muse science cases galaxies at intermediate redshifts: 0.2...
TRANSCRIPT
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
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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
....
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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
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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
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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)
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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
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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)
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Main Main topicstopics
1.Galaxy Kinematics
2.Chemical abundances
3.Stellar populations
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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
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Spectral Spectral featuresfeaturesLyon, 7-9 Novembre 2007
Star-forming
Early-type
Hβ[OIII]4959,5007
[SII
]671
7,67
31
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
0 < z < 0.25
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Spectral Spectral featuresfeaturesLyon, 7-9 Novembre 2007
Star-forming
Early-type
[OII]3727
Hβ[OIII]4959,5007
[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
0.25 < z < 0.4
Hδ
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Spectral Spectral featuresfeaturesLyon, 7-9 Novembre 2007
Star-forming
Early-type
[OII]3727
Hβ[OIII]4959,5007
[NeI
II]3
869
0.2<z<1.5 zCOSMOS
composite spectra (Lilly et al. 07)
Hβ4
861
Hδ4
101
D4000
0.4 < z < 0.85
Hδ
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Spectral Spectral featuresfeaturesLyon, 7-9 Novembre 2007
Star-forming
Early-type
[OII]3727[N
eIII
]386
9
Hδ
0.2<z<1.5 zCOSMOS
composite spectra (Lilly et al. 07)
Hδ4
101
D4000
0.85 < z < 1.3
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Spectral Spectral featuresfeaturesLyon, 7-9 Novembre 2007
Star-forming
Early-type
[OII]3727
0.2<z<1.5 zCOSMOS
composite spectra (Lilly et al. 07)
1.3 < z < 1.5
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1. 1. GalaxyGalaxy kinematicskinematics
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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
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1. 1. GalaxyGalaxy kinematicskinematics
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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)
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1. 1. GalaxyGalaxy kinematicskinematics
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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
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1. 1. GalaxyGalaxy kinematicskinematics
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Evolution of the Tully-Fisher
relation up to z~1
Velocity σ
S/N
Rotating disks followthe local TF relation
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1. 1. GalaxyGalaxy kinematicskinematics
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Evolution of the Tully-Fisher
relation up to z~1
Velocity σ
S/N
Dispersion
in TF relation due to galaxies
w/ perturbed kinematics
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1. 1. GalaxyGalaxy kinematicskinematics
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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
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1. 1. GalaxyGalaxy kinematicskinematics
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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
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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
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2. 2. ChemicalChemical abundancesabundances
Metal
enrichment
of galaxies: evolution
of the M-Z relation
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zCOSMOS
- IAB
<22.5(Contini
et al. 08)
VVDS - IAB
<24 (Lamareille
et al. 07)
z ~ 0
z ~ 2 z ~ 0.9
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2. 2. ChemicalChemical abundancesabundances
Metal
enrichment
of galaxies: evolution
of the M-Z relation
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zCOSMOS
- IAB
<22.5(Contini
et al. 08)
VVDS - IAB
<24 (Lamareille
et al. 07)
z ~ 0
z ~ 2 z ~ 0.9
MUSE
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2. 2. ChemicalChemical abundancesabundances
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
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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
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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
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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
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