Title: The multiwavelength polarization VLBI
1EVN 8th Symposium 26 29 September, 2006 Torun,
Poland
The multi-wavelength polarization VLBI
structure of 3 BL Lacertae objects Vladislavs
Bezrukovs, Dr. Denise Gabuzda
University College Cork
Cork Institute of technology
ENIGMA, Irish team
2Introduction
- Kuhr and Schmidt BL Lacerate objects sample
- 1308326
- Intensity and polarization model fitting
- Helical B Field in the jet?
- Polarization rotation in 43 GHz.
- 0828493
- Intensity and polarization model fitting
- Helical B Field in the jet?
- 1803784
- Intensity and polarization model fitting
- Helical B Field in the jet?
- RM gradient in the jet.
3Project background
- My project
- To analyze VLBA data from Kuhr and Schmidt
sample of BL Lac objects gt 1 Jy at 43 GHz, 22 GHz
and 15 GHz (May 2002, August 2002, November 2004)
4Kuhr and Schmidt sample of BL Lac objects
5BL Lac objects properties
- BL Lac objects are active galactic nuclei with
- relatively low-luminosity optical line emission
- in many cases their optical continua are
completely featureless - strong and variable polarization in wavebands
ranging from optical through radio - compact, flat-spectrum radio structure
- point-like optical structure
- the radio emission and much of the optical
emission is believed to be synchrotron radiation.
- the VLBI core polarizations have values ranging
from 2-7 per cent, and occasionally reaching
values as high as 10 per cent. - 6070 per cent of BL Lac objects have jets that
have transverse magnetic fields. At the same
time, a sizeable minority of about 30 per cent
have longitudinal jet magnetic fields. (Gabuzda,
Pushkarev, Cawthorne et el 1999)
61308326(August 2002)
71308326. Model fitting.
- 22 GHz map
- Intensity (mJy)
- 1) 1811.0
- 2) 161.0
- 3) 163.0
- 4) 57.4
- 5) 53.7
- Polarization (mJy)
- and EVPA (deg)
- 1) 57.9 67.08
- 1.5 54.37
- 3) 15.1 -26.23
43 GHz map Intensity (mJy) 1) 1310.0 1b)
230.5 2) 82.8 3) 113.2 Polarization
(mJy) and EVPA (deg) 1) 98.6 33.592
15 GHz map Intensity (mJy) 1) 1510.8 2)
184.1 3) 137.0 4) 148.0 5)
44.9 Polarization (mJy) and EVPA (deg) 1)
57.9 96.578 2) 10.9 63.087 3) 18.5 -5.44
81308326. Model fitting.
91308326. Spectral index maps.
Spectrum in core region positive -gt core
optically thick
Spectrum in core region negative -gt core
optically thin
101308326. Rotation measure.
Why we rotate polarization angle in 43 GHz to 90o?
111308326. Rotation measure.
121308326. November 2002 epoch compare with MOJAVE
data.
15 GHZ Intensity map with polarization sticks
MOJAVE Sample
MOJAVE Sample
130828493(November 2004)
140828493. Model fitting.
43GHz map Intensity (mJy) 1) 114.2 2) 51.5 3)
103 Polarization (mJy) and EVPA (deg) 1) 4.09
89.146
22GHz map Intensity (mJy) 1) 143.6 2) 79.2 3)
100.2 Polarization (mJy) and EVPA (deg) 1) 2.2
80.06 2) 3.2 116.06
15GHz map Intensity (mJy) 1) 153.4 2) 65.9 3)
134.8 Polarization (mJy) and EVPA (deg) 1) 2.3
94.132 2) 2.9 121.132 3) 2.4 7.132
150828493. Model fitting.
160828493. Rotation Measure.
RM made from 15 and 22 GHz.
171803784(May 2002)
181803784. Model fitting.
43 GHz map Intensity (mJy) 1) 1091.0 2)
146.0 3) 173.0 Polarization (mJy) and EVPA
(deg) 1) 37.0 129.65 2) 12.7 76.4
22 GHz map Intensity (mJy) 1) 1688.7 2)
144.5 3) 270.0 Polarization (mJy) and EVPA
(deg) 1) 60.7 132.87 2) 28.6 78.81
15 GHz map Intensity (mJy) 1) 1709.0 2)
174.6 3) 278.4 4) 47.9 Polarization
(mJy) and EVPA (deg) 1) 57.4 139.74 2) 33.9
81.74
191803784. Model fitting.
201803784. May 2002 Epoch compare with MOJAVE
data.
MOJAVE Sample
211803784. Rotation measure.
221803784. Rotation measure.
RM gradient change direction !!!
Zavala and Taylor et. el. 2003 (epoch 2000)
Mehreen Mahmud image (epoch 2003)
23Summary.
- Possibility of Helical magnetic field in these
sources - 1308326 transverse magnetic field in jet
- 0828493 longitudinal polarization in sheath
- 1803784 asymmetric RM distribution across the
jet - 1308326 core changes from optically thick in 15
and 22 GHz to optically thin between 22 and 43
GHz taking into account gives core rotation
measure 3500 rad/m2 - Produced and tested version of VISFIT program in
Linux (intensity and polarization model fitting)
available to all interested.
24Acknowledgements to
Dr. Denise Gabuzda, Radio Astronomy Lab at
UCC, Enigma, Irish Group.