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Physics and Astrophysics of Supermassive Black Holes July 10 - July 14, 2006 Santa Fe, New Mexico （ Monday, July 10 th , 4:40 pm – 5:00 pm ）. (Oscillations) Beats and Rotation of the Accretion Disk around Super massive Black Hole s SgrA*. Makoto Miyoshi （ NAOJ ）.
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Physics and Astrophysics of Supermassive Black Holes
July 10 - July 14, 2006 Santa Fe, New Mexico
（Monday, July 10th,4:40 pm – 5:00 pm）
Makoto Miyoshi（NAOJ）
WithZhi-Qiang Shen, T. Oyama , S. Kameno,H. Nagai, A. Doi , R. Takahashi , Y. Kato, & K. Asada
The most convincing Black Hole today from Density Measurement.
Precise Mass Measurements M~3.6*106Msun
MBH at the Closest Distance ~8kpc
The Largest Apparent SchwarzschildRadius
Rs ~ 8micro-arcsec
Black Hole Shadow
will be observed
soon at SgrA*
(Falcke, Melia et al 00)—Bardeen’s talk
--Mueller’s too
Quasi Periodic Variation at Flare of IR&X-ray
(Genzel03, Eckart06:Aschenbach04)
?Existence of Bright Blob Moving
at the Last Stable Orbit ?
?Does the Period mean an Orbital Period?
Precise Period Determination is important but difficultbecause the Flare is not so Frequent. Also because the Flare Duration is less than about 3 hours.
SgrA*
Motions of Stars at GC.
NIR Observations
(Genzel et al)
Periodicity was found during NIR flaring of SgrA* P=16.8±2.0 min.(Genzel 03)
P=22 min.( Eckart et al 06)
Genzel et al. 2003
Periodicity is also found from X ray flare. P~100 s, 219 s, 700 s, 1150 s, and 2250 s were suggested
(analysis by Achenbach et al. 2004)
–Belanger’s Talk
1. At Radio SgrA* is always bright enough to observe (1Jy at 43GHz). 2. At mm to sub-mm Radio wave also short time flaring are detected (Miyazaki et al. Zhao et al…). --We can expect to detect similar kinds of QPO in radio wave. We checked the data of SgrA* obtained VLBA. We detected the radio QPO from observations at 43GHz taken at 8th March 2004, just 1.5 days after the millimeter wave short time flare.
↑Example of Radio Flaring of SgrA* ( New detection by Miyazaki).
１ｍａｓ
VLBA,86GHz(3.5mm）
Shen et al. (2005)
VLBI gives us high spatial resolution(～0.1mas）.So we can also investigate the spatial distributions of QPOs in the image of SgrA* if exist.
NGC4258
(Herrnstein et al 99,
Miyoshi et al 95)
A example of investigations of spatial distributions of water maser line in the image.
At 43GHz
(VLBA)
(whole time integrations)
Rectangulars0.1mas（10Rs)×0.15mas（15Rs)
We defined 209 rectangular regions
and measured time series of flux densities within the regions from 360 snap shot maps with 5 min integrations.
209（＝19×11） in all
Then we check the spatial distributions of the QPOS.
We define these 209 small regions.
Intensity
time
Time variations of intensity in the 209 rectangulars ( red line=noise level)
661-05min
Left (0.1 mas east)
Center
Right (0.1 mas west)
Noiselevel
Time variations of flux densities in the central 3 rectangulars, & sum-up
Periods Spectra of the central 3 rectangulars (MEM)
peaks
６２．２
２９．３
１９．４
１７．０
１３１．６
５５．３
３０．２
１７．３
１２．８
２２４．８
４８．４
２３．８
１７．７
１４．３
Left, 0.1mas-east
center
Right 0.1mas-west
We show you the statistics of the whole 209 rectangulars
Sum-up amplitude of 209 regions
Central 3 regions
Statistics on spatial distributions of the periods
Strong confinements occur around P=12.9,17.2,30.1, ＆ 55.8 min.
（also check at P＝22.2min）
Sum up 209 rectangulars
P=２２．２m
P=17.2 m
P=55.8 m
P=12.9 m
P=30.1 m
Period (min)
Distribution size (1sigma)
Size=SQRT((X^2+Y^2)
Ｘ-direction
Y-direction
Period (min)
We found Periodic Structure Change Patterns
with the 4 Periods
1) We searched periodic structure change patterns around the 5 periods.
2) And found characteristic change patterns of the 4 periods. (P=16.8, 22.2, 31.35, &56.35 min.)
3) First, we show you the mapping method for searching periodic structure change patterns in the next slides.
P=56.35, 31.35, 16.8min
P=22.2 min
← →oneperiodcircle( P min)
← → sub-divisions (8 phases)
→ phase 1 map
→ phase 2 map
→ phase 3 map
→ phase 4 map
1) This manner will enhance
the periodic structure change pattern
in images.
2) Very similar, almost the same uv- coverages
– free from the instrumental effect of
different synthesized beam shape -
→ phase 5 map
→ phase 6 map
→ phase 7 map
→ phase 8 map
uv coverage of each phase map
phase １ phase 2 phase 3 phase 4
phase 5 phase 6 phase 7 phase 8
change pattern
of the P=56.35 min
① 1 peak
② 2 peaks
③ 2 peaks
2 peaks appear
during the half period.
④ 2 peaks
⑤ 2 peaks
⑥ 1 peak
1 peak appears during
the other half period.
⑦ 1 peak
⑧ 1 peak
change pattern
of the P=56.35 min
① 1 peak
② 2 peaks
This seems as if the central intensity of the period is larger than those of next outer radii.
We observe the change with edge-on angle.
③ 2 peaks
④ 2 peaks
⑤ 2 peaks
⑥ 1 peak
⑦ 1 peak
⑧ 1 peak
change pattern
of the P=31.35 min
① 2 peaks
② 1 peak
③ 2 peaks
Opposite
Opposite
④ 2 peaks
⑤ 1 peak
Opposite
Opposite
⑥ 2 peaks
All Phase maps show different opposite peak number
with the corresponding map half periods apart.
⑦ 1 peak
⑧ 1 peak
change pattern of
the P=31.35 min
① 2 peaks
This can be explained with 3 bright arms model.
We observe the pattern motion from edge-on angle. Far side is unseen.
② 1 peaks
Opposite
③ 2 peaks
Opposite
④ 2 peaks
Opposite
⑤ 1 peak
Opposite
⑥ 2 peaks
⑦ 1 peak
⑧ 1 peak
change pattern
of the P=22.2 min
Peak is the cross in the figure.
Peak position moves
along east-west direction
with the period.
P=22.2min
enlarged images along east-west direction
This become clearer
at P=16.8 min case.
change pattern
of the P=16.8 min
P=16.8min
① Peak at right side
② Peak at center side
The peak position seems to move with the period.
This can be explained with one arm structure pattern rotating with the period.
And we observe it from edge-on .
③ Peak at left side
④ Peak at left side
⑤ Peak at left side
⑥ Peak at center
⑦ Peak at right side
⑧ Peak at right side
of the P=16.8 min
Distribution of Amplitude of the P=16.8min
We Fourier-Transformed the Time Series Variations of each Cells in the 8 Phase Maps, derived the Amplitude & Delay Phase of the P=16.8min Change Pattern.
Distribution of Phase Delay of the P=16.8min
If we cut out at the east-west line….
Three Phase Jumps at the Center
(degree)
(Jy)
Phase------
Phase connected------
Amplitude----
Radius from the center (mas)
P=16.8min
P=16.8, 22.2, 31.35, 56.35min
Roughly saying ３：４：６：１０
（20:15:10:6 in frequency domain)
P=16.8 & 22.2 min; circular change pattern one-arm (?) structure
P=31.35 min; three-arms (?) structure.
P=56.35 min; confined at the center.
The motion changes are too rapid v > c, light velocity
The changes are not real motion but pattern changes.
These should relate to oscillations of accretion disk!
A Example of Disk Oscillation Modes
Lense-Thirring Precession of Accretion Disks
Draza MarkovicFrederick K. Lamb
University of Illinois at Urbana-Champaign
http://research.physics.uiuc.edu/CTA/movies/lt/index.html
Line of sight velocitycan be estimated from QPO spectra
In real data there are the indications.Intrinsic periodic oscillations occurred at the disk will be Doppler shifted by the rotation velocity in the disk when we observe from outside.
A
B
C
A B C
Bump moves
Intensity Maps of the Periods
P= 62.15min(upper）
P=131.6min（middle）
P=224.8min（bottom）
The Peak Position Moves
From East to West as Periods
Become Long.
P= 131.6min
P= 224.8min
Rotation！
1.9mas,(about193Rs)
Intensity Maps of rather wideband periods
(from the top)
P= 5- 80min
P= 80-160min
P= 160-240min
P= 240-320min
P= 320-400min ≒ｃｏｎｓｔ.
The Peak Position Moves
Towards west as Periods
Become long.
P= 80-160min
P= 160-240min
P= 240-320min
P= 320-400min
If this means the effect
of Doppler shift,
It must be Rotation!
1.9mas,about 193Rs
↑Displacement of the peak position
in P=16.80 min. phase-maps
↑Doppler shift obtained from the tendency of the whole periods (QPO) distributions :
<east> blue shifted --------------------------------- red shifted <west>
Assuming the structural change pattern of P=16.8min has the same direction of the disk rotation, the above two facts mean that the disk is almost edge-on, tilted the north side towards us about some degrees.
PQPO-1 ∝MBH
In Stellar Black Hole
1kHz (103Hz) QPO ; BH mass=1 Msun
In Case of SgrA*
P=55.3min(3380sec) ー 3×10-4Hz
means MBH=3.4×106Msun！
--Almost the same as the precise measurements with IR M~3.6×106Msun --
The Confined P=55.3min QPO of SgrA*
should be the similar kind of ‘kHz QPO’
The intrinsic image is obscured and broadened because of scattering effect by circum-nuclear or inter stellar plasma (∝λ２）.
Shen 他(05), Bower他(04) investigated the effect.
Interstellar Plasma Scatters the Radios Image of SgrA* (Scattered Size ∝λobs２）.
So VLBI Images of SgrA* are Believed to have No Intrinsic Information so far.
But our results suggest that the image are NOT TOTALLY OBSCURED.
There remain some imprints!
VLBI images of the SgrA*(Lo et al. ’99)
From GC1998.
1. Radio images of SgrA* has some imprints of intrinsic structure at 43GHz (though scattered and broadened).
2. 4 QPO periods ( P=16.8,22.2, 31.15, & 56.35min) are real variation periods. Clear periodic change patterns seen at these 4 periods. These mean disk oscillations.
3. Using Doppler effected QPO spectra, line of sight velocity can be measured.
4. VLBI SgrA* image is almost edge-on rotating disk.
P=56.35, 31.35, 16.8,&22.2min
QPO observations with spatial resolution will reveal the black hole accretions disk.
But we need the understanding what is QPO in detail.
おしまい
That’s all.
Thanks!
