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Transcript of Thanks to our sponsor
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Thanks to our sponsor
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• M. Aller (UM)• R. Bender (Munich)• G. Bower (NOAO)• A. Dressler (OCIW)• S. Faber (UCSC)• A. Filippenko (UCB)• K. Gebhardt (Texas)• R.Green (NOAO)• L. Ho (OCIW)
• T. Lauer (NOAO)• J. Kormendy (Texas)• J. Magorrian (C U)• J. Pinkney (Michigan)• D. Richstone (Mich)• C. Siopis (Mich)• S. Tremaine
(Princeton)
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3c175
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Weighing planets, stars, galaxies or black holes
vcirc = GM/r
depends on the orbit
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Kepler
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M84
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Orbit Superposition (Schwarzschild’s method)
• Assume a mass distribution.• Compute the gravitational forces.• Follow all the orbits.• Sum the orbits to match the observed
velocities.• Failure rules out the mass distribution.
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The current demographic picture
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Results of 15 year effort
• Most bulges have BH (97% so far).• BH mass tracks main-body
parameters (L, ).
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Second parameter?
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• Bulge M/L ~ 3x10-3 h• Density - 2.5x105 Msun/Mpc³ for h=.65 (Yu &
Tremaine) - 4.8x105h² Msun/Mpc³ (Aller &
Richstone) - consistent results from different
datasets.- S = 2.2x105 Msun/Mpc3
- 6 – 9x105 (Fabian & Iwasawa) qso+X-ray background (and similar from Barger).
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?BIG PROBLEM?The X-ray background energy exceeds
the available sources of energy in known supermassive black holes.
(the known population of SBH seems just adequate for the quasar energy).
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A note on backgrounds• Any background can be expressed
in terms of the cosmic microwave background energy density (about 1eV/cm3).
• uqso ~ 10-4
bh ~ uqso-1(1 - -gw – ejections)• ustars ~ 1
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What should theorists learn from the observations?
• BH can accrete stars, gas, degenerate objects, dark matter; only gas accretion yields the correct Soltan number.
• Most BH growth has occurred during the quasar epoch. Is this also the epoch of bulge formation? Of major mergers?
• How does BH growth connect to galaxy formation and evolution?
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Collapse vs mergers
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Ideas for the M4 relation in the context of collapse or evolution
• The bh growth is limited by a mass budget - competition w/ star formation(Burkert & Silk).
• BH growth limited by energy conservation (Silk & Rees, Blandford, A.R.King). Ciotti & Ostriker, pure core collapse).
• The bh growth is limited by a momentum budget (Fabian)
• BH growth is limited by angular-momentum (AGR).
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Feedback versus initial conditions
• Most feedback models are likely to eject material only in certain directions (for example, bubble break-out along direction of fastest density gradient).
• Condition dependent models are fragile against changes in the environment.
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Antennae
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• Any initial formation mechanisim evolves through the merger hierarchy (investigated through SAMs by Haehnelt & Kaufman).
• BH merge or form binaries, triples, etc. – Ejections? The “last parsec” problem? – The dispersion of the M- relation is an
important clue.
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LISA sky
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Grav waves.
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Implications• BH growth spurt during quasar era (is
this the epoch of bulge formation?). – What is the pedigree of BH and
galaxies?• M- relation is a powerful clue. • Co-Evolution! --- feeding, bar disruption,
core scouring, mergers --- bh growh connected to galaxy evolution.
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Cognitive style of powerpoint