Transcript 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.

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)
Nuclear Star formation in
AGNs
the distant (D=66 Mpc)
starburst & Seyfert NGC 7469
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
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 connection
There appears to be a delay of 50-100 Myr
between starburst & AGN activity
AGN feeding through mass loss from AGB stars in
circum-nuclear star formation ?
Davies et al. 2007
NGC1068
archetypal Sey 2
NACO K + coronograph
circum-nuclear molecular gas
(14 Mpc, 1”=67 pc)
H2 S(1)
pa 15
60pc
40pc
p.a.15
pa 77
NACO
p.a.77
NIRSP
NACO K
1 pc
NACO M & radio/[OIII]
VLTI MIDI
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
Feeding the nucleus in NGC1068
H2 flux at 85mas (6pc) resolution
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
Mueller Sanchez et al. 2009
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
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”
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
2d Hα kinematics: BzK 15504 (z=2.38) is a large,
clumpy & globally unstable disk
0.5”
FWHM
-200
offset (kpc)
0
+65
+130
normalized flux
-10
SINFONI +AO (VLT):
0.2” (1.6 kpc) resolution
10
0
major axis
+200
+400(±130)
-1
velocity (km/s)
-10
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
0
1
0
200
10
major axis
100
0
-100
-200
250mas
100mas
-1
Genzel et al. 1996, Nature 442, 786
10
5
0
Hα
-65
-130
velocity dispersion (km/s)
(4kpc) -260(±33)
BzK15504 z=2.38
-10
200
0
10
major axis
150
100
50
K-cont.
0
0
velocity (km/s)
Hα
-1
-10
0
1
0
10
minor axis (d=0.7")
-50
-100
-150
-200
0
offset (arcsec)
1
-1
0
1
BX 610 (2.2)
MD 41 (2.2)
200
K20-8 (2.2)
-170
SA12 6192 (1.51)
150
BX 599 (2.33)
100
80
-100
BzK 6004 (2.4)
- 90
-170
-70
+ 130
170
BzK 4165 (1.7)
120
145
BzK 15504 (2.4)
-200
GK2471 (2.43)
170
-240
-145
K20-9 (2.0)
-160
200
K20-6 (2.2)
+200
-250
70
-95
-160
BX389 (2.2)
65
BX663 (2.4)
280
-60
D3a 4751 (2.27)
70
-80
160
+100
-70
110
30
-5
SMMJ09431 (3.35)
70
H7
-70+500
80
+60
H6
1” (8 kpc)
SMMJ105141 (1.21)
+300
+380
BX 404 (2.03)
SA12 8768 (2.2)
-45
-100
BX528 (2.3)
120
-35
The SINS survey
of galaxy kinematics at z~1.5-2.5
(Förster Schreiber et al. 2009a,
Cresci
et al.
2009)
SMMJ131201
(3.41)
-150
K20-7 (2.2)
merger
merger
-70
HDF 242 (2.49)
+160
-280
+200 -60
-30
GK2252 (2.41)
+250
-120
+50
BX 405 (2.03)
40
HDF 169 (1.2)
240
160
N2 850.2 (2.45)
BM 1163 (1.41) GK 167 (2.58)
30 -220
30
-120
-170
1” (8 kpc)
BX482 (2.2)
-200
ZC782941 (2.2)
HDF 76 (2.20)
SA12 6339 (2.3)
BX 502 (2.16)
-100
-50
35
-20
+100
30
-170
ZC1101592 (1.41)
240
D3a 6397 (1.51)
-80
K20-5 (2.2)
170
+200
-30
-350
GK 2113 (1.61)
-200
50
N2850.4 (2.38)
0
-300
+350
empirical evidence for secular growth of
central disk/bulge
NGS/LGSF data sets: ~0.15-0.4” resolution (1.6 kpc)
z=2.4
-200
BX 482
z=2.2
-240
+210
+190
BzK-ZC782941
z=2.2
BzK 6004 z=2.4
-130
Mdyn( 0.4")/Mdyn( 1.2")
BzK 15504
1”
(8 kpc)
0.5
0.4
0.3
0.2
+160
0.1
-160
0.1
+ 140
1
t*=M*/SFR (Gyr)
M(≤3 kpc)/M(≤15 kpc)~0.15-0.4
Genzel et al. 2008, Förster Schreiber et al. 2009