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Quasar Host Galaxies: Growing up with Monstrous Middles Kim K. McLeod, Wellesley College George Rieke, U. of Arizona Lisa Storrie-Lombardi, IPAC Brian.

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Presentation on theme: "Quasar Host Galaxies: Growing up with Monstrous Middles Kim K. McLeod, Wellesley College George Rieke, U. of Arizona Lisa Storrie-Lombardi, IPAC Brian."— Presentation transcript:

1 Quasar Host Galaxies: Growing up with Monstrous Middles Kim K. McLeod, Wellesley College George Rieke, U. of Arizona Lisa Storrie-Lombardi, IPAC Brian McLeod, CfA Jill Bechtold, U. of Arizona McLeod/Scientific American

2 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)

3 Why can’t grown astronomers tell a spiral from an elliptical? (even our C students can do this…) Argument by Analogy

4 Galaxy Gallery Spirals Elliptical Merger and ULIRG STScI Wellesley students Why we care (deeply!) We have met the enemy…

5 1990’s: What the Near-IR can do for YOU!

6 Hosts on the eve of HST Our 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

7 IR images from ground  Quasars (what kind of galaxies ARE they???)  Seyferts (obviously spirals, and some perfectly normal) K. McLeod/PASP

8 Radial profiles …my favorite way to spend the day! Three evil letters: P oint S pread F unction

9 Survey says: “Beefy black holes require beefy galaxies!” McLeod & Rieke 1995

10 “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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12 Bahcall et al. WFPC2 post PSF subtraction FINALLY BEAUTIFUL FUZZ! Only some of these look normal…and RQQ can live in ellipticals.

13 NICMOS, the best of both worlds!

14 YOUR TAX $$ AT WORK! PG at 1.6um NICMOS arrays on HST 2.4m … and the Steward 2.3m

15 Examples of NICMOS images of z<0.4 hosts McLeod & McLeod 2000 Sing “Ho” for the H- band… good for tracing stellar mass but NOT the best place to look for spiral arms.

16 More fun with profiles (Alas, we STILL can’t always tell a spiral from an elliptical!)

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18 (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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20 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

21 Hosts at higher redshift H K(z=4)

22  Ridgway, Heckman, Calzetti, & Lehnert 2002 Hutchings et al Kukula et al. 2001, with black hole masses from virialized MgII HST at z=2-3

23 Mirrors(HST) + Lenses(Gravitational) = a useful combination! CASTLES project, Peng et al. 2004

24 Kauffmann & Haehnelt 2000 Z=0.4 Z=3 Wyithe & Loeb 2003 M BH /M bulge ~(1+z)^1.5

25 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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27 PANIC at z=4: Stay tuned

28 Martini, Regan, Mulchaey, & Pogge 2003 “A Moon a minute”— P. Martini HST and Seyferts: feeding the monster

29 Astro101 Revisited 2014: “In 2009, HST observations of large samples of hosts (from SDSS samples?) fuzz around z=4 quasars lensed quasars at high z elemental abundances in high-z quasars the 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 T o o !

30 Profiles: some STILL ambiguous

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33 Black hole v. spheroid mass—getting tighter! Haring & Rix 2003

34 ACS Weighs In—Hundreds of Hosts M BH – M Host persists to z=1.3 in B-band rest frame (Grogin et al.)


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