Post on 02-Oct-2020
SUPER-MASSIVE BINARY BLACK HOLE ANDPOLARIZATION IN THE BROAD LINES
-Dorde Savic, Luka C. Popovic, Frederic Marin
Astronomical observatory of BelgradeObservatoire astronomique de Strasbourg
November 13, 2019
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The search for SMBBHs
Supermassive black holes (SMBH) at the center of massive galaxies
Mass range 106–109 M� (Kormendy & Richstone 1995)
SMBHs play an important role in the co-evolution of the host galaxy(Kormendy & Ho 2013)
Growth by accretion – slow process and cannot explain the mostmassive cases (Mayer et al. 2010)
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Galaxy mergers
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Galaxy mergers
Evolution of SMBH via mergers with other SMBHs (Volonteri etal. 2003a,b)
Dynamical friction as a main process for bringing two SMBHstogether (Begelman et al. 1980)
The final parsec problem once the merging of the galaxies completes(Milosavljevic & Merritt)
Growth by accretion – slow process and cannot explain the mostmassive cases (Mayer et al. 2010)
Emission of gravitational waves
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The search for SMBBHs
It is hard to spatially resolve at pc-scale the central part of thenearest galaxiesDouble-peaked Balmer lines may be associated with binary systems(Eracleous & Halpern 2003)Significant number of AGNs show broad line profiles that could notbe explained by ”disk-like“ profilesStrong asymmetric broad line peaksThe broad line profiles and their variability may indicate the SMBBHpresence (Popovic 2012)
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The search for SMBBHs
Indications for SMBBH presence in the center of some active galaxies(see e.g. Bon et al. 2012; Li et al. 2016).
Low probability of finding amongst quasars
Only two candidates from SDSS catalog (Boroson and Lauer 2009)
From simulations 5 ∼ 10 per 10000 sources (Volonteri 2009)
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Unified model
Antonucci (1993)
Figure : Marin 2015
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Polarization observations
A major break-through forthe unified model forNGC 1068 (Antonucci &Miller 1985).
A periscope view of AGNin polarized flux
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The origin of polarization
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Polarization in Sy 1s
Polarization position angle (PA)rotation as evidence forequatorial scattering in Sy 1s.
Weak polarization, typically fewpercents.
Smith et al. 2002
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Polarization of broad lines in Sy 1s
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Modeling (scattering-induced) polarization with STOKES
Full 3D MonteCarloradiative transfer.
Various geometries for theemission/scatteringregions.
Polarization due to(multi) electron scatteringand dust (Mie) scattering.
Resonant line scatteringincluded.
Goosmann & Gaskell(2007); Marin et al.(2012, 2015).
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Polarization in Sy 1s
Two SMBHs with mass5× 107 M�
Two point-like source ofisotropic continuum radiation,Fν ∝ ν−2.
Clumpy BLR, filling factorf = 0.25
Four different cases of BLRconfiguration.
Half opening angle of the BLRis 20◦
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Distant BLR
Orbital separation a = 47.6 ld
Orbital period p = 75 years
x [pc]
-0.025 -0.02 -0.015 -0.01 -0.005 0 0.005 0.01 0.015 0.02 0.025
y[p
c]
-0.01
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
0.006
0.008
0.01f = 0:25
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Contact BLR
Orbital separation a = 16.7 ld
Orbital period p = 15.5 years
x [pc]
-0.015 -0.01 -0.005 0 0.005 0.01 0.015
y[p
c]
-0.01
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
0.006
0.008
0.01f = 0:25
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Mixed BLR
Orbital separation a = 2.97 ld
Orbital period p = 1.17 years
x [pc]#10 -3
-8 -6 -4 -2 0 2 4 6 8
y[p
c]
-0.01
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
0.006
0.008
0.01f = 0:25
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Scattering region
From 0.1 – 0.5 pc
Half opening angle 30◦
Radial optical depth is 3
Thomson scattering
x
y
x
z
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Results: Distant BLRs
2.8
3
3.2
3.4
3.6
10 -4
-0.03 -0.02 -0.01 0 0.01 0.02 0.03-0.015
-0.01
-0.005
0
0.005
0.01
0.015
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
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Results: Distant BLRs
0
0.01
0.02
0.03
0.04
-0.03 -0.02 -0.01 0 0.01 0.02 0.03-0.015
-0.01
-0.005
0
0.005
0.01
0.015
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
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Results: Distant BLRs
60
80
100
120
-0.03 -0.02 -0.01 0 0.01 0.02 0.03-0.015
-0.01
-0.005
0
0.005
0.01
0.015
60
80
100
120
60
80
100
120
60
80
100
120
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
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Distant BLR
Orbital separation a = 47.6 ld
Orbital period p = 75 years
Mass ratio q = 0.5
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Results: Distant BLRs
2.8
3
3.2
3.4
3.6
10 -4
-0.03 -0.02 -0.01 0 0.01 0.02 0.03 0.04-0.015
-0.01
-0.005
0
0.005
0.01
0.015
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
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Results: Distant BLRs
0
0.01
0.02
0.03
0.04
-0.03 -0.02 -0.01 0 0.01 0.02 0.03 0.04-0.015
-0.01
-0.005
0
0.005
0.01
0.015
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
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Results: Distant BLRs
60
80
100
120
-0.03 -0.02 -0.01 0 0.01 0.02 0.03 0.04-0.015
-0.01
-0.005
0
0.005
0.01
0.015
60
80
100
120
60
80
100
120
60
80
100
120
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
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Results: Contact BLRs
3
3.5
4
10 -4
-0.02 -0.015 -0.01 -0.005 0 0.005 0.01 0.015 0.02-0.01
-0.005
0
0.005
0.01
3
3.5
4
10 -4
3
3.5
4
10 -4
3
3.5
4
10 -4
3
3.5
4
10 -4
-1 -0.5 0 0.5 1
10 4
3
3.5
4
10 -4
-1 -0.5 0 0.5 1
10 4
3
3.5
4
10 -4
-1 -0.5 0 0.5 1
10 4
3
3.5
4
10 -4
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Results: Contact BLRs
0
0.01
0.02
0.03
0.04
-0.02 -0.015 -0.01 -0.005 0 0.005 0.01 0.015 0.02-0.01
-0.005
0
0.005
0.01
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
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Results: Contact BLRs
60
80
100
120
-0.02 -0.015 -0.01 -0.005 0 0.005 0.01 0.015 0.02-0.01
-0.005
0
0.005
0.01
60
80
100
120
60
80
100
120
60
80
100
120
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
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Results: Mixed BLRs
2.8
3
3.2
3.4
3.6
10 -4
-0.01 -0.008 -0.006 -0.004 -0.002 0 0.002 0.004 0.006 0.008 0.01-0.01
-0.005
0
0.005
0.01
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
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Results: Mixed BLRs
0
0.01
0.02
0.03
0.04
-0.01 -0.008 -0.006 -0.004 -0.002 0 0.002 0.004 0.006 0.008 0.01-0.01
-0.005
0
0.005
0.01
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
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Results: Mixed BLRs
60
80
100
120
-0.01 -0.008 -0.006 -0.004 -0.002 0 0.002 0.004 0.006 0.008 0.01-0.01
-0.005
0
0.005
0.01
60
80
100
120
60
80
100
120
60
80
100
120
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
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Spiral BLR
Orbital separation a = 16.7 ld
Orbital period p = 15.5 years
Model similar as the one by Smailagic & Bon (2015)
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Results: Spiral BLRs
2.8
3
3.2
3.4
3.6
10 -4
-0.05 -0.04 -0.03 -0.02 -0.01 0 0.01 0.02 0.03 0.04 0.05-0.05
0
0.05
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
-1 -0.5 0 0.5 1
10 4
2.8
3
3.2
3.4
3.6
10 -4
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Results: Spiral BLRs
0
0.01
0.02
0.03
0.04
-0.05 -0.04 -0.03 -0.02 -0.01 0 0.01 0.02 0.03 0.04 0.05-0.05
0
0.05
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
-1 -0.5 0 0.5 1
10 4
0
0.01
0.02
0.03
0.04
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Results: Spiral BLRs
60
80
100
120
-0.05 -0.04 -0.03 -0.02 -0.01 0 0.01 0.02 0.03 0.04 0.05-0.05
0
0.05
60
80
100
120
60
80
100
120
60
80
100
120
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
-1 -0.5 0 0.5 1
10 4
60
80
100
120
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Polarization maps: I
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Polarization maps: Q
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Polarization maps: U
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Conclusions
Spectropolarimetry is powerful tool for the SMBBHs search
Position angle profiles show variable W - or M-like profiles
Unpolarized lines show periodic variations
Spatially resolved polarization maps are highly sensitive to thepresence of SMBBHs
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