# Presentation: 124378

## Galaxies in clusters and their progenitors

- Pieter van Dokkum (Yale)

## General properties of cluster galaxies

**General properties of cluster galaxies**

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

- (Dressler 1980)

**Notes:**
Add image center Coma + 2 or 3 galaxies

## 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)

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

- Terlevich, Caldwell,
- Bower 2001

**Notes:**
Add nice CM relation, from Terlevich

## 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

**Notes:**
Add plot showing sigma distribution current halos Ly-break galaxies, Baugh et al. 1998

## 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

- 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 et
- al. 2003

## Observational programs

- HST: morphologies, structure, sizes
- 8-10m telescopes: kinematics, line strengths

- z=0.83
- elliptical

- Keck+LRIS
- 4 hours

**Notes:**
Hst images galaxy, model, residual + spectrum Kelson (eg)

## Observational programs

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

- Stanford et
- al. 2001

**Notes:**
Hst images galaxy, model, residual + spectrum Kelson (eg)

## 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)***

**Notes:**
Hst images galaxy, model, residual + spectrum Kelson (eg)

## 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)

**Notes:**
Hst images galaxy, model, residual + spectrum Kelson (eg)

## 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)**

**Notes:**
Hst images galaxy, model, residual + spectrum Kelson (eg)

## What have we learned ?

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

- z=10

- z=3

- z=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 98
- Dressler et al. 1997   van D et al 00,01
- Lubin 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 and
- groups 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=0.39
- Treu et al. 2003

## 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!

- Would not be selected by any current method!

## 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
- (Natascha
- Forster 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, 11⁄2 hrs
- vD 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

## Progenitors of massive galaxies

- Substantial population of massive galaxies at z>2 with rest-optical colors similar to normal nearby galaxies
- Ideas have evolved rapidly .. not settled at all !
- <1996: Radio galaxies, EROs
- 1996: Lyman breaks
- 2000: Scuba sources, hard X-ray sources
- 2003: “K20” objects, DRGs (J-K>2.3)
- 2004: Gemini Deep Deep Survey galaxies

- Franx et al 03, vD et al 03,04, Daddi et al 03, Foerster Schreiber et al 04

## 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-South
- 10’x10’
- RJK composite
- K<21.5, J-K>2.3
- MUSYC project
- (Ryan Quadri)

- 30’x30’ field
- (1/60 of SNAP
- deep 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?

- HDF-South
- 10’x10’, K-band
- CTIO 4m+ISPI
- MUSYC project
- (Ryan Quadri)

- HDF-South
- 10’x10’
- RJK composite
- MUSYC project
- (Ryan Quadri)

- HDF-South
- 10’x10’
- RJK composite
- K<21.5, J-K>2.3
- MUSYC project
- (Ryan Quadri)

- HDF-South
- 10’x10’
- RJK composite
- K<21.5, J-K>2.3
- MUSYC project
- (Ryan Quadri)

- K-band
- 5σ limit = 21.6

- R-band
- 5σ limit = 26.5

**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 et
- al., 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

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

- K = 20.1
- phot 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