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IX Russian-Finnish Symposium on Radio Astronomy

"Multi-Wavelength Investigations of Solar and Stellar Activity and Active Galactic Nuclei"

Program and abstracts

15­20 October 2006, Nizhnij Arkhyz


RUSSIAN ACADEMY OF SCIENCES

IX Russian-Finnish Symposium on Radio Astronomy

"Multi-Wavelength Investigations of Solar and Stellar Activity and Active Galactic Nuclei"
15­20 October 2006

Nizhnij Arkhyz 2006


Scientific Organizing Committee Marat Mingaliev, chair, Yury Parijskij, Aleksander Stepanov, Merja Tornikoski, Esko Valtao ja

Lo cal Organizing Committee Sergei Truskhin (chair), Vladimir Bogod, Ekaterina Filippova, Larisa Martynova, Julia Sotnikova, Larisa Opeikina, Abdulah Uzdenov

The organizers of the Symp osium Central Astronomical Observatory at Pulkovo Pulkovo chaussee 65/1, Saint-Petersburg, 196140 Special Astrophysical Observatory RAS, Nizhnij Arkhyz, Karachaevo-Cherkassia, 369167

Sp onsoring Institutions Russian Academy of Sciences Special Astrophysical Observatory of RAS Central Astronomical Observatory at Pulkovo Russian Foundation of Basic Research (RFBR)


Program of the IX Russian-Finnish Symp osium on Radio Astronomy, Nizhnij Arkhyz, 15-20 Octob er 2006

October 15, Sunday
09:00-24:00 Day of arrival 19:00-20:00 DINNER 18:00-21:00 Registration of participants

October 16, Monday
08:00-09:00 BREAKFAST 08:30-09:30 Registration of participants 09:30-09:45 Opening ceremony Session 1. AGNs Chair: Marat Mingaliev 09:45-10:15 Valtao ja E. The problem of high-energy emission from AGN 10:15-10:45 Tornikoski M. Metshovi AGN pro jects contributing to the Planck foreground science 10:45-11:05 COFFEE BREAK 11:05-11:35 Hovatta T. Long-term radio time scales of Active Galactic Nuclei 11:35-12:05 Kovalev Yu. Nature of Active Galactic Nuclei from Massive Instantaneous Radio Spectra Study with RATAN-600 in 1997-2006 supplemented by VLBA experiments 12:05-12:35 Gorshkov A. Extragalactic source variability studies of complete samples with RATAN-600 12:35-13:00 Volvach A. The combined radio and optical investigations of the intraday variability of active galactic nuclei 13-00-14:30 LUNCH

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Session 2. Extragalactic Sources Chair: Esko Valtao ja 14:30-15:00 15:00-15:30 15:30-15:50 15:50-16:10 16:10-16:40 16:40-17:00 17:00-17:25 17:25-17:50 17:50-18:15 Lahteenmki A. Planck ­ unlocking the secrets of the Universe Parijskij Yu. Very deep SKY surveys with RATAN-600 Bursov N. RZF Survey Khabibullina M. Mean spectral index of the faintest NVSS ob jects from RZF data Larionov M. Radio spectra properties of a complete sample of sources near the North Celestial Pole COFFEE BREAK Torniainen I. Radio spectra of GPS galaxies Temirova A. New ob jects from the "Cold" survey Niepp ola E. Spectral energy distributions and 37 GHz monitoring of BL Lacertae ob jects

19:00-20:00 DINNER

October 17, Tuesday
08:00-09:00 BREAKFAST Session 3. Extragalactic Sources Chair: Merja Tornikoski 09:00-09:25 Shap ovalova A. A link between variable optical continuum and radio emission of a compact jet in the radio-loud Seyfert galaxy 3C390.3 09:25-09:50 Burenkov A. Spectral monitoring of NGC 5548 in 1996-2004 09:50-10:15 Trushkin S. New WMAP catalog sources or how many bright sources are on the sky 10:15-10:40 Doroshenko V. Continuum and broad emission line variability of Seyfert galaxy

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10:40-11:00 COFFEE BREAK 11:05-11:30 Efimov Yu. Study of a magnetic field structure in blazar jets from optical photopolarimetric data 11:30-11:55 Verkho danov O. Open WEB-resources of SAO RAS for extragalactic research Session 4. Sun Chair: Aleksander Stepanov 12:00-12:30 Riehokainen A. Multi-frequency observations of the polar radio structures 12:30-13:00 Bogo d V. RATAN-600 microwave spectral solar observations ­ today and future 13-00-14:30 LUNCH 14:30-14:55 Borovik V. Multiwave RATAN-600 observations of post-eruptive processes on the Sun 14:55-15:20 Golub china O. Results of the prominence observations at microwaves during the maximal phase of the total solar eclipse of March 2006 15:20-15:45 Korzhavin A. RATAN-600 observations of microwave structure of the quiet Sun 15:45-16:15 Gelfreikh G. Peculiarities of QPOs of microwave emission of the flaring solar active regions 16:15-16:40 Korzhavin A. Estimations of effective height, size and brightness temperature of the solar cyclotron sources 16:40-17:00 COFFEE BREAK 17:00-17:25 Mo din E. On the theory of resonant transitive radiation of decimetric radiation of flares 17:25-17:50 Kotelnikov V. About a double inversion sign of polarization microwave emission flare-productive active region 19:00-20:00 DINNER

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October 18, Wednesday
08:00-09:00 BREAKFAST Session 5. Sun Chair: Georgy Gelfreikh 09:00-09:25 Tlatov A. Reversal background magnetic field in the solar polarized radio emission at 17GHz 09:25-09:50 Tlatov A. Oscillation of the polarized radio emission "The Sun as a star" 10:00-13:00 Visit to RATAN-600 13-00-14:30 LUNCH Session 6. Galactic Sources Chair: Yury Parijskij 14:30-15:00 Lehto H. Polarization observations of mCVs 15:00-15:25 Trushkin S. Recent data of the multi-frequency monitoring of microquasars 15:25-15:50 Stepanov A. Radio pulsations from the AD Leo flare and electric current diagnostics 15:50-16:15 Fabrika S. The supercritical accretion disk in SS433 and ultraluminous X-ray sources 16:15-16:35 Zinchenko I. Physical and chemical structure of high mass star forming regions 16:35-16:55 COFFEE BREAK 16:55-17:15 Vdovin V. Developments of low-noise mm receivers for radio astronomy 17:15-17:55 1. Gosachinskij I. On the sky spectroscopy with RATAN-600 2. Gosachinskij I. The investigation of interaction between supernova remnants and the interstellar medium 19:00-20:00 DINNER

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October 19, Thursday
08:00-09:00 BREAKFAST 09:00-12:00 Visit to the Optical telescopes site 12:00-18:00 Excursion to the Mountains area, Barbecue

October 20, Friday
08:00-09:00 BREAKFAST 09:00-24:00 Day of Departure

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ABSTRACTS
(alphabetically ordered)

8


PECULIARITIES OF QPOS OF MICROWAVE EMISSION OF THE FLARING SOLAR ACTIVE REGIONS
V.E. Abramov-Maximov, G.B. Gelfreikh Central Astronomical Observatory at Pulkovo, Saint-Petersburg, Russia gbg@saoran.spb.su Quasi-p erio dic oscillations of solar coronal structures are effectively registered in particular at microwave waves. The physical nature of p erio dical pro cesses in the corona is clearly connected with plasma structures of the solar atmosphere. On the other hand, the mo dern conception is that pro cesses leading to eruption of energy in solar flares are results of energy accumulation in the corona or chromosphere pro duced by some reconstruction of plasma structures. In spite of developments of the mo dern observations predominantly using cosmic techniques, we are still far from a satisfactory observational understanding of the ab ove processes. The QPOs of solar active regions were found decades ago and their connections with the flares were detected. Nevertheless, the physical nature and p ossible forecasting applications are still far from a reasonable level of knowledge. New development of microwave instruments with a high spatial resolution and regular observations (NoRH, RATAN­600, SSRT at Badary) op ened a new era in such studies. Oscillations with p erio ds from few minutes to hours were investigated and their time variations were sp ecially analysed. So, we may conclude that investigations of these parameters for ARs with different levels of flare activity, time variations including, may lead to a b etter understanding of the physics of the problem. Some preliminary results of such studies are presented in this rep ort, based on an analysis of the Nob eyama radio maps of the Sun with the 10 sec averaging and covering p erio ds of hours of observations (dates 11 Sep 2001, 07 Oct 2002, including), and comparing these with sp ectral parameters of the regions obtained with RATAN­600. This study was partially supp orted by the Program of the Presidium or the Russian Academy of Sciences.

A LINK BETWEEN VARIABLE OPTICAL CONTINUUM AND RADIO EMISSION OF A COMPACT JET IN THE RADIO-LOUD SEYFERT GALAXY 3C390.3
T.G. Arshakian1 , A.P. Lobanov1 , V.H. Chavushyan2 , A.I. Shap ovalova3 , J.A. Zensus 1 , N.G. Bo chkarev4 , A.N. Burenkov3
2

Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany, Instituto Nacional de Astrof´ isica, Optica y Electr´ onica, Apartado Postal 51. C.P. 72000. Puebla, Pue., M´ exico, 3 Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia, 4 Sternb erg Astronomical Institute, University of Moscow, Universitetskij Prosp ect 13, Moscow 119899, Russia tigar@mpifr-b onn.mpg.de

1

We present an observational evidence for a relation b etween variability of radio emission of the compact jet, nucleus optical continuum emission and ejections of new jet comp onents 9


in the radio galaxy 3C390.3. We combine results from the monitoring of 3C390.3 in the optical region (Shap ovalova et al. 2001; Sergeev at al. 2002) with ten very long baseline interferometry (VLBI) observations of its radio emission at 15 GHz carried out from 1992 to 2002 using the VLBA (Kellermann et al. 2004). For ten VLBA images, we identified five moving comp onents (C4-C8) and two stationary comp onents (D,S1). Prop er motions of the moving comp onents corresp ond to apparent velo cities from 0.8c to 1.5c. No significant correlation exists for the moving features b etween optical continuum and radio emission. However the variations of optical continuum are correlated with radio emission from a stationary feature (S1) in the jet. The optical emission follows radio flares with the mean delays t(S1-opt)0.4 year. Most probably the optical continuum is pro duced near the lo cation of radio emission of the S1 stationary comp onent. The lo calization of the source of optical continuum with the innermost part of the jet near S1 implies that the broad line emission originates in a conical region (dimension 100 light days) at a distance of 0.4 p c from the central engine. For the comp onents C4-C7, the ep o chs t(S1) of separation from the stationary feature S1 are coincident, within the errors, with maxima in optical continuum. This suggests that radio ejection events of the jet comp onents are coupled with the long-term variability of optical continuum. We supp ose that the broad emission lines having a double-p eaked structure originate in two kinematically and physically different regions of 3C390.3: 1. BLR1 ­ the traditional BLR (Accretion Disk (AD) and the surrounding gas). It is at the distance 30 light days from the nuclei (Shap ovalova et al. 2001). 2. BLR2 ­ in a subrelativistic outflow surrounding the jet in the cone within 100 light days at a distance of 0.4 p c from the central engine. During the nucleus maximal brightness p erio ds most of the continuum variable radiation is emitted from the jet and ionizes the surrounding gas, creating a BLR2 that mainly determines the broad line emission. During the brightness minima the jet contribution to the ionizing continuum is decreasing and the main broad line emission comes from the "classical" BLR1 (AD), ionized by nuclei continuum related with the acctretion at BH. Such a scenario explains two maxima ( 30d and 100d) found in the cross-correlation function describing the time-lag of broad line variations relatively to continuum on the base of the results of 3C390.3 optical monitoring in 1996-2000 (Shap ovalova et al. 2001). Acknow ledgements. This work was supp orted by grants: CONACYT 39560F (Mexico), INTAS (N96-0328) and RFBR (00-02-16272; 03-02-17123 and 06-02-16843, Russia). References Shap ovalova et al.: A&A, 2001, 376, 775. Sergeev et al.: ApJ, 2002, 576, 660; Kellermann et al.: ApJ, 2004, 609, 539.

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RATAN-600 MICROWAVE SPECTRAL OBSERVATIONS OF THE SUN ­ TODAY AND FUTURE
V.M. Bogo d Sp ecial Astrophysical Observatory of RAS, Saint-Petersburg, Russia vb og@gao.sb.ru Problems of solar radio emission study with the help of the RATAN-600 radio telescop e are considered. It is shown that the main scientific results were attained due to the continual improvement of instrumental parameters. In the case of solar investigations many new features of active solar plasma were detected, in particular: · A small-scale radio emission structure of the Quiet Sun (a so-called "radio granulation"); · Neutral line asso ciated sources in solar active regions; · Non-thermal radio emission ab ove sunsp ots groups, so named "the decimetre halo"; · Cyclotron lines in the active regions; · Multiple p olarization inversions in flare-pro ductive active regions; · Relations b etween the double p olarization inversions effect at microwaves and Noise Storms activity at meter waves; · The short-wave increasing of p olarization flux b efore big flares; · The "darkening" radio emission effect in flare-pro ductive active regions; · An evolution of p olarization flux sp ectrum b efore big flares; · Discovery of micro-bursts and their relation with Noise Storms; · Detection of a frequency b oundary b etween S- and B-comp onents and others. Examples of the features listed ab ove are describ ed. A p ossible future development of solar investigations with RATAN-600 is discussed.

MULTIWAVE RATAN-600 OBSERVATIONS OF POST-ERUPTIVE PROCESSES ON THE SUN
V.N. Borovik1 , V.V. Grechnev2 , V.E. Abramov-Maksimov1 , I.Y. Grigorieva1 , V.M. Bogo d3 , V.I. Garaimov3 , T.I. Kaltman3 , A.N. Korzhavin3
1

3

Central Astronomical Observatory of RAS, Saint-Petrsburg, Pulkovsko je shosse, 65, 2 Institute of Solar Terrestrial Physics, Irkutsk, Sp ecial Astrophysical Observatory of RAS, Saint-Petrsburg, Pulkovsko e schosse, 65, Russia b orovik@saoran.spb.su 11


During two last decades, authors of some studies of p ost-eruptive arcades rep eatedly came to the following unexp ected conclusions. Microwave emission of arcades was excessively p olarized, presumably due to contribution of non-thermal electrons. Their lifetime was much longer than the estimated co oling times, presumably due to the p ost-eruptive energy release. Finally, the plasma pressure exceeded the magnetic pressure ( 1) in their hot top parts. CORONAS-F/SPIRIT observations in the high-temp erature (10 MK) line MgXI I and multi-wave RATAN-600 observations along with data from other sp ectral domains provided imp ortant information to verify these conclusions and assumptions. All ab ove facts were confirmed in analyses of this data set. They were explained in terms of the standard flare mo del ("CSHKP") elab orated by Yokoyama & Shibata (1998) to qualitative account for the chromospheric evap oration, but applied to late p ost-eruptive phase. In this case, high conditions indicate magnetic reconnection pro cesses resp onsible for the prolonged heating and particle acceleration. This approach allows to reconcile the listed facts with known estimates of parameters of the coronal plasma in p ost-eruptive arcades, and to remove seeming contradictions with habitual conceptions. We consider long-lived p ost-eruptive arcades observed on 22 Octob er 2001, 2 Novemb er 1992, and 28­ 30 Decemb er 2001 and demonstrate that these conclusions are valid, b ecause high-density hot regions in their top parts (thus, high regions) existed for a long time, and their radio emission contained non-thermal comp onent, which is indicative of the presence of accelerated particles. References Yokoyama T., Shibata K.: 1998, ApJ, 494, L113.

SPECTRAL MONITORING OF NGC 5548 IN 1996 ­ 2004
A.N. Burenkov1 , A.I. Shap ovalova1 , N.G. Bo chkarev2 , V.H. Chavushyan3 , S. Collin4 , V.T. Doroshenko2 , L. Pop ovi´5 , N. Borisov1 , L. Carrasco3 , D. Ili´6 , J.R. Valdes3 , V.V. c c 1 2 Vlasuyk , V.E. Zhdanova Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia Sternb erg Astronomical Institute, University of Moscow, Universitetskij Prosp ect 13, Moscow 119899, Russia 3 Instituto Nacional de Astrof´ isica, Optica y Electr´ onica, Apartado Postal 51. C.P. 72000. Puebla, Pue., M´ exico 4 LUTH, Observatoire de Paris, Section de Meudon, Place Janssen, 92195, Meudon, France 5 Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia 6 Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia
2 1

We present results of a sp ectral monitoring program of the Seyfert galaxy NGC 5548 with the 6m and 1m telescop es of SAO (Russia) and with the 2.1m telescop e of Guillermo Haro Observatory at Cananea, M´ exico. Sp ectra were obtained with long-slit sp ectrograph, A A covering the sp ectral range (4000­7500) ° with a (4.5­15) ° resolution. We found that: ­ Both the flux in the lines and continuum gradually decreased, reaching minimum values during May-June 2002. In the minimum state, the wings of H and H b ecame 12


extremely weak, corresp onding to a Sy1.8 typ e, not to a Sy1, as observed previously when the nucleus was brighter. ­ When the line profiles were decomp osed into variable and constant comp onents, the variable broad comp onent is well correlated with the continuum variation. It consists of a double p eaked structure with radial velo cities of ±1000 km/s relative to the narrow comp onent. A constant comp onent, whose presence is indep endent of the continuum flux variations, shows only narrow emission lines. The mean, rms, and the averaged over years, observed and difference line profiles of H and H reveal the same double p eaked structure at the same velo cities. The relative intensity of these p eaks changes with time. During 1996, the red p eak was the brightest, while in 1998­2002, the blue p eak b ecame the brighter one. Their radial velo cities vary in the range 500­1200 km/s. ­ In 2000­2002 a distinct third p eak app eared in the red wing of H and H line profiles. The radial velo city of this feature decreased b etween 2000 and 2002: by the observed profiles, from +(2500­2600) km/s to +2000 km/s and it is clearly seen on the difference profiles. ­ The fluxes of various parts of the line profiles are well correlated with each other and also with the continuum flux. The blue and red parts of the line profiles at the same radial velo cities vary in an almost identical manner. ­ Our results favor the formation of the broad Balmer lines in a turbulent accretion disc with large and moving "optically thick" inhomogeneities, capable of repro cessing the central source continuum. We made an attempt to investigate the variability of physical parameters in the BLR of NGC 5548 using the Boltzmann plot metho d given by Pop ovi´ (2003). We applied the c metho d on the broad Balmer lines, and found that variability seen in lines is also present in the electron temp erature (T). We found that the average T for the considered p erio d was 10000K, and that it varies from 6000K (in 2002) till 15000K (in 1998). This variation correlates with the optical continuum flux (r = 0.85) and may indicate existence of an accretion disk in the BLR of NGC 5548. We found that Partial Lo cal Thermo dynamical Equilibrium approximation is valid for at least one part of the BLR of NGC 5548. The detailed discussion of these results is done in our pap ers (Shap ovalova at al. 2004; Pop ovi´ et al. 2005). c Acknow ledgements. This work was supp orted by grants from CONACYT 39560-F (Mexico), RFBR 06-02-16843 (Russia) and the Ministry of Science and Environment Protection of Serbia. References Pop ovi´ L. C.: ApJ, 2003, 599, 140. c Pop ovi´ L. C. et al.: Astro-ph/0511676, 2005 (in press). c Shap ovalova A. I. et al.: 2004, A&A, 422, 925.

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MEAN SPECTRAL INDEX OF THE FAINTEST NVSS OBJECTS FROM RZF DATA
N.N. Bursov1 , M.L. Khabibullina
1 2

Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia 2 Kazan State University, Kazan, Russia nnb@sao.ru

A sp ectral index of a 'mean' radio source from NVSS catalog was estimated by summarizing of the drift scans of the RZF survey. In the area of RZF servey (RA2000:0-24; DEC2000:40.5-42.5) there are 28000 NVSS sources with a total flux density from 2 to 400 mJy at 1.4 GHz. These NVSS sources are considered as p oint ones. We have divided this flux range to 12 bins: 2­4, 4­6, 6­8, 8­10, 10­13, 13­17, 17­24, 24­35, 35­60, 60­110, 110­220, 220­400 mJy. We summarized 7500 intercepts of one-hour records at 4 GHz of RZF survey by a numb er of NVSS sources in each bin. Indeed we 'detected' a 'avarage' source in each bin of NVSS sample and obtained 'average' flux densities at 4 GHz for each flux bin: 0.9, 1.7, 2.6, 3.7, 4.3, 6.9, 7.6, 10.5, 17.2, 27.5, 60.0, 177 mJy resp ectively. The data give a rough estimate of the 'average' sp ectral indices (1.4­4 GHz) for each NVSS sources bin. We found that an 'average' sp ectral index is a function of NVSS flux densities. A comparison with exp ected mean sp ectral indices and the reliability of such a estimate are discussed. However, in the bin of 3­8 mJy the sp ectra have sp ectral index equal to ­0.8, i.e. the relative fraction of the steep sp ectrum sources decreased probably b ecause a numb er of FRI I radio sources decreases just in this flux range (Jarvis & Rawlings, 2004). References Jarvis M.J., Rawlings S.: New Astron.Rev., 2004, 48, 1173.

RZF SURVEY
N.N. Bursov, E.K. Ma jorova, T.A. Semenova, M.G. Mingaliev, A.B. Berlin, N.A. Nizhel'skij, P.G. Tsibulev Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia nnb@sao.ru The completed second version of the RZF catalog at 7.6 cm wavelength is presented. A reality of faint and new ob jects of the catalog is evaluated. Radio sp ectra of NVSS ob jects are plotted and a new distribution of sp ectral indices is found. New information ab out a contribution of background of the faint radio sources with inverted sp ectrum and ab out a "sub-mJy" p opulation of the background radio sources in the cm range is found. It is shown that an average sp ectral index of radio sources at the mJy level is flatter, a p ercentage of classical radio galaxies FRI I typ e drops, but the p opulation of ob jects with inversion sp ectra is negligible. Candidates of the most distant radio galaxies (z > 4 - 5) catalog are selected by colors from the SDSS counterparts. A decrease of white noise of radiometers is achieved by a large integration time at pixel that is b elow the level of WMAP exp eriment. 14


The synchrotron comp onent of the foreground Galaxy emission with high accuracy at earlier unstudied angular scales was removed.

CONTINUUM AND BROAD EMISSION LINE VARIABILITY OF SEYFERT GALAXIES
V.T. Doroshenko1,2 , S.G. Sergeev2 , V.I. Pronik
1 2

Crimean Lab. of the Sternberg Astronomical Institute, Moscow University, Russia 2 Scientific-Research Institute, Crimean Astrophysical Observatory, Ukraine; p/o Nauchny, 98409, Crimea, Ukraine vdorosh@sai.crimea.ua

We fo cused on the observed prop erties of some Seyfert galaxies without detailed discussion of underlying physical mechanisms. Our purp ose was to show a diversity of observed effects due to variability in sp ectra of six galaxies (NGC 4151, NGC 5548, Mrk 6, Ark 120, 3C 390.3, Arp 120B), optical sp ectral and photometric monitoring of which was carried out in the Crimean Astrophysical Observatory and Crimean Lab oratory of the Sternb erg Astronomical Institute over many years. This monitoring shows that · All light curves demonstrate a variability on different time scales from days to years. · Amplitude of variations increases with increasing of the time interval of observations. · The flux in emission lines changes in resp onse to the flux variation of the ionizing continuum source with some time delay. Thus, the emission lines "echo" or "reverb erate" the continuum changes. This time delay is due to light-travel time effects within the BLR. · The time delay of the broad H emission line flux relative to optical continuum in the vicinity of the H line lies in an interval from 9.2 days for Arp 102B to 80 days for 3C 390.3. This means that a region of the most effective emission in the H and H lines is fairly small, and it is lo cated at a distance of ab out 9 ­ 80 light days from the continuum source. · We found one very strange and inexplicable case (3C 390.3) when a lag calculated from the broad H line significantly exceeds that of the H . In all other cases, the H and H lines have a similar lag. · We revealed a slightly different lag for two time intervals for NGC 5548: 26 days in 1972­1988 and 18 days in 1989­2001. · Analysis of the lag as a function of the radial velo city do es not show any reliable evidence of the pure radial dominated outflow, p ossibly, except for NGC 4151. A weak evidence of radial inflow was found in Mrk 6 and Ark 120. Predominantly, we found that there is no pure radial inflow or outflow in the BLR of the considered galaxies. In all cases, the kinematics mainly lo oks like a chaotic or rotational motion. · We also found that the lag for the central part of the broad H emission line is slightly larger than for wings (NGC 5548). 15


· The lag slightly increases with increasing of the continuum flux (Ark 120). This fact is consistent with a virial relation b etween the velo city field and the distance of the emitting region: the velo city field diminishes with increasing distance from the central continuum source. This implies that the velo city field is dominated by a central massive ob ject. · Not only the flux of broad emission line but also the line profiles appreciably changed with time. The emission-line profile changes usually o ccur on a time scale that is much longer than the light-travel time scale. · In all cases, the excess b etween the normalized Balmer profiles and the mean normalized profile shows a very complicated b ehavior b oth over time and wavelength, and it can hardly b e related to the exp ected reverb eration signal from the simple disk mo del. The profile evolution for some galaxies (NGC 4151, Mrk 6, 3C 390.3) can b e repro duced to larger or smaller extent with the two-comp onent mo del in which profile changes are due to changes in the relative strength of two variable comp onents with a fixed shap e. The double p eaked profile was often observed among the discussed ob jects. Profile decomp osition gives one comp onent that dominates in the central part of the profile, while the double p eaked comp onent dominates in the profile wings. However, the moving features of the profile shap es observed, e.g., in 3C 390.3, NGC 4151, and Arp 102B can b e a result of rotating redistribution of matter in the Keplerian disk. Acknow ledgements.The research was made in partly by the award UP 1-2549-CR-03 of the US Civilian Research and Development Foundation for the Indep endent States of the Former Soviet Union (CRDF) and by the Russian Foundation for Basic Research (RFBR) grant 06-02-16843.

THE STUDY OF A MAGNETIC FIELD STRUCTURE IN BLAZAR JETS BY OPTICAL PHOTOPOLARIMETRIC DATA
Yu.S. Efimov1 , E.Yu. Vovk
1 2

RSI "Crimean Astrophysical Observatory", Nauchny, Crimea, 98409, Ukraine 2 National State University, Kiev, 01033, Ukraine Yuri.Efimov@mail.ru

There are no direct metho ds to measure magnetic field intensity in sources of synchrotron radiation. Usually estimations of magnetic field intensity are obtained from the Faraday rotation measure in radio region with additional data ab out a path length and an electron density. Besides the Faraday rotation of p olarization plane there are observational parameters which are connected directly with the intensity of magnetic field and its structure: a p olarization degree and a sp ectral index. Both these parameters can b e obtained from optical observations. On the other hand, various theoretical mo dels connect magnetic field intensity with p olarization degree. From two p olarimetric mo des observed in blazars: circular and linear, the last one is rather 16


large (from 1% to 40%) and can b e detected easily in contrast to the circular p olarization which is very small (fraction of p ercentage). In its turn, the linear p olarization is directly connected with sp ectral index. So, the comparison of theoretical predictions from various mo dels of magnetic field with observed dep endencies b etween p olarization degrees and sp ectral indices allows to significantly confine an uncertainty of the magnetic field intensity estimations. The first such attempt had b een made ab out 30 years ago by Nordsieck (1976). Moreover, such a comparison allows to follow the variations of the magnetic field intensity from observed variations of p olarization degree and sp ectral index. In this rep ort we present a result of such comparison for two well-known blazars 3C 66A and OJ 287. It was shown that in b oth sources the decrease of p olarization and sp ectral index indicate: an increasing disorder of magnetic fields of relativistic jets. References Nordsieck K.H.: ApJ, 1976, 209, 653.

THE SUPERCRITICAL ACCRETION DISK IN SS433 AND ULTRALUMINOUS X-RAY SOURCES
S. N. Fabrika Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia fabrika@sao.ru SS433 is the only known p ersistent sup ercritical accretor, it may b e very imp ortant for understanding ultraluminous X-ray sources (ULXs) lo cated in external galaxies. We describ e main prop erties of the SS433 sup ercritical accretion disk, jets and its radio nebula W50. Basing on observational data of SS433 and published 2D simulations of sup ercritical accretion disks we estimate parameters of a funnel in the disk/wind of SS433 and discuss formation of jets and a nebula. Critical observations which may throw light up on nature of ULXs come from nebulae observations around ULXs. We present results of 3D-sp ectroscopy of nebulae around several ULXs lo cated in galaxies at distances of 3-6 Mp c. We found that nebulae are p owered by their central black holes. The nebulae are sho cked and dynamically p erturb ed probably by jets.

17


RESULTS OF THE PROMINENCE OBSERVATIONS AT MICROWAVES DURING THE MAXIMAL PHASE OF THE TOTAL SOLAR ECLIPSE OF MARCH 2006
O.A. Golub china, V.M. Bogo d, A.N. Korzhavin, N.N. Bursov, S. Kh. Tokhchukova SPb branch of SAO RAS, St.Petersburg, Russia oag@OG4466.spb.edu Results of the prominence radio emission study according to observations of the solar eclipse on 2006 March 29 with the Northern sector and with the Southern sector with the Flat mirror of RATAN-600 are discussed. Investigation of the prominence lo cated in the NE solar limb is executed in the (1.03-5.0) cm wavelength range. These observations are unique b ecause the solar eclipse was observed with one telescop e simultaneously by two different metho ds. This enables to supplement mutually the data received by observations with two different sectors and gives an opp ortunity to control some obtained results. The angular resolution of the antenna in the horizontal direction is from 17.5 arcsec up to 47 arcsec in the (1.88-5.0) cm wavelength range with the Southern sector and the Flat mirror and from 0.44 arcmin to 1.68 arcmin in the (1.03-3.9) cm range with the Northern sector of the RATAN-600. An average angular size of the prominence source in the sp ecified wavelength range is ab out 30 arcsec. From observations with the Northern and Southern sectors, the p osition of maximum of the prominence radio source have b een found to coincide with the prominence top of the solar image in the He I I 304 line (SOHO, =45o , NE limb of the Sun). The radio fluxes of the prominence were obtained in the wavelength range from 1.03 to 5.0 cm. The fluxes in the range = 1.38 - 4.0(cm) are equal to F()=0.8-0.01(s.f.u.). These values coincide for observations with b oth sectors of RATAN-600, meanwhile the metho ds of the observations and the techniques of data pro cessing of the observations with two sectors were different. The obtained sp ectrum of the prominence defined a thermal mechanism of the prominence radio emission in the (1.03-5.0) cm range. There is a sharp decrease of the prominence radio flux down to value F = 0.02 s.f.u. in comparison with exp ected value for the 1.03 cm wavelength, according to received dep endence F (). Possibly it is caused by the Mo on closing the prominence at the moment of observation. A relative p osition of the Mo on and the Sun at the moment of the solar eclipse maximum phase allowed to estimate the height of the prominence ab ove the photosphere. The derived brightness temp eratures of the prominence are equal to Tb = (5450 - 17900)o K in the (1.84-4.21) cm wavelength range. It was registered a bip olar structure of the radio source asso ciated with the prominence. The degree of circular p olarization of the source is: p = (5 - 10)% for the (1.84-5.0) cm wavelengths. Acknow ledgements. This work is supp orted by the RFBR grant N05-02-16228.

18


EXTRAGALACTIC SOURCE VARIABILITY STUDIES OF COMPLETE SAMPLES WITH RATAN-600
A.G. Gorshkov1 , M.G. Mingaliev
1 2

Sternb erg Astronomical Institute, Moscow State University, Universitetskij pr., 13, Moscow, 119992, Russia 2 Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia algor@sai.msu.ru

We present preliminary results of the study and analysis of complete and limited in flux density source samples from the Zelenchuk and MGB surveys carried out with the RATAN-600 radio telescop e. This work pursues two the main aims: · Investigation of general statistical characteristics of a discrete source sample; · Investigation of variability pro cesses in discrete sources in a wide range of wavelengths. That assumes a study of the amplitude and frequency characteristics of variability on all time scales from several years to several days. The following results of this investigation have b een revealed (or confirmed): 1. The long-term variability with a time-scale more than several years. Our observations have allowed to trace a complete evolution cycle of the isolated flare in a numb er of sources from its o ccurrence b efore decay and to sp ecify its amplitude and frequency characteristics. There is no plateau at the maximum of a flare, a flare increase and decay are well describ ed by a exp onential temp oral law. Such a form of flare is not describ ed by any mo del. 2. The variability with a time-scale ab out tens of days. We consider the variability with a week time scale as an imp ortant result of our investigation. It is a new typ e of the variability and, as it was found out, it is widespread enough. Approximately 10% of sources with flat sp ectra have a similar variability. The variability often has a cyclic nature and, basically, is exp osed at frequencies b elow 10 GHz. 3. The existence of variability with a time-scale ab out four days for all compact radio sources. We are sure that the given typ e of variability is not a prop erty of a radio source, but a result of radiation propagation in inhomogeneous interstellar medium.

19


ON THE SKY SPECTROSCOPY WITH RATAN-600
I.V. Gosachinskij Saint-Petersburg Branch of the Sp ecial Astrophysical observatory of RAS, 196140, Saint-Petrsburg, Pulkovsko je schosse, 65, Russia gos@sao.ru Observations of radio lines with the RATAN-600 radio telescop e are b eing carried out during 30 years in the domain of ­ systematical investigations of a cloudy structure of the Galactic interstellar medium in the lines of HI at 21 cm, OH at 18 cm, H2 CO at 6.2 cm and H2 O at 1.35 cm with the aim of understanding its structure, dynamics, evolution and interaction with other Galactic p opulations; ­ investigation of physical and evolutionary status of large structures of interstellar gas; ­ a search of gas clouds at cosmological distances with the help of their probable line emission. The most interesting results were obtained in the investigation of HI gas around SNR's and HI I regions, recombination line H110 in the Orion nebula, HI Sup er Shells, a formaldehyde cloud in the source Sgr B2, statistical characteristics, "scale relations" and internal motions of the HI clouds and prop erties of interstellar gas at high Galactic latitudes.

INVESTIGATION OF INTERACTION BETWEEN SUPERNOVA REMNANTS AND INTERSTELLAR MEDIUM
I.V. Gosachinskij, A.P. Venger, Z.A. Alferova Saint-Petersburg Branch of the Sp ecial Astrophysical Observatory of RAS 196140, Saint-Petersburg, Pulkovsko je shosse, 65, Russia gos@sao.ru During 1999-2006 the second stage of investigation of HI distribution around sup ernova remnants (SNRs) was carried out with the RATAN-600 radio telescop e. In contrast to a previous stage during 1985-87 now SNR of large angular dimension (greater than 10 ) and sp ecific typ e ­ S (shell) were selected, indep endently from their radio brightness. It is obvious that namely such ob jects have sufficiently large ages for demonstrating a evidence of interaction b etween their sho ck waves and surrounding neutral gas. Such a evidence could b e detected in the "Right Ascension ­ Velo city" ( - V ) maps as ring like structures, whose parameters may bring information ab out sizes, ages and energy of sup ernova explosion. Now we have observed ab out 130 SNRs and 105 -V maps are plotted. Some interesting ob jects (such as S147, Cygnus Lo op, HB3) were studied in detail and results were published separately. So on all - V maps will b e available at our web-site.

20


LONG-TERM RADIO TIME SCALES OF ACTIVE GALACTIC NUCLEI
T. Hovatta 1 , M. Tornikoski 1 , M. Lainela 2 , E. Valtao ja 2 , I. Torniainen 1 , M.F. Aller 3 , H.D. Aller 3 Mets¨ vi radio Observatory aho Mets¨ vintie 114 02540 Kylm¨ a, Finland aho al¨ Tuorla Observatory, University of Turku, Finland Department of Astronomy, University of Michigan tho@kurp.hut.fi
1

2 3

We have studied long-term variability time scales of a large sample of Active Galactic Nuclei at several frequencies b etween 4.8 and 230 GHz. The sample consists of 80 sources from different classes of AGN. In our sample we have quasars, BL Lacertae ob jects and Radio Galaxies. Our sample consists of sources from the Mets¨ vi monitoring programme aho where a sample of compact extragalactic radio sources has b een monitored for over 25 years. In addition we use lower frequency data from the University of Michigan monitoring programme and data obtained from the SEST-telescop e b etween 1986 and 2003. We used the first order structure function, the discrete auto-correlation function and the Lomb-Scargle p erio dogram to study the characteristic time scales of variability. We were interested in finding differences and similarities b etween classes and frequencies. Also the metho ds were compared in order to find the most efficient one for different purp oses. We have also compared the results of this study with earlier structure function analysis by Lainela & Valtao ja (1993). In the earlier analysis the structure function was used to study 42 sources from the Mets¨ vi monitoring sample at 22 and 37 GHz frequencies. We aho wanted to find out how the time scales have changed after the amount of monitoring data has more than tripled. The main conclusion of our study is that in these sources smaller variations happ en also in short time scales but larger outbursts only in time scales of many years. Therefore in order to study how often sources are in active state and how long these flares typically last the long-term monitoring is needed. References Lainela M., Valtao ja E.: ApJ, 1993, 416, 485.

RADIO VARIABLE SOURCES WITH THE RT32 RADIO TELESCOPE
M. Harinov1 , S.A. Trushkin2 , A. Mikhailov
1

Institute of Applied Astronomy of RAS, SAO RAS, Saint-Petersburg, Sp ecial astrophysical observatory of RAS, Nizhnij Arkhyz, Russia kharma78@rambler.ru We discussed first results of radio observations of AGNs and micro quasars with the RT32 radio telescop e (Zelenchuk) during 2004-2006. We carried out more than 20 sets of observations of the micro quasars: SS433, Cyg X-3 and LSI+61d303 at frequencies 2.3 and 21


8.45 GHz. Usually during 1-3 days these sources were observed in a multi-scanning mo de, when the antenna elevation or the antenna azimuth were changed following a cosmic source. Thus, for 3-5 daily observations with a duration of 30-60 minutes we integrated up to 100 single scans, which could b e used to study a fast intra-day variability. The flux sensitivity of ab out 10-20 mJy was reached at b oth frequencies. From Novemb er 2004 to August 2006 in twelve two-day sets of observations the sample of 50 bright variable extragalactic sources from 3 and WMAP catalogs and from the sources list selected for the Russian-Finnish program of AGNs was studied. It is imp ortant for such programs that from March 2005 the RT32 observations were regularly carried out simultaneously at b oth frequencies 2.3 and 8.5 GHz in two circular p olarizations. A go o d agreement of the RATAN and RT32 flux measurements of micro quasars and AGNs was obtained. Acknow ledgements. The authors are thankful to the RFBR and Presidium of RAS for supp ort by grants. S.T. is very thankful to the IAA Program Commitee for regular allo cation of the RT32 observation time. References Trushkin S.A., Harinov M.A., Michailov A.G.: 2005, ATel, N488, 1 Trushkin S.A., Po oley G., Harinov M.A., Mikhailov A.G.: 2006, ATel, 828, 1 Trushkin S.A., Bursov N.N., Valtao ja E., Nizhelskij N.A., Tornikoski M., Mikhailov A.G. Harinov M.: HEA-2006, Abstract b o ok, Moscow, Dec 24-28 2006.

ESTIMATIONS OF EFFECTIVE HEIGHT, SIZE AND BRIGHTNESS TEMPERATURE OF SOLAR CYCLOTRON SOURCES
A.N. Korzhavin, T.I. Kaltman Sp ecial Astrophysical Observatory of RAS, Saint-Petersburg, Russia arles@mail.ru The mo deling of microwave emission from a sp ot-asso ciated cyclotron source was done to refine the metho d of estimations of effective brightness temp erature, size and height ab ove photosphere in the pro cessing of RATAN-600 observations. The simple mo del of a source with a dip ole distribution of magnetic field and with a two-step transition region b etween the cold dense chromosphere and the hot corona was used. When a source approaches the limb the decrease of a source visible size in E-W direction takes place due to the pro jection effect, which causes the decrease of its effective size in pro cessing of a one-dimensional scan of RATAN-600. The subsequent Gauss-analysis would overestimate values of brightness temp eratures if necessary corrections were not done. The same pro jection effect leads to the fact, that the size of source observed in p olarized emission (Stokes parameter V) exceeds the size of the source in full intensity emission (Stokes parameter I) due to non circular distribution of p olarized emission. The metho d of estimates of the effective height of emission ab ove photosphere level by measurements of an emission centre of weight declination from a source geometrical centre at approaching to the limb was mo deled and presented. This work was supp orted by the RFBR grants 05-02-16228 and 06-02-17034a. 22


RATAN-600 OBSERVATIONS OF MICROWAVE STRUCTURE OF THE QUIET SUN
T.I. Kaltman, V.M. Bogo d, A.N. Korzhavin, S.Kh. Tokhchukova Sp ecial astrophysical observatory of RAS, Saint-Petersburg, Russia arles@mail.ru To investigate microwave emission of the quiet Sun the observations with RATAN-600 from Septemb er, 2005 to March, 2006 in the range 6-16.4 GHz with the 1% frequency resolution were used. We present an analysis of observational data for several days with different p ositional angles. A small-scaled structure with the size of 20-40 arc sec is regularly observed with RATAN-600 one-dimensional observations. A high degree of correlation for separate elements of the structure in the different frequencies channels at all band of the observations exists. Our estimates of an average life time are several hours. There is a direct dep endence b etween the sizes and life of time for separate elements. The sp ectra of brightness temp eratures grow with wavelength. The emission p olarization is very likely negligible. The characteristics of presented observed structure are very close to ones of a sup er granulation (chromosphere network) which is not sufficiently investigated in microwaves. The separated bright sources are identified with bright X-ray p oints or bip olar magnetic structure. Our mo deling demonstrates that the structure of the chromosphere network can exist in a wide spatial range, but really only the sources with the sizes of 20-40 sec of arc can b e detected at microwaves. Possible mechanisms of such radio emission are discussed. The daily monitoring with RATAN-600 observations provides p ossibilities to regularly estimate a state of the quiet Sun by emission characteristics of microwave small-scaled structure and to trace rises of new centers of activities. This work was supp orted by the RFBR grants 05-02-16228 and 06-02-17034a.

ABOUT A DOUBLE INVERSION SIGN OF POLARIZATION MICROWAVE EMISSION FROM FLARE-PRODUCTIVE ACTIVE REGION
V. Kotelnikov1 , V. Bogo d1 , L. Yasnov
1 2

Saint-Petersburg branch of Sp ecial Astrophysical Observatory of RAS Pulkovsko e Shosse, 65, Saint-Petersburg, Russia 2 Saint-Petersburg State University 198904 Saint-Petersburg, St. Peterhof, Ul'anovskaya street 1 vasian.spbu@mail.ru

Polarization inversions have b een detected in some microwave sources by Piddington et al. (1951) and by Peterova at al. (1974). Tokhchukova et al. (2002) have shown that a more complex phenomenon is observed in the flare-active regions: b efore a p owerful flare the sign of circular p olarization changed twice within a narrow frequency range. Here we discuss observations of flare-pro ductive active regions. These observations were carried out with the RATAN-600 radio telescop e in a broad radio range for a p erio d from 2000 to 2004. 23


The double inversion has b een observed in several events b efore p owerful proton flares. We prop ose two alternative mo dels for explanation of this phenomenon. The first mo del is the existence of the magnetic "hole" in active the region and the second mo del is the propagation of radio waves through a layer with zero magnetic field. References Peterova N.G., Akhmedov S.B.: Soviet Astronomy, 1974, 17, 168. Piddington J. H., Minnnett H. C.: Austral. J. Sci. Res., 1951 A4, 131. Tokhchukova S. Bogo d V.: Solar Physics., 2002, 212, 99.

RADIO PULSATIONS FROM THE AD LEO FLARE AND ELECTRIC CURRENT DIAGNOSTICS
E.G. Kouprianova1 , A.V. Stepanov1 , V.V.Zaitsev
1 2

Central Astronomical Observatory at Pulkovo, Pulkovo Chaussee 65/1 Saint Petersburg 196140, Russia 2 Instutute of Applied Physics, Nizhny Novgorod, Russia lioka@gao.spb.ru Using pulsations characteristics of AD Leo radio flares observed by Bastian et al. (1990) with the Arecib o 300m and by Stepanov et al. (2001) with the Effelsb erg 100m radio telescop es the values of electric currents (7­40) â 1011 A and plasma parameters in stellar flares are determined. It was shown that radio pulsations can b e due to b oth "sausage" oscillations as well as current RLC-oscillations in a flare lo op (Zaitsev et al. 1988, 2004). Explanation of very intense radio bursts (Tb 1015 K) in terms of coherent plasma emission gives the magnetic field value (100­300 G) and the electron numb er density (1010 ­1011 cm-3 ) in the flares. The energy of electric current stored in the flares was estimated as (1­50) â 10 25 J. It is shown that < 10% of stored energy was released in the flares. References Bastian T., Bo okbinder J., Dulk G.A., Davis M.: Astrophys. J., 1990, 353, 265. Stepanov A.V., Kliem B., Zaitsev V.V. et al.: Astron. Astrophys., 2001, 374, 1072. Zaitsev V.V., Stepanov A.V., Urp o S., Pohjolainen S.: Astron. Astrophys., 1998, 337, 887. Zaitsev V.V., Kislyakov A.G., Stepanov A.V., Kliem B., Fuerst E.: Astron. Lett., 2004, 30, 319.

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NATURE OF ACTIVE GALACTIC NUCLEI FROM MASSIVE INSTANTANEOUS RADIO SPECTRA STUDY WITH RATAN­600 IN 1997­2006 SUPPLEMENTED BY VLBA EXPERIMENTS
Yu.A. Kovalev1 , Y.Y. Kovalev1,2 , G.V. Zhekanis3 , N.A. Nizhelsky
1 3

Astro Space Center of Leb edev Physical Institute, Profsoyuznya 84/32, 117997 Moscow, Russia 2 Max-Planck Institute fur Radioastronomie, ¨ Auf dem Hugel 69, 53121 Bonn, Germany ¨ 3 Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167 Russia ykovalev@avunda.asc.rssi.ru

We present results of observations of 1­22 GHz instantaneous continuum sp ectra of ab out 3000 active galactic nuclei p erformed in 1997­2006 with the 600 meter ring transit radio telescop e RATAN­600. An analysis of typ es and structure of the measured instantaneous sp ectra has lead us to a conclusion that almost all sp ectra could b e mo deled as a sum of two main sp ectral comp onents: LF-comp onent (decreasing with frequency) and HF-comp onent (with a maximum in cm-mm band). In the framework of a mo del with longitudinal magnetic field, the HF-comp onent is explained by synchrotron radiation of a continuous compact relativistic jet emerging from the nucleus, the LF-comp onent -- by radiation of optically thin extended p eripheral structures which accumulate jet particles. Long term variability is studied in ab out 600 AGNs. It is dominated in the same mo del by the variable emission of a compact jet (HF-comp onent) and is explained by variable flow of relativistic particles injected in the jet base. We also apply another mo del, a standard homogeneous blob of relativistic particles with synchrotron self-absorption, for sources with simple parsec scale structure and p eaked sp ectral shap e. On the basis of our combined RATAN and VLBA measurements, we estimate the magnetic field in jet regions of these sources and compare it with estimations provided by the mo del with longitudinal magnetic field.

PLANCK -- UNLOCKING THE SECRETS OF THE UNIVERSE
A. L¨ teenm¨ 1 , M. Tornikoski1 , J. Aatrokoski1 , E. Valtao ja ah aki
1 2

Mets¨ vi Radio Observatory, Helsinki University of Technology aho Mets¨ vintie 114, 02540 Kylm¨ a, Finland aho al¨ alien@kurp.tkk.fi
2

Tuorla Observatory, University of Turku, Finland

The Planck satellite is a Europ ean Space Agency ESA's mission capable of mapping the whole sky at several radio wavelengths. The ultimate purp ose of the satellite is to measure, with a high resolution, the cosmic microwave background (CMB) anisotropy pattern, and thus define the geometry and content of our Universe. At the same time all foreground radio sources in the sky, including extragalactic radio sources, will b e measured, to o. The bypro ducts of the CMB map cleaning pro cess, the foreground source maps, will b ecome useful 25


scientific results in themselves. Hence the task is two-fold. First, to provide the cosmologists with to ols for cleaning the CMB maps, and second, to extract scientific information out of the high radio frequency all-sky foreground source catalogs. One of the most imp ortant goals of our Planck pro ject is the acquisition of complete sky surveys at several high radio frequencies --an unprecedented event that should solve at least some of the op en questions regarding active galactic nuclei (AGNs). Even though we do have a general idea of the basic structure and nature of AGNs, the detailed structure and precise physical pro cesses at work are not yet well understo o d. AGNs emit at all electromagnetic frequencies from the radio to the gamma-ray region, and all these frequencies are connected, each frequency adding to the complete picture. The future of the AGN research is in multifrequency studies p erformed with sophisticated ground-based and space-b orne instruments or instrument networks, and Planck will b e a significant contributor to this work. The Mets¨ vi and Tuorla Planck team has develop ed a sp ecial software called the aho Quick Detection System (QDS), that will b e used for detecting strong, p ossibly flaring, radio sources in the time-ordered data stream of the Planck satellite within one week from the time of observation. This is essential for follow-up observations since the actual data pro duct of the satellite will not b e available until after two years after the mission has started, and even the Early Release Compact Source Catalog (ERCSC) will b e available only approximately nine months after the first full sky observation cycle has b een completed. The QDS will give us a unique opp ortunity to get our hands on the Planck foreground data months b efore anyb o dy else, to trigger virtually simultaneous follow-up observations of interesting events, and also help monitor the quality of the satellite data at an early stage. QDS will b e op erated in the Planck Low Frequency Instrument (LFI) Data Pro cessing Centre (DPC) in Trieste, Italy, by our team. The launch date of the Planck satellite is currently set for early 2008, and the op eration of the QDS will start as so on as the test p erio d of the satellite has b een completed. In this pap er we describ e the Planck mission; the instruments and the science it has b een designed to study. A sp ecial emphasis will b e made on the Finnish participation in the pro ject. This includes, for example, the 70 GHz receivers that were designed and build in Finland, and many asp ects of the science we are currently involved in.

POLARIZATION OBSERVATIONS OF mCVs
H.J.Lehto, S.Kata jainen Tuorla Observatory and Department of Physics FIN-21400 University of Turku hlehto@utu.fi We have observed magnetic variable stars in p olarized light in UBVRI with the NOT. We will discuss some of our recent results.

26


RADIO SPECTRA PROPERTIES OF A COMPLETE SAMPLE OF SOURCES NEAR THE NORTH CELESTIAL POLE
M.G. Mingaliev1 , M.G. Larionov2 , J.V. Sotnikova1 , N.N. Bursov1 , N.S. Kardashev
1 2

Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia; 2 Astro Space Center, Lebedev Physical Institute of RAS, Moscow, Russia marat@sao.ru

The RATAN-600 radio telescop e was used to study sp ectral prop erties for a complete sample of 504 sources from the NVSS catalogue near the North Celestial Pole. The main task of the work was to determine instantaneous sp ectra of radio sources with the purp ose to select ob jects with inverted sp ectra near the 22 GHz frequency for subsequent investigation under the space VLBI Pro ject "RadioAstron". The high angular resolution of the pro ject "RadioAstron" which is to b e achieved 10-6 arcsec imp oses strict demands to angular dimension of sources. These must b e sup er-compact ob jects with a high value of the correlated flux. Such ob jects form a considerable part of ob jects just with inverse and flat sp ectra. At present there are no complete high-frequency catalogues of such ob jects up to low flux density levels (0.2 Jy at 22 GHz). The only available data on the North Celestial Pole are the VLA survey (NVSS) at 1.4 GHz. It is imp ortant to obtain sp ectral characteristics up to the highest frequency of 22 GHz planned in the work of the space interferometer. The following criteria were used in selection of sources from the catalogue NVSS: 1. 00h RA2000 24
h o

2. +75o D E C 2000 +88

3. Flux density: S [1.4GHz] 200 mJy from the NVSS catalog The total numb er of sources is 504. After data reduction we obtained flux densities of sources and their sp ectral characteristics. The sources sp ectral typ es were determined: 65% ­ normal, 24% ­ steep, 7.3% ­ flat, 2.3% ­ inverted, and 1.4% ­ sp ectra with a maximum at centimeter wavelengths (GPS). Eleven sources with inverted sp ectra were detected. The statistics of the sources sp ectra from our sample contrasts with sp ectral characteristics of the sample of ob jects with the same initial parameters but carried out at the frequency 20 GHz by Sadler et al. (2006). We obtained that there is a 25% deficit of sources with the inverted sp ectra in our sample. This can b e explained by the sp ectral prop erties of the "subliminal" sources, which did not fall into the initial sample at the frequency of 1.4 GHz. References Sadler E.M., Ricci R., Ekers R. D., Ekers J. A., Hanco ck P.J., Jackson C. A., Kesteven M.J., Murphy T., Phillips Ch., Reinfrank R. F., Staveley-Smith L., Subrahmanyan R., Walker M. A., Wilson W.E., de Zotti, G.: MNRAS, 371, 898.

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ON THE THEORY OF RESONANT TRANSITIVE RADIATION OF DECIMETRIC RADIATION OF FLARES
E.V. Mo din, L.V. Yasnov Saint-Petersburg State University 198904 Saint-Petersburg, St. Peterhof, Ul'anovskaya street 1, Russia Mo din.Egor@gmail.com In this work a mechanism of resonant transitive radiation (RTR) with reference to its p ossible application for interpretation of decimetric radio emission of solar flares is analyzed. Such radiation dep ends on a numb er of parameters of the radiating media. In particular, on the parameter of sp ectrum of small-scale inhomogeneity of electronic density, . Platonov & Fleishman (2002) derived the formulas for factors RTR in dep endence on the frequency of radiation for = 2. On the whole these formulas describ e the b ehavior of RTR precisely, however in narrow frequency intervals they can give either negative or infinite values. In this work, using the approaches similar to those develop ed by Platonov & Fleishman (2002), factors of RTR for an arbitrary parameter have b een obtained. These factors, in particular, did not give negative and infinite values. On their basis the RTR factors integrated on frequency have b een obtained. These factors were used for the analysis of decimetric radiation of the flare on Decemb er 24, 1991. It has b een shown, that the RTR of this flare N 2 could originate in plasma with small-scale inhomogeneities with = 2.5 · 10-5 . N2 References Platonov K.Yu., Fleishman G.D.: UFN, 2002, 172, 3, 241.

SPECTRAL ENERGY DISTRIBUTIONS AND 37 GHz MONITORING OF BL LACERTAE OBJECTS
E. Niepp ola1 , M. Tornikoski1 , A. L¨ teenm¨ 1 , E. Valtao ja ah aki aho Mets¨ vi Radio Observatory Mets¨ vintie 114, 02540 Kylm¨ a, Finland aho al¨ 2 Tuorla Observatory V¨ al¨ tie 20, 21500 Piikki¨ Finland ais¨ an o, eni@kurp.hut.fi BL Lacertae ob jects (BL Lacs) are a group of active galactic nuclei (AGN) characterized by strong and rapid variability, strong optical p olarization and a lack of prominent emission lines in their sp ectra. We have determined sp ectral energy distributions (SED) for over 300 of these ob jects using archival multi-frequency data and fitted a parab olic function to the synchrotron comp onent of the SED (Niepp ola et al. 2006). The p eak frequencies of the synchrotron comp onents range b etween log peak = 12.67­21.46. We divided the sample into low-energy (LBLs), intermediate energy (IBLs) and high-energy (HBLs) BL Lacs according to their log peak . The correlation b etween log peak and the luminosity at peak was not significant, in contradiction with the "blazar sequence" scenario (Fossati et al. 1998). We also rep ort a summary of the first 3.5 years of observations with the extensive BL Lac 28
1 2


sample at 37 GHz. The BL Lac source list contains 398 sources, all of which were observed at least once. Roughly 34% of the sample was detected at S/N > 4. Most of the detected sources were LBLs, b eing intrinsically more luminous at radio wavelengths than HBLs. Acknow ledgements. The authors made use of the database CATS (Verkho danov et al. 1997) of the Sp ecial Astrophysical Observatory. References Fossati, G., Maraschi, L., Celotti, A., Comastri, A. and Ghisellini, G.: MNRAS, 1998, 299, 433. Niepp ola, E., Tornikoski, M. and Valtao ja E.: A&A, 2006, 445, 441. Verkho danov, O.V., Trushkin, S.A., Andernach, H. and Chernenkov, V.N.: ASPC, 1997, 125, 322.

DEEP SKY SURVEYS WITH RATAN-600
Yu.N. Parijskij Sp ecial Astrophisical Observatory of RAS Nizhnij Arkhyz, 369167, Russia par@sao.ru Blind Sky surveys with RATAN-600 were suggested by the general PROJECT of AVP (1968). A Flat mirror was included into the main CIRCLE structure to carry out quick allsky survey, as successfully was made with the Kraus telescop e of Ohio University. In 1960th the Sky seemed to b e filled by first generation young ob jects with inverted and SSA sp ectra, which were missing in the meters wavelengths catalogs. The Sternb erg Astronomical Institute of the Moscow State University group have surveyed the sky zone DEC:0-14deg with sub-Jy sensitivity at the 2-8 cm wavelength and the first big (8500) list of ob jects detected at 4 GHz ob jects was published just b efore the famous 87GB catalog app eared (see the Zelenchuk survey catalog in CATS data base). The CMB anisotropy studies were early on included in the high priority scientific targets. The first deep blind sky survey was done at 4 cm wavelength in the winter 1975-1976 with sub-mK sensitivity, but only results interesting for CMB p eople were published, and they reject all available in 70-th variants of the theories of galaxies formation. The second ep o ch of deep blind surveys started after installation of the world b est cryo-receiver at 7.6 cm (with 2mK/s1/2 sensitivity). The first 17 Feb. 1980 24h- drift scan demonstrated that ab out 200 details may b e found on this record and may b e classified as radio sources, and we integrated p oint sources (PS) and CMB anisotropy tasks in the exp eriment. Several regions were selected for deep surveys, including the celestial Pole, the Declination of SS433 strip, and the Declination of 3C84 (near the RATAN zenith) strip. Weakness of the CMB anisotropy requires a great averaging (hundreds daily scans) and we observed some regions during many years. At all frequencies lower 10 GHz we see a confusion limit, and we prop osed ways to suppress this noise using sp ecific shap e of the RATAN-600 b eam. It helps us to reach the few mJy level at cm wavelengths and much b elow by P(D) analysis. The multi-frequency mo de of observations, imp ortant for SCREENS (foregrounds) cleaning in the CMB exp eriments, turned out to b e useful for a sp ectral classification of the PS app earing on the scans. Now it is clear for all CMB groups, that the depth of the CLEANING from PS is the real limit of CMB 29


dedicated exp eriments, including the PLANCK mission. The problem with PS ob jects at CMB frequencies connects with an absolutely unknown Source Population (b etween IRAS and NVSS, or GB). At RATAN-600 we try to use SELF CLEANING mo de, using much higher resolution than required by CMB physics (sub-degree scales). A huge amount of data collected during the CMB exp eriments should b e used by PS p eople. I shall present the p ositive and negative exp erience, connected with the international BIG TRIO program, and problems with detection of a new p opulation at cm wavelengths. The present state of RATAN-600 "Cold" and RATAN-600 Zenith Field (RZF) blind surveys will b e mentioned, as well as the present-day situation with High Frequencies Sky Surveys. This presentation describ es results of several groups in SAO and in SPb-branch of SAO, and now is partially supp orted by the RFBR grant 05-02-17521, OF RAS, SPb Center of RAS.

MULTI-FREQUENCY OBSERVATIONS OF THE POLAR RADIO STRUCTURES
A. Riehokainen1 , A.G. Tlatov
1 2 2

Tuorla Observatory 21500, Piikkio, Finland; Pulkovo Astronomical Observatory, St. Petersburg, Russia alerie@utu.fi

In this work we present a comparison of the enhanced temp erature regions (ETRs) in the radio emission of the Sun with other manifestations of solar p olar structures over some days in 2003-2005. The radio observations at 37 GHz were made with the Metsahovi Radio Telescop e (Finland). We compared our radio data with different SOHO/EIT and SOHO/MDI images for the same p erio ds. We also sup erp osed the intensity contours of the full-radio maps obtained in Metsahovi on the Meudon Sp ectroheliograph CaI I(k3) and H(alpha) images. We tried to find difference b etween ETRs inside and outside of coronal holes. We find that the ETRs are clearly connected to brightness structures seen in the CaI I(k3)/H and magnetic field sources seen in SOHO/MDI. Thus we can conclude that ETRs have chromospheric origin.

NEW OBJECTS FROM THE "COLD" SURVEY
N.S. Sob oleva, A.V. Temirova, N.N. Bursov, Yu.K. Zverev Sp ecial astrophysical observatory of RAS, Saint-Petersburg, Russia adelina.temirova@mail.ru Results of deep surveys of a ±10 strip of the sky centered on the declination of SS433 carried out on the Northern sector of the RATAN-600 telescop e at 2.7 and 7.6 cm wavelength in 1987-2000 are discussed. Ab out 600 ob jects at the 7.6 cm wavelength were identified with NVSS sources. Eighteen sources detected at 2.7 cm were not detected at 7.6 cm but could b e identified with NVSS ob jects. It cannot b e ruled out that some of these are sources with inverted sp ectra. At b oth wavelengths there is a fairly large numb er of Gaussian profiles 30


which are not identified with NVSS ob jects (106 at 2.7 cm and 43 at 7.6 cm); it is quite p ossible that not all of these cases are false. The survey ob jects are cross-identified with sources in the NVSS catalog and the corresp onding two-frequency sp ectral indices determined. We find a decrease in the mean sp ectral index in the transition from ob jects with flux densities S21 30 mJy to those with 15 < S21 < 30mJy. The constructed log N - log S relation at 2.7 cm has a slop e of 3/2 at flux densities 300 mJy and flattens at weaker flux densities. The 1.4 GHz (NVSS), 3.94 GHz (RATAN-600), and 11.11 GHz (RATAN-600) data are used to estimate the numb er of ob jects p er square degree at a wavelength of 1 cm.

REVERSAL BACKGROUND MAGNETIC FIELD IN THE SOLAR POLARIZED RADIO EMISSION AT 17 GHz
A.G. Tlatov1 , A. Riehokainen
1 2

Kislovo dsk Solar Station of the Pulkovo Astronomical Observatory, Russia 2 Tuorla Observatory, Turku University, Finland solar@narzan.com

Polarization of radio emission on the solar disk was studied with the Nob eyama radio heliograph observations during 1992-2006. The latitude-time diagrams of p olarization circular radio emission were constructed. To decrease the noises we used several solar images for a day. We found drifts of radio emission p olarization in the high-latitudes activity and in the latitude band of sunsp ots. Pro cess of the magnetic field reversal of the large-scale magnetic field in p olarization of radio emission of the Sun was found during 22-23 cycles. An analysis of p olarization for structures of various brightness temp eratures has b een carried out.

OSCILLATION OF THE POLARIZED RADIO EMISSION "THE SUN AS A STAR"
A.G. Tlatov1 , A. Riehokainen
1 2

Kislovo dsk Solar Station of the Pulkovo Astronomical Observatory, Russia 2 Tuorla Observatory, Turku University, Finland solar@narzan.com

We investigated variations of the radio emission of the whole Sun at 1.76 cm wavelength obtained and archived at the Nob eyama radio heliograph in 1992-2006. For this purp ose the daily data of the intensity and also right/left circular p olarization of the radio emission with one-second average were pro cessed. It was found that 3 minutes oscillations are present at the different phases of solar activity, including the minimum of activity. Esp ecially conspicuous these oscillations present in a difference b etween the right and the left circular p olarization. Intensity of the oscillations changes with a level of the solar activity. Sp ectral analysis of the presence of 3-minute oscillations in p olarization of the solar radio emission shows that there exist a mo dulation with the p erio ds of 27 and 157 days. During the 31


minimum activity the main p erio ds of the 3 minutes oscillations are slightly shorter than during the maximum activity.

RADIO SPECTRA OF GPS GALAXIES
I. Torniainen1 , M. Tornikoski1 , M. Aller2 , H. Aller2 , M. Mingaliev
1 3

Mets¨ vi Radio Observatory, Helsinki University of Technology aho Mets¨ vintie 114, FIN-02540 Kylm¨ a, Finland aho al¨ 2 Department of Astronomy, University of Michigan 3 Sp ecial Astrophysical Observatory of RAS ilo@kurp.hut.fi

Gigahertz-p eaked sp ectrum (GPS) sources are active galactic nuclei which are characterized by a convex radio continuum sp ectrum p eaking at the GHz-frequencies. Their nature is still unclear, but currently the strongest scenario suggests that at least some of them are newb orn radio sources in which the activity has b een triggered on only 100 ­ 1000 years ago. There are b oth quasar and galaxy typ e GPS sources, which have a similar shap e of sp ectrum but the nature and the physics of sources are thought to b e different. Our earlier study (Torniainen et al. 2005) showed that a considerable prop ortion of quasar-typ e GPS sources are more likely misidentified flat-sp ectrum quasars ­ not GPS sources at all. We have collected 96 GPS galaxies from the literature, observed them and collected all p ossible radio data for them to study how pure the galaxy typ e GPS samples are. Our sample includes b oth frequently monitored sources and sources with only a few detections. The sp ectra of the sample show that less than a third of our sample were definitely or highly probably GPS sources whereas less than a third did not have enough data for any solid classification. Five sources had a convex sp ectrum but high variability and the rest had steep or flat sp ectrum. These results show that the GPS galaxy samples have more genuine GPS sources than the quasar samples but yet a remarkable share of them cannot b e classified as GPS sources. Difference b etween the quasar and galaxy samples can partly b e explained by selection effects: the quasar sample was selected from the Mets¨ vi monitoring sample which has aho b een monitored over 25 years whereas the galaxy sample was gathered from the GPS literature and included b oth weak or rarely observed sources and more frequently monitored sources. Acknow ledgements. The authors made use of the database CATS (Verkho danov et al. 1997) of the Sp ecial Astrophysical Observatory. References Torniainen I., Tornikoski M., Ter¨ asranta H., Aller M.F., Aller H.D.: A&A, 2005, 435, 839. Verkho danov O.V., Trushkin S.A., Andernach H., Chernenkov V.N.: ASP Conference Series, 1997, 125, 322.

32


¨ METSAHOVI AGN PROJECTS CONTRIBUTING TO THE PLANCK FOREGROUND SCIENCE
M. Tornikoski1 , A. L¨ teenm¨ 1 , T. Hovatta1 , E. Niepp ola1 , I. Torniainen1 , E. Valtao ja ah aki
1 2

Helsinki University of Technology, Mets¨ vi Radio Observatory aho Mets¨ vintie 114, 02540­Kylm¨ a, Finland aho al¨ 2 Tuorla Observatory, University of Turku, Finland merja.tornikoski@tkk.fi

During recent years we have had a sp ecial fo cus in our Mets¨ vi observing pro jects. We aho have put an emphasis on the understanding of AGNs that could contribute to the extragalactic foreground that will b e detectable by the Planck satellite. First of all, we have observed completely new source samples. Many AGN samples have b een excluded from high-frequency radio observations earlier simply b ecause they were assumed to b e to o faint or "uninteresting". One of our largest new source samples was the complete BL Lacertae Ob ject (BLO) sample. In addition to the few-ep o ch observations of large source samples we have b een interested in the long-term variability b ehaviour of a densely monitored set of sources. We have analysed these data in order to improve our understanding of the variability b ehaviour of these sources: how often do flares typically o ccur in a certain source, and how likely is e.g. the Planck satellite to detect a source in a flaring state at a random observing ep o ch? We are also working our way towards predicting, or at least making "educated guesses" ab out, the activity b ehaviour of radio-bright AGNs. In this presentation we will discuss our source samples and show some recent results.

NEW WMAP CATALOG SOURCES OR HOW MANY BRIGHT SOURCES ARE ON THE SKY
S.A. Trushkin Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia satr@@sao.ru We continued studies of the WMAP-sources after publishing results of three years (Hinshaw et al.; Jarosik et al.; Page et al.; Sp ergel et al. 2006). Trushkin (2003) presented compiled radio sp ectra of 205 extragalactic sources from the catalog, compiled from the WMAP survey data at 23-94 GHz in the first year of its op eration. We have shown that 205 WMAP-sources are reliably identified with radio sources from known catalogs (FIRST, NVSS and so on). 50% of the sources have flat or inverted sp ectra, 15% ­ sp ectra with the p eaks at 5-20 GHz (GPS-sources), 10% ­ p ower-law sp ectra and 10% ­ show the comp osite sp ectra (as 3C84). We discussed recent results of the radio observations of the AGNs from the WMAP catalog with the RATAN-600 and RT32 telescop es. Now the final 3-year catalog contains 323 sources, while four identified sources from the former version were not included in the new one. Using again the search select and match and sp ectra plotting pro cedures in our CATS data base (Verkho danov et al. 1997) we have found optical and radio identifications for the most of new 120 WMAP-sources 33


from the radio and optical catalogs in the CATS data base. Now we discuss results for new 120 sources, their sp ectra and features. The statistics for typ es of the sources did not generally changed. We have found that 313 WMAP-sources have optical counterparts: 220 ­ quasars, 30 ­ galaxies, 32 ­ AGNs, 30 ­ BL Lac ob jects and one ­ the planetary nebula IC418. We have observed some of the new WMAP-sources with RT32 (IAA) at 2.3 and 8.5 GHz. Comparison fluxes from the first version catalog and second one allows us to estimate of the variability of the sample. As was exp ected, the index of the variability at 63 GHz is higher than at 23 GHz. There are the sources with 100% changes of the fluxes on the effective time scale ab out one year, (3yr-1yr)/2 in the WMAP3-catalog. Using an analogous metho d of the source selection from the CATS data base we have found that a probable numb er of the sources brighter 400 mJy at 23 GHz is equal to 13001500 on the sky. Thus there is a strong effect of confusion dramatically decreasing the numb er (323) of detected sources in the WMAP survey. We hop e that such studies will help in the future PLANCK CMB-exp eriment dataprecessing. Acknow ledgements. We are thankful to RFBR for supp ort, the grant N05-02-17556. References Hinshaw G. et al.: astro-ph/0603451. Jarosik N. et al.: astro-ph/0603452. Page L. et al.: astro-ph/0603450. Sp ergel D.N. et al.: astro-ph/0603449. Trushkin S.A.: Bul letin of SAO RAS, 2003, 55, 90. Verkho danov O.V., Trushkin S.A., Andernach H., Chernenkov V.N.: ASP Conference Series, 1997, 125, 322.

RECENT DATA OF THE MULTI-FREQUENCY MONITORING OF MICROQUASARS
S.A. Trushkin Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia satr@sao.ru We discuss results of recent radio observations of the micro quasars SS433, GRS1915+105 and Cyg X-3 with the RATAN-600 and RT32 (IAA) radio telescop es. We have carried out long monitoring programs of daily observations sets for microquasars with the RATAN radio telescop e at frequencies of 1, 2.3, 4.8, 7.7, 11, 21.7 and 30 GHz. Flaring events were detected when the fluxes increased by a factor of 2-200. The flaring synchrotron emission indicates the jets formation, coupling with accretion disk activity in the Galactic micro quasars and in the active galactic nuclei (AGN). The multi-frequency light curves are compared with the XTE ASM data at 2-12 keV to study correlations during the flares. Indeed in many cases such correlations were detected. Radio flaring events of SS433, Cyg X-3, LSI+61d303 were often optically thin at >5 GHz, and follow to general predictions of the relativistic outflows of mass or fast electrons from binaries. On the other hand, we have often measured the inverted (optically thick) 34


sp ectra of flaring events in the active states of GRS1915+105, Cyg X-3 and V4641 Sgr with the sp ectral indices >+1 at >1 GHz. We have detected a clear X-ray/radio asso ciation in light curves of GRS 1915+105 during Octob er-Novemb er 2005, when it was very active (0.5-3 Crabs at 2-12 keV). After 18 days of the quenched state (10 mJy) Cyg X-3 exhibited the 1Jy- radio flare on 1 Feb 2006. Such a remarkable prop erty ­ b efore a flare the radio emission fall down in deep (lo cal) minimum of fluxes ­ is probably a general feature of the radio/X-ray binaries. The flare of 1 Feb was also detected with the Nob eyama 45m and NMA telescop es (Tsub oi et al. 2006), and for the first time a flat radio sp ectrum of the flaring event from Cyg X-3 was directly measured in the quasi-simultaneous observations from 2 to 110 GHz. Then two following flaring events (5 and 17 Jy) were detected later during 100 days. Their durations were 50 and 30 days resp ectively. The very fast rising flare, from 1 to 2 Jy during 3 hours, was detected with the RT32 telescop e (Trushkin et al. 2006) on 05 June. At last on 25 July we have detected a very p owerful flare (15 Jy) from Cyg X-3 again. All these flares happ ened during a long p erio d (Feb 1 ­ Aug 1) when X-ray emission was relatively high (0.3 crabs), variable and hard. We studied evolution of the p owerful flares from the optically thick state to the optically thin one at the lower frequencies. We have to draw an unexp ected conclusion: during the stage of initial rising (ejection stage) the density of thermal electrons is also rising resulting in the higher optical depths at frequencies lower than 1 GHz just near maximum of the flare. Acknow ledgements. This research was supp orted by the Russian Foundation of Basic Research grant N 05-02-17556 and by the Program of the Presidium of Russian Academy of Science. References Tsub oi M. et al. : ATel, 2006, #729. Trushkin S.A. et al.: ATel, 2006, #828.

THE PROBLEM OF HIGH-ENERGY EMISSION FROM AGN
Esko Valtao ja Tuorla Observatory, University of Turku, FI-21500 Piikkio, Finland esko.valtao ja@utu.fi The basic framework for radio-bright AGNs, which are also the only typ es of extragalactic sources known to emit a significant amount of high-energy radiation, is a relativistic jet with sho cks emb edded in it. Presumably, the most significant intrinsic prop erties of the source are then the absolute luminosity of the jet/sho cks, the flow sp eed (the Lorentz factor) and the angle which the jet makes to the line of sight. The more detailed nature of the flow (accelerating/decelerating flow, turbulence, particle acceleration/reacceleration, magnetic field configuration, jet op ening angle and curvature, duty cycle of the sho ck activity, etc.) as well as the jet surroundings (in particular, density of the ambient photon field) must also play a role. The sp ectral energy distributions of radio-bright AGN, often called blazars, can b e approximated by two parab olas. The first one is caused by synchrotron radiation from the jet 35


and from the sho cks, the second one by an inverse Compton radiation from the relativistic electrons in the jet, upscattering ambient photons into X-to-TeV energies. Both theoretically and observationally, our understanding of the blazar emission remains rather p o or. I discuss some new attempts to mo del the sp ectral energy distributions of blazars, fo cusing on correlations b etween various observed and intrinsic prop erties, and on the problems of the prop osed theoretical mo dels for the high-energy emission.

OPEN WEB-RESOURCES OF SAO RAS FOR EXTRAGALACTIC RESEARCH
O.V. Verkho danov 1 , S.A. Trushkin 1 , A.I. Kopylov1 , V.N. Chernenkov1 , H. Andernach 2 , N.V. Verkho danova 1 , V.K. Kononov 1
1 2

Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia Departamento de Astronom´ Universidad de Guana juato, Mexico ia, vo@sao.ru

The sky survey at various wavelength bands is one of the most imp ortant branches of the mo dern observational astrophysics. To the present moment, several data bases unify resulting data of such surveys. We consider here Web-resources designed for radio astronomical and extragalactic study and op erating in the Sp ecial Astrophysical Observatory. We describ e structure, op eration, standard tasks and the current status of the largest data bases in resp ective astrophysics fields. They are the data base of radio astronomical and astrophysical catalogs CATS (http://cats.sao.ru) (Verkho danov et al. 1997, 2005) and the SED (Verkho danov et al. 2000) which is an analysis system of sp ectral energy distribution (http://sed.sao.ru). These servers were unified in a one cluster and are used b oth for separate source and statistical studies in astrophysics and cosmology. A new site (cmb.sao.ru) is prepared for cosmology. It was worked out with the same approach as the ab ove mentioned. It bases on the GLESP (Doroshkevich et al. 2005) package and allows a user to transform spherical harmonics to full sky maps. It contains the WMAP CMB and foreground maps and corresp onding files with a m co efficients of spherical harmonics. We plan to unify all three servers into one cluster for acceleration of investigation in the field of cosmology and astrophysics. Acknow ledgements. This work is supp orted particularly by the Russian Foundation of Basic Research (grant No 05-07-90139). References Doroshkevich A.G., Naselsky P.D., Verkho danov O.V., Novikov D.I., Turchaninov V.I., Novikov I.D., Christensen P.R., Chiang L.-Y.: Internat. J. Mod. Phys. D, 2005, 14, 275 (astro-ph/0305537) Verkho danov O.V., Trushkin S.A., Andernach H., Chernenkov V.N.: In "Astronomical Data Analysis Software and Systems VI", eds. G.Hunt & H.E. Payne, 1997, ASP Conf. Ser., 125, 322 (astro-ph/9610262) Verkho danov O.V., Kopylov A.I., Zhelenkova O.P., Verkho danova N.V., Chernenkov V.N., Parijskij Yu.N., Sob oleva N.S., Temirova A.V.: The software system "Evolution of radio galaxies". Atsron. Astrophys. Trans., 2000, 19, 662, (astro-ph/9912359) 36


Verkho danov O.V., Trushkin S.A., Andernach H., Chernenkov V.N.: Bul letin of SAO of RAS, 2005, 58, 118

PHASE ANALYSIS IN STUDY OF COSMIC MICROWAVE BACKGROUND
O.V.Verkho danov1 , P.D.Naselsky2 , L.-Y.Chiang2 , A.G.Doroshkevich3 , I.D.Novikov
1 3,2

Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia 2 Niels Bohr Institute, Cop enhagen, Denmark 3 AstroSpace Center, Moscow, Russia vo@sao.ru

Phase analysis based on the complex values of spherical harmonics of the CMB fluctuation expansion is an extremely imp ortant metho d of observational cosmology. We consider several asp ects of phase analysis in the CMB study. They concern the problems of signal restoration (Naselsky et al. 2005), search for non-Gaussianity (Chiang et al. 2003) and study of the foreground contamination of this separated CMB signal (Naseslky et al. 2003, 2004, 2005). Using the GLESP (Gauss-LEgendre Sky Pixelization) package (Doroshkevich et al. 2005) for CMB analysis we pro duce phase data for spherical harmonics in the form of a m = | m | exp(i m ), where a m -s are co efficients of spherical harmonics of the ­ multip ole in the m­mo de, | m | is their amplitude, m is a phase, and i is the imaginary unit. Considering the minimum in correlation of phases of CMB and foregrounds we can separate the signal corresp onding to these prop erties at low ( 100) where the p oint source influence is minimal. Another imp ortant moment is the study of the Gaussianity problem in the CMB observational data. To check statistical prop erties of the data we pro duce phase diagrams. These diagrams demonstrate the strong non-Gaussianity for all accessible maps of CMB. The high phase correlations b etween CMB and foregrounds hint us ab out problems of signal separation. Similar approaches are develop ed for the Planck mission. Acknow ledgements. This work is supp orted particularly by the Russian Foundation of Basic Research (grants No 05-07-90139 and 05-02-16302). References Chiang L.-Y., Naselsky P.D., Verkho danov O.V., Way M.J." Astrophys. J., 2003, 590, L65 (astro-ph/0303643) Naselsky P.D., Doroshkevich A.G. , Verkho danov O.V.: Astrophys. J., 2003, 599, L53 (astro-ph/0310542) Naselsky P.D., Doroshkevich A.G., Verkho danov O.V.: MNRAS, 2004, 349, 695 (astroph/0310601) Naselsky P.D., Chiang L.-Y., Novikov I.D., Verkho danov O.V.: Internat. J. Mod. Phys. D, 2005, 14, 1273 (astro-ph/0405523) Doroshkevich A.G., Naselsky P.D., Verkho danov O.V., Novikov D.I., Turchaninov V.I., Novikov I.D., Christensen P.R., Chiang L.-Y.: Internat. J. Mod. Phys. D, 2005, 14, 275 (astro-ph/0305537)

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THE COMBINED RADIO AND OPTICAL INVESTIGATIONS OF THE INTRADAY VARIABILITY OF ACTIVE GALACTIC NUCLEI
A.E. Volvach1 , V.S. Bychkova2 , N.S. Kardashev2 , M.G. Larionov2 , V.V. Vlasyuk3 , O.I. Spiridonova 3 SRI Crimean Astrophysical Observatory, Ukraine, Astro Space Centre of the Leb edev Physical Institute, Russia Sp ecial Astrophysical Observatory of the Academy Science, Russia volvach@crao.crimea.ua
2 1

3

The combined radio and optical observations of the active galactic nuclei 0133+476, 1633+382, 2145+067, 2251+158 were p erformed in 2004-2006. The aim of analysis was to detect an intraday flux variability and to search for its p ossible correlation in radio and optical wavelengths. Observations were conducted with the use of the RT-22 radio telescop e (SRI CrAO) at 22 and 36 GHz and the 1-m Zeiss-1000 reflector of SAO RAS with CCD camera. During observations we found no significant fluctuations of fluxes at b oth ranges. At the level of 10% from the average amplitude more high activity of the ob ject 1633+382 was detected at 36 GHz in May 2004 then the one in May 2005. The reason of it may b e a passive phase of the ob ject after the burst in 2002. The observable flux variation in 0133+476 at the time scale of one hour were noticed in Octob er 2005 but not optical range. Such flux b ehaviour may indicate to absence of the identical area for radio and optical emission after matter collimation in the black hole p olar region. References Volvach A.E., Larionov M.G., Aller M., Aller H.: Radio Astronomy and Radio Physics, 2005. 10, N.4, 377.

PHYSICAL AND CHEMICAL STRUCTURE OF HIGH MASS STAR FORMING REGIONS
I.I. Zinchenko Institute of Applied Physics of the Russian Academy of Sciences 46 Uljanov str., Nizhny Novgoro d 603950, Russia zin@appl.sci-nnov.ru In recent years we surveyed several tens of high mass star forming regions in various molecular lines and in millimeter wave continuum. Basic physical prop erties of detected clumps and molecular abundances were derived. One of the problems is a selection of the b est tracer of mass distribution. In particular, we found that in regions of high mass star formation the CS emission correlates well with the dust continuum emission and is therefore a go o d tracer of the total mass while the N2 H+ distribution is frequently very different. This is opp osite to their typical b ehavior in low-mass cores where a freeze-out plays a crucial role in the chemistry. The b ehavior of other high density tracers varies from source to source but most of them are closer to CS. Radial density profiles in massive cores are fitted by p ower laws with indices ab out -1.6, as derived from the dust continuum emission. The radial 38


temp erature dep endence on intermediate scales is close to the theoretically exp ected one for a centrally heated optically thin cloud. The velo city disp ersion either remains constant or decreases from the core center to the edge. Several cores including those without known emb edded IR sources show signs of infall motions. They can represent the earliest phases of massive protostars. There are implicit arguments in favor of small-scale clumpiness in the cores. Acknow ledgements. The work was supp orted by the Russian Foundation for Basic Research grant 06-02-16317 and by the Program "Extended ob jects in the Universe" of the Russian Academy of Sciences.

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Author's index
Aatrokoski J. 25 Abramov-Maksimov V.E. 9,11 Alferova Z.A. 20 Aller H. 21,32 Aller M. 21,32 Andernach H. 36 Arshakian T.G. 9 Berlin A.B. 14 Bo chkarev N.G. 9,12 Bogo d V.M. 11,11,18,23 Borisov N. 12 Borovik V.N. 11 Burenkov A.N. 9,12 Bursov N.N. 14,14,18,30 Bychkova V.S. 38 Carrasco L. 12 Chavushyan V.H. 9 Chernenkov V.N. 36 Chiang L.-Y. 37 Collin S. 12 Doroshenko V.T. 12,15 Doroshkevich A.G. 37 Efimov Y.S. 16 Fabrika S.N. 17 Garaimov V.I. 11 Gelfreikh G.B. 9 Golub china O.A. 18 Gorshkov A.G. 19 Gosachinskij I.V. 20,20 Grechnev V.V. 11 Grigorieva I.Y. 11 Harinov M. 21 Hovatta T. 21,33 Ili´ D. c 12 Kaltman T.I. 11,22,23 Kardashev N.S. 38 Kata jainen S. 26 Khabibullina M.L. 14 Kononov V.K. 36 Kopylov A.I. 36 Korzhavin A.N. 11,18,22,23 Kotelnikov V. 23 Kouprianova E.G. 24 Kovalev Yu.A. 25 Kovalev Y.Y. 25 40


L¨ teenm¨ A. ah aki 25,28,33 Lainela M. 21 Larionov M.G. 27 Lehto H.J. 26 Lobanov A.P. 9 Ma jorova E.K. 14 Mikhailov A. 21 Mingaliev M. 14,19,27,32 Mo din E.V. 28 Naselsky P.D. 37 Niepp ola E. 28 Nizhelskij N.A. 14,25 Novikov I.D. 37 Parijskij Y.N. 29 Pop ovi´ L. c 12 Riehokainen A. 30,31,31 Semenova T.A. 14 Sergeev S.G. 15 Shap ovalova A.I. 9,12 Sob oleva N.S. 30 Sotnikova J.V. 27 Stepanov A.V. 24 Temirova A.V. 30 Tlatov A.G. 30,31,31 Tokhchukova S.Kh. 18,23 Torniainen I. 21,32 Tornikoski M. 21,25,28,32,33 Trushkin S.A. 21,33,34,36 Tsibulev P.G. 14 Valdes J.R. 12 Valtao ja E. 21,25,28,35 Venger A.P. 20 Verkho danova N.V. 36 Verkho danov O.V. 36,37 Vlasuyk V.V. 12 Vovk E.Yu. 16 Yasnov L.V. 23,28 Zaitsev V.V. 24 Zensus J.A. 9 Zhdanova V.E. 12 Zhekanis G.V. 25 Zinchenko I.I. 38 Zverev Yu.K. 30

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