J/MNRAS/462/2747 S4 1030+61 VLBA observations, 2009-2014 (Kravchenko+, 2016)
Multiwavelength observations of the γ-ray flaring quasar
S4 1030+61 in 2009-2014.
Kravchenko E.V., Kovalev Y.Y., Hovatta T., Ramakrishnan V.
<Mon. Not. R. Astron. Soc., 462, 2747-2761 (2016)>
=2016MNRAS.462.2747K 2016MNRAS.462.2747K (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Radio sources ; Gamma rays
Keywords: galaxies: active - galaxies: jets - quasars: general -
quasars: individual: S4 1030+61
Abstract:
We present a study of the parsec-scale multifrequency properties of
the quasar S4 1030+61 during a prolonged radio and γ-ray
activity. Observations were performed within Fermi γ-ray
telescope, Owens Valley Radio Observatory 40-m telescope and MOJAVE
Very Long Baseline Array (VLBA) monitoring programmes, covering five
years from 2009. The data are supplemented by four-epoch VLBA
observations at 5, 8, 15, 24 and 43GHz, which were triggered by the
bright γ-ray flare, registered in the quasar in 2010. The S4
1030+61 jet exhibits an apparent superluminal velocity of (6.4±0.4)c
and does not show ejections of new components in the observed period,
while decomposition of the radio light curve reveals nine prominent
flares. The measured variability parameters of the source show values
typical for Fermi-detected quasars. Combined analysis of radio and
γ-ray emission implies a spatial separation between emitting
regions at these bands of about 12pc and locates the γ-ray
emission within a parsec from the central engine. We detected changes
in the value and direction of the linear polarization and the Faraday
rotation measure. The value of the intrinsic brightness temperature of
the core is above the equipartition state, while its value as a
function of distance from the core is well approximated by the power
law. Altogether these results show that the radio flaring activity of
the quasar is accompanied by injection of relativistic particles and
energy losses at the jet base, while S4 1030+61 has a stable, straight
jet well described by standard conical jet theories.
Description:
The source S4 1030+61 was observed (code S2087E) with the VLBA of the
National Radio Astronomy Observatory (NRAO) during four sessions:
2010-05-24, 2010-07-09, 2010-08-28 and 2010-10-18 (noted as 'epochs'
below).
We supplemented our analysis with the data obtained within the MOJAVE
programme. Observations are done at 15.4GHz with VLBA at 10 epochs:
2009-06-25, 2009-12-26, 2010-12-24, 2011-04-11, 2011-05-26,
2011-07-15, 2012-01-02, 2012-03-27, 2012-11-11 and 2013-07-08.
Public data (http://www.astro.caltech.edu/ovroblazars/) of S4 1030+61
observations within the OVRO 40-m Telescope monitoring programme
were used in the analysis. Observations are done at 15GHz in a 3GHz
bandwidth from 2008-06-20 to 2014-01-21 about twice per week.
The γ-ray fluxes in the range 0.1-200GeV were obtained with
the LAT onboard the space Fermi γ-ray observatory from
2008-08-04 to 2014-02-23.
Objects:
----------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------
10 33 51.43 +60 51 07.3 S4 1030+61 = OHIO L 651
----------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 12 20 VLBA central frequencies
table2.dat 27 18 Amplitude corrections for the S2087E VLBA
experiment
table3.dat 69 158 Results of Gaussian model fitting and component
parameters at 4.6-43.2 GHz
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Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Band IEEE band
4 I1 --- IF [1/4] Number of the frequency channel
6- 12 F7.1 MHz Freq Frequency
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Ant Antenna name
4- 5 A2 --- Band Radio band name
7- 9 A3 --- Epoch Observation epoch (1)
11- 13 A3 --- IF Number of the frequency channel
15- 22 A8 --- Pol Polarization (right of left circular)
24- 27 F4.2 --- Corr Amplitude correction coefficient
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Note (1): Epochs are labeled as follows:
1 = 2010-05-24
2 = 2010-07-09
3 = 2010-08-28
4 = 2010-10-18
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.1 GHz Freq Frequency
6- 15 A10 "date" Date Observation date
17- 20 A4 --- Name Name of the component
("U" stands for unclassified components)
22- 27 F6.4 Jy S Integrated flux density in the component
29- 34 F6.4 Jy e_S rms uncertainty on S
36- 40 F5.3 mas Dist Radial distance of the component center
from the center of the map
42- 46 F5.3 mas e_Dist rms uncertainty on Dist
48- 53 F6.1 deg PA [] Position angle of the component relative to
the map center
55- 59 F5.3 mag amaj FWHM major axis of the fitted Gaussian
61- 63 F3.1 --- Ratio Axial ratio of major and minor axes of
fitted Gaussian
65- 69 F5.1 deg PAmaj ?=- Major axis position angle of
fitted Gaussian
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Feb-2018