radiopol

physics of extragalactic plasma elements
through high cadence radio polarisation monitoring of blazars
Emmanouil Angelakis1 & Ioannis Myserlis1
A. Kraus1, V. Pavlidou2,3, L. Fuhrmann1, V. Karamanavis1, J. A. Zensus1
1Max-Planck-Institut
fuer Radioastronomie, Auf dem Huegel 69, 53121 Bonn, Germany
for Research and Technology - Hellas, IESL, Voutes, 7110 Heraklion, Greece
3Department of Physics and Institute for Plasma Physics, University of Crete, 71003, Heraklion, Greece
2Foundation
the RadioPol program:
APEX
30 m IRAM
100 m Effelsberg
part of the f-gamma program: ➡ almost
➡ 2.64
90 mostly Fermi sources
- 142 GHz at 10 frequency steps circularly polarized feeds ➡ LP
at 2.64, 4.85, 8.35, 10.45 and 14.6
➡ CP
at 2.64, 4.85, 8.35, 10.45, 14.6, 23.05
➡ mean
cadence 1.3 months
➡ uncertainty
0.1 FPU
Angelakis et al. 2010, astro-ph.CO/1006.5610
Fuhrmann et al. 2007, 2007, AIP Conf. Series, Vol. 921, 249–251
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
the RadioPol program:
2007.0
45
2008.0
2009.0
2010.0
2011.0
2012.0
2013.0
2015.0
2.64 GHz
4.85 GHz
8.35 GHz
10.45 GHz
14.60 GHz
23.05 GHz
32.00 GHz
42.00 GHz
86.00 GHz
142.33 GHz
228.93 GHz
J2253+1608, 3C454.3
40
35
Flux Density (Jy)
2014.0
30
25
20
15
10
5
0
54000.0
54500.0
55000.0
55500.0
56000.0
56500.0
57000.0
MJD
part of the f-gamma program: ➡ almost
➡ 2.64
90 mostly Fermi sources
- 142 GHz at 10 frequency steps circularly polarized feeds ➡ LP
at 2.64, 4.85, 8.35, 10.45 and 14.6
➡ CP
at 2.64, 4.85, 8.35, 10.45, 14.6, 23.05
➡ mean
cadence 1.3 months
➡ uncertainty
0.1 FPU
Angelakis et al. 2010, astro-ph.CO/1006.5610
Fuhrmann et al. 2007, 2007, AIP Conf. Series, Vol. 921, 249–251
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
the RadioPol program:
2007.0
45
2008.0
2009.0
2010.0
2011.0
2012.0
2013.0
2015.0
2.64 GHz
4.85 GHz
8.35 GHz
10.45 GHz
14.60 GHz
23.05 GHz
32.00 GHz
42.00 GHz
86.00 GHz
142.33 GHz
228.93 GHz
J2253+1608, 3C454.3
40
35
Flux Density (Jy)
2014.0
30
25
20
15
10
5
0
54000.0
54500.0
55000.0
55500.0
56000.0
56500.0
57000.0
MJD
part of the f-gamma program: ➡ almost
➡ 2.64
90 mostly Fermi sources
- 142 GHz at 10 frequency steps circularly polarized feeds ➡ LP
at 2.64, 4.85, 8.35, 10.45 and 14.6
➡ CP
at 2.64, 4.85, 8.35, 10.45, 14.6, 23.05
➡ mean
cadence 1.3 months
➡ uncertainty
0.1 FPU
Angelakis et al. 2010, astro-ph.CO/1006.5610
Fuhrmann et al. 2007, 2007, AIP Conf. Series, Vol. 921, 249–251
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
incoherent synchrotron:
intrinsically polarised
credit: S. Kiehlmann
relativistic magnetised plasma laboratories
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
in
Opt
icall
EVPA parallel to
projected B-field
y t
h
EVPA perpendicular
to projected B-field
y th
ick
Op
tic
all
α ≃ —0.7, ml ≃ 72%
α = +2.5, ml≃11%
linear component:
νQ=0.44 νm ➝ τ ≃ 7
circular component:
Pacholczyk Pergamon Press, 1977
νV=0.49 νm ➝ τ ≃ 5
optical depth
EVPA flip
ml → 0
mc → 0
S → Smax
frequency, time
EVPA flip
ml → 0
mc → 0
S → Smax
frequency, time
optical depth
optical depth
M. Turler et al. 2000; Marscher & Gear, 1985ApJ...298..114M
http://www.isdc.unige.ch/~turler/jets/
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
EVPA flip
ml → 0
mc → 0
S → Smax
frequency, time
optical depth
optical depth
M. Turler et al. 2000; Marscher & Gear, 1985ApJ...298..114M
http://www.isdc.unige.ch/~turler/jets/
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
EVPA flip
ml → 0
mc → 0
S → Smax
frequency, time
optical depth
optical depth
M. Turler et al. 2000; Marscher & Gear, 1985ApJ...298..114M
http://www.isdc.unige.ch/~turler/jets/
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
Stokes I
(Jy)
2006.7 2007.3 2007.8 2008.4 2008.9 2009.5 2010.0 2010.6 2011.1 2011.7 2012.2 2012.7 2013.3 2013.8 2014.4 2014.9
30
2.64
25
4.85
20
8.35
15
10.45
14.6
10
15 (MOJ)
5
0
ml (%)
20
15
10
5
0
EVPA (deg)
400
300
optical from Smith et al. 2009, arXiv0912.3621S
200
100
Spectral
index
mc (%)
0
1
0.8
0.6
0.4
0.2
0
-0.2
-0.4
-0.6
-0.8
-1
1
0.5
low
med
0
-0.5
-1
54000
54200
54400
54600
54800
55000
55200
55400
55600
55800
56000
56200
56400
56600
56800
57000
Stokes I
(Jy)
2006.7 2007.3 2007.8 2008.4 2008.9 2009.5 2010.0 2010.6 2011.1 2011.7 2012.2 2012.7 2013.3 2013.8 2014.4 2014.9
30
2.64
25
4.85
20
8.35
15
10.45
14.6
10
15 (MOJ)
5
0
ml (%)
20
15
10
5
0
EVPA (deg)
400
300
optical from Smith et al. 2009, arXiv0912.3621S
200
100
Spectral
index
mc (%)
0
1
0.8
0.6
0.4
0.2
0
-0.2
-0.4
-0.6
-0.8
-1
1
0.5
low
med
0
-0.5
-1
54000
54200
54400
54600
54800
55000
55200
55400
55600
55800
56000
56200
56400
56600
56800
57000
Stokes I
(Jy)
2006.7 2007.3 2007.8 2008.4 2008.9 2009.5 2010.0 2010.6 2011.1 2011.7 2012.2 2012.7 2013.3 2013.8 2014.4 2014.9
30
2.64
25
4.85
20
8.35
15
10.45
14.6
10
15 (MOJ)
5
0
ml (%)
20
THICK → thin
15
thin → THICK
10
5
0
EVPA (deg)
400
300
optical from Smith et al. 2009, arXiv0912.3621S
200
100
Spectral
index
mc (%)
0
1
0.8
0.6
0.4
0.2
0
-0.2
-0.4
-0.6
-0.8
-1
1
0.5
low
med
0
-0.5
-1
54000
54200
54400
54600
54800
55000
55200
55400
55600
55800
56000
56200
56400
56600
56800
57000
Stokes I
(Jy)
2006.7 2007.3 2007.8 2008.4 2008.9 2009.5 2010.0 2010.6 2011.1 2011.7 2012.2 2012.7 2013.3 2013.8 2014.4 2014.9
30
2.64
25
4.85
20
8.35
15
10.45
14.6
10
15 (MOJ)
5
0
ml (%)
20
THICK → thin
thin → THICK
15
thin → THICK
10
5
0
EVPA (deg)
400
300
optical from Smith et al. 2009, arXiv0912.3621S
200
100
Spectral
index
mc (%)
0
1
0.8
0.6
0.4
0.2
0
-0.2
-0.4
-0.6
-0.8
-1
1
0.5
low
med
0
-0.5
-1
54000
54200
54400
54600
54800
55000
55200
55400
55600
55800
56000
56200
56400
56600
56800
57000
Stokes I
(Jy)
2015.7
2006.7 2007.3 2007.8 2008.4 2008.9 2009.5 2010.0 2010.6 2011.1 2011.7 2012.2 2012.7 2013.3 2013.8 2014.4 2014.9
30
2.64
25
4.85
20
8.35
15
OVRO
10.45 (Hovatta)
14.6
10
15 (MOJ)
5
0
ml (%)
20
THICK → thin
thin → THICK
15
→ thin
thin → THICK
10
5
0
EVPA (deg)
400
300
optical from Smith et al. 2009, arXiv0912.3621S
200
100
Spectral
index
mc (%)
0
1
0.8
0.6
0.4
0.2
0
-0.2
-0.4
-0.6
-0.8
-1
1
0.5
low
med
0
-0.5
-1
54000
54200
54400
54600
54800
55000
55200
55400
55600
55800
56000
56200
56400
56600
56800
57000
our setup:
270 d
➡ component
‣
1
adiabatic ~150 d and fast adiabatic
~240 d
600 d
140 d
240 d
➡ components
2: follows the entire
path after 1000 d ➡ quiescent
➡B
of ~0.05 Jy uniformity: =0.2 (20%)
➡ identical
power
is unidirectional for the 2
components at the fiducial angle of
-10o
optical depth
➡ B-field
Myserlis, EA et al. in prep.
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
our setup:
270 d
➡ component
‣
1
adiabatic ~150 d and fast adiabatic
~240 d
600 d
140 d
240 d
➡ components
2: follows the entire
path after 1000 d ➡ quiescent
➡B
of ~0.05 Jy uniformity: =0.2 (20%)
➡ identical
power
is unidirectional for the 2
components at the fiducial angle of
-10o
optical depth
➡ B-field
Myserlis, EA et al. in prep.
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
optical depth
Myserlis, EA et al. in prep.
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
optical depth
Myserlis, EA et al. in prep.
E. Angelakis, Max-Planck-Institut für Radioastronomie
Kraków, April 20-24, 2015
➡a
rich dataset of polarization data is available (RadioPol / F-GAMMA): ‣ 90 most fermi bright sources
‣ 8 years ‣ cadence 1 — 1.3 months
‣ 8 frequencies
➡ within
the framework of traveling shocks we can reproduce the observed
behaviors:
‣ 2 components on a similar evolutionary path
‣ equal power
‣ 20% uniform field
➡ within
this framework we can learn: ‣ the jet composition (e+- vs e - ion) from the enhancement of polarization(Jones
1988)
‣ mc/mi can tell you the FR conversion and rotation coefficients and estimate
the thermal content of the plasma ‣ B field strength and uniformity
‣ …. Dmitry Blinov’s talk on: “Rotations of Optical Polarization Plane in
Blazars as Seen by RoboPol”
➡ Note:
thank you
Emmanouil Angelakis & Ioannis Myserlis
Max-Planck-Institut für Radioastronomie, Auf dem Huegel 69, Bonn 53121, Germany