High energy emission and cosmic rays	

from AGN (wind) feedback	
NGC 1068 as AGN-(rather than star-)burst galaxy	Susumu Inoue (RIKEN), Ruo-Yu Liu (MPIK)	

AGN winds at subkpc: fast, highly ionized winds	

UV/optical/NIR emission/absorption lines -> few 1000 km/s	

The Astrophysical Journal, 739:69 (40pp), 2011 October 1

NGC 1068 	

[SiV] emission	Müller-Sánchez et al.

θopen~50-60 deg	Sanchez-Mueller+ 11	

Figure 3. [Si vi] emission-line profiles from different regions in the central 4!! × 4!! (280 × 280 pc) of NGC 1068. The spectra have been extracted from apertures of5

10

Rest-frame energy (keV)

AGN winds at subpc: ultra-fast outflows (UFOs)	

blue-shifted X-ray absorption lines	
 PDS 456	
- ~40 % of all AGNs	

both radio-quiet/radio-loud 	- fast outflow: v~0.05-0.3c	

- highly ionized: Fe XXV/XXVI	

Nardini+ 15�
- high column density:	

NH~1022-1024 cm-2	

- variable: tvar>~ks	

Relative flux

Flux (10 −12 erg s −1 cm − 2 )4

Data/modelFig. 3. Fit with a P-Cygni line model. Adopting the samebaseline continuum of Fig. 2 (red curve), we fitted the emission and absorption residuals characterizing the Fe-K bandby means of a self-consistent P-Cygni profile from a spherically symmetric outflow (green curve). The results are shownfor the merged Obs. 3 and Obs. 4, which are separated by only
3 days and are virtually indistinguishable at 2 to 30 keV (Fig. 1).
The two NuSTAR modules were combined into a single spectrum (plotted in blue; T1 SD error bars) for display purposes
only. The inset contains a graphical explanation of the key
parameters of this model: the characteristic energy Ec, corresponding to the onset of the absorption component, andthe wind terminal velocity vV = 0.35 T 0.02 c, which can be
regarded as a measure of the actual outflowing speed of thegas.The bottom panel shows the ratio between the data andthe best-fit model. The residual structures above 10 keV are
due to the Kb and K edge absorption features from Fe XXVI.
These are not included in the P-Cygni model but are detectedwith high significance (table S2) and remove any ambiguity inthe identification of the ionic species.

3

v∞

1.3
1.0

Ec

0.7
5

10

Rest-frame energy (keV)

2

K edge
Kβ

1.2
1.0
0.8

5

10

Rest-frame energy (keV)862

20 FEBRUARY 2015 • VOL 347 ISSUE 6224

4 Rs)	

- R~0.0003-0.03
pc(~10-10.	
- M~0.01-1 Msun/yr	

Lkin~0.01-1 LEdd	

- broad opening angle ~<100 deg	- independent of relativistic jet	

Lkin vs Lrad�
Tombesi+ 13�

sciencemag.org SCIENCEξioaccretion disk winds: formation mechanism(s)	

thermal? radiation (continuum or line)? magnetic?	

hybrid (thermal+radiation, radiation+magnetic)?...�

Figure 5. Conﬁdence contour plots for (a) temperature kTbbb and inclination θ and (b) trunca
and 99%, also indicated by the best-ﬁt model (B) (cross). See Table 2 for details.

radiation (line) -driven model	

Proga+ 98�

MHD+radiation model	

Fukumura+ 15�

Figure 6. (a) Geometrical identiﬁcation of the observed Fe XXV/Fe XXVI from theXMM-New
show the global magnetic ﬁeld lines (thick solid lines), normalized wind density log(n (r , θ )arrows), and the inferred location of Fe XXV and Fe XXVI. See Table 2 for details. (b) Sche

AGN winds at >~kpc: massive molecular outflows	CO, OH etc. emission	

A&A 562, A21 (2014)-> v~100-1000
km/s, M~few 10-100MΘ/yr, Lkin~<Lbol	

!"#$
!,#$

!&#$

-800 < v (km/s) < -400($)*&$

Mrk 273 	

 CO	
 !+#$
Cicone+ 14	
pos.
[arc]

!'#$

!%#$

v [km/s]
400 < v (km/s) < 900($)*&$

black hole - galaxy bulge scaling relations	likely consequence of AGN feedback	

Kormendy & Ho 13�
self-regulating mechanical feedback by AGN winds?	

Silk & Rees 98, King 03, …	

Garcia-Burillo+ 14	
evidence of AGN feedback in action	

S. García-Burillo
et al.: 1068
Molecularemissionin NGC 1068 imaged with ALMA.
ALMA observationsof NGC
	
line
D=14
Mpc	

bow shock arc	circumnuclear	disk	

349 GHz	ut for the CO(6–5) line, obtained with a single field mosaic. Contour levels are: 5 , 10 , 20 ,1
1
0 , where
1
=
2
Jy
km
s
beam
. The filled
at the bottom Garcia-Burillo+right corner represents
14	
theevidence of AGN feedback
inellipse
action	

ALMA observations of NGC 1068 	
 D=14 Mpc	ry Large Telescopeüller-Sánchez
et al.
CO(3-2)	

featuresare also
black:
v-vdesys=-50 km/s	

–5) mapofFig.
white:
v-v4c.
km/s
	
 in NGC 1068 imaged with ALMA. I.
S. García-Burillo
al.: Molecularline emission
syset=+50
ower-level emissiono the stellar bar reon is detected along
ostly parallel to the
et al. 1988; Bland000; Emsellem et al.
leading edge moren the corotation of
ated in Fig. 5, whicho velocity channels
vsys = 50 km s 1
7 ± 3 km s 1 as deng the bar’s leading
foremission
gasmapfalling
ected
continuumof NGC 1068 obtained with ALMA at 349 GHz. The map is shown in color scale (in Jy beam units as
1

1

Garcia-Burillo+ 14	
evidence of AGN feedback in action	

S. García-Burillo et al.: Molecular line emission in NGC 1068 imaged with ALMA. I.
ALMA observations of NGC 1068 	
 D=14 Mpc	velocity field	

distribution	

he CO(3–2) integrated intensity map obtained with ALMA using an eleven-field mosaic in the disk of NGC 1068. The map is shown
ale with contour levels 5 , 10 , 20 , 30 , 45 , 70 , 100 to 500 in steps of 50 , and 600 to 800 in steps of 100 , where 1 =s 1 beam 1 . The filled ellipse at the bottom right corner represents the CO(3-2) beam size (0.00 6 ⇥ 0.00 5 at PA = 60 ). b) Same as a) but
n on the CND region. c) Same as b) but for the CO(6–5) line, obtained with a single field mosaic. Contour levels are: 5 , 10 , 20 ,
70 , 90 , 120 to 240 in steps of 40 , where 1 = 2 Jy km s 1 beam 1 . The filled ellipse at the bottom rightΘcorner represents the0000
eam size (0. 4 ⇥ 0. 2 at PA = 50 ).
41

olecular ring imaged with the Very Large Telescopein the 2.12 µm H2 line by Müller-Sánchez et al.
). The brightest CO(3-2) emission features are also deCO (3-2)	
HST
and spatially resolvedin the CO(6–5) map of Fig.
4c. Paα	ar: the CND appears connected to lower-level emission
extends farther out in the disk into the stellar bar reOn these scales the CO(3–2) emission is detected alongnes, o↵set by 2 400 , which run mostly parallel to themajor axis (PA = 46 ± 2 ; Scoville et al. 1988; Blandhorn et al. 1997; Schinnerer et al. 2000; Emsellem et al.
These are reminiscent of the gas leading edge morgy that is expected to prevail between the corotation ofr and the ILR region. This is illustrated in Fig. 5, which
the emission of CO(3–2) at two velocity channels
etrically located relative to vsys : v vsys = 50 km s 1
349 GHz	22 GHz	50 km s 1 , with vsys (HEL) = 1127 ± 3 km s 1 as dened in Sect. 6.1.1. Gas emission along the bar’s leading
appears at the velocity range expected for gas fallingdM/dt~ 60 M /yr>>SFR	

Lkin,mol~5x10 erg/s	

Fig. 15. Overlay of the residual mean-velocity fi(hVres i) of Fig. 14, in color scale, with the conto
representing: the integrated intensity of CO(3–2)
contours as in Fig. 14), the 349 GHz continuum emsion (b); contours as in Fig. 1), the HST Pa↵ emsion (c): with contours 0.2%, 0.5%, 1% to 5% in sof 1%, 10% to 90% in steps of 20% of the peak valu
1000 counts s 1 pixel 1 ), and the 22 GHz VLA m
of Gallimore et al. (1996) (d): with contours 1%,
5%,10%, 15%, 20%, 30%, 50%, 70%, and 90% of
peak value = 36 mJy beam 1 ).

kpc-scale radio “jet” in NGC 1068	

18cm	

Gallimore+ 96	kpc-scale radio “jet” in NGC 1068	

Gallimore+ 96	

6cm	

no measurement of velocity or power	

estimate from Lrad-Lkin correlation -> Lkin~1042-1043 erg/s	Garcia-Burillo+ 14	
evidence of AGN feedback in action	

ALMA S.observationsof NGC 1068 	
 D=14 Mpc	García-Burillo et al.: Molecular line emission in NGC 1068 imaged with ALMA. I.
01'
1.
1%
5

!"#$%&'(")*+"'(%,"(-.

% α%

!"#
$

2%6
5

% 7% "

%

"%

4
2 %3

$
!"#"

#

$

,'/%&'.
(%,"((")*+"'

%&'()

.
(%,"('"+*)"(,'/%&'%&'()*'+,-./01

!"#

%&'()
$
"
#
!"

!"#$%&'(")*+"'(%,"(-.

7. A revised version of the kinematic model of the NLR, first proposed by Tecza et al. (2001) and Cecil et al. (2002), which now accoun
olecular outflow (denoted in figure as CO outflow) detected by ALMA in the CND (seen in projection in N and S, for northern and sou!

!

hods. Both the complete sample of 69 galaxies (containing eight LAT sources) and analyzedFermi(containing
six LAT sources).
observationsof “starburst”+normal galaxies	

Ackermann+ 12	

s

e
nt
e
s
d

f
e
y

Starbursts
NGC 1068
NGC 1068 (H.E.S.S.)
M82
M82 (VERITAS)
NGC 4945
NGC 253
NGC 253 (H.E.S.S.)

1040
E2 dN/dE (erg s-1)

5
n
-

1041

1039
1038
1037

Local GroupMilky Way Global Model
M31
LMC
SMC

1036
103

105
107
Energy (MeV)

109

Figure 6. Gamma-ray luminosity spectra of star-forming galaxies detected byFermi observations of “starburst”+normal galaxies	

 Ackermann et al. A

al Journal,
755:164 (23pp),
2012 August
The AstrophysicalJournal,755:16420(23pp), 2012 August 20

Ackermann+ 12	
SFR (M yr -1)

10-1

103 10

1 10-2 1010-1 102 1

1043

LAT Non-detected43(Upper Limit)
LAT Non-detected (Upper Limit)

10

LAT Non-detected with AGN (Upper
Limit)LAT Non-detectedwith AGN (Upper Limit)
Arp 220

LAT Detected
LAT Detected with AGN

Best-fit
Fit Uncertainty
Dispersion

Best-fit
Fit Uncertainty
Dispersion NGC 2146

L0.1-100 GeV (erg s-1)

10

41

10

Calorimetric Limit50(E η = 10 erg)
SN

Arp 220

NGC 1068

Calorimetric Limit50(E η = 10 erg)
SN

40

10

M83

1039

M82
NGC 4945

NGC 253

NGC 6946
IC 342

NGC 6946
IC 342Milky Way

M31

M33

M83

M82
NGC 4945

NGC 253

Milky WayNGC 1068

NGC 2146

M33

SMC

1019

10

1020

LAT Detected
LAT Detected with AGN

41Best-fit
Fit Uncertainty
Dispersion

Best-fit
NGC 2146
Fit Uncertainty
NGC 1068
Dispersion

10

SN

40

10

1039

1037

19

10
1021

-2

103 1010

M83

LAT Non-detected (Upper Limit)
LAT Non-detected (Upper Limit)
5
10with AGN (Upper
LAT Non-detectedwith AGN (Upper Limit)
LAT Non-detected
Limit)

103SMC

1039M31

10

M83

M31

Milky WayNGC 4945
NGC 253
NGC 6946
IC 342Milky Way

M33

LMC

1037

10-2
-1

M82

NGC 4945
NGC 253
NGC 6946
IC 342SMC

8109 1012
1010
1011
109
101010 1011
L8-1000 µm (L )L8-1000 µm (L )SFR (M yr -1)
102

NGC

SN

40

SFR (M yr -1)-11010 102 1

NGC 2146

1038

108

1024

Arp 220

Calorimetric Limit50(E η = 10
M82 erg)

LMC

SMC

1 10

10

M33

1020 10231021 1024
1022
1023
1022
L1.4 GHz (W Hz-1) L1.4 GHz (W Hz-1)

10-1

41

Calorimetric Limit50(E η = 10 erg)1038

SFR (M yr -1)
10-2

10

LMC

37

1

LAT Non-detected with AGN LAT(UpperLimit)
Non-detectedwith AGN (Upper Limit)
LAT Detected
LAT Detected with42AGN

10

10310

110-2 1010-1 102 1

LAT Non-detected43(Upper Limit)
LAT Non-detected (Upper Limit)

M31

1038
LMC

10-1

SFR (M yr -1)

42

10
L0.1-100 GeV (erg s-1)

LAT Detected
LAT Detected with42
AGN

10-2

103

102

L0.1-100 GeV (erg s-1)

10-2

SFR (M yr -1)

SFR (M yr -1)

10-1

-2

110

SFR (M yr -1)-11010 102 1

10310

LAT Non-detected (Upper Limit)
LAT Non-detected (Upper Limit)-1
10
Non-detectedwith AGN (Upper Limit)
LAT Non-detected with AGN LAT(UpperLimit)

1

F

of 0.2.
10−1 of this figure is available in the online journal.)(A color version

10
10−2
10−1
10−9

100

Total Flux
2
Pion 10
Decay
Bremsstrahlung
Inverse Compton

101

Frequency [GHz]on the left. The changes in the total radio spectrum as the fraction of absorbed synchrotron
ht. While we able −10
to obtain a relatively good fit to the radio with the lower mass (right), we
10higher bremsstrahlung losses at low energies. Model parameters are set at (left) p = 2.2,8−1−3
mol = 3 × 10 M# and (right) p = 2.2, η = 0.04, Urad = 500 eV cm , nion = 350 cm ,line denotes total radio flux, the dashed line represents the unabsorbed synchrotron radio
orbed synchrotron
radio emission in the hot, diffuse gas, and the dot-dashed line represents
10−11; triangles), Williams & Bower (2010; circles), Ricci et al. (2006; squares), and Peng et al.
tween 0.1 and 1.0 and the black line represents a radio spectrum with an absorption fraction

10−12
10−1

101

100

102

102

103

104

Energy [GeV]

Yoast-Hull+ 14	

101
100

Flux [Jy]E2 dN/dE [GeV cm−2 s−1 ]difficultyof starburst interpretation	

−8

10−1
10−2
10−3
10−4
10−5
10−1

100

101

Frequency [GHz4

Flux [Jy]Abstract:	

102
Figure 5. γ -ray (left) and radio (right) spectra for NGC 1068. While
our models always underestimate the observed γ -ray flux, we also
Total Flux
…our starburst model
1
7
10 are set at p = 2.0, η = 0.1, Mmol = 5 × 10 Synchrotron
Model parameters
M# , Urad = 104 eV cm−3 , nion = 400 cm−3 , vadv = 0 km s−1 , and B
lung
Absorbed
Synch et al.
for Fermi data and squares for HESS data
(Ackermann2012). Data with downward arrows represent upp
consistently
mpton represented as triangles
010Free-Free et al. 2004), red square (CMZ upper limit; Gallimore et al. 19
HESS data. Radio data are represented by blue triangles (S2; Gallimore
underestimates theHönig et al. 2008).
10−1(A color version of this figure is available in the online journal.)
observed γ -ray flux and−2
10
while we are producing the same amount of secondary electrons
10−3 at both masses, there are fewer electrons/positronsand positrons
available10
to−4
produce inverse Compton and synchrotron emission
due to an increasein bremsstrahlung.
−5
10

10−1

100

101

[GHz]
4.2. NGC Frequency
1068 Results

102

overestimates
the weradio
As with NGC 253,
intended to tes
sets ofparameterswith which
to model N
flux
for
NGC 1068;
these
found NGC1068besignificantly
harder toissueswouldresolved
The upper bound on the supernova rifspectrum
the AGNis lower
the primarythat isby a factor of onl
However,bound on the supersourceofaγlower-rays.	

γ -ray spectrum that is nearly two ordedifficulty of starburst interpretation	

– 19 –NGC 253

M 82

Eichman & Becker Tjus	

arXiv:1510.03672	
NGC 4945

NGC 1068

q0e [10 18 cm 3 s 1 ]
1.5
1.0
9.3
208
q0p [10 20 cm 3 s 1 ]
2.0
1.4
7.0
130
↵
2.15
2.15
2.3
2.35
A
10 5
10 4
10 4
10 4
B [µG]
109
611
178
178
Nt [cm 3 ]
291
477
178
291
–
19
–
vadv [107 cm/s]
5
10
10
5
le [1017 cm]
5
1
1
5
p
M 820.5 NGCNGC
qe1 /qe2 ( = ⌫GHz /⌫s ) NGC
2.4 253
2.5 0.8
1.2 4945
0.9
1.9 1068
1.6
3gamma-ray
1cm
The
radio
(right)dataasasthe
wellbest-fit
as 208the model
best-fitoq⌫0eSN[10s 1 ]and gamma-ray
1.5
1.0
9.3
e.—:
radio
(left)(right)data[yr18and] (left)
4
3 as well
28649
p
20 cm 3 s 1 ]q[10
2.0 represent
1.4 represent
7.0the
NGC
and
NGC
1068.
Open
squaressetusedthatforis45
and4945
NGC
1068.
Open
squaresthe data
set data
that130
is0
Table 2:: Best-fit
parameters↵2.15 model
2.15
2.3
2.35
Abstract:	

5 supernovae
4 the dominant…Another important result isA
10that10 4 can not
10 be
10 4
sourcein NGCand NGC
1068…	

e case ofBNGC
253relativistic
and M 82particles
the best-fit
model4945
describes
thelarge
data set[µG] of
109
611
178
178of the rad
3 ] well. Also the best-fit
ma-ray bandvery
NGC 1068178
agrees very 291
well with theNt [cm
291 model of477

wind shocks: electron & proton acceleration 	

SI & Liu	

in prep. 	
main parameters	

vout, Lnuc, next: observed	

Le, Lp < Lkin: obs. constrained	

Rs: few Rg- Rbulge	Bs (εB= B2/8π / Lkin/4π R2 vout), Dext(E)	
dynamical time tdyn=R/vout, tlc=Rs/c=500 s	

-2 E/ceB	

acceleration
time
t
~10
(v
/c)
acc
s
	

external radiation field follows Ghisellini & Tavecchio 09	

accretion disk+broad line region+dusty torus		electron loss time	

tesyn=3 me2c3/4σTuBEe	

2c3/4σ u E
t
=3
m
u
~u
eIC
e
T
ph
e
ph
ext	

	

proton loss time	

tpp=(κppσppnpc)-1	

tpγ ∝ ∫ κpγ(x)σpγ(x)x dx ∫ nph(x)dx)-1 x=hv/mec2	leptonicmodel	

R=100 pc, v=1000km/s, B=100µG, pe=2	

Le=2x1041 erg/s, Lnuc=1044 erg/s	

NGC 1068	

dust	
nucleus	

syn	

EC	

EC (opt-UV): dash	EC (IR): dot 	

EC (X): dash-dot	

EC of opt+UV (BLR) dominant over SSC	cutoff at >~300 GeV	

SSC
O(2

hadronic R=100 pc, v=1000km/s, B=100µG, pp=2.2	

 NGC 1068	

Lp=2x1042 erg/s, Lnuc=1044 erg/s	
next=250cm-3	

model	

Dext(GeV)	

=1027 cm2/s	

dust	
nucleus	pp	
e+- EC	e+- syn	SSCO(2π0 bump, hard extension to ~10 TeV -> CTA!	

syn+EC from secondary e+- important	

UHECR, neutrinos?	

Eichman & Becker Tjus	

gger than the commonly used ratio of (mp /me )(↵ 1)/2 .
rator as well as the secondary electrons from hadronic
synchrotron radiation as well as the gamma radiation
relativistic electrons. However, the main constituent

JCAP08(2015)014

GC 253, M 82, NGC 4945 and NGC 1068 that results
e dashed lines represent IceCube limits for the specific

Moharana & Razzaque 15	m http://mnras.oxfordjournals.org/ at University of Tokyo Library on September 18, 2015

observable signature of AGN wind feedback	Wang & Loeb 15� also Nims+ 15	

R=5.88 kpc�z~1	radio, X-ray	observable	

by SKA, Athena	->	probe of SMBH	

feedback in action�

->	UH
R=147 kpc�coProbing gaseous galaxy haloes
841
identifiable with	

 SM
radio emission	

of radio-quiet	

quasars?	

Figure 3. Dependence of outflow hydrodynamics and emission on baryon fraction in the disc fd . We fix Mhalo = 1012 M! and z = 1.0. Panels (a) and (b)show the shell velocity and radio synchrotron flux at 1 GHz as a function of radius. The dotted and dashed vertical lines mark the position of Rdisc and Rvir ,respectively. The upper x-axis of panel (b) marks the angular diameter of the outflow shock. Panel (c) shows the radio synchrotron flux as a function of time.
The dashed vertical line corresponds to the point when the AGN shuts off. Time is scaled to the Hubble time tH on the upper x-axis. Panel (d) demonstrates themomentum flux boost of the shell. The solid lines represent the numerical result, while the dashed lines correspond to predictions in the energy-driven regime.
Panels (e) and (f) illustrate snapshots of non-thermal emission power and flux at Rdisc and Rvir , respectively. The solid, dashed and dotted lines correspond tosynchrotron emission, IC scattering of accretion disc photons and CMB photons, respectively.

MNRAS 453, 837–848 (2015)

Zakamska	

& Green 14	
Dowsummary	

 AGN feedback and particle acceleration	
- widespread existence of fast, powerful, baryonic(ionic)	

winds in AGN, independent of relativistic jets	- likely to provide important feedback onto host galaxy gas	

directly observed in some nearby objects like NGC 1068	

- GeV (+radio) observed from NGC 1068:	

starburst interpretation difficult	- interpretation plausible in terms of particle acceleration via	AGN wind (or jet) feedback (interaction with host gas)	

either leptonic or hadronic feasible	

-> discriminate with CTA	- new type of particle accelerator:	

search for other similar objects warranted	

- new perspective on observing the effects of AGN feedback	-U-