Your SlideShare is downloading. ×
0
DDeetteerrmmiinniinngg tthhee SSppiinn ooff 
SSuuppeerrmmaassssiivvee KKeerrrr BBllaacckk HHoolleess 
aass AAGGNN CCeenntt...
• Rotating BH drags the spacetime around it 
(LLeennssee –– TThhiirrrriinngg 11991188). 
• Particle in an orbit with an ax...
BBaarrddeeeenn –– PPeetttteerrssoonn ((11997755) 
Kerr BH + Disk 
Alignment 
+ Viscosity
How 
can it be observed? 
From tthhee sshhaappee ooff tthhee aaccccrreettiioonn ddiisskk 
Warped disk RBP
How 
can it be observed? 
FFrroomm tthhee 
PPrreecceessssiioonn ooff 
ppcc ssccaallee jjeettss 
Right Ascension (02h 40m) ...
How 
can it be observed? 
FFrroomm tthhee 
ssttrruuccttuurree 
ooff tthhee 
rraaddiiooggaallaaxxyy 
iinn kkppcc ssccaallee...
Large scale Radio Structure (kpc) 
Radio Jet (pc) 
Warped disk 
RBP
JJeett pprreecceessssiioonn iinn ppcc ssccaalleess 
How do we observe 
them 
1 pc 1 mas 
VLBI: 
Very Long Baseline Interfe...
VLBI
3C279 
superluminal 
velocities 
1992 
1994 
1996 
1998 
light years 20 40 60 80
3C273 
Jets 
are 
wiggled
Angle with the line 
of sight is different 
Velocity of each component is constant 
Velocity is different for the differen...
We find a sistematic effect in bobs vs. h, 
sugesting precession precessão 
x observer 
jet 
W f 
h 
y 
(Abraham & Romero ...
13 
11 
9 
7 
5 
3 
1960 1965 1970 1975 1980 1985 1990 1995 2000 
Time 
bobs 
C2 
C4 
C5 
C6 
C7 
C8 
C9 
C3 
C10 
-50 
-7...
Precession ooff QQSSOO JJeettss aatt kkppcc SSccaalleess
Precession model using the 
Bardeen-Peterson effect
Locus of Pprec/MBH = constant 
3C345 
3C279 
BH spin (a *) log (RBP/Rms) 
3C273 
OJ287 
3C120 
(Caproni, Mosquera Cuesta &...
Precession from a BH binary system 
(Abraham & Romero 1999)
Locus of Pprec/MBH = Constant 
3C345 
BH spin (a *) log (RBP/Rms) 
3C273 
3C279 
OJ287 
3C120
RBP is too small to be measured with current ang. resolution !! 
SShhaappee ooff tthhee aaccccrreettiioonn ddiisskk 
Keple...
NGC 1068 
7 ´ 6 arc min 
Optical image 
(1.1 m Hall telescope) 
30 arc sec 
HST
1 kpc 
HST VLA 
Wilson & Ulvestad 1987
NGC 1068: Seyfert 2 Gallimore et al.(2004) 
VLBA 1.4 GHz 
core 
counter jet 
100 pc 
2 pc 
VLBA 5 GHz 
masers H2O 
free-fr...
Lodato & Bertin, A&A 398, 517 (2003)
Initial jet direction MBN = (0.8 – 1.2) ´ 107 
MMd = (8.6 – 9.4) ´ 106 M 
S= (1.1 – 1.5) ´ 106 g cm-2 
0 Σd (ξ )=Σ0 ξs 
...
Talign = < 1.5 ´ 105 Y 
Alignment Time should be smaller than Lifetime of the AGN and 
Jet Phases ~ (1-2)*10^5 years
(derived from the movement 
of the components close to the core) 
NGC 1068 in kpcscales: Wilson & Ulvestad (1987) 
1 
kpc ...
dJ BN 
dt 
=−2πsinϕ∫ΩLT Ld (r )rdr 
ϕ(t )=ϕ0e 
( t−t0)/Tali} Sheuer & Feiler (1996) 
(t−t0 )/T ali 
Pprec (t )=P0 e 
P0≃T ...
The way to infer the KBH Radius: 
Combining info from: 
RBP vs. a* and Talign vs. a*
The End
Determining the Spin of Supermassive Kerr Black Holes as AGN Central Engines
Determining the Spin of Supermassive Kerr Black Holes as AGN Central Engines
Upcoming SlideShare
Loading in...5
×

Determining the Spin of Supermassive Kerr Black Holes as AGN Central Engines

238

Published on

0 Comments
0 Likes
Statistics
Notes
  • Be the first to comment

  • Be the first to like this

No Downloads
Views
Total Views
238
On Slideshare
0
From Embeds
0
Number of Embeds
8
Actions
Shares
0
Downloads
1
Comments
0
Likes
0
Embeds 0
No embeds

No notes for slide

Transcript of "Determining the Spin of Supermassive Kerr Black Holes as AGN Central Engines"

  1. 1. DDeetteerrmmiinniinngg tthhee SSppiinn ooff SSuuppeerrmmaassssiivvee KKeerrrr BBllaacckk HHoolleess aass AAGGNN CCeennttrraall EEnnggiinneess HHeerrmmaann JJ.. MMoossqquueerraa CCuueessttaa ((IICCRRAANNeett//IIttaallyy -- IICCRRAA//BBrraazziill) AAnnddeerrssoonn CCaapprroonnii ((UUNNIICCSSUULL//BBrraazziill) ZZuulleemmaa AAbbrraahhaamm ((IIAAGG--UUSSPP//BBrraazziill)
  2. 2. • Rotating BH drags the spacetime around it (LLeennssee –– TThhiirrrriinngg 11991188). • Particle in an orbit with an axis non-parallel to the spin of the BH will experience torques • The orbit will precess Kerr BH + Particle Precession
  3. 3. BBaarrddeeeenn –– PPeetttteerrssoonn ((11997755) Kerr BH + Disk Alignment + Viscosity
  4. 4. How can it be observed? From tthhee sshhaappee ooff tthhee aaccccrreettiioonn ddiisskk Warped disk RBP
  5. 5. How can it be observed? FFrroomm tthhee PPrreecceessssiioonn ooff ppcc ssccaallee jjeettss Right Ascension (02h 40m) Radio Jet (pc) S2 NE Warped disk RBP Declination (-00o 13') 07s.4 07s.0 30" 35" C S1 Right Ascension Offset (arcsec) 0.8 0.4 0.2 0.0 -0.2 -0.4 0.4 0.2 0.0 06s.6
  6. 6. How can it be observed? FFrroomm tthhee ssttrruuccttuurree ooff tthhee rraaddiiooggaallaaxxyy iinn kkppcc ssccaalleess
  7. 7. Large scale Radio Structure (kpc) Radio Jet (pc) Warped disk RBP
  8. 8. JJeett pprreecceessssiioonn iinn ppcc ssccaalleess How do we observe them 1 pc 1 mas VLBI: Very Long Baseline Interferometry 1.4 GHz
  9. 9. VLBI
  10. 10. 3C279 superluminal velocities 1992 1994 1996 1998 light years 20 40 60 80
  11. 11. 3C273 Jets are wiggled
  12. 12. Angle with the line of sight is different Velocity of each component is constant Velocity is different for the different components Position angle in the plane of the sky of each component is different
  13. 13. We find a sistematic effect in bobs vs. h, sugesting precession precessão x observer jet W f h y (Abraham & Romero (1999) plane of the sky line of sight γ= 1 √1−β2 b b sin f =  = 3.9o f0 app - b f 1 cos = 10o h0 = -120 g= 10.8 
  14. 14. 13 11 9 7 5 3 1960 1965 1970 1975 1980 1985 1990 1995 2000 Time bobs C2 C4 C5 C6 C7 C8 C9 C3 C10 -50 -70 -90 -110 -130 -150 -170 C9 1960 1965 1970 1975 1980 1985 1990 1995 2000 Time h (deg) C2 C3 C4 C5 C6 C7 C8 C10 P = 16 years
  15. 15. Precession ooff QQSSOO JJeettss aatt kkppcc SSccaalleess
  16. 16. Precession model using the Bardeen-Peterson effect
  17. 17. Locus of Pprec/MBH = constant 3C345 3C279 BH spin (a *) log (RBP/Rms) 3C273 OJ287 3C120 (Caproni, Mosquera Cuesta & Abraham, 2004, ApJ, 616, L99)
  18. 18. Precession from a BH binary system (Abraham & Romero 1999)
  19. 19. Locus of Pprec/MBH = Constant 3C345 BH spin (a *) log (RBP/Rms) 3C273 3C279 OJ287 3C120
  20. 20. RBP is too small to be measured with current ang. resolution !! SShhaappee ooff tthhee aaccccrreettiioonn ddiisskk Keplerian outer disk Rigid body Warped disk RBP
  21. 21. NGC 1068 7 ´ 6 arc min Optical image (1.1 m Hall telescope) 30 arc sec HST
  22. 22. 1 kpc HST VLA Wilson & Ulvestad 1987
  23. 23. NGC 1068: Seyfert 2 Gallimore et al.(2004) VLBA 1.4 GHz core counter jet 100 pc 2 pc VLBA 5 GHz masers H2O free-free continnum
  24. 24. Lodato & Bertin, A&A 398, 517 (2003)
  25. 25. Initial jet direction MBN = (0.8 – 1.2) ´ 107 MMd = (8.6 – 9.4) ´ 106 M S= (1.1 – 1.5) ´ 106 g cm-2 0 Σd (ξ )=Σ0 ξs s = 1 Rex = 1 pc How long does it take to get aligned? What is the value of RBP
  26. 26. Talign = < 1.5 ´ 105 Y Alignment Time should be smaller than Lifetime of the AGN and Jet Phases ~ (1-2)*10^5 years
  27. 27. (derived from the movement of the components close to the core) NGC 1068 in kpcscales: Wilson & Ulvestad (1987) 1 kpc υjet=0.17c Jet was formed 104 years ago
  28. 28. dJ BN dt =−2πsinϕ∫ΩLT Ld (r )rdr ϕ(t )=ϕ0e ( t−t0)/Tali} Sheuer & Feiler (1996) (t−t0 )/T ali Pprec (t )=P0 e P0≃T alin
  29. 29. The way to infer the KBH Radius: Combining info from: RBP vs. a* and Talign vs. a*
  30. 30. The End
  1. A particular slide catching your eye?

    Clipping is a handy way to collect important slides you want to go back to later.

×