+160 -120 BX663 (2.4) -170 170 MD 41 (2.2) +240 -160 K20-9 (2.0) +380 -80 K20-7 (2.2) -100 80 K20-8...
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+160 -120 BX663 (2.4) -170 170 MD 41 (2.2) +240 -160 K20-9 (2.0) +380 -80 K20-7 (2.2) -100 80 K20-8 (2.2) 70 -70 D3a 4751 (2.27) SA12 6339 (2.3) -50 30 SA12 8768 (2.2) 80 -45 GK2471 (2.43) -170 170 ZC1101592 (1.41) -240 240 -170 170 K20-5 (2.2) -120 120 BzK 4165 (1.7) 35 -20 BX 502 (2.16) BX 405 (2.03) -35 40 -30 30 BM 1163 (1.41) BX 404 (2.03) -5 30 -70 150 SA12 6192 (1.51) merger-like rotat ion- dominated -60 70 K20-6 (2.2) -80 100 BX 599 (2.33) -30 50 GK 2113 (1.61) GK 167 (2.58) -60 30 -70 70 GK2252 (2.41) + 130 - 90 BzK 6004 (2.4) 200 -200 BzK 15504 (2.4) -70 + 110 + 160 BX528 (2.3) -160 +160 ZC782941 (2.2) -140 140 D3a 6397 (1.51) -280 280 BX389 (2.2) 1” (8 kpc) -170 200 BX 610 (2.2) -260 +210 BX482 (2.2) increasing dispersion Förster, Bouché,Cresci, Genzel, Shapiro et al. 06-08 SINS SINS 70 Galaxies 1.5-2.5 Disk: 30-40% (v/σ ~ 2 – 4) Disp: 30% (v/σ < 1) Merger: 20-30% Forster Schreiber et al. 09 Shapiro et al. 09
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Transcript of +160 -120 BX663 (2.4) -170 170 MD 41 (2.2) +240 -160 K20-9 (2.0) +380 -80 K20-7 (2.2) -100 80 K20-8...
+160
-120
BX663 (2.4)
-170
170
MD 41 (2.2)
+240
-160
K20-9 (2.0)
+380
-80
K20-7 (2.2)
-10080
K20-8 (2.2)
70
-70
D3a 4751 (2.27)
SA12 6339 (2.3)
-50
30
SA12 8768 (2.2)
80
-45
GK2471 (2.43)
-170
170
ZC1101592 (1.41)
-240
240
-170
170
K20-5 (2.2)
-120
120BzK 4165 (1.7)
35
-20
BX 502 (2.16)BX 405 (2.03)
-35
40
-30
30BM 1163 (1.41)
BX 404 (2.03)
-5
30
-70
150
SA12 6192 (1.51)
mer
ger-
like
rotation-
dominated
-60
70
K20-6 (2.2)
-80
100BX 599 (2.33)
-3050
GK 2113 (1.61)
GK 167 (2.58)
-60
30
-70
70
GK2252 (2.41)
+ 130
- 90
BzK 6004 (2.4)
200
-200
BzK 15504 (2.4)
-70
+ 110
+ 160
BX528 (2.3)
-160
+160
ZC782941 (2.2)
-140
140D3a 6397 (1.51)
-280
280BX389 (2.2)
1” (8 kpc)
-170
200
BX 610 (2.2)
-260
+210
BX482 (2.2)
increasing dispersion
Förster, Bouché,Cresci,Genzel, Shapiro et al. 06-08
SINS
SINS70 Galaxies 1.5-2.5Disk: 30-40% (v/σ ~ 2 – 4)Disp: 30% (v/σ < 1)Merger: 20-30%
Forster Schreiber et al. 09Shapiro et al. 09
SINS “rotators”
Cresci et al. 09
SINS “rotators”
Cresci et al. 09
SINS “rotators”
Cresci et al. 09
Étude des galaxies à faible masse
MUSE Workshop March 18/19
N. Bouché (MPE LATT)
The Hubble sequence still unexplained
Need to study progenitors!
Why study low-mass galaxies?
Ocvirk, Teyssier 08
VVDS
SINS
LBG
Where are the baryons?
S. White & co (SDSS)
M halo
New insights in galaxy formation
• Scaling relations (SFR-Mass, TF, etc..)see H. Flores, M. Puech, L. Tresse
Z=2 GOODS sBzK K<22.5 Daddi + Elbaz 07
Z=0 SDSS
Puech 08, Cresci 09
Mergers not dominant
Questions
• Why SFR ~ 200 M/yr at z=2?
• Origin of scaling relations: TF, SFR-Mass?
• Role of feedback in low-mass end (z=2)?
• What happens at z>5 ?
the millenium cosmological
simulation
high-sigma halos: fed by relatively thin, dense filaments → cold flows
typical halos: reside in relatively thick filaments, fed ~spherically → no cold flows
Genel et al. 08
DM
acc
retio
n ra
te
M halo
Insights from Millennium Simulation
EPS
dM/dt ~ 35 Mh1.0 (1+z)2.2 SFR =ε 0.18 dMh/dt
SIN
S
ε must be ~1
Dark + baryon accretion
• Prediction: >>50% baryons accreted as cold gas! (but clumpy)
New insights in galaxy formation
• Scaling relations (SFR-Mass, TF, etc..)see H. Flores, M. Puech, L. Tresse
Z=2 GOODS sBzK K<22.5 Daddi + Elbaz 07
Z=0 SDSS
EPS
f_baryon at z=0
Observation at z=0Toy model prediction Strongly tied to only assumption
Gas fractions
• @z=2.2: 50%• @z=1 : 30%• @z=0 : 10%
30-50%Tacconi/Daddi
30% Tacconi
10% Ω(HI)/Ω(star)
Accretion prediction Observations
Questions
• Why SFR ~ 200 M/yr at z=2?
• Origin of scaling relations: TF, SFR-Mass?
• Role of feedback in low-mass end (z=2)?
• What happens at z>5 ?
Galaxy formation with MUSE
Need Resolved spectroscopy ( Mdyn, Mh, SFR, O/H,
etc..) of low-mass galaxies
A. Feedback processes (IGM, MZ relation)(z~0.7 – 1.0)
B. High redshift Lyman alpha emitters
C. Cold accretion
Galaxy formation with MUSE
Need Resolved spectroscopy ( Mdyn, Mh, SFR, O/H,
etc..) of low-mass galaxies
A. Feedback processes (IGM, MZ relation)(z~0.7 – 1.0)
B. High redshift Lyman alpha emitters
C. Cold accretion
Galaxy formation with MUSE
Need Resolved spectroscopy ( Mdyn, Mh, SFR, O/H,
etc..) of low-mass galaxies
A. Feedback processes (IGM, MZ relation)(z~0.7 – 1.0)
B. High redshift Lyman alpha emitters
C. Cold accretion (z~3)
1’
How?
• Study low-mass galaxies at z~1 [OII]
• Study filaments at z~3 [Lya]
• LAE at z~4,5
• LAE at z>6
Verhamme
Need KMOS (OII)
Measure ε_SFR (M halo)
Need KMOS / Hawk-I etc
SF
UDF
MDF
MDF
