A CONCEPT FOR CHERENKOV TELESCOPES FOR ULTRA-II Florian Goebel, Anton Kabelschacht, Eckart Lorenz.
The structure of the nuclear stellar cluster of the Milky Way and A. Eckart, R. Genzel,D. Merritt,...
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Transcript of The structure of the nuclear stellar cluster of the Milky Way and A. Eckart, R. Genzel,D. Merritt,...
![Page 1: The structure of the nuclear stellar cluster of the Milky Way and A. Eckart, R. Genzel,D. Merritt, T. Alexander, A. Sternberg, J. Moultaka, T. Ott, C.](https://reader030.fdocuments.in/reader030/viewer/2022032605/56649e745503460f94b73d60/html5/thumbnails/1.jpg)
The structure of the nuclear stellar clusterof the Milky Way
andA. Eckart, R. Genzel,D. Merritt, T. Alexander, A. Sternberg,
J. Moultaka, T. Ott, C. Straubmeier, F. Kul, L. Meyer
Rainer Schödel
IAU AssemblyPragueAugust 2006
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Stellar Cusps around Supermassive Black Holes
age of a galaxy nucleus > relaxation time steady state solution of Fokker-Planck equation predicts stellar cusp
• single mass: ~r -7/4 (Bahcall & Wolf, 1976; Lightman & Shapiro 1977)
• multiple masses: ~r -3/2-7/4 (depending on stellar mass)
• size of cusp ~0.1-0.2 rinfluence, BH
relaxation time in center of Milky Way a few 109 yr we expect to observe a stellar cuspGC is only such system that can be resolved into individual stars.
Amaro-Seoane et al. (2004)
cusp
collisions destroy stars
large scale cluster
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distance from Sgr A* (arcsecs)
First AO results with NACO/VLT
0.1
1
10
100
0.1 1 10 1000.1
1
10
100
isothermal cluster modelbroken power law, α1 =1.37, α2=2NACO Ks≤17, correctedSHARP, K≤15, *5.5NAOS/CONICA, H≤19.8, low confusion
radius from SgrA* (arcsecs)
ρ*( R )=3x107 (R/arcsec)-1.4M pc-3
Genzel et al. 2003
Cusp
large scale cluster
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New Analysis of GC Stellar Cluster• use of uniform data sets: seeing limited + AO assisted
• extent of cusp/location of break radius?
• spatially variable extinction taken into account
• Refined methods: PSF fitting with spatially variable PSF analysis of number counts and background light no binning of counts
• 2D structure of cluster, symmetry of cluster
Above all ... to convince the remaining skeptics!
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640
light
yea
rsSeeing Limited Imaging
ISAAC/VLT 2.09 mFWHM ~0.4”(color image from J+2.09 m imaging)
150”
/ 1
8 lig
ht y
ears
IRS 7
Sgr A*N
EFOV of AOobservations
Point source extractionand background estimation with StarFinder(Diolaiti et al., 2000)
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Background light density inner 2.5 pc
broken power-law: good fit!
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AO Imaging Data
NACO/VLTadaptive opticsresolution ~0.06”
~40”40” FOV
~10000 stars with magK ≤ 17.5
IRS 16
IRS 13
IRS 7
Sgr A*
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Extinction in the Central pc
IRS 16
IRS 13
IRS 7
Sgr A*
“mini-cavity”
Extinction derivedfrom narrow-bandimaging (2.00, 2.06, 2.24,& 2.27 m, = 0.06 m);assumption stars are blackbodies with T = 5000 K, AK~-1.75
AK = 1.8 - 3.6 mag(contours AK = 0.2 mag)
Outflow directed SSWfrom IRS 16/Sgr A*?(see poster by K. Muzic)
Schödel et al., subm. to A&A
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2D extinction corrected density map
Adaptively smoothed:40 stars for each pixel
smoothing radius~0.5” near Sgr A*~1” near edge of image
Some “clumps” appearto be present in the cluster.One of them is the well-known co-moving groupIRS 13E.(see Maillard et al., 2004;Schödel et al., 2005)
Schödel et al., subm. to A&A
Sgr A*
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Stellar surface number density inner 0.5 pc
magK= 9.75 - 17.75
single power law: no satisfying fit!
rbreak = 7”1”
broken power-law: good fit!
αcusp = 0.250.1αcluster = 0.60.1
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Horizontal branch/red clump stars
magK= 14.75 - 15.75
Dominated by low mass/old stars
young/high mass stars
see also Genzel et al. (2003), Paumard et al. (2006)
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Summary
1. Extinction: New method for deriving extinction Indications for outflow? No significant influence on number counts
1. Extinction: New method for deriving extinction Indications for outflow? No significant influence on number counts
2. Structure of Cluster: Clearly a broken power-law! Presence of “clumps” - relation to recent star formation?
1. Extinction: New method for deriving extinction Indications for outflow? No significant influence on number counts
2. Structure of Cluster: Clearly a broken power-law! Presence of “clumps” - relation to recent star formation?
3. Cusp: Detected with high significance; shallower than Bahcall-Wolf (~R-0.75) solution (due to mixing of different masses) Extent of cusp: ~7” (~0.25 pc) Effects of mass segregation.
1. Extinction: New method for deriving extinction Indications for outflow? No significant influence on number counts
2. Structure of Cluster: Clearly a broken power-law! Presence of “clumps” - relation to recent star formation?
3. Cusp: Detected with high significance; shallower than Bahcall-Wolf (~R-0.75) solution (due to mixing of different masses/classes) Extent of cusp: ~7” (~0.25 pc) Effects of mass segregation.Results are in good agreement with theory. Models can now be fine-tuned with the exact values for the GC cluster.
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Thank you for
your attention!