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. • 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. BBaarrddeeeenn –– PPeetttteerrssoonn ((11997755)
Kerr BH + Disk
Alignment
+ Viscosity

4. How
can it be observed?
From tthhee sshhaappee ooff tthhee aaccccrreettiioonn ddiisskk
Warped disk RBP

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. How
can it be observed?
FFrroomm tthhee
ssttrruuccttuurree
ooff tthhee
rraaddiiooggaallaaxxyy
iinn kkppcc ssccaalleess

7. Large scale Radio Structure (kpc)
Radio Jet (pc)
Warped disk
RBP

8. JJeett pprreecceessssiioonn iinn ppcc ssccaalleess
How do we observe
them
1 pc 1 mas
VLBI:
Very Long Baseline Interferometry
1.4
GHz

9. VLBI

10. 3C279
superluminal
velocities
1992
1994
1996
1998
light years 20 40 60 80

11. 3C273
Jets
are
wiggled

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. 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. 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. Precession ooff QQSSOO JJeettss aatt kkppcc SSccaalleess

16. Precession model using the
Bardeen-Peterson effect

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. Precession from a BH binary system
(Abraham & Romero 1999)

19. Locus of Pprec/MBH = Constant
3C345
BH spin (a *) log (RBP/Rms)
3C273
3C279
OJ287
3C120

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. NGC 1068
7 ´ 6 arc min
Optical image
(1.1 m Hall telescope)
30 arc sec
HST

22. 1 kpc
HST VLA
Wilson & Ulvestad 1987

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. Lodato & Bertin, A&A 398, 517 (2003)

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

27. Talign = < 1.5 ´ 105 Y
Alignment Time should be smaller than Lifetime of the AGN and
Jet Phases ~ (1-2)*10^5 years

28. (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

29. 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

31. The way to infer the KBH Radius:
Combining info from:
RBP vs. a* and Talign vs. a*

32. The End