SAO-BNO Conference 2018

International Conference

The multi-messenger astronomy:
gamma-ray bursts, search for electromagnetic counterparts to neutrino events and gravitational waves

7-14 October 2018.     Nizhnij Arkhyz (SAO) and Terskol (BNO)

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Fee and accomodation



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Special Astrophysical Observatory of RAS

BNO page
Baksan Neutrino Observatory of INR RAS


Sunday, October 7. Arrival day.

There will be several transport runs from Mineral Waters airport to Nizhnij Arkhyz as Conference participants arrive.
16:00 - 18:00   Registration

Monday, October 8.

8:15 - 9:00    Registration
9:00 - 9:10    The Conference opening (V.V. Vlasyuk, V.V. Sokolov)
     Section: Multimessenger, neutrino, gamma and gravitation astronomy
    Chairman: Sokolov V.V.
09:10 - 09:40   V.V. VLASYUK and V.V. Sokolov (SAO RAS).
Multi-messenger astronomy: the alert observations of gamma-ray bursts afterglows, supernovae and search for optical counterparts to neutrino events and gravitational waves
Preliminary abstract
    The study and monitoring of sources of cosmic gamma-ray bursts (GRBs), identification of sources of gravitational waves and neutrino signals from supernovae, fast radio bursts. We plan to carry out (to continue) follow-up observations of localization areas (identification) of newly-discovered gamma-ray bursts, neutrino and gravitational signals, and supernovae (in the mode of Target of Opportunity Observation). The telescopes: BTA, Zeiss-2000 (TB INASAN), Zeiss-100 (SAO RAS) in the modes of photometry, spectroscopy, fast photometry and polarimetry. Alerts from missions Swift, Fermi, INTEGRAL, Lomonosov and others. The aim of the search for optical/electromagnetic components with SCORPIO and MANIA at BTA is the sources (related to GRBs) of neutrino and gravitational waves (GW events) detected by LIGO (Laser Interferometer Gravitational-wave Observatory) and Virgo.
09:40 - 10:10   S. FABRIKA, G. Valyavin, A. Valeev, V. Vlasyuk, Yu. Balega, V. Sasyuk (KFU), S. Bondar (RPC-PCI), I. Romanyuk, T. Fatkhullin, E. Emelianov, V. Sinyansky, A. Marukhno, P. Radchenko (SAO RAS).
New robotic telescopes at SAO RAS.
    We present a new observatory of four 0.5m robotic telescopes nearby 6m BTA telescope (Special Asrophysical Observatory, Russia). The observatory is under constraction, the first one was completed in December 2017, the second one in November 2018, the third one in 2019. We would suggest the fourth one in Chile or in the same at BTA telescope. Our main goal is the identification of GRBs (gamma-ray bursts) and to take their spectra from the BTA telescope. The same is FRBs (fast radio bursts) when we observe at RATAN-600 (Western sector) and try to observe with the first robotic telescope at exposure less than 1 sec in optical. We also hope to merging black holes or NSs and IceCube. The second goal is exoplanets. The accuracy for 12 mag star is 0.001 mag. The third one is SNe, CVs, magnetic WDs, Ap/Bp magnetic stars.
10:10 - 10:40   Bisikalo D.V., SAVANOV I.S., Shugarov A.S. (INASAN, Moscow).
The network of of wide-angle telescopes of INASAN
    Multimessenger astronomy and distributed observational networks are one of the modern prioritized directions of observational astronomy that allow to perform fundamentally new types of research. The main task of the proposed project is the creation of a specialized network for mass observations optical radiation from sources of gravitational waves recorded with the help of the gravitational telescope LIGO. For the reliable detection of objects related to gravitational events a network of telescopes with an aperture of about 2 m, coupled with modern photodetectors is proposed.
10:40 - 11:00               Coffee break
11:00 - 11:30   Shashi Bhushan Pandey (Aryabhatta Research Institute of Observational Sciences ARIES, India).
The 3.6m DOT and study of energetic cosmic transients. (Via Internet)
    I summarize about the 3.6m DOT project along with proposed plans to study transients in near future. Longitudinal advantage of India is very much suitable for the time domain astronomy and particularly for time critical observations. Recently installed 3.6m Devasthal optical telescope along with back-end instruments are well suited for observations of energetic cosmic transients like Supernovae and Gamma-ray bursts.
11:30 - 12:00   Lorenzo Amati (Istituto di astrofisica spaziale e fisica cosmica INAF - IASF Bologna, Italy).
The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) (Via Internet)
    The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a mission concept developed in the last years by a large European consortium. As detailed in Amati et al. 2017 (arXiv:1710.04638) and Stratta et al. 2017 (arXiv:1712.08153), THESEUS aims at exploiting high-redshift GRBs for getting unique clues to the early Universe and, being an unprecedentedly powerful machine for the detection, accurate location (from ~arcmin to ~arcsec) and redshift determination of all types of GRBs (long, short, ~high-z, under-luminous, ultra-long) and many other classes of transient sources and phenomena, at providing a substantial contribution to multi-messenger time-domain astrophysics. Under these respects, THESEUS will show a beautiful synergy with the large observing facilities of the future, like E-ELT, TMT, SKA, CTA, ATHENA, in the electromagnetic domain, as well as with next-generation gravitational-waves and neutrino detectors, thus enhancing importantly their scientific return.
12:00 - 12:30   R.V. NOVOSELTSEVA, M.M. Boliev, I.M. Dzaparova, M.M Kochkarov, A.N. Kurenya, Yu. F. Novoseltsev, V.B. Petkov, P.S.Striganov, A.F. Yanin (INR RAS, BNO).
A search for neutrino bursts in the Galaxy at the Baksan Underground Scintillation Telescope; 38 years of exposure
    The Baksan Underground Scintillation Telescope has been operating under the program of searching for neutrino bursts since the middle of 1980. The target is two parts of the facility, the D1 and the D2, with the total scintillator mass of 240 t. The count rates of background events are 0.02 s -1 in the D1 and 0.12 s -1 in the D2. The actual observation time over the period from June 30, 1980, to December 31, 2017, is 32.1 years. No candidate for the stellar core collapse has been detected during the observation period. The upper bound for the mean rate of the supernova core collapse in our Galaxy is 0.072y -1 (90% CL).
12:30 - 14:00               Lunch break
14:00        Chairman: Vlasyuk V.V.
14:00 - 14:30   ULANOV M.V., Aptekar R.L., Golenetskii, S.V., Frederiks D.D., Svinkin D.S. (Ioffe Institute, StPetersburg).
The Helikon-I and Konus-UF gamma-ray burst experiments
    We present Konus-UF and Helikon-I, the future space-based experiments designed to study temporal and spectral characteristics of gamma-ray bursts, solar flares, soft gamma repeater bursts, and other transient phenomena over a wide energy range from 10 keV to 15 MeV. The instruments will be mounted onboard the World Space Observatory Ultraviolet (WSO-UV) and the InterhelioProbe spacecraft. The spacecraft orbits are going to be far from the Earth's magnetosphere, which enables nearly uninterrupted observations of the entire sky under stable background conditions. .
14:30 - 15:00   Mimoza HAFIZI, Lindita Hamolli (Department of Physics, Tirana University, Albania).
THESEUS as a probe for exoplanet population in other galaxies
    Quasar microlensing is called the lensing effect on quasars, caused by compact objects in the mass range 10-6 ≤ M/MSun ≤ 103, inside a lens galaxy. It is shown that quasar microlensing provides a possibility to probe extragalactic planets in the lens galaxy. THESEUS will observe Quasars and AGN-s with a certain spectral resolution. We would discuss about the ability of THESEUS to probe, by this way, extragalactic planets.
15:00 - 15:30   TRUSHKIN S. A., Fabrika S., Tsybulev P., Nizhelskij N.A., Bursov N. N. (SAO RAS; KFU, Kazan).
Search of fast radio bursts. The first year of the blind survey at 4.7 GHz with RATAN radio telescope
    We are carrying out the search program of the bright rare fast radio bursts (FRB) [1] with the RATAN-600 radio telescope. Daily during ten months and 24 hours we use the special antenna, the Western Sector and secondary mirror (SM) with new design (N5). Its effective area is near 1100 meter in square at elevation H=52deg (Dec=33d08). The special three high sensitivity receivers at 4.7 GHz established in the focal plane of SM. The total frequency band of 600 MHz of each receiver was divided by the microwave filters on four sub-bands of 150 MHz and all signals of 12 channels of back-end are recorded with the maximal temporary resolution 0.5 ms. The special routine on the powerful PC analyzes the coming signals in order to find the fast bursts (5 sigma = ~3-5 Jy), shifted in time due to the interstellar (or intergalactic) dispersion (DM ~ 100-1500 pc/cm3) in dependence on the sub-band frequencies events with expected fluxes 1-30 Jy and error box of coordinates will be send to the robotic optical wide-angular small telescopes array constructing. The relatively big field of view of the three-beam system in the 24-hours survey allows detecting some FRB per year. In 2017-18 we have carried out the pilot observations of the bright and close pulsar PSR B0329+54 at 2.3 and 4.7 GHz with wide-band (120 and 600 MHz respectively). We have detected up to 100 pulses with the own spin period P=0.71452s getting in the antenna beams, recorded with time interval 0.5ms. The width of the average pulse (w50) is equal to 10 ms at 4.7 GHz. Such measurements are a well test for the FRB search. We see that the most suitable time is the night hours with almost total absence of the interference. We have detected a lot of usual discrete sources in the area of the survey when we summarized the sub-bands and daily records. We have changed the elevation to H=32deg i.e. to DEC of the Crab Nebula pulsar =22d01m) of the survey in May 2018 in order to improve the condition of the search: the smaller interference and the larger field of view and search for giant pulses from the 33-ms pulsar. So far we have not detected the dispersed pulses - FRB - during almost year of the survey.
[1] D. R. Lorimer, M. Bailes, M. A. McLaughlin, et al. (2007) Science, 318, 77
[2] S. Trushkin, S.N. Fabrika, P.G. Tsybulev, N.A. et al. (2018) Proceedings of The International Conference "SN 1987A, Quark Phase Transition in Compact Objects and Multimessenger Astronomy", Russia Nizhnij Arkhyz (SAO RAS), 2-8 July 2017.
15:30 - 16 :00              Coffee break
16:00 - 16:30   Jacek Szabelski (National Center for Nuclear Research, Lodz, Poland).
Multi-messenger capabilities of EUSO-like telescopes
    JEM-EUSO Collaboration (now: Joint Experiment Missions - Extreme Universe Space Observatory) is realizing several smaller experiments towards the main target: large space telescope observing the Earth night atmosphere for extreme energy cosmic rays (CR) measurements. High energy CR interacting with atmosphere nuclei are producing particle cascades called Extensive Air Showers (EAS). Majority of these particles go with speed nearly equal to the speed of light in vacuum, and they are producing Cherenkov light and molecular nitrogen fluorescence (in near UV spectrum region). EUSO telescopes could see these fluorescence light directly and Cherenkov light reflected from the Earth (clouds, snow, sea).The very fast camera (now 400 000 frames/s) allows to measure EAS development in time. With light curve it is possible to evaluate the primary CR particle energy and direction. The method would be used to observe the particles with energy approximately above 5E19eV, and if they are protons, their directions should point to the origin sources. Since the telescope would observe a huge area, a 3 year observation statistics would excess several times the Pierre Auger Observatory and the Telecope Array Observatory ultra high energy CR event gains. Using the same device for the Northern and Southern sky would allow for better CR anisotropy study.
    Observing very large mass of the atmosphere (and surface layer) some ultra high energy neutrino observations are expected. Most of them would be identified as upward going EAS. Very energetic atmospheric events like lightnings and TLE's would be measured with a fine time resolution. Atmospheric night emission of UV light would be measured as a part of UV background (sky light reflection, human activities etc.).
    Three test experiments were realised, so far: EUSO-Balloon (to show functionality of measurement methods), TA-EUSO (for calibration trigger tests, located at the Telescope Array experiment in Utah desert) and SPBEUSO (Super Pressure Balloon, for more detailed tests). The Russian TUS Experiment (Tracking Ultraviolet Set-up) at the M. Lomonosov Platform is a part of JEM-EUSO Collaboration missions, now. The Mini-EUSO (to measure UV background from ISS) and SPB2-EUSO are planned within coming year.
    Contribution from our group would be presented, too. Especially some electronic hardware solutions which would allow for multi-messenger observations.
16:30 - 17:00   TSVETKOVA A., D. Frederiks, D. Svinkin, S. Golenetskii, A. Lysenko, M. Ulanov, R. Aptekar (Ioffe Institute, StPetersburg).
Konus-Wind observations of gamma-ray bursts with known redshifts
    We present the results of a systematic study of GRBs with reliable redshift estimates detected in the Konus-Wind (KW) experiment from the beginning of the afterglow era to the middle of 2018. The sample represents the largest set of cosmological GRBs studied to date over a broad energy band. We consider the behavior of the rest-frame GRB parameters in the hardness-duration and hardness-intensity planes (the "Amati" and "Yonetoku" relations) and examine if the correction for the jet collimation improves these correlations for the KW sample.
    Accounting for the instrumental bias, we estimate the KW GRB luminosity evolution, luminosity and isotropic-energy functions, and the evolution of the GRB formation rate.

Tuesday, October 9.

09:00        Chairman: Savanov I.S.
09:00 - 09:30   N.V. OREKHOVA4, G.M. Beskin1,2, S.V. Karpov1,2,6, A.V. Biryukov3,2, S.F. Bondar4, E.A. Ivanov4, E.V. Katkova4, A.V. Perkov4, and V.V. Sasyuk2,5 (1SAO RAS; 2KFU, Kazan; 3SAI MSU; 4Open Joint-stock Company Research-and-Production Corporation Precision Systems and Instruments, Arkhyz Optical Observation Station, Nizhnii Arkhyz; 5Parallax Limited Liability Company, Kazan; 6CEICO, Institute of Physics, Czech Academy of Sciences, Prague, Czech Republik).
Search and study of optical transients with MiniMegaTORTORA.
    We present the four-year observation results of the Mini-MegaTORTORA (MMT-9) nine-channel wide-field optical sky monitoring system with subsecond temporal resolution. This instrument scans the sky on every clear night with a FoV as large as 900 deg2. It is used for real-time detection and classification of optical transients, three-filter photometry close to Johnson's BVR system, and polarimetry of detected objects. The limiting magnitude of the system is V = 11m for 0.1 s (one frame duration) temporal resolution, and reaches V = 13-14 m for an exposure of several minutes. The system is equipped with a powerful computing facility and a dedicated software pipeline to perform automatic detection, real-time classification, and investigation of transient events of a different nature moving in the near-Earth space located in the Galaxy and at cosmological distances. Properties of meteors and satellite samples, variable stars, and GRBs detected using MMT-9 are discussed.
09:30 - 10:00   NALIVKIN M.A., Shugarov A. (INASAN, Moscow).
A multi-aperture survey telescope for the INF project
    A new project of dedicated network of robotic wide-field telescopes INF (INASAN NEO Finder) for 10-m size hazardous NEOs search and optical transients was proposed. The INF multi-aperture telescope consists of 8 wide-field telescopes (Terebizh VT-78d) on direct drive mount. The optical system of VT-78d telescope provides a unique combination of parameters: aperture (250mm), focal ratio f/1.58, star image quality Δ″80=5 arcsec on a field of view 2ω=10°. The INF total field of view is 574 sq.deg (298 Mpixels) with 5.2 arcsec/pixel image scale.
    The INF project main features are short cadence time (1h for S/N=7) of all-sky survey 20000 sq.deg. and moderate limiting magnitude 19m on integral light. The possibility of high time resolution survey mode (0.2...1s) with a perspective sensor GSENSE 6060BSI is discussed.
10:00 - 10:30   NAROENKOV S.A., Nalivkin M.A. (INASAN, Moscow).
The robotic telescope of INASAN
    The Institute of stronomy is working on the develompent of robotic monitoring systems for solving a wide range of astrophysical problems. As a result of the work, a robotic optical system with a 20-cm wide-angle telescope was created. The special software has been developed. This software allows fulfilling observations in the automatic mode without operator's participation. The robotic telescope IRT-20 is located on the Zvenigorod Observatory of INASAN. Photometric observations of variable stars and searching of optical transients are carried out on the telescope in a constant mode.
10:30 - 11 :00              Coffee break
11:00 - 11:30    Wang Xiang-Gao (Guangxi University, Nanning, Guangxi, China).
Gamma-ray Burst Afterglow and GRBs Observing Plan
    Using a large sample of GRBs with optical afterglow data, we perform a systematic study to address the question:
(1) How is the possible emission components and their physics in the optical light curve?
(2) How bad or good are the external forward shock models?
(3) How is the jet break in the optical observation?
We also present our GRB observing plan in the recently.
11:30 - 12:00   Zhang Jin ( National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China).
Radiation Properties of the Jets in AGNs: from the Core to Extended Regions
    On the basis of a large sample of the observed spectral energy distributions (SEDs) and the leptonic jet model, we studied the jet radiation properties of AGNs at small and large scales. We found that:
    (1) the flat spectrum radio quasar (FSRQ) jets are highly magnetized with high radiation efficiencies while the BL Lac jets may be dominated by particles with low radiation efficiencies, and the narrow-line Seyfert 1 galaxy (NLS1) jets are intermediate between them;
    (2) GRB jets are highly magnetized with high radiation efficiency, similar to FSRQ jets;
    (3) the Eddington ratio may be the fundamental parameter to unify the BL LacNLS1FSRQ sequence;
    (4) The luminosity ratio of radio to X-ray may be an indicator to distinguish between hotspots and knots in large-scale jets of AGNs. And the inverse Compton scattering of the cosmic microwave background process may be the origin for the high-energy emission in large-scale jets.
12:00 - 12:30   Liang Enwei (Center for Astrophysics and Space Sciences, Guangxi University, Nanning, China).
Magnetar as Central Engine of Gamma-Ray Bursts: Central Engine-Jet Connection, Wind-Jet Energy Partition, and Origin of Some Ultra-Long Bursts (presented by Wang Xiang-Gao)
    The shallow-decaying segment observed in the early X-ray afterglow lightcurves of Swift gamma-ray bursts (GRBs) may be dominated by the magnetic dipole (MD) radiation wind of a newly-born magnetar, which may serve as central engine of these GRBs. By selecting a sample of 117 long GRBs whose jet and MD wind radiations can be separated, we derive the parameters of the magnetars with the X-ray data and investigate possible relations of these parameters to the isotropic energy release of prompt gamma-ray and X-ray emission from their jets (Ejet, iso). We show that the initial spin period (P0) of the magnetars is tightly correlated with E jet, is, i.e., P0 ∝ (Ejet, iso)(-0.36 0.03). This relation suggests that a magnetar with faster rotating speed can power a more energetic GRB. The energy releases of the jets and winds are tightly correlated, i.e., Ewind ∝ (Ejet, iso)(0.89 0.07). This may indicate that the energy partition between the jet and wind among these GRBs are quasi-universal, being independent from the properties of the magnetars. Within this jet-wind paradigm, we propose that GRB 101225A-like ultra-long GRBs with soft, steady gamma-ray/X-ray emission may be attributed to their MD wind emission owing to off-axis observations to their jets.
12:30 - 13:00    Xin Liping (CAS Key Laboratory of Space Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China).
The observations of GRB afterglows and the plan to search for optical counterparts of gravitational wave.
    I will give a brief overview of the follow-up observations for GRB afterglows by 0.8m TNT telescope in China, which has been carried out for more than 130 GRBs in the last ten years. Our recent works will be introduced about the research on the micro-parameters for several GRBs based upon the multi-wavelength afterglow observations. Finally I also would like to give a little talk about our new observation program named as GRANDMA, which consists of more than 16 telescopes in the world wide to seek the optical counterparts of GW in O3.
13:00 - 14:00               Lunch break .
14:00        Chairman: Fabrika S.N.
14:00 - 14:30   A.J.Castro-Tirado (Instituto de Astrofisica de Andalucia IAA-CSIC, Granada, Spain).
The monitoring of gamma-ray burst afterglows and search for optical counterparts to neutrino events and gravitational wave signals. (Via Internet)
    I will highlight how the new Era of Gravitational Wave Astronomy has just been opened thanks to the detection of the first electromagnetic counterpart to GW 170817 and will discuss the implications of the short-duration GRB associated to it, just before the opening of the forthcoming O3 LIGO-Virgo run in 2019.
14:30 - 15:00   Sergeev A.V. (Terskol Branch of INASAN RAS).
The photometer for detection of ultra-high-frequency variability at deficiency of quanta.
    This device is designed to measure rare quantum flows, when there are not enough quanta to explore the light curve.
15:00 - 15:30   Matwey V. KORNILOV, M.V. Pruzhinskaya, K.L. Malanchev, E.E.O. Ishida, F. Mondon, A.A. Volnova, V.S. Korolev (Sternberg Astronomical Institute, Moscow University).
Machine learning techniques for analysis of photometric data from the Open Supernova catalog
    The next generation of astronomical surveys will revolutionize our understanding of the Universe, raising unprecedented data challenges in the process. One of them is the impossibility to rely on human scanning for the identification of unusual/unpredicted astrophysical objects. Moreover, given that most of the available data will be in the form of photometric observations, such characterization cannot rely on the existence of high resolution spectroscopic observations.
    The goal of this project is to detect the anomalies in the Open Supernova Catalog with use of machine learning. We will develop a pipeline where human expertise and modern machine learning techniques can complement each other. Using supernovae as a case study, our proposal is divided in two parts: a first developing a strategy and pipeline where anomalous objects are identified, and a second phase where such anomalous objects submitted to careful individual analysis. The strategy requires an initial data set for which spectroscopic is available for training purposes, but can be applied to a much larger data set for which we only have photometric observations. This project represents an effective strategy to guarantee we shall not overlook exciting new science hidden in the data we fought so hard to acquire.
15:30 - 16:00              Coffee break
16:00       Poster session
Chairman: Sokolov V.V.
16:00 - 16:10   Kovalev Yu.A., Kardashev N.S., Kovalev Y.Y., Zhekanis G.V., Sotnikova Yu.V., Nizhelsky N.A., Tsibulev P.G., ERKENOV A.., Bursov N.N. (Astro Space Center, LPI RAS, Moscow; SAO RAS).
RATAN-600 reveals the neutrino association B0506+056 as a typical variable quasar on the basis of 20-years monitoring of its radio spectrum (Poster)
    Results for 10 AGNs including this one are presented for 66 sets of radio observations of instantaneous 1-22 GHz spectra at 4-6 frequencies in 1997-2018 (2-6 spectra per a year) with RATAN-600. About 600 AGNs are monitored within the program to study the nature of their long term variability. The currently ongoing radio ?are in B0506+056 has started in 2013 and was slowly evolving until reaching its first maximum in December 2017. The second maximum in May-June 2018 has flux densities of about 0.7-0.9 Jy for the flattened spectra. A model comparison of the monitored objects shows that the shapes, structure and variability of the B0506+056 spectra are typical for variable AGNs. Their evolution is caused by a variable synchrotron spectrum emitted by relativistic particles which are ejected out from an active nucleus in a longitudinal magnetic field (details see in Kovalev et al., 2000, PASJ, v.52, 1029). The uniqueness of this quasar may be associated to relativistic protons, which are necessary to produce the high-energy neutrino. The protons should be effectively accelerated in its active nucleus and emit in the jet. In opposite to that, nuclei of other quasars might accelerate particles less efficiently and as a result their jets produce synchrotron emission by relativistic electrons. The Space VLBI mission RadioAstron has observed this object in 2015-2016 but did not detect it. This might be explained by the low level of brightness of the jet in B0506+056 as seen within the MOHAVE VLBA program during the beginning phase of the flare. Our model analysis of the presented variable radio spectra supports this hypothesis.
16:10 - 16:20    Z. Debicki, K. JEDRZEJCZAK, M. Kasztelan, W. Marsza l,J. Orzechowski J. Szabelski, P. Tokarski (National Center for Nuclear Research, Astrophysics Division in Lodz, Poland).
Measurements of thermal neutron flux in underground laboratories, a standard proposal for the BSUIN project (Poster)
    One of the goals of the BSUIN project is to propose standard methods for the characterization of underground laboratories (UL). We have proposed scheme for thermal neutron flux measurement: simple and low-cost but still very reliable. A pilot measurements were made in mines in Freiberg (Germany) and Pyhasalmi (Finland). Data analysis is in progress
16:20 - 16:30    P. Jalas1, V. Isoherranen1, J. Joutsenvaara1, E.-R Niinikoski1, R. Heikkila1, T. Makkonen1, H. Ahola2, P. Aro2, T. Vuorela2, J. Kisiel3, K. Karpa3, K. Szkilniarz3, M. Laaksoharju4, M. Ohlsson4, W. Pytel5, D. Horner6, H. Mischo6, R. Giese7, K. Jaksch7, V. Mockus8, T. Valys8, K.Jedrzejczak9, M. KASZTELAN9, J. Szabelski9, V. Gostilo10, V. Shekov11, A. Stepanov12, T. Lindborg13, V. Karu14, A. Paat14 (1University of Oulu; 2Oulu University of Applied Sciences, Oulu, Finland; 3 University of Silesia, Katowice, Poland; 4Swedish Nuclear Fuel and Waste Management Co., Stockholm, Sweden; 5KGHM S.A., Research development center Cuprum, Wroclaw, Poland; 6TU Bergakademie Freiberg, Freiberg, Germany; 7German Research Centre for Geosciences, Potsdam, Germany; 8Vilnius University, Vilnius, Lithuania; 9National Center for Nuclear Research, Astrophysics Division in Lodz, Poland; 10Baltic ScientiIfic instruments, Riga, Latvia; 11Karelian Research Center of Russian Academy of Sciences, Petrozavodsk, Russia; 12Khlopin Institute, St Petersburg, Russia; 13Sotkamo Silver AB, Stockholm, Sweden; 14Tallinn University of Technology, Department of Geology, Tallinn, Estonia).
BSUIN - Baltic Sea Underground Innovation Network (Poster)
    The aim of the BSUIN project is to join efforts in making the underground laboratories in the Baltic Sea region more accessible for innovation, business development and science by improving the availability of information about the underground facilities, service offerings, user experience, safety and marketing.
16:30 - 16:40   BALAKINA E.A., Pruzhinskaya M.V., Moskvitin A.S. (Sternberg Astronomical Institute, Moscow University; SAO RAS).
Optical Photometry and Modeling of the Type IIb Supernova 2017gpn (Poster)
MASTER OT J033744.97+723159.0/SN 2017gpn was discovered in the error-box of LIGO/Virgo G299232/PGW170826 gravitational event. The spectrum of SN 2017gpn is consistent with a Type IIb supernova. In this work we present the photometry of 20 epochs of observations performed with CCD-photometer on the Zeiss-1000 telescope. The light curves in B and Rc filters were obtained. The multicolour light curves were also modelled numerically using the one-dimensional radiation hydrodynamical code STELLA (Blinnikov et al. 1998, 2006).
16:40 - 16:50   AVAKYAN A.L., Malanchev K., Lipunova G. (Sternberg Astronomical Institute, Moscow University).
Accretion disk wind influence on the evolution of LMXB outburst (Poster)
    According to the light curves obtained from observations of LMXB (Low-Mass X-ray Binary), within the framework of the Shakura-Sunyaev model it was found that the alpha viscosity parameter, which characterizes the mass transport in the accretion disk, lies in the range of 0.2-1. But simulations of the magnetorotational instability give values an order of magnitude smaller (about 0.03). In this work, we considered an additional source of matter transfer, namely, wind. We simulated the disk with the influence of the wind, which can decrease value of alpha parameter. As the result we receive the dependence of the change in the alpha on wind parameters. And if the decrease in alpha parameter is strong enough we conclude that the presence of wind can strongly affect the viscosity value, as well as the entire evolution of the disk as a whole.
16:50 - 17:00   TAVLEEV A.S., Malanchev K., Lipunova G. (Sternberg Astronomical Institute, Moscow University).
Vertical structure of accretion disks in LMXB (Poster)
    LMXB (Low-mass X-ray binary) is a binary system where one of the components is either a neutron star or a black hole. The other component (donor, usually main sequence star) fills its Roche lobe and therefore accretes mass to the compact object. This leads to the formation of the accretion disk. The vertical structure of the accretion disk is calculated. We use a flexible calculation system, a choice of the equation of state, the opacity law and the chemical composition depends on the model. Our calculations can improve the accuracy of the modeling of LMXB outbursts.
17:00 - 17:10   Gorbunov I.A. (Sternberg Astronomical Institute, Moscow University).
Test of modified gravitational theories in PSR J1903+0327.
    In our work we observed the mixed binary system J1903+0327 consisting of a pulsar and a main sequence star. All observations were made with the 2,5-meter SAI telescope. As a result we obtained the high-precision photometric data of the optical component of the considered system in the J, H, K-bands. These measurments are 3-percent more accurate than those already existing, which will make it possible to determine the mass of the pulsar in two independent ways for their further comparison and verification of alternative theories of gravity.
17:10 - 18:00              Discussion

Wednesday, October 10

9:00       Section: Gamma-ray and neutrino astronomy
   Chairman: Kazalov V.V.
09:00 - 09:30    Sinev V.V. (INR RAS, Moscow).
Solar CNO neutrinos or terrestrial 40K antineutrinos?
    The Earth thermal flux value varies from 50 up to 250 TW according different estimations. Upper limit could be achieved only if potassium abundance in the Earth exceeds 2%. In Borexino data the valley between beryllium neutrinos and 11C spectrum is filled with betas from 210Bi. But it also contains CNO neutrinos. CNO cycle in the Sun could be depressed according to last researches. This means that part of CNO spectrum could be from terrestrial 40K antineutrinos because their spectra are very similar.
9:30 - 10:00   V.B. Petkov (BNO INR RAS).
The multi-messenger astronomy: experiments in the Baksan Neutrino Observatory.
10:00 - 10:30   KOCHKAROV M. M.1, Boliev M. M.1, Dzaparova I. M.1,2, Novoseltsev Yu. F.1, Novoseltseva R. V.1, Petkov V. B.1,2, Yanin A. F.1 (1INR RAS, BNO; 2INASAN, Moscow).
Fast neutrons in the Baksan Underground Scintillation Telescope: the background for core-collapse supernova searches.
    We report on the measurement of the flux and spectra of the fast neutron background at the BUST with a rock overburden of about 850 m. w. e., using a special method for the neutron flux estimation based on neutron activation analysis. The neutron-induced events are identified by a two-pulse signature of neutron inelastic scattering process.
10:30 - 10:45               Coffee break
10:45 - 13:00          Excursion to the 6-meter telescope BTA
13:00 - 14:00               Lunch break .
14:00        Chairman: Petkov V.B.
14:00 - 14:30   E.N.Alexeev, Yu.M.Gavrilyuk, A.M.Gangapshev, A.M.Gezhaev, V.V.Kazalov, V.V.KUZ'MINOV, S.I.Panasenko, S.S.Ratkevich (INR RAS, Moscow).
Results of three years search for the 213Po half-life variations
    Description of the TAU-3 installation intended for long-term monitoring of the half-life value (T½ ) of the 213 is presented. Isotope 229Th is used as a source of the mother's chain. The methods of measurement and processing of collected data are reported. Solar-daily variation with an amplitude ASo = (5.3 ± 1.1) · 10 -4, lunar-daily variation with an amplitude AL = (4.8 ± 2.1)·10 -4 and sidereal-daily variation with an amplitude AS = (4.2 ± 1.7) · 10-4 were found as a results of a treatment of the 622 days data series (July 2015 March 2017). An averaged value of the 213Po nuclei decay half-life was found to be to T½ = 3.705 ± 0.001 μs. A half-life value data set with the week duration step was constructed for the 922 days measurement time. Features of the half-life time behavior were analyzed.
14:30 - 15:00   V.S. ROMANENKO1, V.B. Petkov1, 2, D.D. Dhzappuev1, A.S. Lidvansky1, E.A. Gorbacheva1, I.M. Dzaparova1, 2, A.U. Kudzhaev1, N.F. Klimenko1, A.N. Kurenya1, O.I. Mikhailova1, K.V. Ptitsyna1, M.M Khadzhiev1, A.F. Yanin1 (1INR RAS, BNO; 2INASAN, Moscow).
Limits on the isotropic diffuse gamma-ray flux between 100 TeV and 1 PeV: experiments Carpet-2 and Carpet-3.
    An experiment for measuring the flux of gamma rays of cosmic origin with energy above 100 TeV is currently being prepared at the Baksan Neutrino Observatory (the Carpet-3 experiment). The experiment implies extension of the existing Carpet air shower array by increasing areas of both muon detector and surface scintillation detectors. In this paper we present estimates of sensitivity of the experiment to showers from primary gamma-rays for different configurations of the accomplished array. Using experimental data of the previous version of the array (Carpet-2) accumulated for 9.2 years, preliminary estimates of the flux upper limit is deduced for cosmic gamma-rays with energies above 700 TeV.
15:00 - 16:30   Yu. M. Gavrilyuk1, A. M. Gangapshev1, V. V. KAZALOV1, V. V. Kuzminov1, S. I. Panasenko2, A.D. Petrenko2, S. S. Ratkevich2, D. A. Tekueva1, and S. P. Yakimenko1 (1Institute for Nuclear Research, RAS, Moscow, Russia; 2V.N.Karazin Kharkiv National University, Kharkiv, Ukraine).
Search for double K-capture of 124Xe with the large volume copper proportional counter.
    During several years at the Baksan Neutrino Observatory INR RAS is undergoing the experiment for searching of 2K (2ν)-capture in 124Xe. This isotope has several advantages: 1) it has the largest kinetic energy of transition among candidates of nuclei for which predicted the existence of ECEC; 2) since xenon is the noble gas, then it could be easily use as a system isotope-detecting medium in a gas detector. To search for 2K-capture in 124Xe the large volume copper proportional counter (CPC) is used.
    In our work, we present the results of the simulation, with the Geant4 package, of CPC background from the decays of 238U and 232Th nuclei in the construction materials of the CPC case, as well as in elements of the low-background shield. The influence of neutrons produced in the rock of the underground laboratory from the decay of 238U and 232Th, where the experimental setup is located, on the production of the isotope 125I in the working gas of the detector, upon capture of thermalized neutrons by the 124Xe isotope is considered. The 125I isotope can have a significant influence on the background of the experiment since the total energy release in its decay belongs to the same energy region as ROI of 2K-capture in 124Xe.
15:30 - 16:00               Coffee break
16:00 - 16:30   A.N. Kurenya (BNO INR RAS).
DAQ system for the complex of the BUST Andyrchy Carpet-2 facilities
16:30 - 17:00   I.M. DZAPAROVA1,2, I.S. Savanov2, V.B. Petkov1,2, A.V. Sergeev1,2, D.D. Dzhappuev1, A.N. Kurenya1, V.B. Puzin2, E.A. Gorbacheva1, O.I. Mikhailova1, M.A. Nalivkin2, S.A. Naroenkov2, A.A. Shlyapnikov3 (1INR RAS, BNO; 2INASAN, Moscow; 3CrAO RAS, Crimea).
Quick search for optical partners of bursts of very high energy gamma-ray radiation
    Quick search for optical partners of bursts of very high energy gamma-ray radiation of high and ultrahigh energy range in conjunction with optical flares are conducted using the facilities of the Baksan Neutrino Observatory (BNO) of the INR RAS and a complex of astronomical telescopes at peak Terskol Observatory of the Institute of Astronomy of RAS. The search for bursts of cosmic ray intensity and cosmic gamma radiation is carried out at a complex of BNO facilities. The search and subsequent study of optical flares associated with the detected BNO events are carried out on a complex of astronomical telescopes at the peak Terskol. To search by external target designations (from GCS installations, the GCN network, etc.) of transient phenomena in the optical range a universal program for managing a complex of astronomical telescopes was developed and created. The report discusses the current state and preliminary results of the experiment.
20:00 - 21:00         Excursion to the modern art exhibition. Installation dedicated to SAO.
The modern media art project Station YE5 investigates the influence of specific geography of the place and the heritage of the era of Soviet modernism in the village of Nizhny Arkhyz.

Thursday, October 11.

09:00        Chairman: Novoseltseva R.
09:00 - 09:30   Semenov S.V.(Kurchatov Institute, Moscow).
Calculation of neutrino-nucleus cross section on the base of nuclear reactions data
    Neutrino-nucleus interaction, which has many applications, such as neutrino detection, neutrino oscillations study, nucleosynthesis processes examination is considered. Appropriate cross sections values depend on nuclear matrix elements, which are the goal of calculations for a variety of nuclear models. For there is a certain spread of results of these estimations it is reasonable to obtain nuclear matrix elements by the model-independent approach, which use experimental data on nuclear reactions. These are beta decay processes, charge exchange reactions, nuclear resonance fluorescence, which can give direct information on nuclear structure. The corresponding model-independent cross section calculations are produced and compared with existing experimental data on neutrino-nucleus interaction.
     Section: Compact astrophysical objects and the QCD phase transition
09:30 - 10:00   Grzegorz Wiktorowicz (National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China).
Origin of GW170817 from binary evolution studies. (Via Internet)
    The first double neutron star merger was also the first gravitational wave emission event to be observed in various bands of electromagnetic radiation. Its properties may have therefore a profound effect on our understanding of double compact object formation mechanisms. Three main scenarios are currently being thoroughly investigated: 1) the isolated formation in galactic disks; 2) the dynamical formation in globular clusters; and 3) dynamical formation in galaxies' nuclear clusters. Nonetheless, the calculated merger rates are orders of magnitude below the one inferred from the observation. Therefore, either the higher statistics of the events in future observational runs will lower the inferred merger rate, or our understanding of binary star formation and evolution needs significant improvement.
10:00 - 10:30   Agnieszka Janiuk (Center for Theoretical Physics of Polish Academy of Science, Poland).
Astrophysical sources of gravitational radiation
    In this talk, I will discuss the possible origin, cosmic environment, and fate of the binary compact objects responsible for gravitational wave radiation detected so far. First, I will present the LIGO assembly of binary black holes that was established since the discovery of GW150914. These systems contain very massive black holes, whose origin poses a puzzle for the stellar evolution models. One of the possibilities is a process of direct collapse of massive stars. The feedback from a rotationally supported innermost parts of the star during the collapse may however help unbind the outer layers and halt accretion.
    This will have a consequence for both the ultimate mass of the black hole, and its resultant spin. I will also discuss the possible electromagnetic counterparts of the gravitational wave sources. The binary neutron star merger GW170817 was connected with the gamma ray emission observed as a weak short burst, which peculiar properties pose constraints for its progenitor model. Moreover, at lower energies the follow-up surveys have shown the presence of a kilonova emission from the merger's dynamical ejecta. These ejecta masses are broadly consistent with the estimated r-process production rate, required before to explain the Milky Way isotopes abundances. It is possible that the magnetically driven winds launched due to the accretion in the GRB central ngine may also contribute to the kilonova emission from NS-NS merger. Finally, the electromagnetic signal is in general not expected from a BH-BH merger. However, the wear transient detected by Fermi GBM detector 0.4 seconds after GW 150914 has been generating much speculation. I will briefly present the scenarios that aimed to account for such a coincident signal.
10:30 - 11:00               Coffee break
11:00 -11:30   Pankaj Jain (Indian Institute of Technology, Kanpur, India)
Statistical Study of Spin Dynamics in Precessing black hole binaries in Eccentric Orbits. (Via Internet)
    We study the dynamics of spinning black hole binaries (BBHs) when gravitational waves (GWs) from such sources enter the observational frequency band of interferometric GW detectors. It has been shown in earlier studies that spin precession dynamics have a characteristic imprint on the distribution of spins of a population of BBH depending on the initial conditions. A substantial fraction of BBHs whose spins are initially anisotropically distributed subsequently get trapped into a spin-orbit resonance (SOR) configuration by the time GWs from these sources enter the frequency band of interferometric detectors. However, in general, binaries have non-zero eccentricity which was ignored in these studies as well as in the analysis of GW events, detected in advanced LIGO and advanced VIRGO. Taking eccentricity into account, we find that a much smaller number of BBHs evolve in the SOR configuration than the BBHs in the circular orbit. Most of BBHs are precessing freely in the observational bands of advanced LIGO and advanced VIRGO. The measurement of spin orientations can provide an essential link between GW measurements and astrophysics. Notably, the distribution of the relative orientations of spins can be used to constrain the models of formation of BBHs. This implies that the circular orbit and circular waveform approximation potentially lead to large biases in the measurement and determination of properties of BBHs through GW observations. Our study emphasizes the need for inclusion of eccentricity in studying the properties of a population of BBHs through the measurement of spins.
11:30 - 12:00    Gong Yungui (School of Physics, Huazhong University of Science and Technology, Wuhan, Hubei, China).
On the polarization of gravitational waves in alternative theories of gravity
    According to the Newman-Penrose formalism, in general there are six polarizations for general theories of gravity. In particular, the presence of the longitudinal mode means that the theory has all six polarizations. For massive scalar-tensor theory of gravity or f(R) theory, the longitudinal mode presents, but the theory has only three dynamical degrees of freedom, it seems that there is inconsistency somewhere. We point out that the Newman-Penrose formalism is not directly applicable to massive mode, the polarization of the massive scalar field is a mix of breathing and longitudinal mode and the longitudinal mode is proportional to the mass, when the mass becomes zero, the mix mode becomes the pure breathing mode which is consistent with the Newman-Penrose formalism. Since the longitudinal mode is proportional to the mass, so it can be detected only in very low frequency band, like the PTA band. The result is fundamentally important for the understanding of the nature of gravity. If we only detect the plus and cross polarizations, then we know that graviton is massless spin 2 particle. In addition to the plus and cross polarizations, if we also detect the breathing polarization, then we know that gravitation is mediated by both massless spin 2 and spin 0 particles. Apart from the above three polarizations, if we also detect the longitudinal polarization, then we know that gravitation propagated by massless spin 2 and massive spin 0 particles.
12:00 - 12:30   MOISEEV A.V.1, Lozinskaya T.A.2 (1SAO RAS; 2SAI MSU, Moscow).
A hypernova remnant in the galaxy IC10.
12:30 - 14:00               Lunch break .
14:00 - 14:30   FABRIKA S.N., Atapin K.E., Kostenkov A.E., Vinokurov A.S., Solovyeva Yu.N., Sholukhova O.N. (SAO RAS).
New data in ULXs
    The origin of ultraluminous X-ray sources (ULXs) in external galaxies whose X-ray luminosities exceed those of the brightest black holes in our Galaxy by hundreds and thousands of times. The new results were discovered, ULX-pulsars and high-velocity outflows up to 0.2c. They are in accordance with the super-Eddington accretion. Here we analyze the variability properties of the only five ULXs which show flat-topped noise (FTN) and QPO in their X-ray power density spectra. In each ULX the mass accretion rate may vary up to 3-4 times, and with decreasing the accretion rate (reduction the spherization radius), the hardness ratio and luminosity increase, and FTN and QPO may disappear. However, the strongest evidences come from optical spectroscopy. The spectra of the ULX counterparts are very similar to that of SS433 and WNLh type or LBVs in their hot state. From SS433 (solar) to ULXs we have decreasing hydrogen, and in two ULXs the hydrogen disappears. These are potential LIGO objects.
14:30 - 15:30   Martin Lopez-Corredoira (Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain).
Problems with the dark matter and dark energy hypotheses, and alternative ideas. (Via Internet)
    Two exotic elements have been introduced into the standard cosmological model: non-baryonic dark matter and dark energy. The success in converting a hypothesis into a solid theory depends strongly on whether we are able to solve the problems in explaining observations with these dark elements and whether the solutions of these problems are unique within the standard paradigm without recourse to alternative scenarios. We have not achieved that success yet because of numerous inconsistencies, mainly on galactic scales, the non-detection so far of candidate particles for dark matter, and the existence of many alternative hypotheses that might substitute the standard picture to explain the cosmological observations. A review of some ideas and facts is given.
15:30 - 15:45               Coffee break
15:45 - 18:00          Excursion to the radio telescope RATAN-600
20:00 - 20:30         Excursion to the local museum.

Friday, October 12.

9:00       Section: GRBs and cosmology
   Chairman: Sinev V.V.
9:00 - 9:30   Attila Meszaros (Faculty of Mathematics and Physics, Astronomical Institute, Charles University in Prague, Czech Republic ).
The spatial distribution of GRBs (both in redshift and in the angular sky position)
    The lecture has two parts.
    At the first part, after a brief review of the GRB topic, some articles about the cosmological origin of GRBs are mentioned from the years 1973-1997, when even the cosmological origin of GRBs were doubt. Also some other i9deas about the redshift distribution of GRBs are provided.
    At the second part the angular distribution of GRBs with the impact on the cosmological principle is discussed.
09:30 - 10:00   MAKAROV D.I.1, Zaitseva N.A.2, Bizyaev D.V.2 (1SAO RAS; 2SAI MSU).
Multiparametric Tully-Fisher relation for late type edge-on galaxies
    We analyzed the influence of additional parameters on the Tully-Fisher (TF) relation, using a sample of edge-on galaxies from the Revised Flat Galaxy Catalog with precise Hi data and photometry. Only the optical colors and Hi-to-optical luminosity ratio are statistically significant in the multiparametric TF relation. It means that only terms directly related to the baryonic matter, the stellar populations and the gas fraction in galaxies, play significant role in the TF relation. The standard deviation of our multiparametric TF relation is 0.32 mag, which makes a sample of flat galaxies a good tool for studies of the bulk motion of galaxies in the Universe.
10:00 - 10:30   I.V. Sokolov, A.J. Castro-Tirado, I. A. Solovyev, O.V. Verkhodanov, O.P. Zhelenkova, and V.V. Sokolov (Terskol Branch of INASAN RAS; SPbSU, StPetersburg; Instituto de Astrofisica de Andalucia IAA-CSIC, Granada, Spain; SAO RAS).
The field galaxies clustering in GRB lines of sight based on observations with BTA and other telescopes
    The characteristic signs of the clustering of field galaxies were detected in the direction to gamma-ray bursts (GRBs). All accessible signs of such clustering in the lines of sight and near the location of GRB021004 were tested. The data from observations with BTA/SCORPIO, HST/ACS, VLT/UVES and from the cluster catalog SDSS-III were used.
10:30 - 11:00              Coffee break
11:00 - 11:30   SHIROKOV S.I., Raikov A.A., Sokolov V.V., Vlasyuk V.V. (SAO RAS; MAO RAS; SPbSU, StPetersburg).
Gamma-ray bursts as an instrument for testing cosmological models
    We present a review of possible cosmological applications of the Gamma-Ray-Bursts multi-wavelength observations. A statistical analysis of the BeppoSAX, BATSE, Fermi and Swift GRB observational data is conducted. The T50-, T90-, Fluence- and Flux- distributions of these data have been studied with dividing them to the short GRB and long GRB subclasses. Luminosities and the Hubble diagram in different cosmological models are constructed. The spatial distribution of GRB sources with known redshifts is analyzed. Selection effects that distort the true source distribution are taken into account by comparing the observed distribution with fractal and uniform model catalogs. The influence of different cosmological models on the estimate of fractal dimensionality is also considered.
11:30 - 12:00   Attila Meszaros (Faculty of Mathematics and Physics, Astronomical Institute, Charles University in Prague, Czech Republic ).
The diversity of GRBs statistically (is there a third group? physical meaning? relation to XRFs?)
12:00 - 12:30   Raikov A.A., SHIROKOV S.I., Sokolov V.V. and Vlasyuk V.V. (SPbSU; SAO RAS; MAO RAS, StPetersburg).
Classification of Short GRBs. Merging and Postmerging.
    We think that separation of gamma-ray bursts in long and short ones is not enough and we propose a new classification of short GRBs based on morphology of burst sources. We found 3 emphasized picks in T90 distribution, that in our opinion are a consequence of collision (merging) of different objects. The first results point out that it's picks are at 0.1, 0.2 and about 1 second. Also it's evidence of thin structure into Eiso vs T90 distribution. The problem of the gravity afterglow of the final object is discussed separately.
12:30 - 13:00   A. N. Baushev, L. del Valle, L. E. Campusano, A. Escala, R. R. Muñoz, G. A. Palma (Bogoliubov Laboratory of Theoretical Physics, Joint Institute for Nuclear Research, Dubna).
Cusps in the center of galaxies: a real conflict with observations or a numerical artefact of cosmological simulations?
13:00 - 14:00               Lunch break
14:00 - 15:00       General discussion
   Chairman: Meszaros A.
19:00   Farewell party

Saturday, October 13.

09:00 - 18:00             Excursion to Baksan Neutrino Observatory or to the ancient Sentinsky temple

Sunday, October 14.

   Leaving Nizhnij Arkhyz

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