from x-ray binaries to agn: the disk/jet connectionbhfeedback2012/uploads/bhfeedback2012... ·...
TRANSCRIPT
From X-ray Binaries to AGN: the Disk/Jet Connection
Rich PlotkinUniversity of Amsterdam (➔ Michigan)
with Sera Markoff (Amsterdam), Scott Anderson (Washington), Niel Brandt (PSU), Brandon Kelly (UCSB), Elmar Körding (Nijmegen, NL),
Ohad Shemmer (N. Texas), Jianfeng Wu (PSU➔CfA)
X-Ray Binaries Can Help Us Learn about Galaxy and SMBH (Co)-Evolution
To better understand feedback, and to exploit AGN as probes of SMBHs, we need more constraints on how radiation ⟺ Ṁ, MBH
Understanding the connection between black hole accretion disks and outflows is crucial
XRBs are scale models of AGN
Springel et al. (2005) - Millenium Simulation
31.25 Mpc/hz=18.3; T=0.2 Gyr
31.25 Mpc/h
z=0; T=13.6 Gyr
I. Two case studies:i. High-energy radiation near the disk/jet interfaceii. Accretion mode, and how it affects AGN
unification and feedback
II. Future insights to be learned from XRBs
Outline: Advantages of Looking at All Types of Black Holes
Black Hole X-ray Binary(~10MSun)
Microquasar Outbursts
GX 339-4 During Outburst
Dunn et al. (2010) StartEnd
Lum
inos
ityLjet or corona/Ldisk
Non-ThermalThermal
Dunn et al. (2010)
XRBs~10 Msun
BLLacs~108--9 Msun
FR I’s~108--9 Msun
LLAGN~107--8 Msun
Sgr A*
~106 Msun
28 30 32 34 36 38 40 42log Lr [erg s-1]
35
40
45
50
55
log
L x’ (M) [
erg
s-1]
Data from Körding et al. (2006)Plotkin et al. (2012a)
log Lradio (erg s-1)
log
L x-ra
y + ξ M
log
MBH
(erg
s-1 )
The Fundamental Plane of Black Hole Activity (Merloni et al. 2003, Falcke et al. 2004) Lx-ray ~ (Lradio)ξR MξM
Constraining how Radiation ⟺ Ṁ, MBH
For low L/LEdd BHs: the conversion of the accretion flow into radiative output at
the disk/jet interface is universal across
the black hole mass scale
XRBs~10 Msun
BLLacs~108--9 Msun
FR I’s~108--9 Msun
LLAGN~107--8 Msun
Sgr A*
~106 Msun
28 30 32 34 36 38 40 42log Lr [erg s-1]
35
40
45
50
55
log
L x’ (M) [
erg
s-1]
Data from Körding et al. (2006)Plotkin et al. (2012a)
log Lradio (erg s-1)
log
L x-ra
y + ξ M
log
MBH
(erg
s-1 )
The Fundamental Plane of Black Hole Activity (Merloni et al. 2003, Falcke et al. 2004) Lx-ray ~ (Lradio)ξR MξM
Constraining how Radiation ⟺ Ṁ, MBH
Lx-ray ~ (Lradio)1.76 M-1.56
If Inverse Compton X-rays from Radiatively Inefficient Accretion:
If Optically Thin Synchrotron X-rays:Lx-ray ~ (Lradio)1.38 M-0.81
What geometry produces the high-energy radiation?
1.2 1.4 1.6 1.8 !R
!1.6
!1.4
!1.2
!1.0
!0.8
!0.6
!0.4
!M
Contracted"R=!0.15
MeritBayes
1.2 1.4 1.6 1.8 !R
Contracted"R=0.00
X-rays from an “average” low L/LEdd BH are Dominated by Optically Thin Jet Synchrotron
43 Galactic BHs, SgrA*, LLAGN10 MSun - 107 MSun
ξ M -
Mas
s Coe
ffici
ent
P12 Bayesian Regression
MeritFunction
Merit Function is a modified χ2 estimator (from Körding et al. 2006)
Bayesian Linear Regression (mlinmix_err developed by Kelly 2007)
Inverse ComptonX-rays
LX ∝"ṁ2
Lx-ray ~ (Lradio)ξR MξM
-1.4
-1.2
-1.0
-0.8
-0.6
LX ∝"ṁ2.3
-1.6
ξR - Radio Coefficient
Plotkin et al. (2012a)
Optically ThinSynchrotron X-rays
Geometry of a low-luminosity “Hard Sate” Black Hole
~10% LEdd
<1-2% LEddNo Wind/Torus
Ine!cient Inner Accretion Flow
Disk Wind Feeding Torus
Most X-rays are optically thin jet synchrotron
e.g., above schematic helps inform us on how to use radiation from nearby low-luminosity AGN to probe the SMBH Mass Function at z=0
Figure Adapted from Trump et al. 2011
I. Two case studies:i. High-energy radiation near the disk/jet interfaceii. Accretion mode, and how it affects AGN
unification and feedback
II. Future insights to be learned from XRBs
Outline: Advantages of Looking at All Types of Black Holes
Explore Accretion Mode with BL Lacs (beamed low-luminosity radio galaxies)
JET
Urry & Padovani (1995)
5
10
15
20
Flu
x. D
ens. (e
rg s
−1 c
m−2
Å−1
)
Ca II H/K
Mg Na
SDSS J080018.79+164557.1 (zspec = 0.309)
10
12
14
16
log i
Fi
(erg
s−1
cm
−2)
log ipeak = 13.5 Hz
100
200
300
400
500
Flu
x. D
ens. (e
rg s
−1 c
m−2
Å−1
)
SDSS J080949.18+521858.2 (zspec = ?, zhg > 0.056)
10
12
14
16
log i
Fi
(erg
s−1
cm
−2)
log ipeak = 15.5 Hz
4000 5000 6000 7000 8000 9000
Wavelength (Å) [Obs. Frame]
0
20
40
60
80
Flu
x. D
ens. (e
rg s
−1 c
m−2
Å−1
)
SDSS J110021.06+401928.0 (zspec = ?, zhg > 0.275)
8 10 12 14 16 18 20
log irest (Hz)
8
10
12
14
16
log i
Fi
(erg
s−1
cm
−2)
log ipeak = 16.2 Hz
Flux
Den
s.
Wavelength (Å)
SDSS Optical Spectrum
Plotkin et al. (2010)
Explore Accretion Mode with BL Lacs (beamed low-luminosity radio galaxies)
JET
Urry & Padovani (1995)Wavelength (Å)
SDSS Optical Spectrum
Plotkin et al. (2010)
5
10
15
20
Flu
x.
De
ns.
(erg
s−1
cm
−2 Å
−1)
Ca II H/K
Mg Na
SDSS J080018.79+164557.1 (zspec = 0.309)
10
12
14
16
log
i F
i (e
rg s
−1 c
m−2
)
log ipeak = 13.5 Hz
100
200
300
400
500
Flu
x.
De
ns.
(erg
s−1
cm
−2 Å
−1)
SDSS J080949.18+521858.2 (zspec = ?, zhg > 0.056)
10
12
14
16
log
i F
i (e
rg s
−1 c
m−2
)
log ipeak = 15.5 Hz
4000 5000 6000 7000 8000 9000
Wavelength (Å) [Obs. Frame]
0
20
40
60
80
Flu
x.
De
ns.
(erg
s−1
cm
−2 Å
−1)
SDSS J110021.06+401928.0 (zspec = ?, zhg > 0.275)
8 10 12 14 16 18 20
log irest (Hz)
8
10
12
14
16
log
i F
i (e
rg s
−1 c
m−2
)
log ipeak = 16.2 Hz
Flux
Den
s.
Weakly Beamed BL Lac
Mid-Infrared Colors with WISE:Most BL Lacs are Missing Dusty Torus Emission
0.0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
W1!
W2
RL BL Lacs (0.1<z<0.3)
Quasars (Extended)
Quasars (Point!like)
Early!Type Galaxies
(a)
(b) Simulated Jet
0 1 2 3 4W2!W3
0.0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
W1!
W2
(c) Simulated Jet + Galaxy
0 1 2 3 4W2!W3
(d) Simulated Jet + Galaxy + Torus
Plotkin et al. 2012b
Simulated Jet+Galaxy+TorusSimulated Jet+Galaxy
Simulated Jet
WISE Infrared Color 2[4.6µm]-[12µm] (mag)
WIS
E In
frare
d Co
lor 1
[3.4
µm]-[
4.6µ
m] (
mag
)
WISE Blazar Strip (Massaro et al.
2011)
WISE Infrared Color 2[4.6µm]-[12µm] (mag)
WIS
E In
frare
d Co
lor 1
[3.4
µm]-[
4.6µ
m] (
mag
)Weakly Beamed BL Lacs
Contours: Simulated IR Colors
Redder
Redder
~10% LEdd
<1-2% LEddNo Wind/Torus
Ine!cient Inner Accretion Flow
Disk Wind Feeding Torus
GX 339-4(~10 MSun)
XRB accretion state (and jet properties) are likely connected to the inner accretion flow
Nature of Inner Accretion Flow Likely Evolves
adapted from Trump et al. 2011
Lum
inos
ity
Ljet or corona/Ldisk
Thermal Non-Thermal
StartEnd
adapted from Dunn et al. 2010
High-Luminosity
Low-Luminosity
Figure Adapted from Trump et al. 2011
Lack of torus emission suggests an accretion mode “divide” for AGN, similar to XRBs
(e.g., see Jackson & Wall 1999; Nicastro 2000; Ghisellini & Celotti 2001; Böttcher & Dermer 2002; Wold et al. 2007; Ghisellini et al. 2009, Hardcastle et al. 2009; Trump et al.
2011; Antonucci et al. 2011, Plotkin et al. 2012b)
~10% LEdd
<1-2% LEddNo Wind/Torus
Ine!cient Inner Accretion Flow
Disk Wind Feeding Torus
Wind Mode?
Radio Mode?
I. Two case studies:i. High-energy radiation near the disk/jet interfaceii. Accretion mode, and how it affects AGN
unification and feedback
II. Future insights to be learned from XRBs
Outline: Advantages of Looking at All Types of Black Holes
Do distinct accretion states launch winds vs. jets, or can “wind” vs “radio” feedback co-exist?
�� ���� �
�
���
�
����
��
����
��
����
�
���
����������������������
����� �
���� ���
��������
-�*/,)&-0�
� �*/..&-)��*0-,&,++�� �*2*.3*).����*1*0&,,)�
��,,2&-�
����
��������$���������! ���5�&+.����
5�&*)����5�&*����
����������!��"�� ���4�&+.����
4�&*)����4�&*����
���*/.)&.))�� �*0.1&+.1�-�*2.03**.�
���� !�!�� �����
Ponti et al. (2012)
XRB winds not detected in hard (i.e jetted) state?
Lum
inos
ity
Ljet or corona/Ldisk
Radio-loud QSOs generally show weaker disk winds
Richards et al. (2011)
weaker disk wind
Radio LoudRadio Quiet
Conclusions1. X-ray binaries help us see the bigger picture
2. There is a robust disk/jet coupling for “Hard State” Black Holes X-rays are predominantly optically thin synchrotron
Constraints on geometry near the black hole help us go from radiation ⟺ Ṁ, MBH
3. BL Lac objects have weak or missing tori
New evidence for an AGN accretion mode “divide”
Implications for “wind” vs “radio” feedback?