NACO& PARSEC imagingof ultraluminous mergers(R.Davies, S.Rabien, D.Bonaccini & LGSF team)

Extragalactic science with adaptive optics

( a few highlights)

Reinhard Genzel and Ric Davies (MPE)

Nuclear Star formation in AGNs

1 kpc

the distant (D=66 Mpc)starburst & Seyfert NGC 7469

Davies et al. 2004

60 Myr nuclear star clusternuclear gas fraction highdynamical calibration ofCO-H2 conversion factor:0.60.2 Galactic

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

Starburst – AGN connectionThere appears to be a delay of 50-100 Myr

between starburst & AGN activity

Davies et al. 2007

AGN feeding through mass loss from AGB stars in circum-nuclear star formation ?

NGC1068archetypal Sey 2

(14 Mpc, 1”=67 pc)

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

NACO K + coronograph

NACO M & radio/[OIII]

pa 15

pa 77

circum-nuclear molecular gas

40pc

H2 S(1)

p.a.15 NACO

60pc

p.a.77 NIRSP

VLTI MIDI

1 pc

H2 flux at 85mas (6pc) resolution

Feeding the nucleus in NGC1068

55pc

10pc

Mclump ~ 2 ×107 Msun

infall timescale ~ 1.3 MyrdM/dt (to a few pc) ~ 15 Msun/yrthis inflow rate is not sustainable Mueller Sanchez et al. 2009

Black Hole masses from Stellar Kinematics: classical vs pseudo bulges

Nowak et al. 2007, 2008, 2010, & PhD thesis

All black hole masses estimated lie on the MBH-σ* relation

Deep imaging(near bright stars)

Ks=23NACO Ks, 1 hour 0.5” seeing,Strehl 0.35

50”

starting withCOME-ON-PLUS….

Cresci et al. 2005, 2006

SWANsurvey(Ks<23, 15 arcmin2)

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

-200

-100

0

100

200

-1 0 1

-10 0 10

250mas100mas

major axis

offset (arcsec)

velo

city

(km

/s)

0

5

10

-1 0 1

-10 0 10

major axis

norm

aliz

ed flu

x

offset (kpc)

0

50

100

150

200

-1 0 1

-10 0 10

major axis

velo

city

dis

per

sion

(km

/s)

-200

-150

-100

-50

0

-1 0 1

-10 0 10

minor axis (d=0.7")

velo

city

(km

/s)

2d Hα kinematics: BzK 15504 (z=2.38) is a large, clumpy & globally unstable disk

Mdyn(<10 kpc) ~1011 M

vc=230 km/s, Rd=4 kpcSFR = 150 Myr-1, Q=0.8Σgas~ 300 M pc-2

, fgas~0.3

Genzel et al. 1996, Nature 442, 786

-200-260(±33) FWHM 0.5”(4kpc)Hα -130

0 +200+65 +400(±130)

-65

+130

SINFONI +AO (VLT): 0.2” (1.6 kpc) resolution

Hα

K-cont.

BzK15504 z=2.38

merger

rotation-

dominated

SMMJ09431 (3.35)

H6

H7+500

-100

+60

HDF 242 (2.49)+50

-150

+100

-300 +350

N2850.4 (2.38)

SMMJ131201 (3.41)

+200

-200

+250

-250

HDF 169 (1.2)

SMMJ105141 (1.21)

+300

-350

HDF 76 (2.20)

-100

+100

N2 850.2 (2.45)

-220

+200

1” (8 kpc)

dispersiondominated

70

-70

D3a 4751 (2.27)

SA12 6339 (2.3)

-50

30

35-20

BX 502 (2.16)

BX 405 (2.03)

-35

40

-30

30BM 1163 (1.41)

BX 404 (2.03)

-5

30

merger

rotation-

dominated

-60

70

K20-6 (2.2)

-80

100BX 599 (2.33)

GK 167 (2.58)

-60

30

-70

70

GK2252 (2.41)

-280

280

BX389 (2.2)

170

K20-5 (2.2)-170

dispersiondominated

-120

120BzK 4165 (1.7)

-70

150SA12 6192 (1.51)

-10080

K20-8 (2.2)

ZC1101592 (1.41)

-240

240

GK2471 (2.43)

-170

170

+ 130

- 90

BzK 6004 (2.4)

-170

200

BX 610 (2.2)

240

-160K20-9 (2.0)

+160

-120

BX663 (2.4)

-70

110

BX528 (2.3)

160

-3050

GK 2113 (1.61)

0+380

-80

K20-7 (2.2)

120

200

-200

BzK 15504 (2.4)

-160

160

ZC782941 (2.2) -200

+200

BX482 (2.2)

SA12 8768 (2.2)

80

-45

1” (8 kpc)

170

-170

MD 41 (2.2)

-145

145

D3a 6397 (1.51)

The SINS surveyof galaxy kinematics at z~1.5-2.5(Förster Schreiber et al. 2009a, Cresci et al. 2009)

-95

65

+ 140

-130

-200

+190

1”(8 kpc)

BzK 15504 z=2.4

BzK 6004 z=2.4z=2.2

-160

BzK-ZC782941

BX 482 z=2.2

+210

-240

+160

empirical evidence for secular growth of central disk/bulge

Genzel et al. 2008, Förster Schreiber et al. 2009

NGS/LGSF data sets: ~0.15-0.4” resolution (1.6 kpc)

M(≤3 kpc)/M(≤15 kpc)~0.15-0.4

0.1

0.2

0.3

0.4

0.5

0.1 1

t*=M

*/SFR (Gyr)

Md

yn(

0.4

")/M

dyn

( 1

.2")