Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.sao.ru/hq/grb/conf_2015/doc/Abstracts.pdf Äàòà èçìåíåíèÿ: Mon Nov 23 14:33:12 2015 Äàòà èíäåêñèðîâàíèÿ: Sun Apr 10 15:08:18 2016 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: earth's atmosphere

The International Workshop on Quark Phase Transition in Compact Objects and Multimessenger Astronomy: Neutrino Signals, Supernovae and Gamma-Ray Bursts

KChR, Nizhnij Arkhyz (SAO) KBR, Terskol (BNO) October, 7 - 14, 2015

Book of abstracts


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Content
Akhmatov Z.A. Cryostatting, modulation and measurement of neutron fluxes in the low background experiments ...................................................................................................... 3 Alvarez-Castillo D.E. Energy bursts from deconfinement in high-mass twin stars ........... 3 Ashikhmin V. V. The search for coincidences of rare events with LVD and BPST detectors ............................................................................................................................... 4 Avrorin A.D. Baikal-GVD: status and plan ....................................................................... 4 Baryshev Yu.V., Paturel G., Sokolov V.V. Sidereal time analysis as a tool for detection of gravitational waves and neutrino SN- bursts in the inhomogeneous Local Universe .... 4 Bryukhanova N. Data from the NEMO neutrino telescope ................................................ 5 Chugunov A., Gusakov M.E., Kantor E.M. Neutron star recycling scenario and constraints on the r-mode instability ................................................................................... 5 Danilenko A.A. Restriction on parameters of the pulsar nebula DA 495 and its pulsar by data of the space observatories Chandra and XMM-Newton .............................................. 6 Demidov S.V. Baikal searches for neutrino signal from the Galactic Center and Dwarf Galaxies................................................................................................................................ 6 Drago A. Long and short GRBs in the two-families scenario ............................................ 7 Dzhappuev D.D. A search for cosmic gamma-rays at the Carpet-2 EAS array: prospects and preliminary results ......................................................................................................... 7 Gorbachev V.V. Radiochemical neutrino experiments today ............................................ 7 Grammatikati K. The data analysis from GBM and LAT monitors from FERMI telescope .............................................................................................................................................. 8 Iosilevsky I.L. Entropic and enthalpic phase transitions in high energy density nuclear matter ................................................................................................................................... 8 Karpov S.V., Beskin G.M., Biryukov A.V., Bondar S.F., Ivanov E.A., Katkova E.V., Perkov A.V., Sasyuk V.V. Observations of transient events with the MiniMegaTORTORA wide-field monitoring system ................................................................. 9 Khokonov A. Kh.-A. The viscosity and surface tension of the hadron matter and quarkgluon plasma ...................................................................................................................... 10 Kuznetsov A.S. Fast optical transient detection by MASTER Global Robotic Net on the example of FERMI alerts ...................................................................................................10 Kuznetsov M.Yu. Primary photons in cosmic rays with energy 1017eV from EAS MSU experiment data ................................................................................................................. 11 Kuzminov V.V. Baksan Neutrino Observatory of the INR RAS: current state and prospects ........................................................................................................................... 11
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Lidvansky A.S. On Burst Activity of the Crab Nebula and Pulsar at High and Ultra-High Energies.............................................................................................................................. 11 Lipunov V.M. The MASTER Global Robotic Net and main physical experiments ......... 12 Nadyozhin D.K. Mechanisms of supernova explosion: modern status ............................. 12 Novoseltsev Yu.F. Search for neutrino burst signals from Supernovae at the Baksan Underground Scintillation Telescope ................................................................................ 13 Novoseltseva R.V. Joint analysis of experimental data on the search for neutrino bursts using the BUST and LVD detectors .................................................................................. 13 Petkov V.B. Prospects of detecting the QCD phase transition in the Galactic supernova neutrino burst with 20-kton scale liquid scintillation detectors ......................................... 13 Rudenko V.N. Current status of the GW-experiment and multi-messenger astronomy ... 14 Ryazhskaya O.G., Semenov S.V. Interaction of electron neutrino with LSD detector .... 14 Sergeev A.V. Terskol Observatory: new technologies of observing fast phenomena on celestial objects with ground-based optical telescopes ...................................................... 15 Sokolov I.V., Castro-Tirado A. J., Verkhodanov O.V., Zhelenkova O.P., Baryshev Yu.V. A cluster of galaxies around the GRB 021004 sight-line at z ~ 0.57 ................................ 15 Sokolov V.V. On the observed mass distribution of compact stellar remnants in close binary systems and possible interpretations proposed for the time being ......................... 16 Shirokov E.V. The MSU neutrino group activity in the projects of deep-sea neutrino detectors ............................................................................................................................. 16 Sholukhova O.N. Ultraluminous X-ray Sources as Super-Eddington Accretion Disks ... 17 Spiering Ch. High-energy neutrino astronomy ­ where are we now, where do we go? ............................................................................................................................................ 17 Verkhodanov O.V. Sokolov V.V., Khabibullina M.L. Correlation between sphere distributions of gamma-ray bursts and CMB fluctuations ................................................. 17 Vlasyuk V.V., Sokolov V.V. The complex of SAO RAS optical telescopes as an instrument for studying transient phenomena in the Universe ......................................... 18 Wiktorowicz G. X-ray binaries and Ultra-luminous X-ray sources .................................18 Xu RenXin 3-flavour symmetry restoration in compressed baryonic matter ................... 19 Yu Yong-Bo Energy injection in Gamma Ray Bursts ...................................................... 19 Yudin A.V. On some exotic properties of hybrid stars..................................................... 20

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Akhmatov Z.A. (Kabardino ­ Balkarian State University), Khokonov A.Kh. ahmatov.z@bk.ru

Cryostatting, modulation and measurement of neutron fluxes in the low background experiments
Streams of ultracold neutrons are used in experiments on measurement of the dipole moment of the neutron, and to test the hypothesis of the existence of neutron-antineutron oscillations with non-conservation of baryon quantum number B = 2. We tested the possibility of cooling and formation of thermal neutron flux by a constructive neutron monitor NM - 64 [1] cooled by liquid nitrogen vapors. For neutron detection in the installation may be used the scintillation method [2] or proportional counters [3] . We also presented a helium cryostat for cooling and formation of neutron fluxes. Calculations have been done for cold neutron flux density by using a cascade generator and reaction t (d, n) 4He at a deuteron energy of 130 keV and for signal / background ratio for various lengths of neutron-antineutron oscillations in vacuumed vertically placed pipe with length L10 m. 1. Khokonov A.Kh., Savoiskii Yu.V., Ilgashev V.S., et.al. Initial Results from Neutron Monitoring at Terskol Peak.Seriya Fizicheskaya, 2011, Vol.75, p.915. 2. Alekseenko V.V. , Gavriluk U.M., Kuzminov V.V. «Features of scintillation detector of thermal neutrons [ZnS (Ag) + 6LiF] in different measurement conditions.» Moscow, Preprint INR RAS 1303/2011, October 2011. 3. Khokonov A.Kh., Savoiskii Yu.V., Kamarzaev A.V. Neutron sensitivity and detection efficiency of 3 He and 10BF3 counters. Physics of Atomic Nuclei, 2010, Vol. 73, 79, pp. 1481 ­ 1485.

Alvarez-Castillo D.E. (Joint Institute for Nuclear Research, Dubna, Russia) alvarez@theor.jinr.ru

Energy bursts from deconfinement in high-mass twin stars
We estimate the energy reservoir available in the deconfinement phase transition induced collapse of a neutron star to its hybrid star mass twin on the "third family" branch, using a recent equation of state of dense matter. The available energy corresponding to the massenergy difference between configurations is comparable with energies of the most violent astrophysical burst processes. An observational outcome of such a dynamical transition might be fast radio bursts, specifically a recent example of a FRB with a double-peak structure in its light curve.

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Ashikhmin, V. V. (INR RAS, Moscow) vole4ka86@mail.ru

The search for coincidences of rare events with LVD and BPST detectors
Results of the search for coincidences of rare events in LVD and Baksan Underground Scintillation Telescope (BUST) detectors are presented. We developed a procedure of the search for events in LVD and BUST detectors which could be induced by interaction between neutrinos and matter contained in them. It was shown that from 2011 to 2014 the coincidences are of random character and their sum quantity remains practically invariable.

Avrorin A.D. (INR RAS, Moscow) for the Baikal Collaboration a.d.avrorin@gmail.com

Baikal-GVD: status and plan
The future next-generation neutrino telescope Baikal-GVD will be a km3-scale array aimed at detection of astrophysical neutrino fluxes. It will have a modular structure and consist of functionally independent sub-arrays ­ clusters of strings of optical modules. The prototyping phase of the project has been completed in 2015 with deployment of the first cluster of Baikal-GVD in the Lake Baikal. We discuss current status and prospects of the Baikal-GVD project.

Baryshev Yu.V. (SPSU, StPetersburg) Paturel G., Sokolov V.V. yubaryshev@mail.ru

Sidereal time analysis as a tool for detection of gravitational waves and neutrino SN- bursts in the inhomogeneous Local Universe
Core-collapse of massive stars produces both neutrino signal and gravitational wave (tensor transversal plus scalar-longitudinal) bursts. In the case of GW detectors having low angular resolution the method of sidereal time analysis of output signals was applied for extraction of GW-bursts from high level noise. This method was suggested by J.Weber, Phys. Rev. Letters 22, 1320, 1969 for signal analysis of his bar detector and developed for the case of existing GW detectors in papers byY. Baryshev and G. Paturel, A&A, 371, 378, 2001 (arXiv: astro ph/0104115), P. Astone et al., CQG, 19,5449, 2002 (arXiv: gr -qc/0210053), G. Paturel and Y. Baryshev, A&A, 398, 377, 2003 (arXiv: astro-ph/0104115), G. Paturel and Y. Baryshev, ApJ Lett., 592, L99, 2003.

The same sidereal time approach can be also applied for low energy neutrino detectors having many years of observational time (e.g. Super-Kamiokande, LVD, Baksan). This method uses following basic things: 1) difference between sidereal and mean solar time (which help to delete noises related to day-night solar time), 2) directivity diagram (antenna pattern) of the detector (which chooses a particular sky region in particular sidereal time), and 3) known position on the sky the inhomogeneous distribution of the
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possible sources of SN signals, such as Galactic plane, Galaxy center, closest galaxies, Virgo galaxy cluster, Super-galactic plane, Great Attractor. Main idea is calculation of the expected number of neutrino events as a function of sidereal time (scanning the sky by Earth rotation) produced by possible sources within fixed depth of the survey. The summation of all output signals within one Earth's revolution (~23h 56m 04s of mean solar day) during several years of observations will reveal certain structure at predicted sidereal hours (by using directivity pattern of a detector), so the detection has statistical sense.
Bryukhanova N. (MSU, Moscow) lorian.grace@gmail.com

Data from the NEMO neutrino telescope
In this work the questions connected with data processing on the NEMO test line will be discussed. In 2014 some preparations for functioning of the system were made, and it was necessary to analyze properties of water at the location (Capo Passero, near Sicily). It is essential for normal data processing in the Cherenkov neutrino telescope. In this work some problems related to the specific character of available data had to be solved. After that, the light signal was extracted and the plot of light attenuation was obtained. In addition, the calibration of photomultipliers was done. After that, using the computer simulation of light propagation, the parameters of environment were determined by fitting the actual attenuation plots to models with different parameters. This data may be suitable for correction of the obtained values. The algorithm can be also useful for other telescopes, and parameters themselves can help to the analysis in the neutrino experiment itself.

Chugunov A. (Ioffe Institute, StPetersburg), Gusakov M.E., Kantor E.M. andr.astro@gmail.com

Neutron star recycling scenario and constraints on the r-mode instability
Recycling scenario imposes important constraints on r-mode instability in neutron stars and thus on neutron star microphysics. Recent Ref. [1] concluded that ungapped interacting quark matter model is consistent with recycling scenario, including radio and x-ray data. However, this model leads to very high neutrino luminosity, thus high temperatures observed for neutron stars in low mass X-ray binaries can hardly be explained. On the contrary, our recent model [2] agrees with these observations, furthermore it is also consistent with neutron star cooling data, because it appeals to the same microphysical parameters as the minimal cooling model does [3]. Within our model, r-mode instability is suppressed because of the resonant interaction of oscillation modes at some internal temperatures ("resonant temperatures"). Here we demonstrate that this model agrees as well with observations of millisecond pulsars and provides observational evidences that the coupling parameter for resonant mode interaction at low temperatures should be rather large, in agreement with theoretical expectations [2]. This study was partially supported by RFBR (grants 14-02-00868-a and 14-02- 31616mol-a), and by RF president programme (grants MK-506.2014.2 and NSh-294.2014.2).
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References [1] M.G. Alford and K. Schwenzer, Phys. Rev. Lett. 113, 251102 (2014). [2] M.E. Gusakov, A.I. Chugunov, and E.M. Kantor, Phys. Rev. Lett. 112, 151101 (2014); Phys. Rev. D 90, 063001 (2014). [3] M.E. Gusakov et al, A&A 423, 1063 (2004); Mon. Not. R. Astron. Soc. 363, 555 (2005).

Danilenko A.A. (Ioffe Institute, StPetersburg) danila.astro@gmail.com

Restriction on parameters of the pulsar nebula DA 495 and its pulsar by data of the space observatories Chandra and XMMNewton
We present spectral and timing analyses of the X-ray emission from the pulsar wind nebula DA 495 and its central object, J1952.2+2925, suggested to be the pulsar, using archival Chandra and XMM­Newton data. J1952.2+2925 has a pure thermal spectrum which is equally well fitted either by the blackbody model with a temperature of 215 eV and an emitting area radius of 0.6 km or by magnetized neutron star atmosphere models with temperatures of 80­90 eV. In the latter case, the thermal emission can come from the entire neutron star surface which temperature is consistent with standard neutron star cooling scenarios. We place also an upper limit on the J1952.2+2925 non-thermal flux. The derived spectral parameters are generally compatible with published ones based only on the Chandra data, but they are much more accurate due to the inclusion of XMM­ Newton data. No pulsations were found and we placed an upper limit for the J1952.2+2925 pulsed emission fraction of 40 per cent. Utilizing the interstellar absorption­distance relation, we estimated the distance to DA 495, which can be as large as 5 kpc if J1952.2+2925 emission is described by the atmosphere models. We compiled possible multiwavelength spectra of the nebula including radio data; they depend on the spectral model of the central object. Comparing the results with other pulsar plus wind nebula systems, we set reasonable constraints on the J1952.2+2925 spin-down luminosity and age. We suggest that the Fermi source 3FGL J1951.6+2926 is the likely gamma-ray counterpart of J1952.2+2925.

Demidov S.V. (INR RAS, Moscow) demidov@inr.ac.ru

Baikal searches for neutrino signal from the Galactic Center and Dwarf Galaxies
We perform the analysis of a data set of Baikal neutrino telescope NT200 to search for neutrino signals from dark matter annihilation in the Galactic Center and in Dwar f Galaxies. From this analysis we set upper limits on dark matter annihilation cross sections for different annihilation channels. Also we discuss sensitivity of the gigaton volume telescope Baikal-GVD to this signal.

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Drago A. (University of Ferrara, Italy)
drago@fe.infn.it

Long and short GRBs in the two-families scenario
I will review the two-families scenario in which hadronic stars having rather small radii and masses not exceeding about 1.5 Ms coexist with quark stars, which can reach masses well above 2 Ms. I will discuss the implications of this scenario in particular for long and short GRBs, using the results of our recent work in which the process of quark deconfinement in compact stars has been revisited. Bibliographical references: 1) "Can very compact and very massive neutron stars both exist?" by Alessandro Drago, Andrea Lavagno, Giuseppe Pagliara. Phys.Rev. D89 (2014) 4, 043014. 2) "Early appearance of isobars in neutron stars" by Alessandro Drago, Andrea Lavagno, Giuseppe Pagliara, Daniele Pigato. Phys.Rev. C90 (2014) 6, 065809. 3) "Combustion of a hadronic star into a quark star: the turbulent and the diffusive regimes" by Alessandro Drago, Giuseppe Pagliara. arXiv:1506.08337 4) "Quark deconfinement and the duration of short Gamma Ray Bursts" by Alessandro Drago, Andrea Lavagno, Giuseppe Pagliara In preparation

Dzhappuev D.D. (BNO INR RAS) dzhappuev@mail.ru

A search for cosmic gamma-rays at the Carpet-2 EAS array: prospects and preliminary results
We analyze Carpet-2 EAS array data in order to search for events with anomalously low content of muons with energies E > 1 GeV in extensive air showers with energy above 100 TeV. Monte-Carlo simulations of showers induced by primary protons and gammas have been performed using the CORSIKA code. The estimation of the upper limit on the flux primary gamma rays is presented.

Gorbachev V. V. (BNO INR RAS) vvgor_gfb1@mail.ru

Radiochemical neutrino experiments today
Radiochemical neutrino detectors have played an important role in the study of neutrinos from the Sun. Features of radiochemical detectors - no external backgrounds and sensitivity only to electron neutrinos - make them a powerful tool for precision measurements of neutrino properties.

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Grammatikati K. (MSU, Moscow)
stikus@mail.ru

The data analysis from GBM and LAT monitors from FERMI telescope
Gamma-ray bursts (GRBs) are thought to originate from collapsing massive stars or merging compact objects (such as neutron stars or black holes), and are associated with the formation of black holes in distant galaxies. Fermi Gamma-ray Space Telescope has two monitors aboard -- the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM). The LAT is a pairconversion telescope that observes photons from 20 MeV to >300 GeV with a 2.4steradian field of view. The GBM consists of 12 sodium iodide (NaI, 8 keV to 1 MeV) detectors and two bismuth germinate (BGO, 200 keV to 40 MeV) detectors, positioned around the spacecraft to view the entire unocculted sky. Gamma-ray burst spectral analysis takes advantage of the unique properties of this phenomenon: a relatively short transient from a point source. For the LAT there will usually not be competing emission from other sources in the field-of-view, while the GBM cannot distinguish spatially between burst photons and those originating from other sources. Therefore, the analysis is one dimensional: we determine the input burst flux from the apparent energies of the events (called 'counts'). For the LAT we select all the counts from a region 1-2 PSF-radii around the burst position from the time range which includes the burst. For the GBM the origin of the counts is unknown, and therefore all the counts from the burst's time range are selected. Consider matrix equation ci = Dijfj+bi , where ci is count spectrum (the index i runs over energy channels), bi is background, fj is photon flux striking the detector in different energy channels and matrix Dij is the 'Detector Response Matrix' (DRM) in the burst community. Note that for the LAT bi~0 but for the GBM bi is substantial, and in many channels will dominate the burst counts. In forward folding a model flux vector f'j is folded through the response, resulting in a model count spectrum c'i. The underlying model flux is usually an analytic function (e.g., a power law) with a small number of spectral parameters. The model c'i is compared to the observed ci, and then a new model flux vector f'j is calculated until the model c'i is sufficiently close to the observed ci, resulting in best-fit spectral parameters. 'Sufficiently close' is usually determined by minimizing 2 or if the number of counts per bin is not large enough, then the Cash statistic should be used instead of 2.

Iosilevsky I.L. (MPTI, Moscow) iosilevskiy@gmail.com

Entropic and enthalpic phase transitions in high energy density nuclear matter
Features of Gas-Liquid (GL) and Quark-Hadron (QH) phase transitions (PT) in dense nuclear matter are under discussion in comparison with their terrestrial counterparts, e.g. so-called "plasma" PT in shock-compressed hydrogen, nitrogen, xenon etc. Both, GLPT and QHPT, when being represented in widely accepted temperature­baryonic chemical potential plane, are often considered as similar, i.e. amenable to one-to-one mapping by
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simple scaling. It is argued that this impression is illusive and that GLPT and QHPT belong to different classes: GLPT is typical enthalpic (e.g. Van-der-Waals-like) PT while QHPT (i.e. "deconfinement-driven" PT) is typical entropic PT. Subdivision of 1st-order fluid-fluid phase transitions into two subclasses: enthalpic and entropic PTs (i.e. H-PT and S-PT), was proposed in [arXiv:1403.8053/1504.05850]. The term "entropic PT" is not equivalent to the term "entropy-driven" PT, which was introduced previously by D. Frenkel. We clarify the difference of two types of PTs. Properties of H-PT and S-PT differ significantly. Entropic PT is always internal part of more general and more extended thermodynamic anomaly ­ domains with abnormal (negative) sign for the set of (usually positive) second cross derivatives of thermodynamic potential. Three of them are of primary importance: so-called Gruneizen coefficient, thermal expansion coefficient and thermal pressure coefficient. Negative sign of all that derivatives lead to violation of relative order and standard behavior in P­V plane for many iso-lines, e.g. isotherms, isentropes, shock adiabats etc. Entropic PTs have more complicated topology of stable and metastable domains within the two-phase region in comparison with conventional enthalpic (VdW-like) PTs. In particular, new additional (third) metastable region, bounded by new additional spinodal, appears in the case of entropic PT. All the features of entropic PTs and accompanying abnormal thermodynamics region have transparent geometrical interpretation -- multi-layered structure of thermodynamic surfaces for temperature, entropy and internal energy as a pressure-volume functions, e.g. for T(P,V), S(P,V) and U(P,V).

Karpov S.V. (SAO RAS, Nizhnij Arkhyz), Beskin G.M., Biryukov A.V., Bondar S.F., Ivanov E.A., Katkova E.V., Perkov A.V., Sasyuk V.V. karpov@sao.ru

Observations of transient events with MegaTORTORA wide-field monitoring system

the

Mini-

Here we briefly summarize our long period experience of constructing and operating wide-field monitoring cameras with sub-second temporal resolution to look for optical components of GRBs, other rapid astrophysical phenomena, fast-moving satellites and meteors. General requirements for hardware for such systems are discussed along with algorithms of real-time detection and classification of various kinds of short optical transients. We also give a status report on the next generation, multi-objective and transforming monitoring system, the MegaTORTORA, whose 9-channel prototype (MiniMegaTORTORA) is now in operation at Russian Special Astrophysical Observatory. This system combines a wide field of view with subsecond temporal resolution in monitoring regime, and is able to reconfigure itself, in a fractions of second, to follow-up mode which has better sensitivity and provides us with multi-color and polarimetric information on detected transients simultaneously. We discuss first results of its work, as well as its prospects.

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Khokonov A. Kh.-A. (BSU, BNO INR RAS) e-mail: azkh@mail.ru

The viscosity and surface tension of the hadron matter and quark-gluon plasma
In present the interest to nuclear matter hydrodynamics increases [1]. The Liquid Drop Model (LDM) is successfully used for semi-empirical formulation of surface and Coulomb terms in Bethe-Weizsacker mass formula. LDM is the foundation for the 5D harmonic oscillator collective nuclear model [2], which allows us interpreting vibration excitations of near-spherical nuclei. In the frame of nuclear liquid drop model an analytical solution for the frequency of capillary oscillations is obtained with taking into account the damping due to viscosity and surrounding medium polarizability. The model has been applied for estimation of even-even spherical nuclei surface tension and viscosity. It has been shown [3] that energy shift of capillary oscillations of even -even spherical nuclei due to viscous dissipation gives viscosities in the interval 4.2-7.6 MeV fm-2 c-1 for nuclei from Pd-106 to Hg-198. For non-zero temperatures the ratio of shear viscosity to entropy density s is estimated and compared with the limit /s > 1/4 motivated by AdS/CFT for quark­gluon plasma [4]. 1. H.Song, S.A.Bass, and U.Heinz, Phys. Rev. C 89, 034919 (2014). 2. D.J.Rowe, K.T.Hecht, J. Math. Phys. 36 (9), 4711 (1995). 3. A.Kh.Khokonov, Liquid drop model of spherical nuclei with account of viscosity. Nucl. Phys. A., 2015, http://dx.doi.org/10.1016/j.nuclphysa.2015.09.013. 4. P.K.Kovtun, D.T.Son, and A.O.Starinets, Phys.Rev.Lett. 94 (2005)

Kuznetsov A.S. (SAI MSU, Moscow)

Fast optical transient detection by MASTER Global Robotic Net on the example of FERMI alerts
Early discovery of an optical afterglow of the gamma-ray burst GRB140801A in the 137° (3- error-box) of the Fermi Gamma-ray Burst Monitor (GBM). GRB140801A is one of the few GRBs whose optical counterpart was discovered solely from its GBM localization. The optical afterglow of GRB140801A was found by the MASTER Global Robotic Net 53 sec after receiving the alert, making it the fastest optical detection of a GRB from a GBM error-box. Spectroscopy obtained with the 10.4-m Gran Telescopio Canarias and the 6-m BTA of SAO RAS reveals a redshift of z=1.32. We performed optical and near-infrared photometry of GRB140801A using different telescopes with apertures ranging from 0.4-m to 10.4-m. GRB 140801A is a typical burst in many ways. The rest-frame bolometric isotropic energy release and peak energy of the burst is Eiso = 5.54-0.24+0.26 â 1052 erg and Ep, rest280 keV, respectively, which is consistent with the Amati relation. The absence of a jet break in the optical light curve provides a lower limit on the half-opening angle of the jet =6.1°. The observed Epeak is consistent with the limit derived from the Ghirlanda relation. The joint Fermi GBM and Konus -Wind analysis shows that GRB140801A could belong to the class of intermediate duration. The rapid detection of the optical counterpart of GRB140801A is especially important regarding the upcoming experiments with large coordinate error-box areas.

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Kuznetsov M.Yu. (INR RAS, Moscow)
mkuzn@ms2.inr.ac.ru

Primary photons in cosmic rays with energy 1017eV from EAS MSU experiment data
We analyze EAS-MSU archival data in order to search for primary photons in cosmic rays at energies ~1017 eV. The method is based on the fact that for hadronic showers of such energies it is highly improbable to have zero muons in a central area of EAS (Extensive Air Shower) while it is possible for primary gamma rays. We performed Monte-Carlo simulations of proton-induced showers using the CORSIKA simulation code with EGS4, QG