Competitive Intelligence Platform - an Example - Yair Dambinsky
with the collaboration of Guido Risaliti, Yair Krongold, Fabrizio Nicastro, Chris Reynolds
description
Transcript of with the collaboration of Guido Risaliti, Yair Krongold, Fabrizio Nicastro, Chris Reynolds
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