Evolution of Evolution of Galaxy Properties Galaxy Properties from High Redshift from High Redshift

to Todayto Today

AGNs: Where do they AGNs: Where do they live?live?

In M*>10In M*>101010MM.. MorphologicallMorphologicall

y similar to y similar to early-types.early-types.

OTOH, recent OTOH, recent SF similar to SF similar to late-types (esp. late-types (esp. in strong AGN).in strong AGN).

Kauffmann et al 2003

AGNs and the AGNs and the red sequence red sequence

AGNs roughly occupy AGNs roughly occupy “green valley”.“green valley”.

Black hole growth Black hole growth occuring in Moccuring in M**~10~1010.510.5--10101111 M M galaxies. galaxies.

Same MSame M** as transition as transition in colors, SFRs, etc. in colors, SFRs, etc.

Cause or effect?Cause or effect?

Kauffmann et al 2004

Clustering: 2PCFClustering: 2PCF =(r/r=(r/r00))--, , ~1.8 and ~1.8 and

rr00~5 Mpc/h.~5 Mpc/h. Departs significantly Departs significantly

from pure power law.from pure power law. Red galaxies have Red galaxies have

steeper x slope.steeper x slope. Mild luminosity Mild luminosity

dependence, dependence, strongest at strongest at luminous end.luminous end.

Zehavi et al. 2003, 2004

Norberg et al 2001

Halo Occupation Halo Occupation DistributionDistribution HOD = P(NHOD = P(Ngg,M,Mhh).).

made up of “1-halo” made up of “1-halo” and “2-halo” terms.and “2-halo” terms.

From this, get bias: From this, get bias: bb≡(≡(gggg//mmmm))1/21/2..

<N(M)> has <N(M)> has character-istic shape; character-istic shape; can derive by can derive by matching matching (r).(r).

Yang et al 2004

Zehavi et al 2003

Conditional Luminosity Conditional Luminosity FunctionFunction

(L|M)dL: (L|M)dL: Luminosity Luminosity fcn in bins of fcn in bins of halo mass.halo mass.

Tune Tune (L|M) (L|M) to reproduce to reproduce LF, LF, (L), and (L), and T-F.T-F.

Depends on Depends on cosmology, cosmology, or anything or anything that affects that affects halo halo abundance.abundance.

Yang et al 2003

Evolution of Evolution of Galaxy Properties Galaxy Properties from High Redshift from High Redshift

to Todayto Today

Galaxy Surveys: Optical & Galaxy Surveys: Optical & NIRNIR

•DEEP2AEGIS

•MS1054

•COMBO17 •MUSYC•Steidel •ELAIS-S1

Lilly-Madau PlotLilly-Madau Plot

Fair amount of Fair amount of scatter, but for scatter, but for z>1 it’s at the z>1 it’s at the ~50% level now.~50% level now.

Half the stars Half the stars formed by z~1.7.formed by z~1.7.

Many issues: Many issues: Dust? IMF? Dust? IMF? Sample overlap?Sample overlap?

Fardal et al 2006

SFR vs. M* buildupSFR vs. M* buildup

Something Something weird: weird: ∫∫>z>zSFR SFR >> **(z).(z).

GloballyGlobally top- top-heavy IMF?heavy IMF?

Pop synth Pop synth models models wrong?wrong?

Fardal et al 2006

0 < z < 1 : Red sequence, blue cloud, green valley ?

Cirasuolo et al. 2006 (UKIDSS)

Franzettiet al. 2006(VVDS)

Color bimodality to z ~ 1 (Bell et al. 2004)

Disappears beyond z ~ 1.5 ?(Wuyts et al. 2006, Cirasuolo et al. 2006…)

Reliability ? Contamination ?

See also the degeneracy of ERO colors(e.g. Cimatti et al. 2002, 2003, Moustakas et al. 2004, Stern et al. 2006)

Late-type

Early-type

0.6<z<0.8

Beyond z ~ 1 : optical selectionsBeyond z ~ 1 : optical selections

1 < z < 4+< log M(stars)/Msun > = 10.3 ± 0.5< SFR > = 30 ± 20 Msun/yr0 < E(B-V) < 0.3 by construction 1/3 < Z/Zsun < 1 r0 ~ 3-5 h-1 Mpc

(Steidel et al. 1996-2004, Adelberger et al.2004, Reddy et al. 2005, Shapley et al. 2003, 2005, Erb et al. 2006)

BM/BX/LBG

Color-selected

Bulk : star-forming galaxies1 < z < 4Wider range of colors (ages/dust)Larger surface density

(e.g. I < 24; Le Fèvre et al. 2005)

Pure flux-limitedoptical selection

No color cuts

Beyond z Beyond z ~ 1 : ~ 1 : NIR-selected star-forming galaxiesNIR-selected star-forming galaxies

1 < z < 3SFR up to ~ 200+ Msun/yr Most sBzKs and some DRGs are ULIRGsStellar masses up to ~ 1011 Msun High specific SFRNearly solar metallicity Merger morphology in rest-frame UVsBzK & DRGs strongly clustered (r0 ~ 8-11 h-1 Mpc)

Cimatti et al. 2002, 2003, Daddi et al. 2004a, 2004b, 2005; De Mello et al 2004, Dannerbauer et al. 2005, Kong et al. 2006, Franx et al. 2003, Forster-Schreiber et al. 2004van Dokkum et al. 2005, Webb et al. 2006, Papovich et al., Doherty et al., Yan et al. Grazian et al. 2006, Quadri et al. 2006, Foucaud et al, Grazian et al. 2006

Dusty EROs Star-forming BzKs (sBzK) B

z

K

DRGs

Passive systems 0.5 - 3 Gyr oldSFH : z(SF onset) > 2-3 + starburstM(stars) > 1011 Msun Strongly clustered

McCarthy et al. 2004, Daddi et al. 2005, Saracco et al. 2005Longhetti et al. 2005, Kong et al. 2006, Kriek et al. 2006

Old/massive systems at z > 4-5 ? (Mobasher et al. 2005, Dunlop et al. 2006, Rodighiero et al. 2006, Wiklind et al. 2006, Mancini et al. )

Cimatti et al. 2004

Beyond z ~ 1 : NIR-selected old/passive systems to z ~ 2.5

Kriek et al. 2006

Optical color -selected (BM/BX, R < 25.5) K-selected (K < 20, Vega)

Example : BM/BX vs BzK (1.4<z<2.5)

BM/BX can miss up to 60%-70% of the K-selected with K<20 (weaker bias for K>21, Reddy et al. 2005)BM/BX selects 3% (23%) with M>1011 (>5x1010) Msun (similar for DRGs; van Dokkum et al. 2006)To K~22, optically selected contribute to most of the SFD traced by OPT+NIR (Reddy et al. 2005)Pure flux-limited optical surveys selects more galaxies vs optical color selection (Le Fèvre et al. 2005)

PassiveStarforming

OPTICAL SELECTION

NEAR-IR SELECTION Narrow

-ban

d&

Slitless

Stellar mass functions High-mass tail : dominated by ETGs to z~1-1.5 High-mass tail : very little evolution (0<z<0.8) N(ETGs, z) mirrored by N(star-forming, z) No much room for “dry” merging at 0<z<1

Downsizing (Cowie et al. 96, see also Gavazzi et al. 1996)

Fontana et al. 2004,2006, Drory et al. 2004,2005, Bundy et al. 2005,Caputi et al. 2006, Pannella et al. 2006, Franceschini et al. 2006Borch et al. 2006…

Drory et al. 2005Bundy et al. 2006 (DEEP2 + K)

Caveat on TP-AGB stars (Maraston)

Morphology evolution

Rapid increase of mergers with redshift

Early and rapid merging (z>1.5) : formation mechanism of massive galaxies(Conselice 2006)

Hubble sequence and morphologicalfractions already in place at z~1(HDF, MDS, GOODS, HUDF…)(Griffith et al., Abraham et al, Conselice et al,…)

Cassata et al. 2005 (K20+GOODS)

The role of environment (0<z<1.5)

Downsizing more pronounced in the highest density environments

Color-density relation

Cucciati et al. 2006(VVDS)

Bundy et al. 2006(DEEP2 + K)

C-D relation stronger for high luminosityC-D relation weakens for increasing z (but see Quadri et al. 2006)

Kodama et al. 2004, Yee et al. 2005, Cooper et al. 2006, Ilbert et al. 2006, Gerke et al. 2006

Stellar mass function