BX663 (2.4)
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BX663 (2.4). rotation- dominated. BX 610 (2.2). -120. BX 404 (2.03). +160. K20-5 (2.2). MD 41 (2.2). -170. 30. -170. -5. 170. BzK 15504 (2.4). ZC782941 (2.2). SA12 8768 (2.2). SA12 6339 (2.3). -200. +160. D3a 6397 (1.51). 170. -50. 140. 30. K20-8 (2.2). BzK 6004 (2.4).

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BX663 (2.4)

rotation-

dominated

BX 610 (2.2)

-120

BX 404 (2.03)

+160

K20-5 (2.2)

MD 41 (2.2)

-170

30

-170

-5

170

BzK 15504 (2.4)

ZC782941 (2.2)

SA12 8768 (2.2)

SA12 6339 (2.3)

-200

+160

D3a 6397 (1.51)

170

-50

140

30

K20-8 (2.2)

BzK 6004 (2.4)

-140

-160

-260

- 90

K20-6 (2.2)

80

ZC1101592 (1.41)

200

240

GK 167 (2.58)

-100

SA12 6192 (1.51)

BX 405 (2.03)

BX 502 (2.16)

150

70

+210

40

-45

200

-60

35

BX482 (2.2)

-60

+ 130

-70

-240

GK2471 (2.43)

BzK 4165 (1.7)

80

120

-35

170

-20

BX389 (2.2)

-170

-170

30

1” (8 kpc)

-120

D3a 4751 (2.27)

-30

50

70

merger-like

BM 1163 (1.41)

30

BX 599 (2.33)

K20-9 (2.0)

-70

100

-160

increasing dispersion

-30

BX528 (2.3)

GK2252 (2.41)

+240

K20-7 (2.2)

-80

280

+ 160

GK 2113 (1.61)

-80

70

-70

-70

+380

+ 110

-280

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

SINS

Förster, Bouché,Cresci,

Genzel, Shapiro et al. 06-08


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?

VVDS

SINS

LBG

Ocvirk, Teyssier 08


Where are the baryons?

M halo

S. White & co (SDSS)


Z=2 GOODS sBzK K<22.5 Daddi + Elbaz 07

Z=0 SDSS

New insights in galaxy formation

see H. Flores, M. Puech, L. Tresse

  • Scaling relations (SFR-Mass, TF, etc..)

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 ?


high-sigma halos: fed by relatively thin, dense filaments → cold flows

typical halos: reside in relatively thick filaments, fed ~spherically → no cold flows

the millenium cosmological simulation


Insights from Millennium Simulation

dM/dt ~ 35 Mh1.0 (1+z)2.2

SFR =ε 0.18 dMh/dt

ε must be ~1

EPS

DM accretion rate

SINS

M halo

Genel et al. 08


Prediction: >>50% baryons accreted as cold gas! (but clumpy)

Dark + baryon accretion


Z=2 GOODS sBzK K<22.5 Daddi + Elbaz 07

EPS

Z=0 SDSS

New insights in galaxy formation

see H. Flores, M. Puech, L. Tresse

  • Scaling relations (SFR-Mass, TF, etc..)


f_baryon at z=0

Toy model prediction

Strongly tied to only assumption

Observation at z=0


@z=2.2: 50%

@z=1 : 30%

@z=0 : 10%

30-50%Tacconi/Daddi

30%Tacconi

10% Ω(HI)/Ω(star)

Gas fractions

Observations

Accretion prediction


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

  • Feedback processes (IGM, MZ relation)

    (z~0.7 – 1.0)

  • High redshift Lyman alpha emitters

  • Cold accretion


Galaxy formation with MUSE

 Need Resolved spectroscopy ( Mdyn, Mh, SFR, O/H, etc..) of low-mass galaxies

  • Feedback processes (IGM, MZ relation)

    (z~0.7 – 1.0)

  • High redshift Lyman alpha emitters

  • Cold accretion


Galaxy formation with MUSE

 Need Resolved spectroscopy ( Mdyn, Mh, SFR, O/H, etc..) of low-mass galaxies

  • Feedback processes (IGM, MZ relation)

    (z~0.7 – 1.0)

  • High redshift Lyman alpha emitters

  • 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

SF

Verhamme

UDF

Need KMOS (OII)

MDF

Need KMOS / Hawk-I etc

MDF

Measure ε_SFR (M halo)


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