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Quasar Host Galaxies:Growing up with Monstrous
Middles
Kim K. McLeod, Wellesley College
George Rieke, U. of ArizonaLisa Storrie-Lombardi, IPACBrian McLeod, CfAJill Bechtold, U. of Arizona
McLeod/Scientific American
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Hosts, in the style of Astro101(“’Scopes for dopes?”)
1984: “In a few quasars, we can actually observe the underlying galaxies in which they are embedded…” (Abell, Realm of the Universe)
1994: “It is very difficult to observe the ‘host galaxy’”
Radio quiet = spiral; Radio loud = elliptical(Kaufmann, Universe)
2004: “Quasars turn out to be located in the centers of galaxies (!)…both spiral and elliptical…many involved in a collision.”
(Fraknoi, Morrison, & Wolff, Voyages)
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Why can’t grown astronomers tell a spiral from an elliptical?
(even our C students can do this…)
Argument by Analogy
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Galaxy Gallery
Spirals
Elliptical
Merger and ULIRGSTScI
Wellesley students
Why we care (deeply!)
We have met the enemy…
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1990’s: What the Near-IR can do for YOU!
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Hosts on the eve of HSTOur program:
--256x256 IR camera
--image 50 z<0.4 quasars and 50 Seyferts
Simultaneous with similar study by Dunlop et al.:--nicely matched samples of RLQ, RQQ, and RG--later got WFPC2 data
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IR images from ground
Quasars (what kind of galaxies ARE they???)
Seyferts (obviously spirals, and some perfectly normal)
K. McLeod/PASP
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Radial profiles…my favorite way to spend the day!
Three evil letters:Point
Spread
Function
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Survey says: “Beefy black holes require beefy galaxies!”
McLeod & Rieke 1995
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“Which of these things is not like the other?”
K. McLeod/Sky&Telescope with thanks to John Bahcall
WFPC2 on patrol!
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Bahcall et al. WFPC2 post PSF subtraction
FINALLY BEAUTIFUL FUZZ!
Only some of these look normal…and RQQ can live in ellipticals.
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NICMOS, the best of both worlds!
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YOUR TAX $$ AT WORK!
PG0947+396 at 1.6umNICMOS arrays on HST 2.4m … and the Steward 2.3m
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Examples of NICMOS images of z<0.4 hostsMcLeod & McLeod 2000
Sing “Ho” for the H-band…good for tracing stellar mass but NOT the best place to look for spiral arms.
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More fun with profiles (Alas, we STILL can’t always tell a spiral from an elliptical!)
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(z<0.4)Quasars follow the BH-bulge relation* and accrete at ~10% Eddington (by product: luminous RQQ often in ellipticals)
*some BH masses measured by reverb mapping or virialized emission lines…
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Growing up with a monster in the middle
Kauffmann & Haehnelt 2000
Hierarchical structure formation: black holes are fueled, and galaxies grow, through mergers
Z=0.4
Z=3
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Hosts at higher redshift
H K(z=4)
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Ridgway, Heckman, Calzetti, & Lehnert 2002
Hutchings et al. 2002
Kukula et al. 2001, with black hole masses from virialized MgII
HST at z=2-3
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Mirrors(HST) + Lenses(Gravitational)
= a useful combination!
CASTLES project, Peng et al. 2004
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Kauffmann & Haehnelt 2000
Z=0.4
Z=3Wyithe & Loeb 2003
MBH/Mbulge~(1+z)^1.5
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Taking the big step to high-z: Do PANIC!
Bechtold and McLeod have been using Magellan (6.5m) and Gemini (8m) to image z=4 quasars in the near-IR
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PANIC at z=4: Stay tuned
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Martini, Regan,
Mulchaey, & Pogge
2003
“A Moon a
minute”—P.
Martini
HST and Seyferts: feeding the monster
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Astro101 Revisited2014: “In 2009, HST observations of
large samples of hosts (from SDSS samples?)fuzz around z=4 quasarslensed quasars at high zelemental abundances in high-z quasarsthe nuclei of dwarf galaxies…(insert your favorites here)…
showed how stars and black holes grow together starting from a seed masses of _______ inside dark matter halos to make the galaxies we see today.”
H S To
o !
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Profiles: some STILL ambiguous
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Black hole v. spheroid mass—getting tighter!Haring & Rix 2003
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ACS Weighs In—Hundreds of Hosts MBH – MHost persists to z=1.3
in B-band rest frame (Grogin et al.)