quasar host galaxies: growing up with monstrous middles

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

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)

Why can’t grown astronomers tell a spiral from an elliptical?

(even our C students can do this…)

Argument by Analogy

Galaxy Gallery

Spirals

Elliptical

Merger and ULIRGSTScI

Wellesley students

Why we care (deeply!)

We have met the enemy…

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

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

IR images from ground

Quasars (what kind of galaxies ARE they???)

Seyferts (obviously spirals, and some perfectly normal)

K. McLeod/PASP

Radial profiles…my favorite way to spend the day!

Three evil letters:Point

Spread

Function

Survey says: “Beefy black holes require beefy galaxies!”

McLeod & Rieke 1995

“Which of these things is not like the other?”

K. McLeod/Sky&Telescope with thanks to John Bahcall

WFPC2 on patrol!

Bahcall et al. WFPC2 post PSF subtraction

FINALLY BEAUTIFUL FUZZ!

Only some of these look normal…and RQQ can live in ellipticals.

NICMOS, the best of both worlds!

YOUR TAX $$ AT WORK!

PG0947+396 at 1.6umNICMOS arrays on HST 2.4m … and the Steward 2.3m

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.

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

(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…

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

Hosts at higher redshift

H K(z=4)

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

Mirrors(HST) + Lenses(Gravitational)

= a useful combination!

CASTLES project, Peng et al. 2004

Kauffmann & Haehnelt 2000

Z=0.4

Z=3Wyithe & Loeb 2003

MBH/Mbulge~(1+z)^1.5

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

PANIC at z=4: Stay tuned

Martini, Regan,

Mulchaey, & Pogge

2003

“A Moon a

minute”—P.

Martini

HST and Seyferts: feeding the monster

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 !

Profiles: some STILL ambiguous

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

ACS Weighs In—Hundreds of Hosts MBH – MHost persists to z=1.3

in B-band rest frame (Grogin et al.)