Galaxies in clusters and their progenitors

Pieter van Dokkum (Yale)

General properties of cluster galaxies

• Morphology-density relation• In core approx. 80% are E and S0 galaxies

(Dressler 1980)

General properties of cluster galaxies

• Cluster galaxies follow tight scaling relations:

– Color-magnitude relation

– Fundamental Plane (Djorgovski & Davis 1987, Dressler et al 1987)

– relation (Faber 1973)

bMg

(e.g., Bower, Lucey, Ellis 1992)

Terlevich, Caldwell,Bower 2001

Motivation for studying cluster galaxies

• Early-type galaxies are massive and old:

Constrain galaxy formation theories

or ?

Motivation for studying cluster galaxies

• Descendants Ly-break galaxies?– Ly-break galaxies already clustered (Giavalisco et al

1998)

– In hierarchical models end up in groups and clusters

Baugh et al. 1998

Ly-break descendants

• Study the evolution of galaxies in the densest environments– Determine when/how galaxies and LSS formed– Test predictions from CDM models

• Such programs require the resolution of HST and collecting area of large ground-based telescopes

Observational programs

Meza etal. 2003

Observational programs

• Several 100 clusters known at 0.2<z<1.0(best selected by SZ-effect, lensing, or X-rays)

Stanford etal. 2001

Observational programs

• Several 100 clusters known at 0.2<z<1.5(best selected by SZ-effect, lensing, or X-rays)

(Lensing NOT effective method beyond z~0.7)

Observational programs

• Several 100 clusters known at 0.2<z<1.0(best selected by SZ-effect, lensing, or X-rays)

• Many (50+) observed with HST (eg ACS GTO team)

Abell 2218 (z=0.18; Ellis et al 04) RX0848 (z=1.27; van D & Stanford 03)

Observational programs

• Several 100 clusters known at 0.2<z<1.0(best selected by SZ-effect, lensing, or X-rays)

• Many (50+) observed with HST (eg ACS GTO team)

• … but only handful outside the inner Mpc

CL1358+62 MS2053-04 MS1054-03 (z=0.33) (z=0.58) (z=0.83)

What have we learned ?

• Early-type galaxies appear to evolve slowly and gradually -> stars formed at high redshift

z=10

z=3z=1.5

Fundamental Plane:van Dokkum/Franx/Kelson/Illingworth/Stanford/vdMarel 96-04

Studies of colors, line strengths, etc:Ellis et al. 1997, Bernardi et al 98,Stanford et al 95/98, vD et al 98,00,Treu et al 99,02, Poggianti et al 03,Blakeslee et al 03, Kodama et al 04

What have we learned ?

RDCS1252 (z=1.24; Blakeslee et al 03; Lidman et al 03)

What have we learned ?

• At the same time, morphological mix evolves

Andreon et al. 1997 Fabricant et al 98Dressler et al. 1997 van D et al 00,01Lubin et al. 1998

Smith et al 04

What have we learned ?

• At the same time, morphological mix evolves• This may affect age estimates of early-type

galaxies (“progenitor bias”; vDF01)• Current idea: evolution driven by infall from the

field

Kodama et al 01(z=0.41; Subaru)

Field spirals andgroups fall in

MORPHS

- Interaction hot gas: “ram pressure stripping” spiral -> S0 galaxy (Gunn & Gott 1972)

- Encounters: “galaxy harassment” spiral -> early-type (Moore et al 98)

Kenney

- Mergers may take place in infalling groups groups -> ellipticals (van Dokkum et al 1999)

Cluster evolution at 0.5<z<1.5

• Need to sample to the virial radius: R~10’• Very inefficient with HST (even with ACS/WF3)

CL0024 at z=0.39Treu et al. 2003 30 arcmin

Surveying clusters at 0.5<z<1.5

• Need to sample to the virial radius: R~10’• Very inefficient with HST (even with ACS/WF3)• Requirements:

– Field of 20-30 arcmin– Near-IR capability to study clusters beyond z=1

• Good match to SNAPlike mission (expect 10-20 clusters in 15 sq degrees of deep survey areas!)

Progenitors at z>2

• Overdensities of young objects found out to z~5

Venemans et al 02; also: Francis et al 97, Steidel et al 00, …

Progenitors at z>2

• Overdensities of young objects found out to z~4• However, rest-UV selection may give biased view

Optical: Palomar digital sky survey UV: GALEX

• L* Sb/c galaxy at z=3: K 23, R 28• Would not be selected by any current method!

Typical Lyman-break galaxyand typical nearby spiral

Selecting “mature” galaxies at z>2

• Use redshifted Balmer- or 4000Å-break

• Adopted criterion: J – K > 2.3 (restframe U – V > 0)

MUSYC Deep(Ryan Quadri)

FIRES Wide(NataschaForster Schreiber)

FIRES Deep(Ivo Labbe)

10 arcmin

Red galaxies at z>2

• Substantial surface density:~ 0.6/arcmin to K=21 (from FIRES/MUSYC)~ 2/arcmin to K=22 (from FIRES)~ 3/arcmin to K=23 (from FIRES)

2

2

2

2

Red galaxies at z>2

• Substantial surface density: ~ 0.6/arcmin to K=21 (from FIRES/MUSYC)~ 2/arcmin to K=22 (from FIRES)~ 3/arcmin to K=23 (from FIRES)

• SEDs very different from Lyman breaks

2

2

2

Förster Schreiber et al., ApJ, submitted

Red galaxies at z>2

• Substantial surface density: ~ 0.8/arcmin to K=21 (from both fields)~ 2/arcmin to K=22 (from HDF-S)~ 3/arcmin to K=23 (from HDF-S)

• SEDs very different from Lyman breaks• Rest-frame optical spectroscopy + SED fits:

massive, dusty, star-forming galaxies

2

2

2

vD et al, ApJ, in press; Foerster Schreiber et al, ApJ, subm.

Red galaxy at z=2.43

Keck/NIRSPEC, 1½ hrsvD et al, ApJ, in press (astro-ph/0404471)

• Best constrained parameter: stellar (and dyn) mass

vD et al, ApJ, in press(astro-ph/0404471)

Correlations with linewidth

• Combining z=3 LBGs and z=2.6 DRGs: linewidth correlates with color and stellar mass

astro-ph/0404471

Evolution of massive galaxies

astro-ph/0404471

Evolution of massive galaxies

?

ERO

Early-type

DRG?

Spiral

LBG

Evolution of massive galaxies

ERO

Early-type

DRG

Spiral

LBG

Mapping matter at z=2-3

• Galaxies highly clustered -> need large fields– Map stellar mass using near-IR selected

galaxies– Map halo mass using Tully-Fisher type

correlations and clustering

HDF-South10’x10’RJK composite

K<21.5, J-K>2.3

MUSYC project(Ryan Quadri)

30’x30’ field(1/60 of SNAPdeep survey!)

Mapping matter at z=2-3

• Galaxies highly clustered -> need large fields– Map stellar mass using near-IR selected

galaxies– Map halo mass using Tully-Fisher type

correlations and clustering• Morphologies

– Fully formed galaxies or mergers?– Sizes: bulges or ellipticals?– Star formation in disks or clumps?– Density? Central point sources?

Red galaxy in Ultra Deep Field:ACS B,V,I,z + NICMOS J,H

B V I z J H

In near-IR, JDEM could be >1000 x more efficient than HST!

Mapping matter at z=2-3

• Galaxies highly clustered -> need large fields– Map stellar mass using near-IR selected

galaxies– Map halo mass using Tully-Fisher type

correlations and clustering• Morphologies

– Sizes / densities– Star formation in disks or clumps?

• How far to the red ?– Current selection: J–K -> z=2-4– In practice: break almost always between J and

H

Quadri etal., in prep

Mapping matter at z=2-3

• Galaxies highly clustered -> need large fields– Map stellar mass using near-IR selected galaxies– Map halo mass using Tully-Fisher type correlations

and clustering• Morphologies

– Sizes / densities– Star formation in disks or clumps?

• How far to the red ?– Current selection: J–K -> z=2-4– In practice: break almost always between J and H– Cutoff at 1.7 micron OK for z=2-3 (need filter!)

• There are exceptions:

• Overlap with ground-based K or IRAC needed to select red z>3 galaxies, and to fit the SEDs

K = 20.1phot z = 3.7

Mapping matter at z=2-3

• Galaxies highly clustered -> need large fields– Map stellar mass using near-IR selected galaxies– Map halo mass using Tully-Fisher type correlations

and clustering• Morphologies

– Sizes / densities– Star formation in disks or clumps?

• How far to the red ?– Current selection: J–K -> z=2-4– In practice: break almost always between J and H– Cutoff at 1.7 micron OK for z=2-3 (need filter!)

Blue: data for K-bright LBGs(Shapley et al; astro-ph/0405187)

Comparison to other star forming galaxies