The evolution of galaxy sizes The evolution of galaxy sizes since z=3since z=3

Ignacio Trujillo (MPIA) & the FIRES teamIgnacio Trujillo (MPIA) & the FIRES team

(Trujillo et al. 2004, ApJ, 604, 521)(Trujillo et al. 2004, ApJ, 604, 521)(Trujillo et al. 2005, ApJ, submitted, astro-ph/0504225)(Trujillo et al. 2005, ApJ, submitted, astro-ph/0504225)

Luminosity-size relation

Stellar Mass-size relation

People InvolvedPeople Involved P.I.: P.I.: M. FranxM. Franx (Leiden Observatory) (Leiden Observatory) I. Labbé I. Labbé (Carnegie Observatories), H. Röttgering, A. (Carnegie Observatories), H. Röttgering, A.

van der Wel, P. van der Werf, L. van Starkenburg van der Wel, P. van der Werf, L. van Starkenburg (Leiden Observatory)(Leiden Observatory)

H.W. RixH.W. Rix (MPIA) (MPIA) N.M. Förster SchreiberN.M. Förster Schreiber (MPE) (MPE), , G. RudnickG. Rudnick(NOAO)(NOAO) A. Moorwood (ESO), E. Daddi (NOAO)A. Moorwood (ESO), E. Daddi (NOAO) P. G. van Dokkum (Yale University)P. G. van Dokkum (Yale University) M. Barden, D. H. McIntoshM. Barden, D. H. McIntosh, … (GEMS team), … (GEMS team)

Size evolution: Theoretical Size evolution: Theoretical ExpectationsExpectations

1.1. Semianalytic, Hierarchical modelsSemianalytic, Hierarchical models (e.g. Mo et al. (e.g. Mo et al. 1998):1998):

- - Scaling relationshipsScaling relationships: M: Mdiskdisk and R and Rdiskdisk reflect reflect MMhalohalo and and halohalo

- - Halos formed at Halos formed at high-zhigh-z were much were much denserdenser- - Expected size scale evolution:Expected size scale evolution:

R HR H-2/3-2/3(z) at a fixed halo mass(z) at a fixed halo mass R HR H-1-1 (z) (z) at a fixed circular halo velocityat a fixed circular halo velocity

Size evolution: Theoretical Size evolution: Theoretical ExpectationsExpectations

2. 2. Infall modelsInfall models (e.g. Cayón et al. 1996): (e.g. Cayón et al. 1996):

- Use the observed local disk properties (gas and - Use the observed local disk properties (gas and stellar profiles, metallicity, etc…) as a reference stellar profiles, metallicity, etc…) as a reference - - Star Formation Rate depends on radius and time Star Formation Rate depends on radius and time following a Schmidt-type lawfollowing a Schmidt-type law- Metal-free gas falls in- Metal-free gas falls in

Bouwens & Silk (2002) propose: R(LBouwens & Silk (2002) propose: R(LBB) 1-0.27z) 1-0.27z

FIRES SampleFIRES Sample

Ultra-deep J, H & K images with the VLT of:Ultra-deep J, H & K images with the VLT of:

Hubble Deep Field SouthHubble Deep Field South

IJK

FIRES SampleFIRES Sample

Ultradeep J, H & K images with the VLT of:Ultradeep J, H & K images with the VLT of:

Hubble Deep Field SouthHubble Deep Field SouthCluster MS1054-03 at z=0.83 (4xHDFs area)Cluster MS1054-03 at z=0.83 (4xHDFs area)

To avoid cluster contamination we To avoid cluster contamination we onlyonly analyze analyze z>1 z>1 galaxiesgalaxies……

MS1054-03

IJK

Luminosity-Size and Mass-Size Luminosity-Size and Mass-Size Relations: The SampleRelations: The Sample

K-band selectedK-band selected and and z>1z>1 objects down to: objects down to: KKs,ABs,AB<23.5 (HDF-S) : 87 galaxies<23.5 (HDF-S) : 87 galaxies KKs,ABs,AB<23 (MS1054-03): 175 galaxies<23 (MS1054-03): 175 galaxies

Structural properties are obtained in its Structural properties are obtained in its optical optical rest-frame bandrest-frame band according to its redshift: according to its redshift:

1<z<1.5 (J1<z<1.5 (Js s band)band)1.5<z<2.6 (H1.5<z<2.6 (H band)band)z>2.6 (Kz>2.6 (Ks s band)band)

zphot and rest-frame Lum. Estimationszphot and rest-frame Lum. Estimations

Rudnick et al. (2003;2005)

Luminosity-Size and Mass-Size Luminosity-Size and Mass-Size Relations: The MassesRelations: The Masses

Stellar massesStellar masses are determined from the relation between are determined from the relation between rest-framerest-frame (B-V) (B-V) colorcolor and and M/LM/L (Bell & de Jong 2001) (Bell & de Jong 2001)

Size estimations at high-z: Size estimations at high-z: TechniqueTechnique

Sizes Sizes and and concentrationsconcentrations are estimated fitting are estimated fitting the galaxies with a Sérsic Model the galaxies with a Sérsic Model

I(r)=I(0)e I(r)=I(0)e-b(r/re)^(1/n)-b(r/re)^(1/n)

disk-like

spheroid-like

Selection effectsSelection effects

MS1054-03

Selection effectsSelection effects

Observed Luminosity-Size RelationObserved Luminosity-Size Relation

disk-like

spheroids-like

SDSS relations: Shen et al. 2003

Observed Luminosity-Size RelationObserved Luminosity-Size Relationdisk-like spheroids-

like

Observed Mass-Size RelationObserved Mass-Size Relation

disk-like

spheroids-like

SDSS relations: Shen et al. 2003

Observed Mass-Size RelationObserved Mass-Size Relation

disk-like spheroids-like

GEMSGEMS((BardenBarden et al. 2005; et al. 2005;McIntoshMcIntosh et al. 2005) et al. 2005)& FIRES& FIRESdisk-like spheroids-like

Size evolution: ConclusionsSize evolution: Conclusions

z=2.5 galaxies with Lz=2.5 galaxies with LVV>3.4x10>3.4x1010 10 LLsunsun(V) were:(V) were:

at a given luminosity, 2.3 times smaller than local at a given luminosity, 2.3 times smaller than local counterparts.counterparts.

z=2.5 galaxies with Mz=2.5 galaxies with M**>3x10>3x101010 M Msunsun were: were:

at a given stellar mass, 1.5 smaller.at a given stellar mass, 1.5 smaller.

We can reconcile these two results because high-z We can reconcile these two results because high-z galaxies have young stellar populations.galaxies have young stellar populations.

Inside-Out Galaxy FormationInside-Out Galaxy Formation

FIRES HDFSFIRES HDFS Data Set Integration Time FWHM 1Data Set Integration Time FWHM 1 SB (AB mag/arcsec SB (AB mag/arcsec22))

WFPC2 UWFPC2 U300300 36.8 h 36.8 h 0.16” 0.16” 29.529.5

WFPC2 BWFPC2 B450450 28.3 h 28.3 h 0.14” 0.14” 30.3 30.3

WFPC2 VWFPC2 V606606 27.0 h 27.0 h 0.13” 0.13” 30.630.6

WFPC2 IWFPC2 I814814 31.2 h 31.2 h 0.14” 0.14” 30.030.0

ISAAC JISAAC Jss 33.6 h 33.6 h 0.45” 0.45” 28.628.6

ISAAC H 32.3 h ISAAC H 32.3 h 0.48” 0.48” 28.128.1 ISAAC KISAAC Kss 35.6 h 35.6 h 0.46” 0.46” 28.128.1

FIRES MS1054-03 FieldFIRES MS1054-03 Field Data Set Integration Time FWHM 1Data Set Integration Time FWHM 1 SB (AB mag/arcsec SB (AB mag/arcsec22))

FORS1 U 4.6 h FORS1 U 4.6 h 0.69” 0.69” 29.029.0 FORS1 B 2.0 h FORS1 B 2.0 h 0.57” 0.57” 29.629.6 FORS1 V 0.5 h FORS1 V 0.5 h 0.65” 0.65” 28.828.8

WFPC2 VWFPC2 V606606 1.8 h 1.8 h 0.21” 0.21” 30.0 30.0 WFPC2 IWFPC2 I814814 1.8 h 1.8 h 0.21” 0.21” 29.2 29.2

ISAAC JISAAC Jss 7+7+6+6=26 h 0.48” 7+7+6+6=26 h 0.48” 27.8-28.0 27.8-28.0 ISAAC H 6.5+6+6+6=24.5h 0.46” ISAAC H 6.5+6+6+6=24.5h 0.46” 27.3-27.6 27.3-27.6 ISAAC KISAAC Kss 8+6.5+6+6=26.6 h 0.52” 8+6.5+6+6=26.6 h 0.52” 27.2-27.6 27.2-27.6

Galaxies with z<1: GEMS surveyGalaxies with z<1: GEMS survey- P.I.: H.-W. Rix- P.I.: H.-W. Rix- GEMS area: 800 arcmin- GEMS area: 800 arcmin22

- Two-color: F606W & - Two-color: F606W & F850LPF850LP

- m- mABAB(F606W)=28.3(5(F606W)=28.3(5))- m- mABAB(F850LP)=27.1(5(F850LP)=27.1(5))- 10000 galaxies with - 10000 galaxies with

photometric z from photometric z from COMBO-17COMBO-17