extragalactic science with adaptive optics ( a few highlights)
DESCRIPTION
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). 1 kpc. - PowerPoint PPT PresentationTRANSCRIPT
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")