1. Extragalactic science with adaptive optics ( a few highlights)
Reinhard Genzel and Ric Davies
(MPE)
NACO& PARSEC imaging
of ultraluminous mergers
(R.Davies, S.Rabien, D.Bonaccini & LGSF team)

2. Piercing the dust in starburst galaxies
near infrared (K)
Piercing the dust in starburst galaxies
optical
L-band 3.8μm
NGC 4945

3. Nuclear Star formation in AGNs
the distant (D=66 Mpc)
starburst & Seyfert NGC 7469
Kinematic evidence (σ-drops) for nuclear disks is seen in ~30% of spiral galaxies
Ganda et al. 2006, Emsellem et al. 2007, Davies et al. 07, Storchi-Bergman et al. 2008, 2009
1 kpc
60 Myr nuclear star cluster
nuclear gas fraction high
dynamical calibration of
CO-H2 conversion factor:
0.60.2 Galactic
Davies et al. 2004

4. Starburst – AGN connection
There appears to be a delay of Myr
between starburst & AGN activity
starburst age (more an upper limit) vs AGN accretion rate relation but don’t over interpret!
position of GC on relation
possible explanations – to do with efficiency of Bondi accretion
eg winds from stars? – AGB stars, high mass loss at low speeds but also supernova might be sufficient: dominates total mass loss
(10% of mass in cluster); although high velocities, the dense ISM would slow shock speed to <100km/s within only a few parsecs
amount of gas need to fuel 10^7Msun BH at L_edd is 0.2Msun/yr (eta=0.1) starburst 1Msun/yr for 10Myr yields 1e6Msun return
would need effectively all to go to centre to feed blackhole don’t go down this road yet…
AGN feeding through mass loss from AGB stars in circum-nuclear star formation ?
Davies et al. 2007

5. NGC1068 archetypal Sey 2 (14 Mpc, 1”=67 pc)
NACO K + coronograph
pa 15
pa 77
circum-nuclear molecular gas
40pc
H2 S(1)
p.a NACO
60pc
p.a NIRSP
VLTI MIDI
1 pc
NACO M & radio/[OIII]
NACO K
Gallimore et al.1997, Greenhill et al. 1997, Rouan et al. 2004, Gratadour et al. 2005, Davies et al. 2005, Jaffe et al. 2004, Schinnerer et al. 2000

6. Feeding the nucleus in NGC1068
55pc
10pc
Mclump ~ 2 ×107 Msun
infall timescale ~ 1.3 Myr
dM/dt (to a few pc) ~ 15 Msun/yr
this inflow rate is not sustainable
H2 flux at 85mas (6pc) resolution
Mueller Sanchez et al

7. Black Hole masses from Stellar Kinematics: classical vs pseudo bulges
All black hole masses estimated lie on the MBH-σ* relation
Nowak et al. 2007, 2008, 2010, & PhD thesis

8. Deep imaging (near bright stars)
starting with
COME-ON-PLUS….
SWAN
survey
(Ks<23, 15 arcmin2)
Ks=23
NACO
Ks, 1 hour
0.5” seeing,
Strehl 0.35
Cresci et al. 2005, 2006
50”

9. clumpy high-z galaxies: mergers or ?
BX610
MD41
BX389
BX482
BX528
Cowie et al. 1996, Giavalisco et al. 1996, Elmegreen et al. 2005, 2007, 2009, Förster Schreiber et al. 2009b, Lotz et al. 2006

10. 2d Hα kinematics: BzK 15504 (z=2
2d Hα kinematics: BzK (z=2.38) is a large, clumpy & globally unstable disk Hα
-200
-260(±33)
FWHM
0.5”
(4kpc) Hα
-130
+200
+65
+400(±130)
-65
+130
SINFONI +AO (VLT):
0.2” (1.6 kpc) resolution
K-cont.
BzK15504 z=2.38
Mdyn(<10 kpc) ~1011 M
vc=230 km/s, Rd=4 kpc
SFR = 150 Myr-1, Q=0.8 Σgas~ 300 M pc-2, fgas~0.3
Genzel et al. 1996, Nature 442, 786

11. rotation- dominated dispersion merger 1” (8 kpc) The SINS survey
SMMJ09431 (3.35) H6 H7
+500
-100
+60
HDF 242 (2.49)
+50
-150
+100
-300
+350
N (2.38)
SMMJ (3.41)
+200
-200
+250
-250
HDF 169 (1.2)
SMMJ (1.21)
+300
-350
HDF 76 (2.20)
N (2.45)
-220
1” (8 kpc)
dispersion 70
-70
D3a 4751 (2.27)
SA (2.3)
-50 30 35
-20
BX 502 (2.16)
BX 405 (2.03)
-35 40
-30
BM 1163 (1.41)
BX 404 (2.03) -5
-60
K20-6 (2.2)
-80
100
BX 599 (2.33)
GK 167 (2.58)
GK2252 (2.41)
-280
280
BX389 (2.2)
170
K20-5 (2.2)
-170
-120
120
BzK 4165 (1.7)
150
SA (1.51) 80
K20-8 (2.2)
ZC (1.41)
-240
240
GK2471 (2.43)
+ 130
- 90
BzK (2.4)
200
BX 610 (2.2)
-160
K20-9 (2.0)
+160
BX663 (2.4)
110
BX528 (2.3)
160 50
GK 2113 (1.61)
+380
K20-7 (2.2)
BzK (2.4)
ZC (2.2)
BX482 (2.2)
SA (2.2)
-45
MD 41 (2.2)
-145
145
D3a 6397 (1.51)
-95 65
The SINS survey
of galaxy kinematics at z~
(Förster Schreiber et al. 2009a,
Cresci et al. 2009)

12. empirical evidence for secular growth of central disk/bulge
NGS/LGSF data sets: ~ ” resolution (1.6 kpc)
+ 140
-130
-200
+190 1”
(8 kpc)
BzK
z=2.4
BzK 6004
z=2.2
-160
BzK-ZC782941
BX z=2.2
+210
-240
+160
M(≤3 kpc)/M(≤15 kpc)~
Genzel et al. 2008, Förster Schreiber et al. 2009

13. what drives star formation at high-z ?
cold flows/streams:
Dekel & Birnboim 2003,2006, Keres et al. 2005, Nagamine et al. 2005, Davé 2007, Kitzbichler & White 2007, Naab et al. 2007, Governato et al. 2008, Ocvirk et al. 2008, Dekel et al. 2009, Agertz et al. 2009
major & minor mergers
Kauffmann et al. 1993, Steinmetz & Navarro 2003, Hernquist, Springel, di Matteo, Hopkins et al , Robertson & Bullock 2008