Quasar & Black Hole Science for GSMT Central question: Why do quasars evolve?
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Transcript of Quasar & Black Hole Science for GSMT Central question: Why do quasars evolve?
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Quasar & Black Hole Science for GSMT
Central question: Why do quasars evolve?
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BACKGROUND
(1) 2DF, SLOAN, 2Mass, First and other surveys are revealing an ever more complete census of the
quasar population from z=0 to 7.
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Background (continued)
The peak of quasar activity was at z~2, when the Universe was only 30% of its present age.
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BACKGROUND (continued)
Reionization of intergalactic hydrogen happened at z= 6.5-7.0
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Background (continued)
A detailed picture of the central engine has been developed Black hole and accretion disk paradigm
Mostly inferred from spectroscopy and spectropolarimetry of spatially unresolved sources, in the X-ray, UV, optical, IR and radio.
Advances in numerical methods and theory
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Background (continued)
Black holes have been linked to the stellar/baryonic/CDM components of galaxies
● M(BH) -- (bulge) correlation has been found out to the Virgo cluster
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Background (continued)
Feedback to the IGM via UV radiation and shock energy is probably also important
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Background (continued)
The quasar phenomenon and the evolution of the quasar luminosity function is thus placed into the context of the evolution of galaxies and large scale structure
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Key Measurements for Quasar Science
(1) Direct imaging of central engines of quasars(2) Extend kinematic measurements of black hole
masses to cosmological distances(3) Study quasar host galaxies(4) Deep quasar surveys● What is the Seyfert galaxy population at z=7● What is the relationship of AGN to protogalaxies
and the IGM, for z=2 - 7
GSMT will enable (2) – (4)
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Synergy with Alma, JWST and Con-X
● Con-X will probe physics of the central supermassive black hole, studying general relativisitic effects in the plasma nearest the black hole
● Alma will probe molecular gas structures in the central engine and trace how black holes are “fed” with gas
● JWST will image dust in the cores of galaxies which is heated by the quasar accretion.
● GSMT will enable high resolution spectroscopy of quasars and their host galaxies, crucial for understanding all these observations, and putting them in the broader context of galaxy formation.
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● Accretion disk: 10^14 – 10^16 cm● Broad Line Region 10 light days for Seyferts 1 light year for quasars● Torus: 10-50 pc (???)● Narrow Line Region: 100 pc to 500 pc● Extended gas & dust disk: 200pc to 1 kpc● Host Galaxy: 10 kpc+
Quasar Structures
Host GalaxyNarrow Line Region And Extended Narrow Line Region
Torus
jet Accretion diskBroad line region
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Diffraction Limit (arcseconds)
Hubble Space Telescope 0.042
JWST (6.5m) 0.032
ALMA 0.010
30m 0.007
20/20 0.002
0.5 m
1 m
1 m
1 m
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