 in the first phase of the experiment, the expected cross sections correspond to a production rate of ∼106events/day. With a nearly 4 π detector acceptance, P ̄ANDA will thus be a hyperon factory. In this study, reactions of the type p ̄p → Ξ ̄ +Ξ∗ - as well as p ̄p → Ξ ̄ ∗ +Ξ- with various decay modes are investigated. For the exclusive reconstruction of the signal events a full decay tree fit is used, resulting in reconstruction efficiencies between 3 and 5%. This allows high statistics data to be collected within a few weeks of data taking
The early afterglow of GRB 190829A
No full textGRB 190829A at z = 0.0785 is the fourth closest long GRB ever detected by the Neil Gehrels Swift observatory, and the third confirmed case with a very high-energy component. We present our multiwavelength analysis of this rare event, focusing on its early stages of evolution, and including data from Swift, the MASTER global network of optical telescopes, ALMA, and ATCA. We report sensitive limits on the linear polarization of the optical emission, disfavouring models of off-axis jets to explain the delayed afterglow peak. The study of the multiwavelength light curves and broad-band spectra supports a model with at least two emission components: a bright reverse shock emission, visible at early times in the optical and X-rays and, later, in the radio band; and a forward shock component dominating at later times and lower radio frequencies. A combined study of the prompt and afterglow properties shows many similarities with cosmological long GRBs, suggesting that GRB 190829A is an example of classical GRBs in the nearby universe
Feasibility studies for the measurement of time-like proton electromagnetic form factors from at at FAIR
No full textInternational audienceThis paper reports on Monte Carlo simulation results for future measurements of the moduli of time-like proton electromagnetic form factors, and , using the reaction at (FAIR). The electromagnetic form factors are fundamental quantities parameterizing the electric and magnetic structure of hadrons. This work estimates the statistical and total accuracy with which the form factors can be measured at , using an analysis of simulated data within the PandaRoot software framework. The most crucial background channel is , due to the very similar behavior of muons and pions in the detector. The suppression factors are evaluated for this and all other relevant background channels at different values of antiproton beam momentum. The signal/background separation is based on a multivariate analysis, using the Boosted Decision Trees method. An expected background subtraction is included in this study, based on realistic angular distributions of the background contribution. Systematic uncertainties are considered and the relative total uncertainties of the form factor measurements are presented
MASTER OPTICAL POLARIZATION VARIABILITY DETECTION IN THE MICROQUASAR V404 CYG/GS 2023+33
No full textOn 2015 June 15, the Swift space observatory discovered that the Galactic black hole candidate V404 Cyg was undergoing another active X-ray phase, after 25 years of inactivity. The 12 telescopes of the MASTER Global Robotic Net located at six sites across four continents were the first ground-based observatories to start optical monitoring of the microquasar after its gamma-ray wake up at 18h 34m 09s U.T. on 2015 June 15. In this paper, we report, for the first time, the discovery of variable optical linear polarization, changing by 4%-6% over a timescale of ∼1 hr, on two different epochs. We can conclude that the additional variable polarization arises from the relativistic jet generated by the black hole in V404 Cyg. The polarization variability correlates with optical brightness changes, increasing when the flux decreases.Fil: Lipunov, V.. M.V.Lomonosov Moscow State University. Physics Department; RusiaFil: Gorbovskoy, E.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Krushinskiy, V.. Kourovka Astronomical Observatory, Ural Federal University; RusiaFil: Vlasenko, D.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Tiurina, N.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Balanutsa, P.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Kuznetsov, A.. M.V.Lomonosov Moscow State University, Sternberg Astronomical Institute; RusiaFil: Budnev, N.. Applied Physics Institute. Irkutsk State University; RusiaFil: Gress, O.. Applied Physics Institute, Irkutsk State University; RusiaFil: Tlatov, A.. Kislovodsk Solar Station of the Main (Pulkovo) Observatory RAS; RusiaFil: Rebolo Lopez, L.. Instituto de Astrofsica de Canarias; EspañaFil: Serra-Ricart, M.. Instituto de Astrofsica de Canarias; EspañaFil: Buckley, D. A. H.. South African Astronomical Observatory; SudáfricaFil: Israelyan, G.. Instituto de Astrofsica de Canarias; EspañaFil: Lodieu, N.. Instituto de Astrofisica de Canarias; EspañaFil: Ivanov, K.. Applied Physics Institute. Irkutsk State University; RusiaFil: Yazev, S.. Applied Physics Institute, Irkutsk State University; RusiaFil: Sergienko, Y.. Blagoveschensk State Pedagogical University; RusiaFil: Gabovich, A.. Blagoveschensk State Pedagogical University; RusiaFil: Yurkov, V.. Blagoveschensk State Pedagogical University; RusiaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Podesta, R.. Observatorio "Felix Aguiklar". Universidad Nacional de San Juan; ArgentinaFil: Lopez, C.. Observatorio "Felix Aguilar". Universidad nacional de San juan; Argentin
Technical design report for the Barrel DIRC detector
No full textThe (anti-Proton ANnihiliation at DArmstadt) experiment will be one of the four flagship experiments at the new international accelerator complex FAIR (Facility for Antiproton and Ion Research) in Darmstadt, Germany. will address fundamental questions of hadron physics and quantum chromodynamics using high-intensity cooled antiproton beams with momenta between 1.5 and 15 GeV/c and a design luminosity of up to 2 × 1032 cm−2 s−1. Excellent particle identification (PID) is crucial to the success of the physics program. Hadronic PID in the barrel region of the target spectrometer will be performed by a fast and compact Cherenkov counter using the detection of internally reflected Cherenkov light (DIRC) technology. It is designed to cover the polar angle range from 22° to 140° and will provide at least 3 standard deviations (s.d.) π/K separation up to 3.5 GeV/c, matching the expected upper limit of the final state kaon momentum distribution from simulation. This documents describes the technical design and the expected performance of the Barrel DIRC detector. The design is based on the successful BaBar DIRC with several key improvements. The performance and system cost were optimized in detailed detector simulations and validated with full system prototypes using particle beams at GSI and CERN. The final design meets or exceeds the PID goal of clean π/K separation with at least 3 s.d. over the entire phase space of charged kaons in the Barrel DIRC
MASTER Optical Detection of the First LIGO/Virgo Neutron Star Binary Merger GW170817
No full textFollowing the discovery of the gravitational-wave source GW170817 by three Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo antennae (Abbott et al., 2017a), the MASTER Global Robotic Net telescopes obtained the first image of the NGC 4993 host galaxy. An optical transient, MASTER OTJ130948.10-232253.3/SSS17a was later found, which appears to be a kilonova resulting from the merger of two neutron stars (NSs). Here we describe this independent detection and photometry of the kilonova made in white light, and in B, V, and R filters. We note that the luminosity of this kilonova in NGC 4993 is very close to those measured for other kilonovae possibly associated with gamma-ray burst (GRB) 130603 and GRB 080503.Fil: Lipunov, V. M.. Lomonosov Moscow State University; RusiaFil: Gorbovskoy, E.. Lomonosov Moscow State University; RusiaFil: Kornilov, V. G.. Lomonosov Moscow State University; RusiaFil: Tyurina, N.. Lomonosov Moscow State University; RusiaFil: Balanutsa, P.. Lomonosov Moscow State University; RusiaFil: Kuznetsov, A.. Lomonosov Moscow State University; RusiaFil: Vlasenko, D.. Lomonosov Moscow State University; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University; RusiaFil: Gorbunov, I.. Lomonosov Moscow State University; RusiaFil: Buckley, D. A. H.. South African Astrophysical Observatory; SudáfricaFil: Krylov, A. V.. Lomonosov Moscow State University; RusiaFil: Podesta, R.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Lopez, C.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Podesta, F.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Mallamachi, C.. Universidad Nacional de San Juan; ArgentinaFil: Potter, S.. South African Astrophysical Observatory; SudáfricaFil: Budnev, N. M.. Irkutsk State University; RusiaFil: Gress, O.. Lomonosov Moscow State University; Rusia. Irkutsk State University; RusiaFil: Ishmuhametova, Yu.. Irkutsk State University; RusiaFil: Vladimirov, V.. Lomonosov Moscow State University; RusiaFil: Zimnukhov, D.. Lomonosov Moscow State University; RusiaFil: Yurkov, V.. Blagoveschensk State Pedagogical University; RusiaFil: Sergienko, Yu.. Blagoveschensk State Pedagogical University; RusiaFil: Gabovich, A.. Blagoveschensk State Pedagogical University; RusiaFil: Rebolo, R.. Instituto de Astrofísica de Canarias; EspañaFil: Serra Ricart, M.. Instituto de Astrofísica de Canarias; EspañaFil: Israelyan, G.. Instituto de Astrofísica de Canarias; EspañaFil: Chazov, V.. Lomonosov Moscow State University; RusiaFil: Wang, Xiaofeng. Tsinghua University; ChinaFil: Tlatov, A.. Kislovodsk Solar Observing Station of Pulkovo Observatory; RusiaFil: Panchenko, M. I.. Lomonosov Moscow State University; Rusi
First gravitational-wave burst GW150914: MASTER optical follow-up observations
No full textThe Advanced LIGO observatory recently reported the first direct detection of the gravitational waves (GWs) predicted by Einstein & Sitzungsber. We report on the first optical observations of the GW source GW150914 error region with the Global MASTER Robotic Net. Between the optical telescopes of electromagnetic support, the covered area is dominated by MASTER with an unfiltered magnitude up to 19.9 mag (5σ). We detected several optical transients, which proved to be unconnected with the GW event. The main input to investigate the final error box of GW150914 was made by the MASTER-SAAO robotic telescope, which covered 70 per cent of the final GW error box and 90 per cent of the common localization area of the LIGO and Fermi events. Our result is consistent with the conclusion (Abbott et al. 2016a) that GWs from GW150914 were produced in a binary black hole merger. At the same time, we cannot exclude that MASTER OT J040938.68-541316.9 exploded on 2015 September 14.Fil: Lipunov, V. M.. Lomonosov Moscow State University; RusiaFil: Kornilov, V.. Lomonosov Moscow State University; RusiaFil: Gorbovskoy, E.. Lomonosov Moscow State University; RusiaFil: Buckley, D. A. H.. South African Astronomical Observatory; SudáfricaFil: Tiurina, N.. Lomonosov Moscow State University; RusiaFil: Balanutsa, P.. Lomonosov Moscow State University; RusiaFil: Kuznetsov, A.. Lomonosov Moscow State University; RusiaFil: Greiner, J.. Max-Planck-Institut für extraterrestrische Physik; AlemaniaFil: Vladimirov, V.. Lomonosov Moscow State University; RusiaFil: Vlasenko, D.. Lomonosov Moscow State University; RusiaFil: Chazov, V.. Lomonosov Moscow State University; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University; RusiaFil: Gabovich, A.. Blagoveschensk State Pedagogical University; RusiaFil: Potter, S. B.. South African Astronomical Observatory; SudáfricaFil: Kniazev, A.. South African Astronomical Observatory; SudáfricaFil: Crawford, S.. South African Astronomical Observatory;Fil: Rebolo Lopez, R.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Serra Ricart, M.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Israelian, G.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Lodieu, N.. Instituto de Astrofacuteisica de Canarias Vía Láctea; EspañaFil: Gress, O.. Irkutsk State University; RusiaFil: Budnev, N.. Irkutsk State University; RusiaFil: Ivanov, K.. Irkutsk State University; RusiaFil: Poleschuk, V.. Irkutsk State University; RusiaFil: Yazev, S.. Irkutsk State University; RusiaFil: Tlatov, A.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Senik, V.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Yurkov, V.. Blagoveschensk State Pedagogical University; RusiaFil: Dormidontov, D.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Parkhomenko, A.. Russian Academy of Sciences. Pulkovo Astronomical Observatory; RusiaFil: Sergienko, Yu.. Blagoveschensk State Pedagogical University; RusiaFil: Podestá, Ricardo César. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: López, Carlos Eduardo. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Podestá, Florencia. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Mallamaci, Claudio Carlos. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; Argentin
Early Optical Observations of Gamma-Ray Bursts Compared with Their Gamma- and X-Ray Characteristics Using a MASTER Global Network of Robotic Telescopes from Lomonosov Moscow State University
No full textWe present the results of early observations for 130 error-boxes of gamma-ray bursts performed with the Mobile Astronomical System of TElescope-Robots (MASTER) global network of robotic telescopes from Moscow State University in fully automatic mode (2011?2017). Among them, GRB 130907A, GRB 120811C, GRB 110801A, GRB 120404A, GRB 140129B, GRB140311B, and GRB 160227A are considered in details. Among these 130 gamma-ray bursts, in the first 60 s after the trigger with the Swift, Fermi, INTEGRAL, MAXI, Lomonosov, and Konus-Wind orbital observatories, the MASTER was pointed on 51 gamma-ray bursts, being the leader in terms of the first pointing. Full observation automation and MASTER own real-time image processing software allowed us to obtain unique data on early optical emission that accompanied 44 gamma-ray bursts (GRB 110801A, GRB120106A, GRB 120404A, GRB 120811C, GRB 120907A, GRB 121011A, GRB 130122A, GRB 130907A, GRB 131030A, GRB 131125A, GRB 140103A, GRB 140108A, GRB 140129B, GRB 140206A, GRB 140304A, GRB 140311B, GRB 140512A, GRB 140629A, GRB 140801A, GRB140907A, GRB 140930B, GRB141028A, GRB 141225A, GRB 150210A, GRB 150211A, GRB 150301B, GRB 150323C, GRB 150404A/Fermi trigger 449861706, GRB 150403A, GRB 150413A, GRB 150518A, GRB 150627A, GRB 151021A, GRB 151215A, GRB 160104A, GRB 160117B, GRB 160131A, GRB 160227A, GRB 160425A, GRB 160611A, GRB 160625B, GRB 160804A, GRB 160910A, GRB 161017A, GRB 161117A, GRB 161119A). We obtain light curves for 13 gamma-ray bursts among the above listed ones and compare the data in the optical (MASTER), X-ray (Swift-XRT), and hard X-ray (Swift-BAT) ranges.We present the results of early observations for 130 error-boxes of gamma-ray bursts performed with the Mobile Astronomical System of TElescope-Robots (MASTER) global network of robotic telescopes from Moscow State University in fully automatic mode (2011?2017). Among them, GRB 130907A, GRB 120811C, GRB 110801A, GRB 120404A, GRB 140129B, GRB140311B, and GRB 160227A are considered in details. Among these 130 gamma-ray bursts, in the first 60 s after the trigger with the Swift, Fermi, INTEGRAL, MAXI, Lomonosov, and Konus-Wind orbital observatories, the MASTER was pointed on 51 gamma-ray bursts, being the leader in terms of the first pointing. Full observation automation and MASTER own real-time image processing software allowed us to obtain unique data on early optical emission that accompanied 44 gamma-ray bursts (GRB 110801A, GRB120106A, GRB 120404A, GRB 120811C, GRB 120907A, GRB 121011A, GRB 130122A, GRB 130907A, GRB 131030A, GRB 131125A, GRB 140103A, GRB 140108A, GRB 140129B, GRB 140206A, GRB 140304A, GRB 140311B, GRB 140512A, GRB 140629A, GRB 140801A, GRB140907A, GRB 140930B, GRB141028A, GRB 141225A, GRB 150210A, GRB 150211A, GRB 150301B, GRB 150323C, GRB 150404A/Fermi trigger 449861706, GRB 150403A, GRB 150413A, GRB 150518A, GRB 150627A, GRB 151021A, GRB 151215A, GRB 160104A, GRB 160117B, GRB 160131A, GRB 160227A, GRB 160425A, GRB 160611A, GRB 160625B, GRB 160804A, GRB 160910A, GRB 161017A, GRB 161117A, GRB 161119A). We obtain light curves for 13 gamma-ray bursts among the above listed ones and compare the data in the optical (MASTER), X-ray (Swift-XRT), and hard X-ray (Swift-BAT) ranges.Fil: Ershova, O. A.. Irkutsk State University; RusiaFil: Ershova, O. A.. Irkutsk State University; RusiaFil: Lipunov, Vladimir. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Lipunov, Vladimir. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gorbovskoy, E. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gorbovskoy, E. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Tyurina, N. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Tyurina, N. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kornilov, V. G.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kornilov, V. G.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Zimnukhov, D. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Zimnukhov, D. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gabovich, A. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gabovich, A. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gress, O. A.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gress, O. A.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Budnev, N. M.. rkutsk State University; RusiaFil: Budnev, N. M.. rkutsk State University; RusiaFil: Yurkov, V. V.. Blagoveshchensk State Pedagogical University; RusiaFil: Yurkov, V. V.. Blagoveshchensk State Pedagogical University; RusiaFil: Vladimirov, V. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Vladimirov, V. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kuznetsov. A. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kuznetsov. A. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Balanutsa, P. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Balanutsa, P. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Rebolo, R.. Instituto de Astrofisica de Canarias; EspañaFil: Rebolo, R.. Instituto de Astrofisica de Canarias; EspañaFil: Serra Ricart, M.. Instituto de Astrofisica de Canarias; EspañaFil: Serra Ricart, M.. Instituto de Astrofisica de Canarias; EspañaFil: Buckley, D.. South African Astrophysical Observatory; SudáfricaFil: Buckley, D.. South African Astrophysical Observatory; SudáfricaFil: Podestá, Ricardo César. Universidad Nacional de San Juan; ArgentinaFil: Podestá, Ricardo César. Universidad Nacional de San Juan; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Lopez, Carlos. Universidad Nacional de San Juan; ArgentinaFil: Lopez, Carlos. Universidad Nacional de San Juan; ArgentinaFil: Podesta, Federico. Universidad Nacional de San Juan; ArgentinaFil: Podesta, Federico. Universidad Nacional de San Juan; ArgentinaFil: Francile, Carlos Natale. Universidad Nacional de San Juan; ArgentinaFil: Francile, Carlos Natale. Universidad Nacional de San Juan; ArgentinaFil: Mallamaci, Claudio Carlos. Universidad Nacional de San Juan; ArgentinaFil: Mallamaci, Claudio Carlos. Universidad Nacional de San Juan; ArgentinaFil: Yazev, S. A.. Irkutsk State University; RusiaFil: Yazev, S. A.. Irkutsk State University; RusiaFil: Vlasenko, D. M.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Vlasenko, D. M.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Tlatov, A.. Russian Academy of Sciences; RusiaFil: Tlatov, A.. Russian Academy of Sciences; RusiaFil: Senik, V.. Irkutsk State University; RusiaFil: Senik, V.. Irkutsk State University; RusiaFil: Grinshpun, V.. Moscow State University. Physics Department; RusiaFil: Grinshpun, V.. Moscow State University. Physics Department; RusiaFil: Chasovnikov, A.. Lomonosov Moscow State University. Physics Department; RusiaFil: Chasovnikov, A.. Lomonosov Moscow State University. Physics Department; RusiaFil: Topolev, V.. Moscow State University. Physics Department; RusiaFil: Topolev, V.. Moscow State University. Physics Department; RusiaFil: Pozdnyakov, A.. Moscow State University. Physics Department; RusiaFil: Pozdnyakov, A.. Moscow State University. Physics Department; RusiaFil: Zhirkov, K.. Moscow State University. Physics Department; RusiaFil: Zhirkov, K.. Moscow State University. Physics Department; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Balakin, F.. Moscow State University. Physics Department; RusiaFil: Balakin, F.. Moscow State University. Physics Department; Rusi
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