Nonthermal multiwavelength and multimessenger signalsfrom fast winds in active galactic nuclei	
Susumu Inoue (RIKEN) in collaboration with	

Ruo-Yu Liu (MPIK)	

Y. Tomono (Tokai U.), M. Hayashida (ICRR)	

et al.	

γ	p/Fe?	

radio	ν?	

ultra-fast outflows (UFOs) in AGN 	

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

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

- highly ionized:	

Fe XXV/XXVI	ξion~103-106 erg s-1 cm	

- high column density:	

NH~1022-1024 cm-2	

- variable: tvar>~ks	Giustini+ 11�ultra-fast outflows (UFOs) in AGN 	

velocity	vs radius�- R~0.0003-0.03 pc	

(~10-104 Rs)	.	
- 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�

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collisionless shocks in AGN winds	

external shocks	

Com2T structure?�

dUdwheSazUphFaucher-Giguere	& Quataert 12�
Rsh,ex~0.1pc -1 kpc�- mechanical/thermal feedback on host galaxy gas	-> origin of MBH - σbulge correlation?	

- particle acceleration and nonthermal emission?	

internal shocks	
observed variability of X-ray lines	

-> internal inhomogeneities	

-> internal shocks possible, Rsh,in~RS-~<Rsh,ex	is thL
spe
dist	e3nAsstem
syst

1dTe
dtdTpdtTopro
Te =F
ture108

radio-quiet AGN with UFO + GeV association	

Ackermann+ 12	

ESO 323-G77: radio-quiet AGN	- known (relatively slow) UFO	 Tombesi+ 10,11,12	
- association with Fermi source -> chance coincidence?		
- correlation
with Auger UHECR event	
Nemmen+ 10, Jiang+ 10 	radio-loud AGNs with UFO + GeV association	

Kataoka+ 11	
3C 111, 3C 120: broad-line radio galaxies	

- known UFOs	 Tombesi+ 12,14	
- association with Fermi sources -> jet related?	

- mixed nonthermal component in X-rays	 de Jong+ 12	

UFO shocks: electron & proton acceleration 	

MBH=108 Msun, vout=0.1c, Lkin=1045 erg/s ~ 0.1 Ledd	

B2/8π=εB Lkin/4π R2 vout	

Liu & SI	in prep. 	

dynamical tdyn=R/vout, tlc=Rs/c=500 s	

acceleration tacc~10 (vs/c)-2 E/ceB		

external radiation field follows Ghisellini & Tavecchio 09	

accretion disk+broad line region+dusty torus		

electron loss	

tesyn=3 me2c3/4σTuBEe	teIC=3 me2c3/4σTuphEe		

proton loss	

tpp=(κppσppnpc)-1	tpγ ∝ ∫ κpγ(x)σpγ(x)x dx ∫ nph(x)dx)-1 x=hv/mec2	

acceleration vs. cooling	 R=0.1 pc, B~3 G~Beq, np~5x103 cm-3	86tdyn	

4t/tlc	teEC	2tesyn	tacc	

0-2-20246810E [GeV]	

electrons up to ~1 TeV, cooling for ~<10 MeV NB: γγ	

protons up to ~3x1018 eV (Fe up to ~1020 eV)	acceleration vs. cooling	 R=0.1 pc, B~0.03 G, np~5x103 cm-3	

86t/tlc	

tdyn	

tacc	

tesyn	

4teEC	

20-2-2

02

4

6

8

10E [GeV]	

electrons up to ~100 GeV, cooling for ~<10 MeV NB: γγ	

protons up to ~3x1016 eV (Fe up to ~1018 eV)	

ESO 323-G77	

Le=1042, Lnuc=5x1044 erg/s (Lkin=1041.4-42.9)	

radio-quiet	

model results	

R=0.3 pc, B=10-4 G	

dust	nucleus	
EC	

syn	

SSCO(2EC (opt-UV): dash	EC (IR): dot 	

EC (X): dash-dot	

EC of opt+UV (BLR) dominant	GeV steepening by KN effects (possibly also γγ)	necessary Le rather high?	

BUT	

no GeV signal	

in 3FGL… 	

model results	 R=0.01 pc, B=10-3 G	

Le=3x1043, Lnuc=5x1044 erg/s Lkin=?	

dust+jet	jet	

3C111	

radio-loud	nucleus(+jet)	
EC	

syn	

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

EC (X): dash-dot	

EC of opt+UV (BLR) dominant	

non-negligible contribution to X-rays possible c.f. de Jong+12 	necessary Le rather high?	

req

NGC 4151	

Le=1040, Lnuc=9x1044 erg/s (Lkin=1041.9-43.6)	
radio-quiet	

model results	 R=1 pc, B>=0.01 G	dust	nucleus	EC	syn	EC (opt-UV): dash	EC (IR): dot 	

EC (X): dash-dot	

GeV upper limits from Tomono, Hayashida, SI+ (this conference)	

IF observed radio sync. from electrons in UFOs -> B>~0.01 G at R~1pc	

-> εB~0.03-1.7, suggest B-driven wind?	

SSCO(2acceleration vs. cooling	 R=0.1 pc, B~3 G~Beq, np~5x103 cm-3	86tdyn	

4t/tlc	teEC	2tesyn	tacc	

0-2-20246810E [GeV]	

electrons up to ~1 TeV, cooling for ~<10 MeV NB: γγ	

protons up to ~3x1018 eV, Fe up to ~1020 eV!	

acceleration vs. cooling	 R=0.001 pc -> Beq~300 G, np~5x107 cm-3	

6tpγe+-	
4tpγπ	

tdyn	2tacc	t/tlc	
0tesyn	-2teEC	-402468

10E [GeV]	

electrons only to ~100MeV NB: internal photons, γγ	protons up to ~1016 eV, limited by photomeson -> ν,n emission	summary	 AGN winds as accelerators/nonthermal emitters	- widespread existence of powerful, mildly relativistic	baryonic outflows in AGN, independent of relativistic jets	- collisionless external or internal shocks	

potential acceleration site of electrons and hadrons	- electron synchrotron may account for the radio emission	

of some radio-quiet AGN with (U)FOs	

- external inverse Compton may explain the gamma rays	(+X-rays in some objects) from nonblazar AGN with (U)FOs	

and GeV associations such as ESO 323-G77, 3C 111, 3C 120	- lower limits on B fields in winds can be derived for objects	

with GeV upper limits, e.g. NGC 4151, if their radio flux	

is synchrotron -> suggest B-driven wind?	

- candidate UHECR sources, especially Fe nuclei,	

if B fields near equipartition	

- candidate PeV neutrino sources, if acceleration occurs	near nucleus