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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