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Transcript of Martin Elvis, MIT, 4 March 2008 Reynolds C. with the collaboration of Guido Risaliti, Yair Krongold,...
Martin Elvis, MIT, 4 March 2008
Reynolds C.
with the collaboration ofGuido Risaliti, Yair Krongold, Fabrizio Nicastro, Chris Reynolds
and many others…
X-ray absorption and AGN Structure
Eclipsing in AGN:
Martin ElvisHarvard-Smithsonian Center for Astrophysics
Martin Elvis, MIT, 4 March 2008
The Quasar Puzzle
Z=6.4 SDSS spectrum, SED
Jiang et al., 2007, ApJL, 666, L9, VanDen Berk et al., 2001,AJ,122, 549
z~6 quasarz~1-3 SDSS template
CIV MgIILy
• AGN SEDs, spectra same– Over 6 decades of Luminosity– Over 13 Gyr of cosmic time
• Unchanging structure– Determined within BH sphere of
influence: “The Nucleus”
• Complex phenomenology– Non-trivial structure
• Answers affect cosmic feedback
Martin Elvis, MIT, 4 March 2008
AGN ‘funnel wind’ StructureElvis 2000 ApJ 545, 63; 2003 astro-ph/0311436; 2009 in
preparation
Conical geometry
Pressure balance
Multi-wavelength approach, uniting all atomic physics features in AGNs
Thin
Wind
Martin Elvis, MIT, 4 March 2008
Eclipses in Astronomy
…but useful in astronomy:earth is a spherebinary starsblack hole masses1st test of GRextrasolar planets…
“These late eclipses of the sun and moon portend no good to us.” King Lear I:2:98
…and for quasars
Martin Elvis, MIT, 4 March 2008
Scales of Quasar/AGN Components
RRss1100
10010000
Warm Absorbe
r
11
molecular torus
Optical/UV continuu
m
Black Hole
High Ionization
CIVHeIIOVI
Low Ionization MgII,
FeII Balmer series
NIR contJHK
101055
NELRH [OIII] Coronal
lines
X-ray Cont.
broad Fe-K
Compton Wind
BELR
X-ray Spectral Variabilityinin absorptionabsorption
Martin Elvis, MIT, 4 March 2008
100,000 Rg:100,000 Rg: Cold Obscuring Torus
RRss1100
10010000
Warm Absorbe
r
11
molecular torus
Optical/UV continuu
m
Black Hole
High Ionization
CIVHeIIOVI
Low Ionization MgII,
FeII Balmer series
NIR contJHK
101055
NELRH [OIII] Coronal
lines
X-ray Cont.
broad Fe-K
Compton Wind
BELR
Martin Elvis, MIT, 4 March 2008
100,000100,000 RRSS The Dusty Molecular Torus
• Flattened optical & X-ray obscuring region Lawrence & Elvis 1982
• type1type2 AGN = ‘Unified Scheme’
• Rsub= 1.3x105 L0.10.5 M8
0.5 T1500-2.8 RS
• NH~1024cm-2; H/R~1• Puffed up by IR on dust?
Krolik 2007, Murray 2007
Is this the whole story?Is this the whole story?
Martin Elvis, MIT, 4 March 2008
NGC1365: an AGN Structure Laboratory
• Face-on barred spiral D~25Mpc
• Bright X-ray source fx~1mCrab, logLx=42.2 Ward et al. 1978 MN 223, 788
• LBol~10-3 Ledd(M/M8)-1
• logMBH ~ 7.3 - 7.8 M
– M-bulge, M-K
• Obscured: NH>1022.5cm-2
• Highly variable NHighly variable NHH::
– Key to study of AGN Key to study of AGN structurestructure
EPIC-MOS
Martin Elvis, MIT, 4 March 2008
NGC1365: Compton thick/Thin Transitions
Constant E<2keV Thermal component
Constant flux narrow Fe-K component
log log NNHH>24.2>24.2
log Nlog NHH~23.5~23.5
log Nlog NHH~23.7~23.7
Compton thickthin transitions are rare:
4/30 Matt et al. 2003
1/11 Guainazzi et al. 2005
NGC1365 transitions reliably often:
~7/13 observations Compton-thin
NGC1365 is a special objectNGC1365 is a special object
Martin Elvis, MIT, 4 March 2008
NGC1365: Fairly Rapid Compton thin/thick transitions
2002Dec 24, t= 0 d2003Jan 16, t=23 d2003Feb 09, t=47 d2003Aug13, t=232d
23 days185
days
Risaliti et al., 2005a, ApJL, 623, L93
NH>~1024cm-2 in 3 weeks:
–requires R<10R<1044RRss <4.5x1017cm,
–ne>109 cm-3
•What is changing?–fx(intrinsic)?
– c.f. disk cooling time > 30R201/2d
– ionization?– (ionization) ~ 103
– NH– Hard to reconcile with standard Hard to reconcile with standard torustorus
Martin Elvis, MIT, 4 March 2008
NGC1365: Really Rapid Compton thin/thick transitions
Risaliti et al., 2007, ApJL, 659, L111
•Chandra: Compton ThinThinThickThickThin inThin in 4 4 daysdays
– NH>~1024cm-2 in 2 days
–ne>109 cm-3
• R(NH) < few 1000 Rs
Inconsistent with Inconsistent with standard torusstandard torus
2 days 2
days
Martin Elvis, MIT, 4 March 2008
3000R3000Rss A More Compact Torus
• Need another ‘torus’ location near BELR
• Accretion disk windAccretion disk wind?– Also toroidal– Large H/R natural– No support problem
• Dust radiation pressure driven?– dust survives in disk to
R>~2000 Rs (Tdisk<1000 K)
• Magnetic support? Kartje, Königl & Elitzur, 1999 ApJ 513, 180
Should see fluorescent Fe-K Should see fluorescent Fe-K from other parts of torusfrom other parts of torus
Elvis et al., 2004, ApJL, 615, L25; Risaliti et al., 2005a, ApJL, 623, L93
Martin Elvis, MIT, 4 March 2008
3000R3000Rss Where is the narrow Fe-K?Suzaku Cycle 2: Elvis (PI) et al.
Suzaku/NGC5548: Fe-K• Suzaku 2-month monitoring of
NGC5548• High S/N 240 ksec spectrum• Fe-K narrow core:
FWHM = 5500 km/s = 50+/-15eV
R~3000RR~3000Rgg = Obscuring material?= Obscuring material?I.e. Rs ~23 l-d MBH = 6.7x107 M
• But factor ~4 in ~30days– Fe-K core = constant
– Larger than 3000 Rs?
– Non-Keplerian motions?– Light travel time smearing?– Not a worry yet.
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.ct
3ct
2ct
Martin Elvis, MIT, 4 March 2008
Moving inwards: Warm Absorbers
RRss1100
10010000
Warm Absorbe
r
11
molecular torus
Optical/UV continuu
m
Black Hole
High Ionization
CIVHeIIOVI
Low Ionization MgII,
FeII Balmer series
NIR contJHK
101055
NELRH [OIII] Coronal
lines
X-ray Cont.
broad Fe-K
Compton Wind
BELR
Dusty Wind
Martin Elvis, MIT, 4 March 2008
3000R3000Rss Where are the Warm Absorbers?
• Highly ionized, blueshifted (~1000km/s): Wind• Common: ~50% of all AGNs and quasars• Location? Factor 106 in radius proposed
– NELR to HiBELR
• Mass loss rate uncertain by factor 106
• Is AGN feedback important to galaxy evolution or not?
Kaspi et al. 2002, ApJ, 574, 643
Chandra HETG: 900ksec NGC3783
Martin Elvis, MIT, 4 March 2008
How to Measure the Warm Absorber Location
Step function change
Gradual WA response
Nicastro et al., 1999, ApJ, 512, 184
WA response to continuum is not instantaneous:
• ‘Ionization time’ and ‘Recombination time’ measure measure nnee
• UX ~ 4 LX/R2
• WA measures Ux
• hence radius, radius, RR
Martin Elvis, MIT, 4 March 2008
Small RWA in NGC4051: XMM/RGS
~30 ksec
High State HSLow State LS
Low State
High State
• 4X flux increase in ~30 ksec• WA changes!
• Not continuous U(r)
• WA is dense & compact• Not NELR
Krongold et al., 2007, ApJ, 659, 1022
Martin Elvis, MIT, 4 March 2008
Small RWA in NGC4051: XMM/EPIC
XMM EPIC Light Curve
log Ux(t), predicted
from photoionization
equilibrium
log Ux(t), measured
Krongold et al., 2007, ApJ, 659, 1022
• Two Warm Absorber components stay close to photo-ionization equilibrium
Martin Elvis, MIT, 4 March 2008
Small RWA in NGC4051: XMM/EPICKrongold et al., 2007, ApJ, 659, 1022
• Low Ionization (LIP) R<3.5 l-dR<3.5 l-d
• High Ionization (HIP) R=0.5-1.0 l-dR=0.5-1.0 l-d
Martin Elvis, MIT, 4 March 2008
NGC4051: An Accretion Disk Scale Warm Absorber
• Rules outRules out Narrow Emission Line Region Narrow Emission Line Region (kpc scale)
• Rules outRules out Obscuring molecular torus Obscuring molecular torus (Krolik & Kriss, 2001)
• Minimum dust radius, rsubl(NGC4051) ~ 12-170 light-days
• Rules outRules out Low Ionization (H Low Ionization (H broad emission line broad emission line regionregion (BELR); R(H) = 5.9 light-days (Peterson et al. 2000) = disk?
• Co-located with High Ionization BELR?: HeII = wind?= wind?• Driven by UV absorption lines, as in O-star winds? Driven by UV absorption lines, as in O-star winds? Murray et al.1995
light-dayslight-days 5510101515
HIP
~HeII ~HeII
BELRBELR
HH BELRBELR
Dusty molecular
torusLIP
Dust sublimation radius
Krongold et al., 2007, ApJ, 659, 1022
Warm Absorber
Martin Elvis, MIT, 4 March 2008
50R50Rs s Narrow Fe-K Absorption
RRss1100
10010000
Warm Absorbe
r
11
molecular torus
Optical/UV continuu
m
Black Hole
High Ionization
CIVHeIIOVI
Low Ionization MgII,
FeII Balmer series
NIR contJHK
101055
NELRH [OIII] Coronal
lines
X-ray Cont.
broad Fe-K
Compton Wind
BELR
Dusty Wind
Martin Elvis, MIT, 4 March 2008
50R50Rs s NGC1365: Compton WindRisaliti et al., 2005, ApJL, 630, L129
EPIC-MOS
K/K observed
observed
Curves of growth
Log NH 23
24
High VtHigh Vt
EW
EW
Log NH
pnmos
• 4 strong absorption lines: FeXXV, FeXXVI K-, K-
• EW~100eV– Broad: vturb~500-1000 km/s
• K/K small - saturated:– High NH>1023.5 Compton thick
• Super-High Ionization WA: – logUX~0, R ~ 50(M/M8)-1 Rs
• Blueshifted • 2500 5000 km/s in
18mo. – acceleration?
Martin Elvis, MIT, 4 March 2008
50R50Rs s NGC1365: Failed Compton Wind
• V(Fe-K) << Vesc ~50,000(M/M8)-1 km/s
– high U– L/LEdd ~ 10-3
– ‘‘failed wind’failed wind’? or transverse
= ‘hitchhiking gas’ ?= ‘hitchhiking gas’ ? Murray & Chiang – Filters X-ray continuum
from outer gas…– Lowers ionization
state…– Enabling UV line driven
acceleration (as in O-star winds)
– Disk geometry essentialDisk geometry essential
Risaliti et al., 2005, ApJL, 630, L129
X-ray continuum
source
Martin Elvis, MIT, 4 March 2008
4.4. <30 R<30 RSS X-ray Continuum Eclipses
RRss1100
10010000
Warm Absorbe
r
11
Optical/UV continuu
m
Black Hole
High Ionization
CIVHeIIOVI
Low Ionization MgII,
FeII Balmer series
NIR contJHK
101055
NELRH [OIII] Coronal
lines
X-ray Cont.
broad Fe-K
Compton Wind
BELR
Dusty Wind
Martin Elvis, MIT, 4 March 2008
NGC1365: Rapid X-ray Continuum Eclipses
Risaliti et al., 2007, ApJL, 659, L111
• Compton ThinThickThin in 4 days•Now consider constraints on X-ray Continuum source 2
days 2 days
Martin Elvis, MIT, 4 March 2008
<30 R<30 RSS X-ray Continuum Eclipses
• Dimensions of X-ray source: Ds = Vc x Tecl
• If Vc ~ 104 km/s DDss ~ 10 ~ 101414 cm cm
• Can’t be much higher (to avoid overionization, from iron line width)¯ If lower, even smaller X-ray source
• Black hole mass in NGC 1365:– Log MBH/M= 7.3 (0.3,0.3) M-
(Ferrarese et al. 2005)
– Log MBH/M= 7.86 (0.15,0.3) M-
LK (Marconi & Hunt 2003)
• X-ray source size < 33 RX-ray source size < 33 RGG
Risaliti et al., 2007, ApJL, 659, L111
VK
X-ray source
Eclipsing matter
Ds
DC
Martin Elvis, MIT, 4 March 2008
Future Continuum Eclipses
Schwartzschild eclipse profile
Kerr eclipse profile
Resolving Eclipse profile:• Size/shape/1-D emissivity
map• Kerr/Schwartzschild? C.Reynolds
• Close to resolving?• Suzaku cycle 3 propoal
Martin Elvis, MIT, 4 March 2008
<30 R<30 RSS X-ray Relativistic Fe-K Eclipses
RRss1100
10010000
Warm Absorbe
r
11
Optical/UV continuu
m
Black Hole
High Ionization
CIVHeIIOVI
Low Ionization MgII,
FeII Balmer series
NIR contJHK
101055
NELRH [OIII] Coronal
lines
X-ray Cont.
broad Fe-K
Compton Wind
BELR
Dusty Wind
Martin Elvis, MIT, 4 March 2008
<30 R<30 RSS Broad Fe-K Eclipses
• Red wing on Fe-K is 1% over continuum. Ambiguous.
• NGC1365 has strong red wing& strong Fe-K absorption lines High Fe abundance?
• Gone in Compton-thick Gone in Compton-thick spectrum.spectrum.
• DDFe-K Fe-K < 10< 101414 cm, <33 R cm, <33 RSS
Risaliti et al., 2007, ApJL, 659, L111
Martin Elvis, MIT, 4 March 2008
<30 R<30 RSS Future: Future: Tomography of Fe-K
Apply Binary physics• Ingress, egress
successively cover/uncover red-/blue- shifted Fe-K
• Clean, definitive experiment
• Establish Establish – Fe-KFe-K– RotationRotation– z(R)z(R)
• Goal of Suzaku Cycle 3 proposal
• More sensitive mission could probe metric in detail
Reynolds, Risaliti, Elvis, …
Blue wing occulted
Red wing occulted
Martin Elvis, MIT, 4 March 2008
Mission for Future Eclipse Mapping of AGNs
• Weeks-long observations of each source - not an observatory-class mission
• 10 x S/N of Chandra in ~1hour vs. 4 hours -large area, high count rate
• Better spectral resolution• Only ~1 arcmin spatial resolution (HPD)
Extreme Physics ExplorerExtreme Physics Explorer5m
40
Elvis, Astro-ph/0403554; 2004, Nucl. Phys. B 134, p.78-80
Martin Elvis, MIT, 4 March 2008
X-ray Eclipses and AGNs
• Several techniques probe scales from 105- 10 Rs
• A simpler, physically driven picture of AGN Structure
• Makes quasar puzzle of uniformity semi-understandable
rr
gg
101010010000
1001001000100000
WA
NAL
HiBEL
Dusty
ObscurerBroadFe-K
X-rayCont.
Compton(failed)Wind
NarrowFe-K
Martin Elvis, MIT, 4 March 2008
Eclipse results confirm & extend ‘funnel wind’ modelElvis 2000 ApJ 545, 63; 2003 astro-ph/0311436
Becoming a secure basis for physical wind models: will allow extrapolation
Martin Elvis, MIT, 4 March 2008
The Restless AGN Accretion Disk
• Replace observational with physical names
• Active Disk ‘atmosphere’ at all radii – mechanism must work at all radii
• Not standard ‘hot corona’• More like Solar Corona
rr
gg
101010010000
1001001000100000
WARWARMM
Dust driven Wind
BroadFe-K
X-rayCont.HOHO
TT
NarrowFe-K
Line driven Wind
Compton driven
Wind
COLDCOLD
failed Wind L<LEdd
failed Wind
UVCont.
Martin Elvis, MIT, 4 March 2008
Reynolds C.
AGN X-ray Eclipses
…give new views of AGN structure