. : http://www.sai.msu.ru/EAAS/rus/confs/abstr_book2.pdf
: Tue Jun 16 22:37:14 2015
: Sun Apr 10 02:14:23 2016
: IBM-866
: narrow band filter

XII -



. .. , . .. 25 30 2015 .



. .. , ..

, 2015


2



, , , , 4 13 26 30 44 77 84 106

3



.. 1,2, .. 1,2, .. 3, .. 3, .. 3, .. 4,1 1 () 2 3 4 TUBITAK, , 1.5- -150 , , , , , , . , . , INTEGRAL, SWIFT, XMM-Newt on, CHANDRA, FERMI . ( ) , , , . . 1.5- - -150, (, ) (INTEGRAL, SWIFT, PLANCK) , ( , , ), , . , -150, .

4


2

.. 1,2, ..1,3,2 . . . .. . .. 3 :
1

2015 . 25 , . , , , , . , . .. XIX , XX , . . , , , () , ( ) ; . . , , , , . , , . , , , , . ,

5


, , . .. . . . .. . .. . ? ? ? , 6 , . , , . .. . . . .. . .. , , , . , , , , . , , . . .. , 40- Cyg X-1 = V1357 Cyg 40- (, ), ASM/RXTE . , , . . , 147/294 . Cyg X-1 ,

6


, , , . . , -. - - ( -1): Teff = 30400500 K, log g = 3.310.07 : 0.4 dex 1.0 dex He, N, Ne, Mg, Si, CNO- -. . . - , 1997 20032004 . ~3%, ~2000 K. - , , . HeII 4686 2D 3D , . 1/4 M/M 1/3. 8- VLT ESO ~100 , . . , ~600 . . .. , - 10- -, - .

7


. . , , , , . .. () , . . : ; . , (, , ) , , . A.M. Mickaelian Armenian Academy of Sciences Astronomical Surveys and Big Data Astronomical surveys are the main source for discovery of astronomical objects and accumulation of observational data for further analysis, interpretation, and achieving scientific results. Recent all-sky and large astronomical surveys and their catalogued data over the whole range of electromagnetic spectrum are reviewed, from Gamma-ray to radio, such as Fermi-GLAST and INTEGRAL in -ray, ROSAT in X-ray, GALEX in UV, SDSS and several POSS1/2 based catalogs (APM, MAPS, USNO, GSC) in optical range, 2MASS and WISE in NIR, IRAS and AKARI in MIR/FIR, NVSS and FIRST in radio and many others, as well as most important surveys giving optical images (DSS, SDSS), variability (GCVS, NSVS, ASAS, Catalina) and spectroscopic (FBS, SBS, HQS, HES, SDSS, CALIFA, GAMA) data. Overall understanding of coverage along the whole wa velength range and comparisons bet ween various surveys are given: galaxy redshift surveys, QSO, radio, Galactic structure, and Dark Energy surveys. Present astronomical archives contain billions of objects, both Galactic and extragalactic, and the

8


vast amount of data on them allow new studies and discoveries. The Big Data era has come. Astrophysical Virtual Observatories (VO) use available databases and current observing material as a collection of interoperating data archives and software tools to form a research environment in which complex research programs can be conducted. Most of the modern databases give at present VO access to the stored information. This makes possible not only the open access but also a fast analysis and managing of these data. VO is a prototype of Grid technologies that allows distributed data computation, analysis and imaging. Particularly important are data reduction and analysis systems: spectral analysis, SED building and fitting, modelling, variability studies, cross-correlations, etc. Computational astrophysics has become an indissoluble part of astronomy and most of m odern research is being done by means of it. Very often dozens of thousands of sources hide a few ver y interesting ones that are needed to be discovered by comparison of various physical characteristics. Cross-correlations result in revealing new objects and new samples. The large amount of data requires new approaches to data reduction, management and analysis. Powerful computer technologies are required, including clusters and grids. The International Council of Scientific Unions (ICSU) has recently created World Data System (WDS) to unify data coming from different science fields for further possibility of exchange and new science projects. .. , , : . . , , . , , , . , 1200 ( . 2013), -CDM. . , , 50300 . , , .

9


, . , , , . , BOSS, CDM , , , - . , , "eBOSS", . .. . . . .. . .. - - , . - OGRAN (Opto-Acoustical Gravitational Antenna) - Red Shift . 1. OGRAN (.. ., 2014). - , - . , , . ( ) 1019 1/2 1.3 ~4 , , . ( ) () . 2. Red Shift ( ., 2014). . .

10


, . , , 8.4 15 . , 2105, GP-A, 30 . . .. . . . .. . .. . , - . , , , , , , , . , , , . (, -) . , , . .. . . . .. . .. .

11


.. . . . .. . .. 13 2014 , 2.5 . , . . .. , .. , .. . . . .. . .. . . , . , , . -. . . >0.1. - <0.1. . .. . . . .. . .. . . , 10 , . . 14 2015 , , . , , .

12


1517 . , , , - , , : , . , . , . , !


.. - : , , , . ~10 . , , . , , : . , (). , , , , , . , : CHARA speckle, , Horch (Hor).

13


, . , , , . , : , , . , . .. . . . .. . .. , . , , 58 /. , - , . .. . . . .. . .. . . , (, .),

14


- , . , . ( ), . , , , , . .. , .. , , () . 1 .. 10 . : , ; , ; MEGNO . , 92 . (85 92) 2/1, 3/1, 5/2 7/3, . 69 . CYBERIA . 15-02-02868.

15


.. . . , , .. . 60- . , , , . - ( ) . . - ( , , , ) . , , . , . , . , - . . , . , .

16


1

.. 1, .. 2 . . . .. . .. 2

- . , . - . , , , . 50 .. 100 .. . ( EIF2013 - 9(15) 46/14/1). .. 1,2, . 2 . .. 2 . ..
1

. - . () . , . , , . . .

17


, , . , . -. , . , . , 2029 ., . , . , . , . .. 1,2, . 2 . .. 2 . ..
1

. , , 7 ., . , - () , , . . : (, , , , ), . .

18


. , , . , 2.86 3/2, 160 , - 10 40 . 0.5 2 . , ( 0.5 ) - ( 1.5 ) , -. ..1, ..2, ..3, ..3 . .. , , . .. , , 3 -4 ,
1

2

- . . . : 23 (20052008 .), 24 (20092013 .). (24 ) . , , (), . - . . 60 .

19


. .. . . . .. . .. 30 000 (13 000 . .. 17 000 . ..) , DE431. , , , . , VSOP2013 TOP2013. , , DE431 , TOP2013, 12 , VSOP2013. , DE431 VSOP2013 TOP2013. .. , .. , .. , . 0.65 63.4 . 26000 27100 . 1:2 17 p:q (15 < |p| < 26, 32 < |q| < 50, 48 < |p| + |q| < 75).

20


. . , . : , , , , , . , , -- . , , , . 3 16 2/. . , , . . . , , , . , . . ( RFMEFI59114X0003) ( 13-02-00026-) .

21


2

.. 1, .. 2 , . . . .. . ..
1

, . . : 2100 . , , : n ( n2), . , , . , , . , 10 / 100 /, 10 /. , . .. 1, .. 2 2 . . . .. . ..
1

- . , . () () . , 50 .. 100 ..,

22


, . , . , , , . ( EIF2013 - 9(15) 46/14/1). .. - .. , , . , , , , , , , , , , . m3 . ( .) ( ) , . , , m1/m2=50. ( ): x10, dx1/dt=0, y1=0, dy1/dt=0, x20, dx2/dt=0, y2=0, dy2/dt=0, x30, dx3/dt=0, y3=0, dy3/dt0. , m1 m2. , () (40C
23


.. - .. , 700000 . ( ) ( ) , . , , , . , : ) () 0; ) 2010 SO16 , , , , ; ) (, , , ) ; ) , - ; ) , , ( ). .. . . . .. . .. ( ~1 mas 50 as ) , . , , .

24


.. 250 . , , .. , , . () . () - () . : 1) ; 2) 3) . 1:2. , . , , , . , . . . .. , .. - , () . : , . : 1) , , ; 2) 100 . , .

25


. .

, , ,
.. , .. . . . .. . .. HDEC HDE (HDEC, III/182 Nesterov V.V., Kuzmin A.V., Ashimbaeva N.T., Volchkov A.A., Roser S., Bastian U. The Henry Draper Extension Charts: A catalogue of accurate positions, proper motions, magnitudes and spectral types of 86933 stars. Astron. and Astrophys. Suppl. Ser., 1995, V. 110, P. 367). 88883 , 3500 ( 1783 ) . CDS. , HDEC. .. , .. , .. () , () . , VizieR, . , , , . , . Aladin, VOPlot, VOSpec VizieR Simbad.

26


.. , , 60% 90% . , . ( , ), ( , , ), ( ), ( ) . , ( ). . , , -, . BDB (Binary star DataBase, http://bdb.inasan.ru) . BSDB - ILB (Identification List of Binaries). .. , .. , (, , ) 1948 . 1801 ( ) .

27


1911 . . 1948 . 7 (), (). () . . , , . .. , .. , , , (R=/~40000) (R>80000) . ( , , ..), . , ( ), , . .. : . , , 2002 . 12 . , , , . ( ), 511 , , ,

28


. . , . -- . , , , . , - , , , , . .. , () 10 310 . , . . , , , , , . . MAST, . HST, GALEX, FUSE, Copernicus, EUVE, IUE . .

29



.. , -- HI. . HI HII. 81, . , .. . 10 104 . , . ~200 . 100 , , ~3 . . .. 1, .. 2,3, .. 1 , -- 2 , 3 . . . .. . ..
1

, . ( , ), () H (I). I I .

30


.. , .. , .. , -- , ( 100 . ) . . CIV, NV, OVI . .. . . . .. . .. HII , ( UBVRI) ( H) 102 (NGC 628, NGC 783, NGC 2336, NGC 6217, NGC 6946, NGC 7331 NGC 7678). HII, , , ( ) . , , Agas, , Astars (). HII . , HII, : 1) B / V 25%; 2) EW(H)>440 . 51 SSP-; Astars = Agas , - , . , , , A(V)=1.010.86. t =5.42.4 . . 105106 , 1.0104 1.3107 . , NGC 628 NGC 6946 (, , ) .

31


.. . .. , , , 1,2, VLT NTT ( ) , (), . , -. . .. , . , S2 ( S02). , , . , R , , R. . , . 2. , , , . , VLT 2003 2009 . , . . .. . . . .. . .. NGC 6946 NGC 6946 , (wooll y) , . . 1.4 1.8; . NGC 6946 , , . , . ,

32


2 . , ( 12). , - , ; , ( ) . 700 ; 132, . NGC 6946 . .. 1, .. 2, .. 1,2 . .. , 2 . ,
1

, , , . . . , k k J , . . . , . , . .. , . - , .





33


. , (.. , . , 2012, . 55, N 6, . 81), (V.M. Koryukin, PoS (Baldin ISHEPP XXII) 024) . , , , , 50 . ( ), , , ( ) ( ). , , ( ). , , , , . , , , . , , . , () , . 1 , - . , , , 10 . , , . ( , ), , .

34


A.M. Mickaelian, G.M. Paronyan, H.V. Abrahamyan Armenian Academy of Sciences Large homogeneous sample of X-ray selected AGNe and its study The joint catalogue of Active Galactic Nuclei (AGNe) selected from optical identifications of X-ray sources was created as a combination of two sources: HamburgROSAT Catalogue (HRC) and ByurakanHamburg ROSAT Catalogue (BHRC). Both are based on optical identifications of X-ra y sources from ROSAT catalogues using low-dispersion spectra of Hamburg Quasar Survey (HQS). HRC used ROSAT Bright Source Catalogue (BSC) and BHRC used brighter sources of ROSAT Faint Source Catalogue (FSC), thus extending the sample to count rates (CR) of photons 0.04 ct/s in the area with galactic latitudes |b| 20 and declinations 0 (the area of HQS). However, HRC and BHRC contain a number of misidentifications and using the recent optical and multiwavelength (MW) catalogues, we have revised both samples excluding false AGNe and adding new genuine AGNe. Thus a new large homogeneous complete sample of 4253 X-ray selected AGNe was created. All these sources are either genuine AGNe or have been classified as candidate AGNe based on HQS low-dispersion spectra. 3352 of them are listed in the Catalogue of QSOs and Active Galaxies (Vron-Cetti & Vron 2010; 13th version) and 387 are also in the Multifrequency Catalogue of Blazars (RomaBZCAT) by Massaro et al. (2012). 901 candidate AGNe are subject for further study. We classified these objects using their SDSS DR10 spectra available for 217 of them. The following activity t ypes were revealed: 95 AGNe (including blazars, the most interesting objects in the sample), 71 absorption -line galaxies, 42 stars, and 9 were classified as "Unknown". A special emphasis is made on narrow-line Sy1.0-Sy1.5 galaxies and QSOs, as many of them have soft X-ray, strong FeII lines, and relativel y narrow lines coming from BLR ("narrow broad lines"); we have classified 45 new AGNe as such objects. As a result, the sample of genuine AGNe was enlarged to 3447 objects. We have retrieved MW data (gamma-, X-ray, UV, optical, IR, and radio) from recent catalogues and carried out statistical investigations for the whole AGN sample. An attempt to find connections between fluxes in different bands for different types of sources, and identify their characteristics thus confirming candidate AGNe have been carried out. We have analyzed X-ra y properties of these sources t o find a boundary bet ween normal galaxies and X-ray AGNe. The sample is a relevant source for identification of new blazars.
1

.. 1, .. 1, . 2 . . , 2 ,

1960- . . . , .. -

35


, , a, b c. . 1979 . .. 143 . , . 1989 . .. . 300 . . 1995 . , , , - . , , S, , . , 50% , . . , . 9 , - . .. 1, .. 2, .. 1 . .. . . . .. . ..
1

2

, . , -. , , .

36


no-z , , , . , 2 , . , in situ , . , , . .. 1,2, . 3, . 3 . , 2 . . . .. . .. 3 , :
1

6- . ( ). , , .. , . , 50200 . . . V.L. Oknyansky1, C.M. Gaskell2,3 Sternberg Astronomical Institute, Lomonosov Moscow University 2 Centro de Astrofsica de Valparaso, Chile 3 University of California, Santa Cruz, USA The relative wavelength independence of IR lags in AGNs: implications for the geometry of the dusty torus
1

As seen from the central source, the torus of AGNe has a puzzlingly high covering factor. This implies a surprisingly small torus half opening angle and a large scale height. The cause of the large vertical scale height is not understood. In cartoons of AGNe the torus is commonly depicted as a doughnut with a radial thickness comparable to its vertical thickness. This

37


would imply that whatever maintains the vertical height operates over a considerable radial distance. If the torus consists of clouds of dust, each with a relatively unobscured view of the higher energy photons from nearer the center of the AGN, the temperature of each dust cloud will fall off as roughly the inverse square root of the radius. Since the dust is heated by the central radiation, in such a model the lag would increase with the wa velength to a power of 2 t o 2.8. We show that, contrary to this simple prediction, for a significant fraction of AGNe the lags of the J, H, K, and L bands with respect to the optical show at best onl y a small difference. This means that rather than there being an extended radial temperature gradient, the hot dust reprocessing the central radiation is effectivel y in a relatively thin shell. Long-term monitoring of NGC 4151 suggests that the geometry might change as the radius of the region with emission from hot dust changes as the mean continuum level changes. We note that a number of the AGNe showing similar J, H, K, and L lags are also Seyferts that have changed between type 1 and type 2. It is not clear whether this is related or is merely a consequence of these objects being well studied for a long time. .. , (1913 1987) 1944 , 1+3 , . - . , 1+1+1+1 - , ( ) , , .

38


.. 1, .. 2, . 2 . . . .. . .. 2 Universit Libre de Bruxelles
1

. . 1017 : . . (RM) , . , 20- . . 4000 RM. , , , , RM . 1 . , , . M. Ryabov1, A. Donskykh2, A. Sukharev1, M. Aller3 Odessa Observatory "URAN-4" of the Radio Astronomical Institute, National Academ y of Sciences, Ukraine 2 I.I. Mechnikov Odessa National University, Ukraine 3 Radio Observatory of Michigan University, Ann Arbor, USA Using Methods of Wavelet Analysis and Singular Spectrum Analysis in the Study of Radio Sources 3C 345, 3C 120, 3C 273 and BLLac
1

We investigated data of extragalactic-source flux density monitoring, performed with the 26-meter radio telescope of the University of Michigan at frequencies of 14.5, 8 and 4.8 GHz. To study flux density of extragalactic radio sources 3C120, 3C273, 3C345, BL Lac, the wavelet analysis and singular spectrum analysis were used. Based on Fourier filtering, we identified OC (short-period) and trend components of flux variables, which were analyzed separately using the method of wa velet analysis. Each of these components is associated with certain physical processes in the "core-accretion disk-jet" system. We constructed timefrequency wa velet spectra showing changes of frequency with time. The

39


trend components of the studied objects' main periods (in years) are ~ 716 yr (BL Lac), 511 yr (3C 273), 412 yr (3C 120), 516 yr (3C 345). The periods of () components are ~ 0.64 yr (BL Lac), 15 yr (3C 273), 0.74 yr (3C 120), 14 yr (3C 345). All of them appear in the time structural changes of the jet. These data were compared with VLBI radio maps, which were obtained by the Moja ve program. Studying radio maps allowed us to investigate features of components moving relative to the VLBI core. The data of observations were also investigated using singular spectrum analysis (Caterpillar-SSA) (N. Golyandina, V. Nekrutkin and A. Zhigljavsky. Analysis of Time Series Structure: SSA and related techniques. 2001, Chapman and Hall/CRC. ISBN 1-58488-194-1). The basis functions used in this method are based on the raw data themselves, in variance with the Fourier and wavelet methods. "Caterpillar-SSA" is based on transformation of the original series in a matrix, followed by its singular value decomposition, as a result of which, the original series is decomposed into additive components. The advantage of "Caterpillar-SSA" is the ability to control the process of filtering stages of decomposition and signal recover y. Depending on object ives of the study, "Caterpillar-SSA" allows you to select the most informative harmonics or to determine their number. . 1, . 1, . 2 -4 2 , 3 273 (, , , , ) 1965 2011 .
1

3 273 (19652011 .) , UMRAO (14.5, 8, 4.8 ), ISDC (http://isdc.unige.ch/3c273). ( 70 19652007 .) 3 273 . . , - () , . - , LombScargle . , , 11, 8, 5 ; , ~

40


3 0.3 . , () . , , . - 3 273. (Mojave VLBI ) . VLBI- . - , -, , . ( UMRAO) ( . , ) 3 273. (20112015) ( SSA) (20002011). . .. , .. , .. , -- -L* L
.. , .. , .. , .. , .. . . . .. . .. NGC 7469 19902014 . NGC 7469 (1990

41


2014.) UBVRI . .. . . . .. . .. : 1917 . , . 19981999 . . , , , . , , , . , . ( 2000 .), 13 . 15 ( HST ) . , ; . .. , .. . . . .. . .. , , . - , , . , , . . . , ,

42


, . , , , . , - , SDSS S4G. , , . ..1, ..2 . . . .. . ..
1

2

, / , , . .. . . . .. . .. 1933 . , ( Coma), , , . . , , , , ( " ") ( ,1987). Supernova Cosmology HighZ Supernova , " ", (, 2013). Coma . , ,

43


. , . Coma , .

,
.. , .. - , , , , , , . , , , . : , , , - . , - . , , - , , ( ) . , , , - . ,

44


. : , , , .. , . , . 3D-, . 3D- . . ( 15-02-02145). .. , .. - , 3D- 3D- , (), , , . ( 3D2D) . ( ) . , , , 3D- 2D-, . , LBI, , , , VLTI NPOI. 3D- . 3D , , . , ,

45


(). 3D- ( 3D1D) (.. .. , 2014). 3D- 2D- . . (), 3D2D . . 3D2D, , , HPBW ~55o. 3D1D. , 3D1D, 55o 90o , 90o . , 20o. 0o . . ( 15-02-02145). .. 1, .. 1, .. 1,2, .. 1,2, .. 3 1 () 2 - 3 Tau IC 348 IC 348 V695 Per V716 Per, AA Tau, . , , AA Tau, , . ,

46


. , . .. 1, .. 1, . 2 , 2 , , Spitzer/EGOs
1

(clumps), (cores). , , , , , , . , . , (YSO Young Stellar Object), . , . , , . , 2 3 (). EGO (Extended Green Objects), Spitzer, ( , PAH) 4.5 . IRAC/Spitzer: 3.6, 4.5, 5.8, 8.0 . ( EGOs), VLA 18 2013 ., VLA (Cyganowski et al. 2009, ApJ 702, 1615) , YSO , . , , .

47


.. , .. . . . .. . .. ( ) , . , , . , . . . . , ( ) . . .. . . . .. . .. , , , , . , T, T. T=(2800...3000) , , (S Car, T Col, RR Sco, R Aql, R Car, o Cet, RR Sgr, S Sco, W Vel, R Leo). , . , , . , . , , .

48


, , . , . 13-02-00136 15-03-03302. .. , .. , .. () 1.5- -150. - , A, B, C, D . , , , . 2006 2015 . 1.5- . . : A 65.43 , B 6.47 , C 10.9 , D 20.26 . . , HeI, HeII , , . . .. 1, .. 1, .. 2, .. 3, .. 1, .. 4, .. 4, .. 5, .. 6, . . 1, . . 3 1 . . . .. . .. 2 - . , 3 , 4 . , 5 . . , 6 , : FL Lyr V0873 Per FL Lyr, .

49


, 7 . . 20132014 V0873 Per, ( ) 0.1 300 . .. V833 V833 Tau (dK2Ve), , 78.25, 18.81, 6.44, 2.52 . . , , . . . . . .. , .. , .. , .. , -- () . (), , . , . Et ~ t2.3 , . , f > ~0.1

50


, . , , , () . .. , . , -- 21 HI 21 . , () () . , , . 0.30.6 , . , . . .. 1, .. 1,2 () 2 -
1

, . - ( -). , , GADGET 2. . , . . UX Ori.

51


.. 1, .. 1, .. 2, .. 2 1 () 2 NSVS 14256825 () NSVS 14256825 HW Vir sdB- . NSVS 14256825, 2012 . -1000 . NSVS 14256825 B, V, R . , . 2MASS J20194773+0434017 RR Lyr m = 0.18m 0.35m 67 . NSVS 14256825, 2012 . 2013 . . 2 40505800 . 7 , sdB-. , , . NSVS 14256825. . sdB- HI, HeI, HeII - . , , , . NSVS 14256825 . , M1 = 0.47 M, , M2 = 0.10 M, A = 0.798 R.

52


NSVS 14256825,