muse science cases galaxies at intermediate redshifts: 0.2...

Science Team Meeting Lyon 6-7/03/06

MUSE Science Cases Galaxies at Intermediate Redshifts: 0.2 < z < 1.5

Thierry ContiniLATT - Toulouse

Formation & Evolution des galaxies dans le contexte de MUSELyon, 7-9 Novembre 2007

Science Team 6-7/3/06

p.2

IntroductionIntroduction

Evolution of galaxies and large-scale structures on cosmological timescales

constraints on models of galaxy formation & evolution

o

When and how did galaxies form?o

Links between high-z ("young") and local ("old") galaxies?

o

Timescales for galaxy evolution?o

Dependance

with environment?o

....

Lyon, 7-9 Novembre 2007


p.3

IntroductionIntroductionNeeds for large statistical samples of galaxies at various epochs

"Local" Universe: ~ 106 galaxies up to z ~ 0.2

"Small" (~ 103 galaxies) samples between z=0.5 and z~4 obtained in the 90’s: CFRS (up to z ~ 1), LBGs (z ~ 3-4), etc

Large (VVDS, DEEP2, COSMOS, GDDS...) surveys on the largest telescopes (VLT, Keck, Gemini...) to gather large numbers of high-redshift galaxies in large volumes, similarly to SDSS & 2dF



p.4

IntroductionIntroductionLyon, 7-9 Novembre 2007

Survey Redshift range

R=λ/Δλ Ngal Limiting

mag

SDSS,2dF z < 0.3 ~2000 ~106 RAB

<17.8/19.5

VVDS 0.2 < z < 1.5 ~250 ~104 IAB

<24

COSMOS 0.2 < z < 1.5 ~600 ~104 IAB

<22.5

DEEP2 0.5 < z < 1.5 ~2000 ~104 RAB

<24

Current

large & deep

spectroscopic

surveys

up to z~1.5


p.5

IntroductionIntroduction

MUSE advantages

for intermediate-z galaxy

studies

no pre-selectionprobe fainter galaxieshigh resolution in AO mode -> spatially-resolved properties

Main drawbackSmaller size samples (~102 galaxies ) compared withcurrent spectroscopic surveys (~104 galaxies)



p.6

SpatiallySpatially--ResolvedResolved spectroscopyspectroscopy

MUSE sensitivity & high-resolutionspatialy resolved properties of galaxies up

to z~1At 0.5 < z < 1, the MUSE AO-corrected PSF (~0.3 arcsec) corresponds to a physical size of ~2 kpcWell suited to study internal variations of:

Stellar population ages & metallicitiesISM properties: metallicity, reddening, etcw/ full 2D star & gas kinematics



p.7

SpatiallySpatially--ResolvedResolved spectroscopyspectroscopy

Evolution of the star formation & metalenrichment histories of spheroïds, disks & irregulars over the last 10 GyrFor each galaxy, relationships between local kinematics, gas metallicity & reddening, and the stellar population ages & metallicitiesCensus of the 0.5 < z < 1.0 galaxy populations at level of details comparable to SDSSCrucial tests for galaxy evolution scenarios(eg. downsizing)



p.8

Main Main topicstopics

1.Galaxy Kinematics

2.Chemical abundances

3.Stellar populations



p.9

Spectral Spectral featuresfeaturesLyon, 7-9 Novembre 2007

Star-forming

Early-type

[OII]3727

Hβ[OIII]4959,5007

[SII

]671

7,67

31

[NeI

II]3

869

Hα+[NII]6584

0.2<z<1.5 zCOSMOS

composite spectra (Lilly et al. 07)

NaD

5892

MgI

5175

Ca,F

e526

9

Hβ4

861

Hδ4

101

D4000

Hδ


p.10


Star-forming

Early-type

Hβ[OIII]4959,5007

[SII

]671

7,67

31

Hα+[NII]6584

0.2<z<1.5 zCOSMOS


NaD

5892

MgI

5175

Ca,F

e526

9

Hβ4

861

0 < z < 0.25


p.11


Star-forming

Early-type

[OII]3727

Hβ[OIII]4959,5007

[NeI

II]3

869

Hα+[NII]6584

0.2<z<1.5 zCOSMOS


NaD

5892

MgI

5175

Ca,F

e526

9

Hβ4

861

Hδ4

101

D4000

0.25 < z < 0.4

Hδ


p.12


Star-forming

Early-type

[OII]3727

Hβ[OIII]4959,5007

[NeI

II]3

869

0.2<z<1.5 zCOSMOS


Hβ4

861

Hδ4

101

D4000

0.4 < z < 0.85

Hδ


p.13


Star-forming

Early-type

[OII]3727[N

eIII

]386

9

Hδ

0.2<z<1.5 zCOSMOS


Hδ4

101

D4000

0.85 < z < 1.3


p.14


Star-forming

Early-type

[OII]3727

0.2<z<1.5 zCOSMOS


1.3 < z < 1.5


p.15

1. 1. GalaxyGalaxy kinematicskinematics


Spatially-resolved

kinematics

from

2D velocity

fields

in emission

lines

Emission-line SB

Velocity

Field

SPH dynamical simulations(courtesy of V. Debattista

& L. Mayer)MUSE 80h integration

Disk galaxy at z~1 with h=0.4”F(EL)=10-17

ergs-1cm-2

At z~1, the velocity field can be mapped with MUSE to ~2 x disk scale length


p.16



Spatially-resolved

kinematics

from

2D velocity

fields

in emission

lines

Overview of the dynamical properties of galaxies (rotating disks, spheroïds, mergers, etc) up to z~1Evolution of the Tully-Fisher relation for diskgalaxiesResolved sub-structures dynamical perturbations due to close companion, starburst-driven gasoutflows, etcRelationships between internal dynamics & othergalactic properties (SFR, metallicity, stellarpopulations, etc)


p.17



Evolution of the Tully-Fisher

relation up to z~1

35 galaxies @ 0.4 < z < 0.753D spectroscopy w/ FLAMES/GIRAFFENo AO

-

seeing ~0.4”-0.8“

–

pixel=0.52”

Kinematical classification:• rotating disks (~35%)• perturbed or complex kinematics

Velocity σ

S/N

Flores et al. 06


p.18




relation up to z~1

Velocity σ

S/N

Rotating disks followthe local TF relation

Flores et al. 06


p.19




relation up to z~1

Velocity σ

S/N

Dispersion

in TF relation due to galaxies

w/ perturbed kinematics

Flores et al. 06


p.20



VVDS220014252z=1.3097

Hα [NII]

On-going 3D NIR spectroscopic observations @ z > 1

Lemoine-Busserolle

et al. 08

ESO LP

(300h –

Contini

et al.)

SINFONI with AO/LGSFoV

= 3”x3”

–

pixel size = 0.1”

~140 VVDS galaxies @ 1 < z < 2


p.21



On-going 3D NIR spectroscopic observations @ z > 1

Also …

2 < z < 3Foerster-Schreiber, Genzel et al. with VLT/SINFONILaw, Erb, Steidel et al. with Keck/OSIRIS

3 < z < 5Maiolino et al. with VLT/SINFONI

And more to come in COSMOS/VVDS field with MOIRCS & SINFONI


p.22

2. 2. ChemicalChemical abundancesabundances

Metal

enrichment

of galaxiesLyon, 7-9 Novembre 2007

Gas-phase metallicity

(O/H) derived from EL ratios:

Redshift

range 0.00 –

0.25 0.25 –

0.40 0.40 –

0.85 0.85 –

1.30

Emission lines

Hβ, [OIII]Hα, [NII]

[OII]

Hβ, [OIII]Hα, [NII]

[OII]

Hβ, [OIII]

[OII], [NeIII], Hδ


p.23


Metal

enrichment

of galaxies: evolution

of the M-Z relation


zCOSMOS

- IAB

<22.5(Contini

et al. 08)

VVDS - IAB

<24 (Lamareille

et al. 07)

z ~ 0

z ~ 2 z ~ 0.9


p.24


Metal

enrichment

of galaxies: evolution

of the M-Z relation


zCOSMOS

- IAB

<22.5(Contini

et al. 08)

VVDS - IAB

<24 (Lamareille

et al. 07)

z ~ 0

z ~ 2 z ~ 0.9

MUSE


p.25


Metal

enrichment

of galaxies

Evolution of the M-Z relation up to z~1.3 extending the VVDS/zCOSMOS studies to lower-mass (~109 Msun) metal-poor galaxiesSpatially-resolved O/H measurements for brighter galaxiesmetallicity

gradients diagnostic for the

building up of galaxy disks



p.26

3. 3. StellarStellar populationspopulations

Stellar

populationsLyon, 7-9 Novembre 2007

Simulations using BC03MUSE 80h integration

Galaxy at z~1 with S/N=15 spectraAge (Gyr)

Stellarm

etallicity

Input SFH/ZMUSE

spectrum

At z~1, the spatially-resolved stellar ages & metallicities

of

galaxies should be recovered from MUSE spectra


p.27

3. 3. StellarStellar populationspopulations

Stellar

populations

High sensitivity, spectral & spatial resolutions of MUSE

spatially-resolved stellar population properties (age, metallicity, etc)Relationships with dynamics, ISM properties, etc

tests for scenarios of stellar mass assembly in massive galaxies



p.28

Conclusion Conclusion Expected

number

density

of galaxies in MUSE field

(based

on VVDS/zCOSMOS

number

counts):

~ 10 per arcmin-2

for IAB

< 22.5~ 5 per arcmin-2

for Fline

> 10-17 ergs-1cm-2

Sample of a few 102 galaxies at

intermediate

redshifts

in

several

Deep

& Medium Deep

MUSE Fields


muse science cases galaxies at intermediate redshifts: 0.2...

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