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IX RussianíFinnish Symposium
on Radio Astronomy
``MultiíWavelength Investigations
of Solar and Stellar Activity and
Active Galactic Nuclei''
Program and abstracts
15--20 October 2006, Nizhnij Arkhyz

RUSSIAN ACADEMY OF SCIENCES
IX RussianíFinnish Symposium on Radio Astronomy
``MultiíWavelength Investigations
of Solar and Stellar Activity and Active
Galactic Nuclei''
15--20 October 2006
Nizhnij Arkhyz
2006

Scientific Organizing Committee
Marat Mingaliev, chair, Yury Parijskij,
Aleksander Stepanov, Merja Tornikoski, Esko Valtaoja
Local Organizing Committee
Sergei Truskhin (chair), Vladimir Bogod, Ekaterina Filippova,
Larisa Martynova, Julia Sotnikova, Larisa Opeikina, Abdulah Uzdenov
The organizers of the Symposium
Central Astronomical Observatory at Pulkovo
Pulkovo chaussee 65/1, SaintíPetersburg, 196140
Special Astrophysical Observatory RAS,
Nizhnij Arkhyz, KarachaevoíCherkassia, 369167
Sponsoring 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 RussianíFinnish Symposium on Radio Astroní
omy, Nizhnij Arkhyz, 15í20 October 2006
October 15, Sunday
09:00í24:00 Day of arrival
19:00í20:00 DINNER
18:00í21:00 Registration of participants
October 16, Monday
08:00í09:00 BREAKFAST
08:30í09:30 Registration of participants
09:30í09:45 Opening ceremony
Session 1. AGNs
Chair: Marat Mingaliev
09:45í10:15 Valtaoja E. The problem of highíenergy emission from AGN
10:15í10:45 Tornikoski M. Metshovi AGN projects contributing to
the Planck foreground science
10:45í11:05 COFFEE BREAK
11:05í11:35 Hovatta T. Longíterm radio time scales of Active Galactic
Nuclei
11:35í12:05 Kovalev Yu. Nature of Active Galactic Nuclei from Massive
Instantaneous Radio Spectra Study with RATANí600
in 1997í2006 supplemented by VLBA experiments
12:05í12:35 Gorshkov A. Extragalactic source variability studies of
complete samples with RATANí600
12:35í13:00 Volvach A. The combined radio and optical investigations
of the intraday variability of active galactic nuclei
13í00í14:30 LUNCH
3

Session 2. Extragalactic Sources
Chair: Esko Valtaoja
14:30í15:00 Lahteenmki A. Planck -- unlocking the secrets of the Universe
15:00í15:30 Parijskij Yu. Very deep SKY surveys with RATANí600
15:30í15:50 Bursov N. RZF Survey
15:50í16:10 Khabibullina M. Mean spectral index of the faintest NVSS
objects from RZF data
16:10í16:40 Larionov M. Radio spectra properties of a complete sample
of sources near the North Celestial Pole
16:40í17:00 COFFEE BREAK
17:00í17:25 Torniainen I. Radio spectra of GPS galaxies
17:25í17:50 Temirova A. New objects from the ''Cold'' survey
17:50í18:15 Nieppola E. Spectral energy distributions and 37 GHz
monitoring of BL Lacertae objects
19:00í20:00 DINNER
October 17, Tuesday
08:00í09:00 BREAKFAST
Session 3. Extragalactic Sources
Chair: Merja Tornikoski
09:00í09:25 Shapovalova A. A link between variable optical continuum
and radio emission of a compact jet in the radioíloud
Seyfert galaxy 3C390.3
09:25í09:50 Burenkov A. Spectral monitoring of NGC 5548 in 1996í2004
09:50í10:15 Trushkin S. New WMAP catalog sources
or how many bright sources are on the sky
10:15í10:40 Doroshenko V. Continuum and broad emission
line variability of Seyfert galaxy
4

10:40í11:00 COFFEE BREAK
11:05í11:30 Efimov Yu. Study of a magnetic field structure in blazar jets
from optical photopolarimetric data
11:30í11:55 Verkhodanov O. Open WEBíresources of SAO RAS
for extragalactic research
Session 4. Sun
Chair: Aleksander Stepanov
12:00í12:30 Riehokainen A. Multiífrequency observations
of the polar radio structures
12:30í13:00 Bogod V. RATANí600 microwave spectral solar observations --
today and future
13í00í14:30 LUNCH
14:30í14:55 Borovik V. Multiwave RATANí600 observations
of postíeruptive processes on the Sun
14:55í15:20 Golubchina O. Results of the prominence observations
at microwaves during the maximal phase of the total
solar eclipse of March 2006
15:20í15:45 Korzhavin A. RATANí600 observations of microwave
structure of the quiet Sun
15:45í16:15 Gelfreikh G. Peculiarities of QPOs of microwave emission
of the flaring solar active regions
16:15í16:40 Korzhavin A. Estimations of e#ective height, size and
brightness temperature of the solar cyclotron sources
16:40í17:00 COFFEE BREAK
17:00í17:25 Modin E. On the theory of resonant transitive radiation
of decimetric radiation of flares
17:25í17:50 Kotelnikov V. About a double inversion sign of polarization
microwave emission flareíproductive active region
19:00í20:00 DINNER
5

October 18, Wednesday
08:00í09:00 BREAKFAST
Session 5. Sun
Chair: Georgy Gelfreikh
09:00í09:25 Tlatov A. Reversal background magnetic field
in the solar polarized radio emission at 17GHz
09:25í09:50 Tlatov A. Oscillation of the polarized radio
emission ``The Sun as a star''
10:00í13:00 Visit to RATANí600
13í00í14:30 LUNCH
Session 6. Galactic Sources
Chair: Yury Parijskij
14:30í15:00 Lehto H. Polarization observations of mCVs
15:00í15:25 Trushkin S. Recent data of the multiífrequency
monitoring of microquasars
15:25í15:50 Stepanov A. Radio pulsations from the AD Leo flare
and electric current diagnostics
15:50í16:15 Fabrika S. The supercritical accretion disk in SS433
and ultraluminous Xíray sources
16:15í16:35 Zinchenko I. Physical and chemical structure
of high mass star forming regions
16:35í16:55 COFFEE BREAK
16:55í17:15 Vdovin V. Developments of lowínoise mm receivers
for radio astronomy
17:15í17:55 1. Gosachinskij I. On the sky spectroscopy with RATANí600
2. Gosachinskij I. The investigation of interaction between
supernova remnants and the interstellar medium
19:00í20:00 DINNER
6

October 19, Thursday
08:00í09:00 BREAKFAST
09:00í12:00 Visit to the Optical telescopes site
12:00í18:00 Excursion to the Mountains area, Barbecue
October 20, Friday
08:00í09:00 BREAKFAST
09:00í24:00 Day of Departure
7

ABSTRACTS
(alphabetically ordered)
8

PECULIARITIES OF QPOS OF MICROWAVE EMISSION OF
THE FLARING SOLAR ACTIVE REGIONS
V.E. AbramovíMaximov, G.B. Gelfreikh
Central Astronomical Observatory at Pulkovo, SaintíPetersburg, Russia
gbg@saoran.spb.su
Quasiíperiodic oscillations of solar coronal structures are e#ectively registered in particular
at microwave waves. The physical nature of periodical processes in the corona is clearly
connected with plasma structures of the solar atmosphere.
On the other hand, the modern conception is that processes leading to eruption of energy
in solar flares are results of energy accumulation in the corona or chromosphere produced
by some reconstruction of plasma structures.
In spite of developments of the modern observations predominantly using cosmic techí
niques, we are still far from a satisfactory observational understanding of the above proí
cesses. The QPOs of solar active regions were found decades ago and their connections with
the flares were detected. Nevertheless, the physical nature and possible forecasting applií
cations are still far from a reasonable level of knowledge. New development of microwave
instruments with a high spatial resolution and regular observations (NoRH, RATAN--600,
SSRT at Badary) opened a new era in such studies. Oscillations with periods from few
minutes to hours were investigated and their time variations were specially analysed. So,
we may conclude that investigations of these parameters for ARs with di#erent levels of
flare activity, time variations including, may lead to a better understanding of the physics
of the problem. Some preliminary results of such studies are presented in this report, based
on an analysis of the Nobeyama radio maps of the Sun with the 10 sec averaging and
covering periods of hours of observations (dates 11 Sep 2001, 07 Oct 2002, including), and
comparing these with spectral parameters of the regions obtained with RATAN--600.
This study was partially supported 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
RADIOíLOUD SEYFERT GALAXY 3C390.3
T.G. Arshakian 1 , A.P. Lobanov 1 , V.H. Chavushyan 2 , A.I. Shapovalova 3 , J.A. Zensus 1 ,
N.G. Bochkarev 4 , A.N. Burenkov 3
1 MaxíPlanckíInstitut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany,
2 Instituto Nacional de AstrofÒÐsica, Optica y ElectrÒonica, Apartado Postal 51. C.P. 72000.
Puebla, Pue., MÒexico,
3 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia,
4 Sternberg Astronomical Institute, University of Moscow, Universitetskij Prospect 13,
Moscow 119899, Russia
tigar@mpifríbonn.mpg.de
We present an observational evidence for a relation between variability of radio emission of
the compact jet, nucleus optical continuum emission and ejections of new jet components
9

in the radio galaxy 3C390.3. We combine results from the monitoring of 3C390.3 in the
optical region (Shapovalova 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 components (C4íC8) and two stationary components (D,S1). Proper motions of
the moving components correspond to apparent velocities from 0.8c to 1.5c. No significant
correlation exists for the moving features between 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(S1íopt)#0.4 year. Most probably the optical continuum is produced near the
location of radio emission of the S1 stationary component. The localization 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 pc from the central engine. For the components C4íC7, the epochs 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 components are coupled with
the longíterm variability of optical continuum.
We suppose that the broad emission lines having a doubleípeaked structure originate in
two kinematically and physically di#erent 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 (Shapovalova 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 pc from the central engine.
During the nucleus maximal brightness periods 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 crossícorrelation
function describing the timeílag of broad line variations relatively to continuum on the base
of the results of 3C390.3 optical monitoring in 1996í2000 (Shapovalova et al. 2001).
Acknowledgements. This work was supported by grants: CONACYT 39560F (Mexico),
INTAS (N96í0328) and RFBR (00í02í16272; 03í02í17123 and 06í02í16843, Russia).
References
Shapovalova et al.: A&A, 2001, 376, 775.
Sergeev et al.: ApJ, 2002, 576, 660;
Kellermann et al.: ApJ, 2004, 609, 539.
10

RATANí600 MICROWAVE SPECTRAL OBSERVATIONS OF
THE SUN -- TODAY AND FUTURE
V.M. Bogod
Special Astrophysical Observatory of RAS, SaintíPetersburg, Russia
vbog@gao.sb.ru
Problems of solar radio emission study with the help of the RATANí600 radio telescope 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 smallíscale radio emission structure of the Quiet Sun (a soícalled ``radio granulaí
tion'');
. Neutral line associated sources in solar active regions;
. Noníthermal radio emission above sunspots groups, so named ``the decimetre halo'';
. Cyclotron lines in the active regions;
. Multiple polarization inversions in flareíproductive active regions;
. Relations between the double polarization inversions e#ect at microwaves and Noise
Storms activity at meter waves;
. The shortíwave increasing of polarization flux before big flares;
. The ``darkening'' radio emission e#ect in flareíproductive active regions;
. An evolution of polarization flux spectrum before big flares;
. Discovery of microíbursts and their relation with Noise Storms;
. Detection of a frequency boundary between Sí and Bícomponents and others.
Examples of the features listed above are described. A possible future development of
solar investigations with RATANí600 is discussed.
MULTIWAVE RATANí600 OBSERVATIONS OF
POSTíERUPTIVE PROCESSES ON THE SUN
V.N. Borovik 1 , V.V. Grechnev 2 , V.E. AbramovíMaksimov 1 , I.Y. Grigorieva 1 , V.M.
Bogod 3 , V.I. Garaimov 3 , T.I. Kaltman 3 , A.N. Korzhavin 3
1 Central Astronomical Observatory of RAS, SaintíPetrsburg, Pulkovskoje shosse, 65,
2 Institute of Solar Terrestrial Physics, Irkutsk,
3 Special Astrophysical Observatory of RAS, SaintíPetrsburg, Pulkovskoe schosse, 65,
Russia
borovik@saoran.spb.su
11

During two last decades, authors of some studies of postíeruptive arcades repeatedly came
to the following unexpected conclusions. Microwave emission of arcades was excessively
polarized, presumably due to contribution of noníthermal electrons. Their lifetime was
much longer than the estimated cooling times, presumably due to the postíeruptive energy
release. Finally, the plasma pressure exceeded the magnetic pressure (# # 1) in their
hot top parts. CORONASíF/SPIRIT observations in the highítemperature (#10 MK)
line MgXII and multiíwave RATANí600 observations along with data from other spectral
domains provided important information to verify these conclusions and assumptions. All
above facts were confirmed in analyses of this data set. They were explained in terms
of the standard flare model (``CSHKP'') elaborated by Yokoyama & Shibata (1998) to
qualitative account for the chromospheric evaporation, but applied to late postíeruptive
phase. In this case, high # conditions indicate magnetic reconnection processes responsible
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 postíeruptive
arcades, and to remove seeming contradictions with habitual conceptions. We consider
longílived postíeruptive arcades observed on 22 October 2001, 2 November 1992, and 28--
30 December 2001 and demonstrate that these conclusions are valid, because highídensity
hot regions in their top parts (thus, high # regions) existed for a long time, and their
radio emission contained noníthermal component, 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. Burenkov 1 , A.I. Shapovalova 1 , N.G. Bochkarev 2 , V.H. Chavushyan 3 , S. Collin 4 , V.T.
Doroshenko 2 , L. PopoviÒc 5 , N. Borisov 1 , L. Carrasco 3 , D. IliÒc 6 , J.R. Valdes 3 , V.V.
Vlasuyk 1 , V.E. Zhdanova 2
1 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia
2 Sternberg Astronomical Institute, University of Moscow, Universitetskij Prospect 13,
Moscow 119899, Russia
3 Instituto Nacional de AstrofÒÐsica, Optica y ElectrÒonica, Apartado Postal 51. C.P. 72000.
Puebla, Pue., MÒexico
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
We present results of a spectral monitoring program of the Seyfert galaxy NGC 5548 with
the 6m and 1m telescopes of SAO (Russia) and with the 2.1m telescope of Guillermo
Haro Observatory at Cananea, MÒexico. Spectra were obtained with longíslit spectrograph,
covering the spectral range #(4000--7500) Ú A with a (4.5--15) Ú A resolution. We found that:
-- Both the flux in the lines and continuum gradually decreased, reaching minimum
values during MayíJune 2002. In the minimum state, the wings of H# and H# became
12

extremely weak, corresponding to a Sy1.8 type, not to a Sy1, as observed previously when
the nucleus was brighter.
-- When the line profiles were decomposed into variable and constant components, the
variable broad component is well correlated with the continuum variation. It consists of
a double peaked structure with radial velocities of # ‘1000 km/s relative to the narrow
component. A constant component, whose presence is independent of the continuum flux
variations, shows only narrow emission lines. The mean, rms, and the averaged over years,
observed and di#erence line profiles of H# and H# reveal the same double peaked structure
at the same velocities. The relative intensity of these peaks changes with time. During 1996,
the red peak was the brightest, while in 1998--2002, the blue peak became the brighter one.
Their radial velocities vary in the range #500--1200 km/s.
-- In 2000--2002 a distinct third peak appeared in the red wing of H# and H# line
profiles. The radial velocity of this feature decreased between 2000 and 2002: by the
observed profiles, from # +(2500--2600) km/s to # +2000 km/s and it is clearly seen on
the di#erence 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
velocities 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 reprocessing 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 method given by PopoviÒc (2003). We applied the
method on the broad Balmer lines, and found that variability seen in lines is also present in
the electron temperature (T). We found that the average T for the considered period 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 Local Thermodynamical
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 papers (Shapovalova at al. 2004;
PopoviÒc et al. 2005).
Acknowledgements. This work was supported by grants from CONACYT 39560íF (Mexí
ico), RFBR 06í02í16843 (Russia) and the Ministry of Science and Environment Protection
of Serbia.
References
PopoviÒc L. ß
C.: ApJ, 2003, 599, 140.
PopoviÒc L. ß
C. et al.: Astroíph/0511676, 2005 (in press).
Shapovalova A. I. et al.: 2004, A&A, 422, 925.
13

MEAN SPECTRAL INDEX OF THE FAINTEST NVSS
OBJECTS FROM RZF DATA
N.N. Bursov 1 , M.L. Khabibullina 2
1 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia
2 Kazan State University, Kazan, Russia
nnb@sao.ru
A spectral index of a 'mean' radio source from NVSS catalog was estimated by summaí
rizing of the drift scans of the RZF survey. In the area of RZF servey (RA2000:0í24;
DEC2000:40.5í42.5) 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 point ones. We have divided this
flux range to 12 bins: 2--4, 4--6, 6--8, 8--10, 10--13, 13--17, 17--24, 24--35, 35--60, 60--110,
110--220, 220--400 mJy. We summarized 7500 intercepts of oneíhour records at 4 GHz of
RZF survey by a number 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 respectively.
The data give a rough estimate of the 'average' spectral indices (1.4--4 GHz) for each
NVSS sources bin. We found that an 'average' spectral index is a function of NVSS flux
densities. A comparison with expected mean spectral indices and the reliability of such a
estimate are discussed.
However, in the bin of 3--8 mJy the spectra have spectral index equal to --0.8, i.e. the
relative fraction of the steep spectrum sources decreased probably because a number of
FRII 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. Majorova, T.A. Semenova, M.G. Mingaliev, A.B. Berlin,
N.A. Nizhel'skij, P.G. Tsibulev
Special 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 objects of the catalog is evaluated. Radio spectra of NVSS objects
are plotted and a new distribution of spectral indices is found.
New information about a contribution of background of the faint radio sources with
inverted spectrum and about a ``subímJy'' population of the background radio sources in
the cm range is found. It is shown that an average spectral index of radio sources at the mJy
level is flatter, a percentage of classical radio galaxies FRII type drops, but the population
of objects with inversion spectra 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 below the level of WMAP experiment.
14

The synchrotron component 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. Doroshenko 1,2 , S.G. Sergeev 2 , V.I. Pronik 2
1 Crimean Lab. of the Sternberg Astronomical Institute, Moscow University, Russia
2 ScientificíResearch Institute, Crimean Astrophysical Observatory, Ukraine;
p/o Nauchny, 98409, Crimea, Ukraine
vdorosh@sai.crimea.ua
We focused on the observed properties of some Seyfert galaxies without detailed discussion
of underlying physical mechanisms. Our purpose was to show a diversity of observed e#ects
due to variability in spectra of six galaxies (NGC 4151, NGC 5548, Mrk 6, Ark 120, 3C 390.3,
Arp 120B), optical spectral and photometric monitoring of which was carried out in the
Crimean Astrophysical Observatory and Crimean Laboratory of the Sternberg Astronomical
Institute over many years. This monitoring shows that
. All light curves demonstrate a variability on di#erent 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 response to the flux variation of the ionizing
continuum source with some time delay. Thus, the emission lines ``echo'' or ``reverí
berate'' the continuum changes. This time delay is due to lightítravel time e#ects
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 e#ective emission in the H# and
H# lines is fairly small, and it is located at a distance of about 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 di#erent lag for two time intervals for NGC 5548: #26 days in
1972--1988 and # 18 days in 1989--2001.
. Analysis of the lag as a function of the radial velocity does not show any reliable
evidence of the pure radial dominated outflow, possibly, 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 looks 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 between the velocity field and the distance
of the emitting region: the velocity field diminishes with increasing distance from
the central continuum source. This implies that the velocity field is dominated by a
central massive object.
. Not only the flux of broad emission line but also the line profiles appreciably changed
with time. The emissioníline profile changes usually occur on a time scale that is
much longer than the lightítravel time scale.
. In all cases, the excess between the normalized Balmer profiles and the mean normalí
ized profile shows a very complicated behavior both over time and wavelength, and
it can hardly be related to the expected reverberation signal from the simple disk
model. The profile evolution for some galaxies (NGC 4151, Mrk 6, 3C 390.3) can
be reproduced to larger or smaller extent with the twoícomponent model in which
profile changes are due to changes in the relative strength of two variable compoí
nents with a fixed shape. The double peaked profile was often observed among the
discussed objects. Profile decomposition gives one component that dominates in the
central part of the profile, while the double peaked component dominates in the profile
wings. However, the moving features of the profile shapes observed, e.g., in 3C 390.3,
NGC 4151, and Arp 102B can be a result of rotating redistribution of matter in the
Keplerian disk.
Acknowledgements.The research was made in partly by the award UP 1í2549íCRí03 of
the US Civilian Research and Development Foundation for the Independent States of the
Former Soviet Union (CRDF) and by the Russian Foundation for Basic Research (RFBR)
grant 06í02í16843.
THE STUDY OF A MAGNETIC FIELD STRUCTURE IN
BLAZAR JETS BY OPTICAL PHOTOPOLARIMETRIC DATA
Yu.S. Efimov 1 , E.Yu. Vovk 2
1 RSI ``Crimean Astrophysical Observatory'', Nauchny, Crimea, 98409, Ukraine
2 National State University, Kiev, 01033, Ukraine
Yuri.Efimov@mail.ru
There are no direct methods 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 about a path length and an electron
density. Besides the Faraday rotation of polarization plane there are observational paramí
eters which are connected directly with the intensity of magnetic field and its structure:
a polarization degree and a spectral index. Both these parameters can be obtained from
optical observations. On the other hand, various theoretical models connect magnetic field
intensity with polarization degree.
From two polarimetric modes observed in blazars: circular and linear, the last one is rather
16

large (from 1% to 40%) and can be detected easily in contrast to the circular polarization
which is very small (fraction of percentage). In its turn, the linear polarization is directly
connected with spectral index. So, the comparison of theoretical predictions from varií
ous models of magnetic field with observed dependencies between polarization degrees and
spectral indices allows to significantly confine an uncertainty of the magnetic field intensity
estimations. The first such attempt had been made about 30 years ago by Nordsieck (1976).
Moreover, such a comparison allows to follow the variations of the magnetic field intensity
from observed variations of polarization degree and spectral index.
In this report we present a result of such comparison for two wellíknown blazars 3C 66A
and OJ 287. It was shown that in both sources the decrease of polarization and spectral
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 XíRAY SOURCES
S. N. Fabrika
Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia
fabrika@sao.ru
SS433 is the only known persistent supercritical accretor, it may be very important for uní
derstanding ultraluminous Xíray sources (ULXs) located in external galaxies. We describe
main properties of the SS433 supercritical accretion disk, jets and its radio nebula W50.
Basing on observational data of SS433 and published 2D simulations of supercritical ací
cretion 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 upon nature of
ULXs come from nebulae observations around ULXs. We present results of 3Díspectroscopy
of nebulae around several ULXs located in galaxies at distances of 3í6 Mpc. We found that
nebulae are powered by their central black holes. The nebulae are shocked and dynamically
perturbed 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. Golubchina, V.M. Bogod, 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 RATANí600 are discussed. Investigation of the prominence located in the NE
solar limb is executed in the (1.03í5.0) cm wavelength range. These observations are unique
because the solar eclipse was observed with one telescope simultaneously by two di#erent
methods. This enables to supplement mutually the data received by observations with two
di#erent sectors and gives an opportunity 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 (1.88í5.0) cm wavelength range with the Southern sector and the Flat mirror and
from 0.44 arcmin to 1.68 arcmin in the (1.03í3.9) cm range with the Northern sector of the
RATANí600. An average angular size of the prominence source in the specified wavelength
range is about 30 arcsec. From observations with the Northern and Southern sectors, the
position of maximum of the prominence radio source have been found to coincide with the
prominence top of the solar image in the He II 304 line (SOHO, #=45 o , 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 í 4.0(cm) are equal to F(#)=0.8í0.01(s.f.u.).
These values coincide for observations with both sectors of RATANí600, meanwhile the
methods of the observations and the techniques of data processing of the observations with
two sectors were di#erent.
The obtained spectrum of the prominence defined a thermal mechanism of the promií
nence radio emission in the (1.03í5.0) cm range. There is a sharp decrease of the prominence
radio flux down to value F = 0.02 s.f.u. in comparison with expected value for the 1.03 cm
wavelength, according to received dependence F (#). Possibly it is caused by the Moon
closing the prominence at the moment of observation. A relative position of the Moon and
the Sun at the moment of the solar eclipse maximum phase allowed to estimate the height
of the prominence above the photosphere. The derived brightness temperatures of the
prominence are equal to T b = (5450 - 17900) o K in the (1.84í4.21) cm wavelength range.
It was registered a bipolar structure of the radio source associated with the prominence.
The degree of circular polarization of the source is: p = (5 - 10)% for the (1.84í5.0) cm
wavelengths.
Acknowledgements. This work is supported by the RFBR grant N05í02í16228.
18

EXTRAGALACTIC SOURCE VARIABILITY STUDIES OF
COMPLETE SAMPLES WITH RATANí600
A.G. Gorshkov 1 , M.G. Mingaliev 2
1 Sternberg Astronomical Institute, Moscow State University, Universitetskij pr., 13,
Moscow, 119992, Russia
2 Special 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
RATANí600 radio telescope.
This work pursues two the main aims:
. Investigation of general statistical characteristics of a discrete source sample;
. Investigation of variability processes 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 been revealed (or confirmed):
1. The longíterm variability with a timeíscale more than several years. Our observations
have allowed to trace a complete evolution cycle of the isolated flare in a number of
sources from its occurrence before decay and to specify its amplitude and frequency
characteristics. There is no plateau at the maximum of a flare, a flare increase and
decay are well described by a exponential temporal law. Such a form of flare is not
described by any model.
2. The variability with a timeíscale about tens of days. We consider the variability with
a week time scale as an important result of our investigation. It is a new type of the
variability and, as it was found out, it is widespread enough. Approximately 10% of
sources with flat spectra have a similar variability. The variability often has a cyclic
nature and, basically, is exposed at frequencies below 10 GHz.
3. The existence of variability with a timeíscale about four days for all compact radio
sources. We are sure that the given type of variability is not a property of a radio
source, but a result of radiation propagation in inhomogeneous interstellar medium.
19

ON THE SKY SPECTROSCOPY WITH RATANí600
I.V. Gosachinskij
SaintíPetersburg Branch of the Special Astrophysical observatory of RAS,
196140, SaintíPetrsburg, Pulkovskoje schosse, 65, Russia
gos@sao.ru
Observations of radio lines with the RATANí600 radio telescope are being 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, H 2 CO at 6.2 cm and H 2 O at 1.35 cm with the
aim of understanding its structure, dynamics, evolution and interaction with other Galactic
populations;
-- 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 HII regions, recombination line H110# in the Orion nebula, HI Super Shells, a formaldeí
hyde cloud in the source Sgr B2, statistical characteristics, ``scale relations'' and internal
motions of the HI clouds and properties 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
SaintíPetersburg Branch of the Special Astrophysical Observatory of RAS
196140, SaintíPetersburg, Pulkovskoje shosse, 65, Russia
gos@sao.ru
During 1999í2006 the second stage of investigation of HI distribution around supernova
remnants (SNRs) was carried out with the RATANí600 radio telescope. In contrast to
a previous stage during 1985í87 now SNR of large angular dimension (greater than 10 # )
and specific type -- S (shell) were selected, independently from their radio brightness. It is
obvious that namely such objects have su#ciently large ages for demonstrating a evidence of
interaction between their shock waves and surrounding neutral gas. Such a evidence could
be detected in the ``Right Ascension -- Velocity'' (#-V ) maps as ring like structures, whose
parameters may bring information about sizes, ages and energy of supernova explosion.
Now we have observed about 130 SNRs and 105 #-V maps are plotted. Some interesting
objects (such as S147, Cygnus Loop, HB3) were studied in detail and results were published
separately. Soon all # - V maps will be available at our webísite.
20

LONGíTERM RADIO TIME SCALES OF ACTIVE
GALACTIC NUCLEI
T. Hovatta 1 , M. Tornikoski 1 , M. Lainela 2 , E. Valtaoja 2 , I. Torniainen 1 ,
M.F. Aller 3 , H.D. Aller 3
1 MetsØahovi radio Observatory
MetsØahovintie 114 02540 KylmØalØa, Finland
2 Tuorla Observatory, University of Turku, Finland
3 Department of Astronomy, University of Michigan
tho@kurp.hut.fi
We have studied longíterm variability time scales of a large sample of Active Galactic
Nuclei at several frequencies between 4.8 and 230 GHz. The sample consists of 80 sources
from di#erent classes of AGN. In our sample we have quasars, BL Lacertae objects and
Radio Galaxies. Our sample consists of sources from the MetsØahovi monitoring programme
where a sample of compact extragalactic radio sources has been monitored for over 25
years. In addition we use lower frequency data from the University of Michigan monitoring
programme and data obtained from the SESTítelescope between 1986 and 2003.
We used the first order structure function, the discrete autoícorrelation function and
the LombíScargle periodogram to study the characteristic time scales of variability. We
were interested in finding di#erences and similarities between classes and frequencies. Also
the methods were compared in order to find the most e#cient one for di#erent purposes.
We have also compared the results of this study with earlier structure function analysis
by Lainela & Valtaoja (1993). In the earlier analysis the structure function was used to
study 42 sources from the MetsØahovi monitoring sample at 22 and 37 GHz frequencies. We
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 happen 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 longíterm monitoring is needed.
References
Lainela M., Valtaoja E.: ApJ, 1993, 416, 485.
RADIO VARIABLE SOURCES WITH THE RT32 RADIO
TELESCOPE
M. Harinov 1 , S.A. Trushkin 2 , A. Mikhailov 1
Institute of Applied Astronomy of RAS, SAO RAS, SaintíPetersburg,
Special astrophysical observatory of RAS, Nizhnij Arkhyz, Russia
kharma78@rambler.ru
We discussed first results of radio observations of AGNs and microquasars with the RT32
radio telescope (Zelenchuk) during 2004í2006. We carried out more than 20 sets of obí
servations of the microquasars: SS433, Cyg Xí3 and LSI+61d303 at frequencies 2.3 and
21

8.45 GHz. Usually during 1í3 days these sources were observed in a multiíscanning mode,
when the antenna elevation or the antenna azimuth were changed following a cosmic source.
Thus, for 3í5 daily observations with a duration of 30í60 minutes we integrated up to 100
single scans, which could be used to study a fast intraíday variability. The flux sensitivity
of about 10í20 mJy was reached at both frequencies. From November 2004 to August 2006
in twelve twoíday sets of observations the sample of 50 bright variable extragalactic sources
from 3 and WMAP catalogs and from the sources list selected for the RussianíFinnish proí
gram of AGNs was studied. It is important for such programs that from March 2005 the
RT32 observations were regularly carried out simultaneously at both frequencies 2.3 and
8.5 GHz in two circular polarizations. A good agreement of the RATAN and RT32 flux
measurements of microquasars and AGNs was obtained.
Acknowledgements. The authors are thankful to the RFBR and Presidium of RAS
for support by grants. S.T. is very thankful to the IAA Program Commitee for regular
allocation of the RT32 observation time.
References
Trushkin S.A., Harinov M.A., Michailov A.G.: 2005, ATel, N488, 1
Trushkin S.A., Pooley G., Harinov M.A., Mikhailov A.G.: 2006, ATel, 828, 1
Trushkin S.A., Bursov N.N., Valtaoja E., Nizhelskij N.A., Tornikoski M., Mikhailov A.G.
Harinov M.: HEAí2006, Abstract book, Moscow, Dec 24í28 2006.
ESTIMATIONS OF EFFECTIVE HEIGHT, SIZE AND
BRIGHTNESS TEMPERATURE OF SOLAR CYCLOTRON
SOURCES
A.N. Korzhavin, T.I. Kaltman
Special Astrophysical Observatory of RAS, SaintíPetersburg, Russia
arles@mail.ru
The modeling of microwave emission from a spotíassociated cyclotron source was done to
refine the method of estimations of e#ective brightness temperature, size and height above
photosphere in the processing of RATANí600 observations. The simple model of a source
with a dipole distribution of magnetic field and with a twoístep transition region between
the cold dense chromosphere and the hot corona was used.
When a source approaches the limb the decrease of a source visible size in EíW direction
takes place due to the projection e#ect, which causes the decrease of its e#ective size in
processing of a oneídimensional scan of RATANí600. The subsequent Gaussíanalysis would
overestimate values of brightness temperatures if necessary corrections were not done.
The same projection e#ect leads to the fact, that the size of source observed in polarized
emission (Stokes parameter V) exceeds the size of the source in full intensity emission
(Stokes parameter I) due to non circular distribution of polarized emission.
The method of estimates of the e#ective height of emission above photosphere level by
measurements of an emission centre of weight declination from a source geometrical centre
at approaching to the limb was modeled and presented.
This work was supported by the RFBR grants 05í02í16228 and 06í02í17034a.
22

RATANí600 OBSERVATIONS OF MICROWAVE STRUCTURE
OF THE QUIET SUN
T.I. Kaltman, V.M. Bogod, A.N. Korzhavin, S.Kh. Tokhchukova
Special astrophysical observatory of RAS, SaintíPetersburg, Russia
arles@mail.ru
To investigate microwave emission of the quiet Sun the observations with RATANí600
from September, 2005 to March, 2006 in the range 6í16.4 GHz with the 1% frequency
resolution were used.
We present an analysis of observational data for several days with di#erent positional
angles. A smallíscaled structure with the size of 20í40 arc sec is regularly observed with
RATANí600 oneídimensional observations. A high degree of correlation for separate eleí
ments of the structure in the di#erent frequencies channels at all band of the observations
exists. Our estimates of an average life time are several hours. There is a direct dependence
between the sizes and life of time for separate elements.
The spectra of brightness temperatures grow with wavelength. The emission polarizaí
tion is very likely negligible. The characteristics of presented observed structure are very
close to ones of a super granulation (chromosphere network) which is not su#ciently invesí
tigated in microwaves. The separated bright sources are identified with bright Xíray points
or bipolar magnetic structure.
Our modeling demonstrates that the structure of the chromosphere network can exist
in a wide spatial range, but really only the sources with the sizes of 20í40 sec of arc can be
detected at microwaves. Possible mechanisms of such radio emission are discussed.
The daily monitoring with RATANí600 observations provides possibilities to regularly
estimate a state of the quiet Sun by emission characteristics of microwave smallíscaled
structure and to trace rises of new centers of activities.
This work was supported by the RFBR grants 05í02í16228 and 06í02í17034a.
ABOUT A DOUBLE INVERSION SIGN OF POLARIZATION
MICROWAVE EMISSION FROM FLAREíPRODUCTIVE
ACTIVE REGION
V. Kotelnikov 1 , V. Bogod 1 , L. Yasnov 2
1 SaintíPetersburg branch of Special Astrophysical Observatory of RAS
Pulkovskoe Shosse, 65, SaintíPetersburg, Russia
2 SaintíPetersburg State University
198904 SaintíPetersburg, St. Peterhof, Ul'anovskaya street 1
vasian.spbu@mail.ru
Polarization inversions have been 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 flareíactive regions: before a powerful flare the sign
of circular polarization changed twice within a narrow frequency range. Here we discuss
observations of flareíproductive active regions. These observations were carried out with
the RATANí600 radio telescope in a broad radio range for a period from 2000 to 2004.
23

The double inversion has been observed in several events before powerful proton flares.
We propose two alternative models for explanation of this phenomenon. The first model
is the existence of the magnetic ``hole'' in active the region and the second model 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. Bogod V.: Solar Physics., 2002, 212, 99.
RADIO PULSATIONS FROM THE AD LEO FLARE AND
ELECTRIC CURRENT DIAGNOSTICS
E.G. Kouprianova 1 , A.V. Stepanov 1 , V.V.Zaitsev 2
1 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 Arecibo 300m and by Stepanov et al. (2001) with the E#elsberg 100m radio telescopes
the values of electric currents (7--40) ½ 10 11 A and plasma parameters in stellar flares are
determined. It was shown that radio pulsations can be due to both ``sausage'' oscillations
as well as current RLCíoscillations in a flare loop (Zaitsev et al. 1988, 2004). Explanation
of very intense radio bursts (T b # 10 15 K) in terms of coherent plasma emission gives the
magnetic field value (100--300 G) and the electron number density (10 10 --10 11 cm -3 ) in the
flares. The energy of electric current stored in the flares was estimated as (1--50) ½ 10 25 J.
It is shown that < #10% of stored energy was released in the flares.
References
Bastian T., Bookbinder 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., Urpo 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.
24

NATURE OF ACTIVE GALACTIC NUCLEI FROM MASSIVE
INSTANTANEOUS RADIO SPECTRA STUDY WITH
RATAN--600 IN 1997--2006 SUPPLEMENTED BY VLBA
EXPERIMENTS
Yu.A. Kovalev 1 , Y.Y. Kovalev 1,2 , G.V. Zhekanis 3 , N.A. Nizhelsky 3
1 Astro Space Center of Lebedev Physical Institute,
Profsoyuznya 84/32, 117997 Moscow, Russia
2 MaxíPlanck Institute fØur Radioastronomie,
Auf dem HØugel 69, 53121 Bonn, Germany
3 Special Astrophysical Observatory of RAS,
Nizhnij Arkhyz, 369167 Russia
ykovalev@avunda.asc.rssi.ru
We present results of observations of 1--22 GHz instantaneous continuum spectra of about
3000 active galactic nuclei performed in 1997--2006 with the 600 meter ring transit radio
telescope RATAN--600. An analysis of types and structure of the measured instantaneous
spectra has lead us to a conclusion that almost all spectra could be modeled as a sum of two
main spectral components: LFícomponent (decreasing with frequency) and HFícomponent
(with a maximum in cmímm band). In the framework of a model with longitudinal magnetic
field, the HFícomponent is explained by synchrotron radiation of a continuous compact
relativistic jet emerging from the nucleus, the LFícomponent --- by radiation of optically
thin extended peripheral structures which accumulate jet particles. Long term variability
is studied in about 600 AGNs. It is dominated in the same model by the variable emission
of a compact jet (HFícomponent) and is explained by variable flow of relativistic particles
injected in the jet base. We also apply another model, a standard homogeneous blob of
relativistic particles with synchrotron selfíabsorption, for sources with simple parsec scale
structure and peaked spectral shape. 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 model with longitudinal magnetic field.
PLANCK --- UNLOCKING THE SECRETS OF THE
UNIVERSE
A. LØahteenmØaki 1 , M. Tornikoski 1 , J. Aatrokoski 1 , E. Valtaoja 2
1 MetsØahovi Radio Observatory, Helsinki University of Technology
MetsØahovintie 114, 02540 KylmØalØa, Finland
alien@kurp.tkk.fi
2 Tuorla Observatory, University of Turku, Finland
The Planck satellite is a European Space Agency ESA's mission capable of mapping the
whole sky at several radio wavelengths. The ultimate purpose 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 be measured, too. The byí
products of the CMB map cleaning process, the foreground source maps, will become useful
25

scientific results in themselves. Hence the task is twoífold. First, to provide the cosmologists
with tools for cleaning the CMB maps, and second, to extract scientific information out of
the high radio frequency allísky foreground source catalogs.
One of the most important goals of our Planck project is the acquisition of complete sky
surveys at several high radio frequencies ---an unprecedented event that should solve at least
some of the open 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 processes at work are not yet well understood. AGNs emit at all electromagnetic
frequencies from the radio to the gammaíray region, and all these frequencies are connected,
each frequency adding to the complete picture. The future of the AGN research is in multií
frequency studies performed with sophisticated groundíbased and spaceíborne instruments
or instrument networks, and Planck will be a significant contributor to this work.
The MetsØahovi and Tuorla Planck team has developed a special software called the
Quick Detection System (QDS), that will be used for detecting strong, possibly flaring,
radio sources in the timeíordered data stream of the Planck satellite within one week from
the time of observation. This is essential for followíup observations since the actual data
product of the satellite will not be available until after two years after the mission has
started, and even the Early Release Compact Source Catalog (ERCSC) will be available
only approximately nine months after the first full sky observation cycle has been completed.
The QDS will give us a unique opportunity to get our hands on the Planck foreground data
months before anybody else, to trigger virtually simultaneous followíup observations of
interesting events, and also help monitor the quality of the satellite data at an early stage.
QDS will be operated in the Planck Low Frequency Instrument (LFI) Data Processing
Centre (DPC) in Trieste, Italy, by our team. The launch date of the Planck satellite is
currently set for early 2008, and the operation of the QDS will start as soon as the test
period of the satellite has been completed.
In this paper we describe the Planck mission; the instruments and the science it has
been designed to study. A special emphasis will be made on the Finnish participation in
the project. This includes, for example, the 70 GHz receivers that were designed and build
in Finland, and many aspects of the science we are currently involved in.
POLARIZATION OBSERVATIONS OF mCVs
H.J.Lehto, S.Katajainen
Tuorla Observatory and Department of Physics
FINí21400 University of Turku
hlehto@utu.fi
We have observed magnetic variable stars in polarized 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. Mingaliev 1 , M.G. Larionov 2 , J.V. Sotnikova 1 , N.N. Bursov 1 , N.S. Kardashev 2
1 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia;
2 Astro Space Center, Lebedev Physical Institute of RAS, Moscow, Russia
marat@sao.ru
The RATANí600 radio telescope was used to study spectral properties 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 spectra of radio sources with the purpose to
select objects with inverted spectra near the 22 GHz frequency for subsequent investigation
under the space VLBI Project ``RadioAstron''. The high angular resolution of the project
``RadioAstron'' which is to be achieved 10 -6 arcsec imposes strict demands to angular
dimension of sources. These must be superícompact objects with a high value of the
correlated flux. Such objects form a considerable part of objects just with inverse and
flat spectra. At present there are no complete highífrequency catalogues of such objects
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 important to obtain spectral
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. 00 h
# RA2000 # 24 h
2. +75 o
# DEC2000 # +88 o
3. Flux density: S # [1.4GHz] # 200 mJy from the NVSS catalog
The total number of sources is 504. After data reduction we obtained flux densities of
sources and their spectral characteristics. The sources spectral types were determined: 65%
-- normal, 24% -- steep, 7.3% -- flat, 2.3% -- inverted, and 1.4% -- spectra with a maximum
at centimeter wavelengths (GPS). Eleven sources with inverted spectra were detected. The
statistics of the sources spectra from our sample contrasts with spectral characteristics of
the sample of objects 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 spectra in our sample. This can be explained by the spectral properties 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., Hancock P.J., Jackson C. A., Kesteven
M.J., Murphy T., Phillips Ch., Reinfrank R. F., StaveleyíSmith L., Subrahmanyan R.,
Walker M. A., Wilson W.E., de Zotti, G.: MNRAS, 371, 898.
27

ON THE THEORY OF RESONANT TRANSITIVE
RADIATION OF DECIMETRIC RADIATION OF FLARES
E.V. Modin, L.V. Yasnov
SaintíPetersburg State University
198904 SaintíPetersburg, St. Peterhof, Ul'anovskaya street 1, Russia
Modin.Egor@gmail.com
In this work a mechanism of resonant transitive radiation (RTR) with reference to its posí
sible application for interpretation of decimetric radio emission of solar flares is analyzed.
Such radiation depends on a number of parameters of the radiating media. In particular, on
the parameter of spectrum of smallíscale inhomogeneity of electronic density, #. Platonov
& Fleishman (2002) derived the formulas for factors RTR in dependence on the frequency
of radiation for # = 2. On the whole these formulas describe the behavior 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 developed by Platonov & Fleishman (2002),
factors of RTR for an arbitrary parameter have been obtained. These factors, in particuí
lar, did not give negative and infinite values. On their basis the RTR factors integrated
on frequency have been obtained. These factors were used for the analysis of decimetric
radiation of the flare on December 24, 1991. It has been shown, that the RTR of this flare
could originate in plasma with smallíscale inhomogeneities with ##N 2
#
N 2
= 2.5 § 10 -5 .
References
Platonov K.Yu., Fleishman G.D.: UFN, 2002, 172, 3, 241.
SPECTRAL ENERGY DISTRIBUTIONS AND 37 GHz
MONITORING OF BL LACERTAE OBJECTS
E. Nieppola 1 , M. Tornikoski 1 , A. LØahteenmØaki 1 , E. Valtaoja 2
1 MetsØahovi Radio Observatory
MetsØahovintie 114, 02540 KylmØalØa, Finland
2 Tuorla Observatory
VØaisØalØantie 20, 21500 PiikkiØo, Finland
eni@kurp.hut.fi
BL Lacertae objects (BL Lacs) are a group of active galactic nuclei (AGN) characterized by
strong and rapid variability, strong optical polarization and a lack of prominent emission
lines in their spectra. We have determined spectral energy distributions (SED) for over 300
of these objects using archival multiífrequency data and fitted a parabolic function to the
synchrotron component of the SED (Nieppola et al. 2006). The peak frequencies of the
synchrotron components range between log # peak = 12.67--21.46. We divided the sample into
lowíenergy (LBLs), intermediate energy (IBLs) and highíenergy (HBLs) BL Lacs according
to their log # peak . The correlation between log # peak and the luminosity at # peak was not
significant, in contradiction with the ``blazar sequence'' scenario (Fossati et al. 1998). We
also report a summary of the first 3.5 years of observations with the extensive BL Lac
28

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, being intrinsically more luminous at radio wavelengths than HBLs.
Acknowledgements. The authors made use of the database CATS (Verkhodanov et al.
1997) of the Special Astrophysical Observatory.
References
Fossati, G., Maraschi, L., Celotti, A., Comastri, A. and Ghisellini, G.: MNRAS, 1998, 299,
433.
Nieppola, E., Tornikoski, M. and Valtaoja E.: A&A, 2006, 445, 441.
Verkhodanov, O.V., Trushkin, S.A., Andernach, H. and Chernenkov, V.N.: ASPC, 1997,
125, 322.
DEEP SKY SURVEYS WITH RATANí600
Yu.N. Parijskij
Special Astrophisical Observatory of RAS
Nizhnij Arkhyz, 369167, Russia
par@sao.ru
Blind Sky surveys with RATANí600 were suggested by the general PROJECT of AVP
(1968). A Flat mirror was included into the main CIRCLE structure to carry out quick allí
sky survey, as successfully was made with the Kraus telescope of Ohio University. In 1960th
the Sky seemed to be filled by first generation young objects with inverted and SSA specí
tra, which were missing in the meters wavelengths catalogs. The Sternberg Astronomical
Institute of the Moscow State University group have surveyed the sky zone DEC:0í14deg
with subíJy sensitivity at the 2í8 cm wavelength and the first big (8500) list of objects
detected at 4 GHz objects was published just before the famous 87GB catalog appeared
(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 1975í1976 with subímK sensitivity, but only results
interesting for CMB people were published, and they reject all available in 70íth variants
of the theories of galaxies formation. The second epoch of deep blind surveys started after
installation of the world best cryoíreceiver at 7.6 cm (with #2mK/s 1/2 sensitivity). The
first 17 Feb. 1980 24hí drift scan demonstrated that about 200 details may be found on
this record and may be classified as radio sources, and we integrated point sources (PS)
and CMB anisotropy tasks in the experiment. Several regions were selected for deep surí
veys, 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 proposed ways to suppress this
noise using specific shape of the RATANí600 beam. It helps us to reach the few mJy level
at cm wavelengths and much below by P(D) analysis. The multiífrequency mode of obserí
vations, important for SCREENS (foregrounds) cleaning in the CMB experiments, turned
out to be useful for a spectral classification of the PS appearing 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 experiments, including the PLANCK mission. The problem with PS objects at
CMB frequencies connects with an absolutely unknown Source Population (between IRAS
and NVSS, or GB). At RATANí600 we try to use SELF CLEANING mode, using much
higher resolution than required by CMB physics (subídegree scales). A huge amount of
data collected during the CMB experiments should be used by PS people. I shall present
the positive and negative experience, connected with the international BIG TRIO program,
and problems with detection of a new population at cm wavelengths. The present state of
RATANí600 ``Cold'' and RATANí600 Zenith Field (RZF) blind surveys will be mentioned,
as well as the presentíday situation with High Frequencies Sky Surveys. This presentation
describes results of several groups in SAO and in SPbíbranch of SAO, and now is partially
supported by the RFBR grant 05í02í17521, OF RAS, SPb Center of RAS.
MULTIíFREQUENCY OBSERVATIONS OF THE POLAR
RADIO STRUCTURES
A. Riehokainen 1 , A.G. Tlatov 2
1 Tuorla Observatory 21500, Piikkio, Finland;
2 Pulkovo Astronomical Observatory, St. Petersburg, Russia
alerie@utu.fi
In this work we present a comparison of the enhanced temperature regions (ETRs) in the
radio emission of the Sun with other manifestations of solar polar structures over some
days in 2003í2005. The radio observations at 37 GHz were made with the Metsahovi
Radio Telescope (Finland). We compared our radio data with di#erent SOHO/EIT and
SOHO/MDI images for the same periods. We also superposed the intensity contours of
the fullíradio maps obtained in Metsahovi on the Meudon Spectroheliograph CaII(k3) and
H(alpha) images. We tried to find di#erence between ETRs inside and outside of coronal
holes. We find that the ETRs are clearly connected to brightness structures seen in the
CaII(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. Soboleva, A.V. Temirova, N.N. Bursov, Yu.K. Zverev
Special astrophysical observatory of RAS, SaintíPetersburg, 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 RATANí600 telescope at 2.7 and 7.6 cm wavelength in
1987í2000 are discussed. About 600 objects 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
be identified with NVSS objects. It cannot be ruled out that some of these are sources with
inverted spectra. At both wavelengths there is a fairly large number of Gaussian profiles
30

which are not identified with NVSS objects (106 at 2.7 cm and 43 at 7.6 cm); it is quite
possible that not all of these cases are false.
The survey objects are crossíidentified with sources in the NVSS catalog and the corí
responding twoífrequency spectral indices determined. We find a decrease in the mean
spectral index in the transition from objects with flux densities S 21 # 30 mJy to those with
15 < S 21 < 30mJy. The constructed log N - log S relation at 2.7 cm has a slope of 3/2 at
flux densities # 300 mJy and flattens at weaker flux densities. The 1.4 GHz (NVSS), 3.94
GHz (RATANí600), and 11.11 GHz (RATANí600) data are used to estimate the number
of objects per square degree at a wavelength of 1 cm.
REVERSAL BACKGROUND MAGNETIC FIELD IN THE
SOLAR POLARIZED RADIO EMISSION AT 17 GHz
A.G. Tlatov 1 , A. Riehokainen 2
1 Kislovodsk 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 Nobeyama radio helií
ograph observations during 1992í2006. The latitudeítime diagrams of polarization circular
radio emission were constructed. To decrease the noises we used several solar images for a
day. We found drifts of radio emission polarization in the highílatitudes activity and in the
latitude band of sunspots. Process of the magnetic field reversal of the largeíscale magnetic
field in polarization of radio emission of the Sun was found during 22í23 cycles. An analysis
of polarization for structures of various brightness temperatures has been carried out.
OSCILLATION OF THE POLARIZED RADIO EMISSION
``THE SUN AS A STAR''
A.G. Tlatov 1 , A. Riehokainen 2
1 Kislovodsk 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 Nobeyama radio heliograph in 1992í2006. For this purpose the
daily data of the intensity and also right/left circular polarization of the radio emission with
oneísecond average were processed. It was found that 3 minutes oscillations are present
at the di#erent phases of solar activity, including the minimum of activity. Especially
conspicuous these oscillations present in a di#erence between the right and the left circular
polarization. Intensity of the oscillations changes with a level of the solar activity. Spectral
analysis of the presence of 3íminute oscillations in polarization of the solar radio emission
shows that there exist a modulation with the periods of 27 and 157 days. During the
31

minimum activity the main periods of the 3 minutes oscillations are slightly shorter than
during the maximum activity.
RADIO SPECTRA OF GPS GALAXIES
I. Torniainen 1 , M. Tornikoski 1 , M. Aller 2 , H. Aller 2 , M. Mingaliev 3
1 MetsØahovi Radio Observatory, Helsinki University of Technology
MetsØahovintie 114, FINí02540 KylmØalØa, Finland
2 Department of Astronomy, University of Michigan
3 Special Astrophysical Observatory of RAS
ilo@kurp.hut.fi
Gigahertzípeaked spectrum (GPS) sources are active galactic nuclei which are characterized
by a convex radio continuum spectrum peaking at the GHzífrequencies. Their nature is
still unclear, but currently the strongest scenario suggests that at least some of them are
newborn radio sources in which the activity has been triggered on only 100 -- 1000 years
ago. There are both quasar and galaxy type GPS sources, which have a similar shape of
spectrum but the nature and the physics of sources are thought to be di#erent. Our earlier
study (Torniainen et al. 2005) showed that a considerable proportion of quasarítype GPS
sources are more likely misidentified flatíspectrum quasars -- not GPS sources at all.
We have collected 96 GPS galaxies from the literature, observed them and collected all
possible radio data for them to study how pure the galaxy type GPS samples are. Our
sample includes both frequently monitored sources and sources with only a few detections.
The spectra 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 spectrum but high variability and the rest
had steep or flat spectrum. 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
be classified as GPS sources.
Di#erence between the quasar and galaxy samples can partly be explained by selection
e#ects: the quasar sample was selected from the MetsØahovi monitoring sample which has
been monitored over 25 years whereas the galaxy sample was gathered from the GPS
literature and included both weak or rarely observed sources and more frequently monitored
sources.
Acknowledgements. The authors made use of the database CATS (Verkhodanov et al.
1997) of the Special Astrophysical Observatory.
References
Torniainen I., Tornikoski M., TerØasranta H., Aller M.F., Aller H.D.: A&A, 2005, 435, 839.
Verkhodanov O.V., Trushkin S.A., Andernach H., Chernenkov V.N.: ASP Conference Seí
ries, 1997, 125, 322.
32

METS Ø
AHOVI AGN PROJECTS CONTRIBUTING TO THE
PLANCK FOREGROUND SCIENCE
M. Tornikoski 1 , A. LØahteenmØaki 1 , T. Hovatta 1 , E. Nieppola 1 , I. Torniainen 1 , E. Valtaoja 2
1 Helsinki University of Technology, MetsØahovi Radio Observatory
MetsØahovintie 114, 02540--KylmØalØa, Finland
2 Tuorla Observatory, University of Turku, Finland
merja.tornikoski@tkk.fi
During recent years we have had a special focus in our MetsØahovi observing projects. We
have put an emphasis on the understanding of AGNs that could contribute to the extraí
galactic foreground that will be detectable by the Planck satellite.
First of all, we have observed completely new source samples. Many AGN samples have
been excluded from highífrequency radio observations earlier simply because they were
assumed to be too faint or ``uninteresting''. One of our largest new source samples was the
complete BL Lacertae Object (BLO) sample.
In addition to the fewíepoch observations of large source samples we have been interested
in the longíterm variability behaviour of a densely monitored set of sources. We have
analysed these data in order to improve our understanding of the variability behaviour of
these sources: how often do flares typically occur 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 epoch?
We are also working our way towards predicting, or at least making ``educated guesses''
about, the activity behaviour of radioíbright 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
Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia
satr@@sao.ru
We continued studies of the WMAPísources after publishing results of three years (Hinshaw
et al.; Jarosik et al.; Page et al.; Spergel et al. 2006). Trushkin (2003) presented compiled
radio spectra of 205 extragalactic sources from the catalog, compiled from the WMAP
survey data at 23í94 GHz in the first year of its operation.
We have shown that 205 WMAPísources are reliably identified with radio sources from
known catalogs (FIRST, NVSS and so on). #50% of the sources have flat or inverted
spectra, #15% -- spectra with the peaks at 5í20 GHz (GPSísources), #10% -- powerílaw
spectra and #10% -- show the composite spectra (as 3C84).
We discussed recent results of the radio observations of the AGNs from the WMAP
catalog with the RATANí600 and RT32 telescopes.
Now the final 3íyear 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 spectra plotting procedures in our CATS data base (Verkhodanov et al. 1997)
we have found optical and radio identifications for the most of new 120 WMAPísources
33

from the radio and optical catalogs in the CATS data base. Now we discuss results for
new 120 sources, their spectra and features. The statistics for types of the sources did not
generally changed. We have found that 313 WMAPísources have optical counterparts: 220
-- quasars, 30 -- galaxies, 32 -- AGNs, 30 -- BL Lac objects and one -- the planetary nebula
IC418. We have observed some of the new WMAPísources 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 expected, 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
e#ective time scale about one year, (3yrí1yr)/2 in the WMAP3ícatalog.
Using an analogous method of the source selection from the CATS data base we have
found that a probable number of the sources brighter 400 mJy at 23 GHz is equal to 1300í
1500 on the sky. Thus there is a strong e#ect of confusion dramatically decreasing the
number (323) of detected sources in the WMAP survey.
We hope that such studies will help in the future PLANCK CMBíexperiment dataí
precessing.
Acknowledgements. We are thankful to RFBR for support, the grant N05í02í17556.
References
Hinshaw G. et al.: astroíph/0603451.
Jarosik N. et al.: astroíph/0603452.
Page L. et al.: astroíph/0603450.
Spergel D.N. et al.: astroíph/0603449.
Trushkin S.A.: Bulletin of SAO RAS, 2003, 55, 90.
Verkhodanov O.V., Trushkin S.A., Andernach H., Chernenkov V.N.: ASP Conference Seí
ries, 1997, 125, 322.
RECENT DATA OF THE MULTIíFREQUENCY
MONITORING OF MICROQUASARS
S.A. Trushkin
Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia
satr@sao.ru
We discuss results of recent radio observations of the microquasars SS433, GRS1915+105
and Cyg Xí3 with the RATANí600 and RT32 (IAA) radio telescopes.
We have carried out long monitoring programs of daily observations sets for microí
quasars with the RATAN radio telescope 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 2í200. The flarí
ing synchrotron emission indicates the jets formation, coupling with accretion disk activity
in the Galactic microquasars and in the active galactic nuclei (AGN). The multiífrequency
light curves are compared with the XTE ASM data at 2í12 keV to study correlations during
the flares. Indeed in many cases such correlations were detected.
Radio flaring events of SS433, Cyg Xí3, 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

spectra of flaring events in the active states of GRS1915+105, Cyg Xí3 and V4641 Sgr with
the spectral indices # >+1 at # >1 GHz.
We have detected a clear Xíray/radio association in light curves of GRS 1915+105
during OctoberíNovember 2005, when it was very active (0.5í3 Crabs at 2í12 keV).
After 18 days of the quenched state (#10 mJy) Cyg Xí3 exhibited the 1Jyí radio flare
on 1 Feb 2006. Such a remarkable property -- before a flare the radio emission fall down in
deep (local) minimum of fluxes -- is probably a general feature of the radio/Xíray binaries.
The flare of 1 Feb was also detected with the Nobeyama 45m and NMA telescopes
(Tsuboi et al. 2006), and for the first time a flat radio spectrum of the flaring event from
Cyg Xí3 was directly measured in the quasiísimultaneous 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 respectively. The very fast rising flare, from 1 to
2 Jy during 3 hours, was detected with the RT32 telescope (Trushkin et al. 2006) on 05
June. At last on 25 July we have detected a very powerful flare (15 Jy) from Cyg Xí3 again.
All these flares happened during a long period (Feb 1 -- Aug 1) when Xíray emission was
relatively high (#0.3 crabs), variable and hard.
We studied evolution of the powerful flares from the optically thick state to the optically
thin one at the lower frequencies. We have to draw an unexpected 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.
Acknowledgements. This research was supported by the Russian Foundation of Basic
Research grant N 05í02í17556 and by the Program of the Presidium of Russian Academy
of Science.
References
Tsuboi M. et al. : ATel, 2006, #729.
Trushkin S.A. et al.: ATel, 2006, #828.
THE PROBLEM OF HIGHíENERGY EMISSION FROM AGN
Esko Valtaoja
Tuorla Observatory, University of Turku, FIí21500 Piikkio, Finland
esko.valtaoja@utu.fi
The basic framework for radioíbright AGNs, which are also the only types of extragalactic
sources known to emit a significant amount of highíenergy radiation, is a relativistic jet with
shocks embedded in it. Presumably, the most significant intrinsic properties of the source
are then the absolute luminosity of the jet/shocks, the flow speed (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 opening angle and curvature, duty cycle of the shock activity, etc.)
as well as the jet surroundings (in particular, density of the ambient photon field) must
also play a role.
The spectral energy distributions of radioíbright AGN, often called blazars, can be approxí
imated by two parabolas. The first one is caused by synchrotron radiation from the jet
35

and from the shocks, the second one by an inverse Compton radiation from the relativistic
electrons in the jet, upscattering ambient photons into XítoíTeV energies.
Both theoretically and observationally, our understanding of the blazar emission remains
rather poor. I discuss some new attempts to model the spectral energy distributions of
blazars, focusing on correlations between various observed and intrinsic properties, and on
the problems of the proposed theoretical models for the highíenergy emission.
OPEN WEBíRESOURCES OF SAO RAS FOR
EXTRAGALACTIC RESEARCH
O.V. Verkhodanov 1 , S.A. Trushkin 1 , A.I. Kopylov 1 , V.N. Chernenkov 1 , H. Andernach 2 ,
N.V. Verkhodanova 1 , V.K. Kononov 1
1 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia
2 Departamento de AstronomÒÐa, Universidad de Guanajuato, Mexico
vo@sao.ru
The sky survey at various wavelength bands is one of the most important branches of
the modern observational astrophysics. To the present moment, several data bases unify
resulting data of such surveys. We consider here Webíresources designed for radio astroí
nomical and extragalactic study and operating in the Special Astrophysical Observatory.
We describe structure, operation, standard tasks and the current status of the largest data
bases in respective astrophysics fields. They are the data base of radio astronomical and
astrophysical catalogs CATS (http://cats.sao.ru) (Verkhodanov et al. 1997, 2005) and
the SED (Verkhodanov et al. 2000) which is an analysis system of spectral energy disí
tribution (http://sed.sao.ru). These servers were unified in a one cluster and are used
both 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
above 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 corresponding files with a #m coe#cients of spherical harmonics. We
plan to unify all three servers into one cluster for acceleration of investigation in the field
of cosmology and astrophysics.
Acknowledgements. This work is supported particularly by the Russian Foundation of
Basic Research (grant No 05í07í90139).
References
Doroshkevich A.G., Naselsky P.D., Verkhodanov O.V., Novikov D.I., Turchaninov V.I.,
Novikov I.D., Christensen P.R., Chiang L.íY.: Internat. J. Mod. Phys. D, 2005, 14, 275
(astroíph/0305537)
Verkhodanov 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 (astroíph/9610262)
Verkhodanov O.V., Kopylov A.I., Zhelenkova O.P., Verkhodanova N.V., Chernenkov V.N.,
Parijskij Yu.N., Soboleva N.S., Temirova A.V.: The software system ``Evolution of radio
galaxies''. Atsron. Astrophys. Trans., 2000, 19, 662, (astroíph/9912359)
36

Verkhodanov O.V., Trushkin S.A., Andernach H., Chernenkov V.N.: Bulletin of SAO of
RAS, 2005, 58, 118
PHASE ANALYSIS IN STUDY OF COSMIC MICROWAVE
BACKGROUND
O.V.Verkhodanov 1 , P.D.Naselsky 2 , L.íY.Chiang 2 , A.G.Doroshkevich 3 , I.D.Novikov 3,2
1 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, Russia
2 Niels Bohr Institute, Copenhagen, 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 important method of observational cosmology. We consider
several aspects of phase analysis in the CMB study. They concern the problems of signal
restoration (Naselsky et al. 2005), search for noníGaussianity (Chiang et al. 2003) and
study of the foreground contamination of this separated CMB signal (Naseslky et al. 2003,
2004, 2005). Using the GLESP (GaussíLEgendre Sky Pixelization) package (Doroshkevich
et al. 2005) for CMB analysis we produce phase data for spherical harmonics in the form
of a #m = |# #m | exp(i# #m ), where a #m ís are coe#cients of spherical harmonics of the #--
multipole in the m--mode, |# #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 corresponding to these properties at low # (# # 100) where the point
source influence is minimal. Another important moment is the study of the Gaussianity
problem in the CMB observational data. To check statistical properties of the data we
produce phase diagrams. These diagrams demonstrate the strong noníGaussianity for all
accessible maps of CMB. The high phase correlations between CMB and foregrounds hint
us about problems of signal separation. Similar approaches are developed for the Planck
mission.
Acknowledgements. This work is supported particularly by the Russian Foundation of
Basic Research (grants No 05í07í90139 and 05í02í16302).
References
Chiang L.íY., Naselsky P.D., Verkhodanov O.V., Way M.J.'' Astrophys. J., 2003, 590, L65
(astroíph/0303643)
Naselsky P.D., Doroshkevich A.G. , Verkhodanov O.V.: Astrophys. J., 2003, 599, L53
(astroíph/0310542)
Naselsky P.D., Doroshkevich A.G., Verkhodanov O.V.: MNRAS, 2004, 349, 695 (astroí
ph/0310601)
Naselsky P.D., Chiang L.íY., Novikov I.D., Verkhodanov O.V.: Internat. J. Mod. Phys.
D, 2005, 14, 1273 (astroíph/0405523)
Doroshkevich A.G., Naselsky P.D., Verkhodanov O.V., Novikov D.I., Turchaninov V.I.,
Novikov I.D., Christensen P.R., Chiang L.íY.: Internat. J. Mod. Phys. D, 2005, 14, 275
(astroíph/0305537)
37

THE COMBINED RADIO AND OPTICAL INVESTIGATIONS
OF THE INTRADAY VARIABILITY OF ACTIVE GALACTIC
NUCLEI
A.E. Volvach 1 , V.S. Bychkova 2 , N.S. Kardashev 2 ,
M.G. Larionov 2 , V.V. Vlasyuk 3 , O.I. Spiridonova 3
1 SRI Crimean Astrophysical Observatory, Ukraine,
2 Astro Space Centre of the Lebedev Physical Institute, Russia
3 Special Astrophysical Observatory of the Academy Science, Russia
volvach@crao.crimea.ua
The combined radio and optical observations of the active galactic nuclei 0133+476, 1633+382,
2145+067, 2251+158 were performed in 2004í2006. The aim of analysis was to detect an
intraday flux variability and to search for its possible correlation in radio and optical waveí
lengths. Observations were conducted with the use of the RTí22 radio telescope (SRI
CrAO) at 22 and 36 GHz and the 1ím Zeissí1000 reflector of SAO RAS with CCD camera.
During observations we found no significant fluctuations of fluxes at both ranges. At
the level of 10% from the average amplitude more high activity of the object 1633+382
was detected at 36 GHz in May 2004 then the one in May 2005. The reason of it may
be a passive phase of the object after the burst in 2002. The observable flux variation in
0133+476 at the time scale of one hour were noticed in October 2005 but not optical range.
Such flux behaviour may indicate to absence of the identical area for radio and optical
emission after matter collimation in the black hole polar 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 Novgorod 603950, Russia
zin@appl.sciínnov.ru
In recent years we surveyed several tens of high mass star forming regions in various molecí
ular lines and in millimeter wave continuum. Basic physical properties of detected clumps
and molecular abundances were derived. One of the problems is a selection of the best 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 good
tracer of the total mass while the N 2 H + distribution is frequently very di#erent. This is
opposite to their typical behavior in lowímass cores where a freezeíout plays a crucial role in
the chemistry. The behavior 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 power
laws with indices about -1.6, as derived from the dust continuum emission. The radial
38

temperature dependence on intermediate scales is close to the theoretically expected one
for a centrally heated optically thin cloud. The velocity dispersion either remains constant
or decreases from the core center to the edge. Several cores including those without known
embedded IR sources show signs of infall motions. They can represent the earliest phases
of massive protostars. There are implicit arguments in favor of smallíscale clumpiness in
the cores.
Acknowledgements. The work was supported by the Russian Foundation for Basic Reí
search grant 06í02í16317 and by the Program ``Extended objects in the Universe'' of the
Russian Academy of Sciences.
39

Author's index
Aatrokoski J. 25
AbramovíMaksimov 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
Bochkarev N.G. 9,12
Bogod 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.íY. 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
Golubchina 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
IliÒc D. 12
Kaltman T.I. 11,22,23
Kardashev N.S. 38
Katajainen 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

LØahteenmØaki A. 25,28,33
Lainela M. 21
Larionov M.G. 27
Lehto H.J. 26
Lobanov A.P. 9
Majorova E.K. 14
Mikhailov A. 21
Mingaliev M. 14,19,27,32
Modin E.V. 28
Naselsky P.D. 37
Nieppola E. 28
Nizhelskij N.A. 14,25
Novikov I.D. 37
Parijskij Y.N. 29
PopoviÒc L. 12
Riehokainen A. 30,31,31
Semenova T.A. 14
Sergeev S.G. 15
Shapovalova A.I. 9,12
Soboleva 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
Valtaoja E. 21,25,28,35
Venger A.P. 20
Verkhodanova N.V. 36
Verkhodanov 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
41