Disk wind interpretation ofthe strong iron K featuresin 1H 0707-495
Kouichi Hagino (ISAS/JAXA)
H. Odaka, C. Done, R. Tomaru, S. Watanabe, T. Takahashi“Prospects, challenges and evolution of AGN modeling in the Astro-H Era”
@Rikkyo University
K. Hagino et al., submitted to MNRAS (arXiv:1509.05645)

Ultra-fast outflows••

Blue-shifted absorption lines with a velocity of ~0.1c is found in a part of local AGN(Chartas+ 2002; Reeves+ 2003; Pounds+ 2003a,b; Tombesi+ 2010)

Indicating a presence of absorbers moving from the source (=black hole) with a very
fast velocity
A spectrum of the ultra-fast outflow➡ Ultra-fast outflow (UFO)2×10−3v~0.3c10−3

FeXXV Lyα
@6.7 keVFeXXVI Heα@7.0 keV

5×10−4keV2 (Photons cm−2 s−1 keV−1)

PDS 456

4••‣

68Energy (keV)

10

Most of the UFOs are detected in AGN with low Eddington ratio (e.g., Tombesi et al. 2010, 2012).
Theoretically, high accretion rate sources should launch the disk wind (e.g., Ohsuga &Mineshige 2011)

Are there any UFOs with high accretion rates?

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A narrow line Seyfert1 galaxy 1H 0707-495
This AGN is thought to be an most convincing evidence of a rapidly spinningblack hole (Fabian+ 2004).
Zoghbi, Fabian et al. 2010

Powerlaw continuum

normalized counts s -1keV 1••

Low mass (MBH~106M⦿), high accretion rate (Lbol LEdd) (e.g., Done&Jin 2015)

10.1

ratio

Reflected
0.01
component

Dovciak et al. 2011

•Reflected component

10 31.41.2
1
0.8
0.6

Softexcess

0.5Powerlaw
continuum

12Energy (keV)

510This model requires extreme conditions:-Black hole spin is close to max.
Incident radiation is strongly focused on the disk inner edge

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Disk wind interpretation••

We propose a disk wind interpretation for the strong Fe-K spectral feature.

➡ The spectral feature inPDS 456 brightest
PDS 456 faintest

10−4 2×10−4

5×10−4

1H 0707-495 seems to bemade by the disk wind
just like the spectra ofPDS 456.

•5×10−5
2×10−5keV2 (Photons cm−2 s−1 keV−1)

10−3 2×10−3

Observed spectra of 1H 0707-495 is very similar to the spectra of achetypal
wind source PDS 456 (MBH~109M⦿, vwind~0.3c, Ṁwind~10M⦿/yr)

1H 0707-495 brightest
1H 0707-495 faintest
25Energy (keV)

If the Fe-K feature in 1H
0707 is from the wind, it isa good example of102015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University

4 / 18Modeling the disk wind spectra•

We modeled the disk wind spectra by assuming the “UV-line driven disk wind”
UV-line driven disk windionizedgas•

Ionized gas is accelerated bygetting a momentum (radiationpressure) from UV photons via
bound-bound transitions•

σbb > 103−4 σT →effectively
accelerate••

AGN radiate a lot of UV photons

centrifugal force

X-ray
radiation
UV radiation

Black hole•accretion
diskThis mechanism may be importantfor launching the AGN outflows
such as “ultra-fast outflows (UFOs)”

We apply our spectral model of the UV-line driven disk winds to theobserved spectra of 1H 0707-495, and examine the disk wind model
can explain its Fe-K features.

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flow•Construct a spectral model

We have already constructed “a new X-ray spectral model” of an accretion
disk wind for the UFO in PDS 456 (Hagino et al. 2015).

n- A 3-D geometry and velocity/

density distributions expected inthe UV-line driven winds

102×10s- Self-consistently calculate bothof the emission and absorption

Unfolded Spectrumof construction
for the accretion
disk wind modelSuzaku
dataof PDS 456!
• Flowyra
1. Determine the ionization structurein the wind (spatial distributions of Te andsimulation
nimile2. 3-D radiation transfer
calculation by using the Monte Carlo simulationrP

ion abundance) by calculating the ionization state along the stream lines

2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University

6 / 18Radiation transfer calculation•Radiation transfer is calculated by simulating the interactions of photons and matterwith Monte Carlo method••

We use our software “MONACO” (Odaka+ 2011) for the Monte Carlo simulations
Biconical geometry is adopted (originally used for disk wind in CV (Knigge+ 1995))
disk wind
Physical processes
accretion disk
X-raysource

•
•
•
•

Photoionization
Photoexcitation
Compton scattering
Doppler effect•

We assume Ω/4π=0.15 (45°−56.3°) (based on the hydrodynamic simulationsof UV-line driven winds (e.g., Proga+ 2000))•The launching radius Rmin is assumed to satisfy vwind=vesc @Rmin

2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University

7 / 18makesan angle
θ0 ≡ (θmin+ θmaxby)/2.
Thus,
R0 = d tan
geometry
is divided
0 . Thelines
2010a).
Thisofgeometry
is defined
threeparameters.
All θstream
in the wind
into converge
100 shells.
shell hasanis equal
width dona logarithmic
scale.
at a Eachfocal point,which
at a distancebelow
the source. Thewind is launched
Radialis defined
as a We
functionof lengthfrom Rvelocityon the disc,first assume
thatalongd = Rtheand Rmax =l 1.5Rmin .
min to Rmax
min streamline
This means that the wind fills a cone between!θmin = 45◦ and"θβmax = 56.3◦ i.e. has solid
Rminangle Ω/4π = 0.15. vWe
defineameanlaunchradius
R0 from the .mean streamline i.e. it (4.5)
r (l) = v0 + (v∞ − v0 ) 1 −We determine the density and velocity distributions
in +thel wind as follows:Rminmakes an angle of θ0 ≡ (θmin + θmax )/2. Thus, R0 = d tan θ0 . The geometry is divided
Outflow
velocity(CAKlaw)：obtainedby solvingscale.
the equation of motion
into
100 shells.
Eachshellvelocity
has an equal
logarithmic
β determines
the windacceleration
law, width
whileonv0 aandv∞ are an initial radial velocity at
Radialvelocity
is definedas (Castor+1975)
a functionof length along
streamlineltheradial
UV-linedrivenwinds
l = 0ofandvelocityatl=∞.
This equation
is an theextensionof theclassical CAK!
"βmodel (section 2.2.5). The azimuthal velocity at thelaunching
point R0 is assumed toRmin
vr (l) = v0 #+ (v∞ − v0 ) 1 −.
(4.5)
Rmin + lbe the Keplerian velocity vφ0 = GM/R0 .
Accordingtovelocity：conservation
angularmomentumlaw,
conservation,
isare
writtenas radiala functionof at
Rofwhile
the angular
βRotational
determines
thewind accelerationv0 andvvφ∞momentum
an initial
velocity

Density / velocity distributions•--l = 0 and radial velocity at l = ∞. This equation is an extension of the classical CAK
R0model (section 2.2.5). The azimuthal
velocityv (R)= vφ0 at the. launching point R0 is assumed to (4.6)#φR
be the Keplerian velocity vφ0 = GM/R0 .
The turbulent
velocity
vturbmomentum
is composedof intrinsic
vof
velocityt andAccording
to angularconservation,vφ isturbulent
writtenas (Schurchavelocity
functionR2007)
Turbulentvelocity：constantturbulence
vt + velocity
shear& Done-shear (Appendix A4 of Schurch & Done 2007).
R0 vr (i 1)v(i)r(4.6)
vturb (i) =vvφt(R)+ = v φ0 R .
vrtotal(i) −massv121)
r (i −According to massconservation,
outflow
Theref√vturb (i) = vt +, rate Ṁwind is constant. (4.7)
The turbulent velocity vturb is composed of intrinsic
turbulent velocity vt and velocity
12
densitydistribution：conservationn is written as
Densityof the mass
shear (Appendix A4 of Schurch & Done 2007).
where index i refers to the shell number and vr is a radialvelocity.
2 ΩṀwind = 1.23m(vr (i)p nv− rv4πDr (i − 1)√vturb (i) = vt +(4.7)
4π,= 1.23mp nvr12
4πD2 (cos θmin − cos θmax ).
(-where challenges
index i andrefers
to ofthenumberandEra”
vr @Rikkyo
is a radial
velocity.
2015.10.22 “Prospects,evolution
AGNshellmodeling
in the Astro-H
University

8 / 18

Ionization structure•The ionization structure (Te, ion abundance distribution) of the wind is sequentiallycalculated from the inner shell to the outer shell. (this is the input of the Monte
Carlo simulation)

X-ray source

Inner shell

EIon abundance, Electron
temperature

EFEE

Ionization
calc.

・・・

Ionization
calc.
EFEIonizationcalc.

Transmitted+Reprocessedphoton

EFEEFE

Direct photonE

Ion abundance, Electron
temperature

Outer shellE・・・

Ion abundance, Electron
temperature

Ionizing spectrum is determined by the observations
2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University

9 / 18•Spectra are extracted 2 different viewing
anglesθincl=46 deg

fast・thin

Normalized
flux flux
Normalized

Simulated spectraθincl=58 deg221••

accretion disk

Blue-shifted absorption & broad emission
like the observation
At lare θincl-high density→deep absorption
observe slower component→broad

0.1
0.05
0.04
0.05
0.04

Normalized
fluxflux
Normalized

X-raysource45<47 deg
θincl=46 deg (Δθ=1deg)

total (Transmitted+reprocessed)

1
0.5 Transmitted
0.4
0.5
0.3
Reprocessed
0.4
0.2
0.3
0.2
0.1

slow・dense45<47 degblue-shifted
absorption
lines

broad
emission line
6810

68

1057<59 deg

1214
Energy (keV)1214
Energy (keV)deg)
2 θincl=58 deg (Δθ=157<59 deg
21

shift to lower energy
abs. edge

total10.5
0.4 Transmitted
0.5
0.3
0.4
0.3
0.2
0.2 Reprocessed
0.1

Width, depth and position varydepending on viewing angle θincl

0.1
0.05
0.04
0.05
6
2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo
University
0.04
6

deep&broad
absorption lines

810

12810

1214

10 (keV)/ 18
Energy14

Application to the observations of 1H 0707-495•

We apply our spectral model to the observed spectra of 1H 0707-495.
Fe-Kfeatures

10−3

•

Continuum absorption:Low ionized gas (ξ=L/nr2 102) is required

10−4

keV2 (Photons cm−2 s−1 keV−1)

Continuum
absorption•Fe-K feature:created by the highly
ionized gas (ξ~103-4)

10−5Soft excess
0.5

12Energy (keV)

510➡ Use our disk wind model for only the Fe-K features. The continuum

spectra are fitted with the partial covering absorption model. The softexcess is not considered here.

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Parameter estimation
We model the spectrum observed in 2010.09.15 (Obs12), which seems to be
free from continuum absorption i.e. steepest spectrum.

•

By using a wind model optimized for PDS 456, we estimate parameters.

Parameters

L2-10 4×1042 erg/s
Γ

2.6v0vturb

vturb

1000 km/s

β1keV2 (Photons cm−2 s−1 keV−1)

•

10−3

10−4

χ2ν=132.0/89
θincl=60.6° (58.8−63.1)

5×106M⦿

Rmin

25Rs0

Ω

0.15−2v∞

0.2c−4r

MBH

10−52

Ṁwind 4×10-2M⦿/yrObs12246Energy (keV)

810➡ Reproduced the structure above ~7 keV2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University

12 / 18

Application to all the observations of 1H 0707
10−3

Obs1

10−410−510−3

keV2 (Photons cm−2 s−1 keV−1)

As in the case of PDS 456, by changing only the viewing angle θincl, we fit all theA disk wind interpretation for 1H 0707-495 7observations.
keV2 (Photons cm−2 s−1 keV−1)

keV2 (Photons cm−2 s−1 keV−1)

•Obs2

10−4

10−52−1
810Obs410−410−51046Energy (keV)

10−38

Obs510−410−52210−3810

Obs710−410−52246
Energy (keV)

10−38−2

Obs810−410−5χ08Obs1010210−310−410−52046
Energy (keV)

86
Energy (keV)

810Obs910−410−520

Obs1110222410−310−3

2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University
210−2

s−1 keV−1)

6Energy (keV)

s−1 keV−1)

48Obs62−2210−310206
Energy (keV)−1keV2 (Photons cm−2 s−1 keV−1)

6Energy (keV)

keV2 (Photons cm−2 s−1 keV−1)

4χχkeV2 (Photons cm−2 s−1 keV−1)

2410−2−20

10−1s−1 keV−1)

10−5
2−22keV2 (Photons cm−2 s−1 keV−1)

6Energy (keV)

χ4keV2 (Photons cm−2 s−1 keV−1)

210−3

10−3

10−4−1−2

χkeV2 (Photons cm−2 s−1 keV−1)
χ0χ

0−2Obs31χχ110−34

6Energy (keV)

8Obs121013 / 18keV2 (Photons cm−2 s−1 kkeV2 (Photons cm−2 s−1 k10−5
210−5
210−4−210−52

As in the case of PDS 456, by changing only the viewing angle θincl, we fit all theobservations.
0χ

χ

0−2

6
Energy (keV)

10−3810Obs1010−410−52

χ0

χ

−246
Energy (keV)

10−38102keV2 (Photons cm−2 s−1 keV−1)

40

Obs11

10−410−5246
Energy (keV)

10−3810Obs1210−410−5200

χ

2keV2 (Photons cm−2 s−1 keV−1)10−4Application to all the observations of 1H 0707
keV2 (Photons cm−2 s−1 keV−1)

keV2 (Photons cm−2 s−1 kχ•10−4−2−2−2−46
Energy (keV)

10−38102Obs13

10−410−5246
Energy (keV)

10−38102keV2 (Photons cm−2 s−1 keV−1)

4keV2 (Photons cm−2 s−1 keV−1)

Obs14

10−410−521

χχ

0−20−1−446
Energy (keV)

810χkeV2 (Photons cm−2 s−1 keV−1)

2−246
Energy (keV)

10−3810Obs15

10−410−521

χkeV2 (Photons cm−2 s−1 keV−1)

20−124

6
Energy (keV)

10−3810246Energy (keV)

810SuzakuObs

10−410−5
20−2246Energy (keV)810

2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University
Figure 5. Observed spectra and MONACO models with v = 0.2c and Ṁ
/Ṁ= 0.2 for all the observations.

14 / 18

10−3Obs310−4χ2ν=52.5/55
θincl=64.1° (57.8−66.9)
10−52keV2 (Photons cm−2 s−1 keV−1)

keV2 (Photons cm−2 s−1 keV−1)

Application to all the observations of 1H 0707
Obs1510−4

χ2ν=43.1/51
θincl=70.9° (67.1−74.6)
10−5
210

χ

r

1

10−3−10−1−22•

46
Energy (keV)

810

246
Energy (keV)

810

Characteristic behavior of the observed spectra are well reproduced, though χ2 is
not very good in some of the observations.

➡ The spectra of 1H 0707-495 can be explained by the ultra-fast outflow (Mwind/MEdd=0.2, v=0.2c)

2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University15 / 18

Comparison with NuSTAR data
The extrapolation of our wind model for Obs15 gives a good fit to theNuSTAR spectra•

Higher energy spectrum is also explained by our disk wind model!!
keV2 (Photons cm−2 s−1 keV−1)•10−3
5×10−4

XMM-Newton Obs15
NuSTAR FPM-A/B (60001102004)
Wind model for XMM Obs15

χ2ν=99.41/80

2×10−410−4
5×10−52×10−52χ

0−2−4510Energy (keV)

2015.10.22 “Prospects, challenges and evolution of AGN modeling in the Astro-H Era” @Rikkyo University

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Launching mechanism of the wind•

We have successfully reproduced the observed spectra by the disk wind model,
but there is a small residual at the emission line

➡ suggesting a larger solid angle of the windrkeV2 (Photons cm−2 s−1 keV−1)

Publications of the Astronomical Society of Japan (2014), Vol. 67, No. 4
10−3

Obs12

Continuum-driven wind insuper-Eddington accretion diskfor r = 100 rS (gray), 500 rS (light green), 2000 rS (lightmagenta), and 4000 rS (blue). Here, this rate is timeaveraged in the elapsed time between t = 70 s and 200 s.
Emission line is10−4
We find in this panel that the velocity of outflow is larger
under-predicted
in axis in the vicinity
than the escapevelocity near the rotation
thismodelof the black hole.
Thewindangularsize of high-velocity outflow
tends to broaden with an increase of the radius. In par10−5
ticular,although the high-velocity outflow appears only in2
the direction of θ ! 35◦ at r = 100 rS , the angular size of0the high-velocity outflow extends up to ∼ 20◦ and ∼ 50◦
at −2
r = 500 rS and 2000 rS . Eventually, the matter is blown◦◦away−4 with speed of >v esc in the wide angle, 0 –85 (see248 rS is not 10that Ṁesc,r615 at r = 4000
r = 4000rS ). We find
0100
200
300
400
Energy (keV)
R/rs Hashizume et al. 2015
so sensitive to the angle. It is slightly smaller near the rotaThewithplanelargersolid angle
is aroundnaturally expected in the continuum driven disktion axis
andwindequatorialand slightly
enhanced20◦ . Notethatinmass
flux via the high-velocity
is mildly colwind
super-Eddington
accretion
limated (compare with sine curve [solid line]). We conclude
The wind in 1H 0707-495 is possibly a continuum-driven disk windthat the mass is blown away with speed of > v esc in all
2015.10.22“Prospects,challengesand evolutionof AGN
in the Astro-H Era” @Rikkyo University
17 / 18.
directions
somewhat
focusingaround20◦modeling•➡

58

Conclusions

We constructed a new X-ray spectral model for the ultra-fastoutflows, and applied it to the observed spectra of 1H 0707-495.

• The strong Fe-K feature in all the observed spectra of 1H0707-495 are successfully reproduced by our disk windmodel.

• The NuSTAR data of 1H 0707-495 is also consistent withthe disk wind model.

• Our disk wind model under-predict the emission lines.

This suggests a continuum radiation driving mechanism
instead of the UV-line driving.

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