2001/3/30 1 X-ray Observation of Accretion Disk in AGN K. Hayashida (Osaka University)

2001/3/301

X-ray Observation of Accretion Disk in AGN

K. Hayashida (Osaka University)

2001/3/302

X-ray 　 Observational Study of AGNs

Spectrum Power Law Cold Absorber Iron Line Soft X-ray Excess Reflection Hump Warm Absorber

Timing Image

Outflow, starburst component etc.

VSOP…Jet … Blazar

2001/3/303

Soft X-ray Excess

Discovery Mkn509 (HEA1 A2 LED+MED), Singh et al., 1985, ApJ, 297, 633. Mkn841 (EXOSAT), Arnaud et al., 1985, MNRAS, 217, 105. Excess Soft X-ray Emission above Extrapolation of Pow

er Law Spectrum determined at High Energy High Energy Tail of the UV-Bump ? Lower kT version of Soft (Disk) Component found i

n Stellar Black Hole Candidates kT~1keV for SBHC T M ∝ -1/4

MKN509MKN841

2001/3/305

Correlation with the UV emission

ROSAT Walter & Fink, 1993, A&A,274, 105

in Soft X-ray band

(Soft Excess / Power Law) @0.2-0.4keV (UV flux / 2keV Flux)

in Soft X-ray band

2001/3/306

IUE / ROSAT / Ginga (Walter et al.,1994, A&A,285, 119)

( ) exp( / )UVcutN E E E E 1.3 3.5( ) exp( / )cutN E E E E fE

Model A Model B

2001/3/307

Spectral Shape (Cut-off energy)

Model A Large Scatter in Ecut

Model B Ecut ranges 40-80eV

2001/3/308

Origin of the Soft Excess Component

Thermal Emission from (Optically Thick) Accretion Disk

Inverse Compton Emission by Hot Corona , Cooled Pairs etc. Seed: UV photons from the Disk

Reprocessing of Hard X-ray photons (Thin Thermal Emission)

2001/3/309

Soft X-ray Excesswith ASCA

NGC4051, Mihara et al. 1994 PG1211+143, Yaqoob et al., 1994. NGC5506, Wang et al., 1996 3C273, Cappi et al., 1998 Reynolds, 1997

24 Type1 AGNs (RQ+RL) ; Soft Excess in 7 objects Murakami, 1997.

10AGNs; Soft Excess (f0.5>0.1) was found in 9 objects BB kT~0.1keV or Brems~0.2keV

2001/3/3010

Soft X-ray Excess (Murakami, 1997)

Correlation with UV-flux

fse(ASCA0.5keV) Correlates with fse(ROSAT0.1-0.4keV) .

BB luminosity >Ledd

More Sophisticated model is needed ?

fse:Soft Excess Comp/ Power Law Comp at 0.5 keV

2001/3/3011

Efficient Way to see the Soft Excess …Narrow Line Seyfert 1 (NLS1)

Seyfert Type 1 whose Broad Emission Line Width is Narrow. (???)

Broad Line Region= High Density Regionn>108 /ccr~0.01pcPermitted Lines.. H_

Narrow Line Region= Low Density Regionn~103-106 /ccr~100pcPermitted + ForbiddenLines.. [OIII]

Type1[OIII]/H_<3

BLS1 yesFWHM>2000km/s (1500km/s)

NLS1 yes FWHM<2000km/s

YesFWHM= 400- 1000km/s

Type2 No(Hidden) Yes

2001/3/3012

Boller et al., 1997

Common for NLS1 at Some Level

X-ray Studies with ROSAT

Prototype=IRAS13224-3809 Steep Soft X-ray Index =4.4±0.2 Rapid & Large Amplitude Variability

2001/3/3013

ASCA … Spectrum Above 2keV

Two Components Spectrum (e.g. Otani et al.1996) Soft Component ~BB kT

=0.1-0.2keV Hard Tail above 2 keV

Hard PL Index Steeper (>2) than BLS1 (Brandt et al., 1997)

See Leighly, 1999.

10-6

10-5

10-4

10-3

10-2

100 101

IRAS13224-3809

Ph

oto

ns/

cm2

/ke

VEnerygy (keV)

Black BodykT = 92.7 eV +-1.9 eV

Power Law =1.93+-0.09

2001/3/3014

Statistical Properties

Narrow HWidth

Steep Soft X-ray Spectrum

Rapid / Large Ampl.X-ray Variability

2001/3/3015

X-ray Spectrum of NLS1s 　（ ASCA)

10-6

10-5

10-4

10-3

10-2

100 101

IRAS13224-3809

Ph

oto

ns/

cm2

/ke

V

Enerygy (keV)

Black BodykT = 92.7 eV +-1.9 eV

Power Law =1.93+-0.09

10-6

10-5

10-4

10-3

10-2

100 101

IZW1

Ph

oto

ns/

cm2

/ke

V

Enerygy (keV)

Black BodykT = 99.7 eV +-40.2 eV

Power Law =2.33+-0.05

2001/3/3016

0.05

0.06

0.070.080.09

0.1

0.2

0.3

0.4

10-2 10-1 100 101 102

Soft Component (BB Fit)

kTB

B (

keV

) @

sour

ce fr

am

e

BB-comp/POWL-comp @ 0.5 keV

PKS0558

IRAS13224

h0707(98)IZw1

Pg1404

h0707(98)

PHL1092

kTBB vs Soft Excess Ratio

2001/3/3017

1039

1040

1041

1042

1043

1044

1045

102 103 104 105 106 107 108

Mass from rbb=3RsMass from rbb=0.5Rs

L Bla

ck B

od

y(e

rg/s

)

Mass (M) from r

bb=3Rs or 0.5Rs

Soft Component (Blackbody Fit)

Eddington Limit

Izw1

NGC4051

PHL1092

BB Fit ->Area->BH SizeL 4R2 BT

4

M R /(0.5or3 3km)

Hayashida， 2000, New Astronomy Review,44,419

2001/3/3019

0

0.125

0.25

0.375

0.5

5 104 1 105 1.5 105 2 105 2.5 105

IRAS13224-3809

Co

un

t R

ate

(c

/se

c/2

SIS

)B

GD

Su

btr

act

ed

Time (sec)

0

0.15

0.3

0.45

0.6

0 100 5 104 1 105 1.5 105 2 105

H0707-495(95mar)

Co

un

t R

ate

(c

/se

c/2

SIS

)B

GD

Su

btr

act

ed

Time (sec)

0

2

4

6

8

0 100 5 104 1 105 1.5 105 2 105

Ark564

Co

un

t R

ate

(c

/se

c/2

SIS

)B

GD

Su

btr

act

ed

Time (sec)

0

0.075

0.15

0.225

0.3

0 100 5 104 1 105 1.5 105 2 105

PG1404

Co

un

t R

ate

(c

/se

c/2

SIS

)B

GD

Su

btr

act

ed

Time (sec)

0

1.5

3

4.5

6

0 100 5 104 1 105 1.5 105 2 105

NGC4051

Co

un

t R

ate

(c

/se

c/2

SIS

)B

GD

Su

btr

act

ed

Time (sec)

ASCA Light Curves of NLS1

2001/3/3020

Lx vs Mvar （ BLSy1 / NLSy1)

Cf Results from Excess VarianceBy Tuner et al.(1999) & Leighly (1999)

BLS ｙ１　 NLSy1

1039

1040

1041

1042

1043

1044

1045

103 104 105 106 107 108 109

Ginga (LAC)

ASCA (GIS)

Lbol

=LEdd

Lbol

=10LEdd

Lbol

=0.1LEdd

Lx

2-1

0ke

V(e

rg/s

)

Mass (M) from X-ray variability

BLS1

MCG-6-30-15

NGC5548

NGC3227

NGC4051NGC4151

1039

1040

1041

1042

1043

1044

1045

103 104 105 106 107 108 109

Lx

2-1

0ke

V(e

rg/s

)

Mass (M) from X-ray variability

NLS1

RE1034RE1034

PHL1092

PKS0558

IRAS13224PG1404

H0707(95)

H0707(98)NGC4051

PG1244

Hayashida， 2000, New Astronomy Review,44,419

2001/3/3021

HFWHM vs Mvar

600

800

1000

3000

5000

7000

103 104 105 106 107 108 109

H

FW

HM

(km

/s)

Mass (M) from X-ray variability

NLS1

PG1211

RE1034

PHL1092

NGC5548

IRAS13224

NGC3227

H0707

Mkn509

NGC4051

PG1404

MCG-6-30

NGC4151

BLS1

BLS1:

107-108Mo

NLS1:

105-107Mo

Hayashida， 2000, New Astronomy Review,44,419

2001/3/3022

103

104

105

106

107

108

103 104 105 106 107 108

Nbb/Npo(0.5keV) > 4

Nbb/Npo(0.5keV) <=4

Mas

s (M

)

from

r bb=

0.5R

s

Mass (M) from X-ray variability

Mass from Variability v.s. Mass from Blackbody Component

IRAS13224

PG1404PHL1092

H0707_98

H0707_95

Akn564

MBBfit(0.5Rs) vs Mvar for NLS1

Hayashida， 2000, New Astronomy Review,44,419

2001/3/3023

Can we reconcile the Contradiction ?

For MBBfit < Mvar Inclination Effect

cos Factor … MBBfit gives under-estimate

Tc > Te Effect MBBfit gives under-estimate, to

o.

cos/)0()( MM

2)/(*)()( TeTcTcMTeM

103

104

105

106

107

108

103 104 105 106 107 108

Nbb/Npo(0.5keV) > 4

Nbb/Npo(0.5keV) <=4

Mas

s (M

)

from

r bb=

0.5R

sMass (M

) from X-ray variability

Mass from Variability v.s. Mass from Blackbody Component

IRAS13224

PG1404PHL1092

H0707_98

H0707_95

Akn564

Hayashida， 2000, New Astronomy Review,44,419

2001/3/3024

Accretion Disk ?

If Soft Component is thermal emission from accretion disk, Observations of NLS1 provide important clue to theoretical work.

e.g. Slim 　 Disk 　 Model (Mineshige et al. 2000, PASJ, 52, 499)

2001/3/3025

Peculiar Spectral Feature around 1keV

Otani et al (1996), Hayashida et al (1997), Leighly et al. (1997)

0.2-0.3c blue shifted absorption edge ?

0.5-0.6c blue shifted absorption line ?

Emission line ?

2001/3/3026

Chandra Observations of BLS １ｓ (NGC3783, NGC5548)

Narrow Absorption Lines from H-like or He-like ions of C, N, O, Ne, Na, Mg, Si, Fe

OVII, OVIII edge were NOT detected. (NGC5548)

V(blueshift)~200-500km/s V(turb)~100-200km/s

NGC5548(LETG;86ks)

2001/3/3027

Reflection from Ionized Disk Model (Ross & Fabian, 1993, MNRAS,261, 74)

2001/3/3028

Chandra / XMM Observation of Soft X-ray Excess in NLS1s

Sensitive to Lower Energy Band Higher Energy Resolution with Gratings No Strong Absorption / Emission Features

in the Soft X-ray Spectra of NLS1s TonS180 (Chandra) Tuner et al., PG1404(Chandra) Nandra et al., Mrk766(XMM)

2001/3/3029

TonS180 ACIS/LETG Simlutaneous with A

SCA and FUSE +HST (UV)

Tuner et al., 2001, ApJ, 548, L13.

No significant absorption feature

Instrumental

2001/3/3030

PG1404 (Chandra MEG) Nandra et al., 2001

2001/3/3031

PG1404 (Chandra MEG)Nandra et al., 2001

2001/3/3032

Sorry, No Time (Ability) to Cover

Comparison with Disk Component in Stellar Black Hole Candid

ates X-ray Spectra of Super Eddington Sources in

nearby galaxies Disk Component and Jet Component in micro

quasars

2001/3/3033

Soft X-ray Excess : Summary

Soft X-ray Excess does exist Correlate with UV Enhanced in NLS1s Examination with Theoretical Accretion Di

sk Model is expected Correlation / Lag to UV, Hard X-ray would

be examined.

2001/3/3034

Fe K Fluorescence Line

Discovery by ArielV ， HEAO-1 Reflection Hump found by Ginga

Interpreted 　 with Reflection Model Line Broadening discovered by ASCA

Disk Line Model

2001/3/3035

Disk Line Model (e.g. Fabian, 2001, astroph.0103438)

2001/3/3037

Luminosity Dependence of the Line Intensity (Nandra et al., 1997, ApJ, 487, L91)

2001/3/3038

XMM Observation of MCG-6-30-15

Williams, Fabain 2001

2001/3/3039

Disk Line

Energy [keV]

Lin

e In

tensi

ty

[ph

s/s/

keV

/cm

^２

]

from Matsumoto

MCG-6-30-15

Tanaka et al., 1995, Nature, 375, 659

i=30deg, 6rg-40rg

2001/3/3040

Alternative Model

Line Emission region must be far away from several Rs

Variability of Continuum / Line(Matsumoto, Inoue, 2000)

2001/3/3041

Energy

Vari

abili

ty

Energy

Flu

xＤｉｓｋｌｉ

ｎｅmodel

EnergyV

ari

abili

ty

Energy

Flu

x(F

obs)

Alternative Interpretation

PL

PL

Two warm absorbers to reproduce the σ(E)　 ξ≈ 50～ 100 　　　 (a dotted line) ξ≈　 500～ 1000

Variable Ionized Absorber

(Matsumoto, Inoue, 2000)

2001/3/3042

Chandra HEG Observation … Narrow Line Component

NGC5548 (Yaqoob, et al.,2001,ApJ,546,759)

•Narrow Line

•6.40+-0.03keV

•FWHM=4515 (+3525-2645)km/s

•*) does not rule out broad component

2001/3/3043

Disk Lines of Other Elements ? Warm Absorber -> Disk (Emission) Line

Brandaurdi-Raymont et al., 2001, A&A, 365, L140

2001/3/3044

Chandra data can be fitted with Warm Absorber Model (Lee,2001, astroph0101065)

2001/3/3045

Disk Line or Fe-K Line

Fe-K Line is found in most of Radio Quiet AGNs Eq. Width is anti-correlated with Lx Broad Line Width and Red Wing are found in se

veral Seyferts, which usually are interpreted with Line emission from several Rs

Little correlation between Line / Continuum is against the simple disk line model

Narrow Line component may be taken into account

2001/3/3046

What can we suggest to VSOP2?

Disk Emission observed in X-rays … No apparent relation to Jet (VSOP’s Main Topic?)

What discriminates Radio Loud / Radio Quiet AGNs ?

Can VSOP(2) resolve accretion disk ? CAUTION: Ultimate Higher Angular Resol

ution will be obtained in X-rays

2001/3/3047

MAXIM mission (X-ray Interferometer)

100arcsec

0.3arcsec

From http://maxim.gsfc.nasa.gov

Also Note XMAS project in Japan