Evolution of Galaxy Properties from High Redshift to Today

AGNs: Where do they live? In M*>10 10 M . In M*>10 10 M . Morphologically similar to early- types. Morphologically similar to early- types. OTOH, recent SF similar to late- types (esp. in strong AGN). OTOH, recent SF similar to late- types (esp. in strong AGN). Kauffmann et al 2003

AGNs and the red sequence AGNs roughly occupy “green valley”. AGNs roughly occupy “green valley”. Black hole growth occuring in M * ~ M  galaxies. Black hole growth occuring in M * ~ M  galaxies. Same M * as transition in colors, SFRs, etc. Same M * as transition in colors, SFRs, etc. Cause or effect? Cause or effect? Kauffmann et al 2004

Clustering: 2PCF  =(r/r 0 ) - ,  ~1.8 and r 0 ~5 Mpc/h.  =(r/r 0 ) - ,  ~1.8 and r 0 ~5 Mpc/h. Departs significantly from pure power law. Departs significantly from pure power law. Red galaxies have steeper x slope. Red galaxies have steeper x slope. Mild luminosity dependence, strongest at luminous end. Mild luminosity dependence, strongest at luminous end. Zehavi et al. 2003, 2004 Norberg et al 2001

Halo Occupation Distribution HOD = P(N g,M h ). HOD = P(N g,M h ).  made up of “1-halo” and “2-halo” terms.  made up of “1-halo” and “2-halo” terms. From this, get bias: b ≡(  gg /  mm ) 1/2. From this, get bias: b ≡(  gg /  mm ) 1/2. has character- istic shape; can derive by matching  (r). has character- istic shape; can derive by matching  (r). Yang et al 2004 Zehavi et al 2003

Conditional Luminosity Function  (L|M)dL: Luminosity fcn in bins of halo mass.  (L|M)dL: Luminosity fcn in bins of halo mass. Tune  (L|M) to reproduce LF,  (L), and T-F. Tune  (L|M) to reproduce LF,  (L), and T-F. Depends on cosmology, or anything that affects halo abundance. Depends on cosmology, or anything that affects halo abundance. Yang et al 2003

Evolution of Galaxy Properties from High Redshift to Today

Galaxy Surveys: Optical & NIR DEEP2 AEGIS MS1054 COMBO17 MUSYC Steidel ELAIS-S1 From Mara Salvato’s web page

Lilly-Madau Plot Fair amount of scatter, but for z>1 it’s at the ~50% level now. Fair amount of scatter, but for z>1 it’s at the ~50% level now. Half the stars formed by z~1.7. Half the stars formed by z~1.7. Many issues: Dust? IMF? Sample overlap? Many issues: Dust? IMF? Sample overlap? Fardal et al 2006

SFR vs. M* buildup Something weird: ∫ >z SFR >  * (z). Something weird: ∫ >z SFR >  * (z). Globally top- heavy IMF? Globally top- heavy IMF? Pop synth models wrong? Pop synth models wrong? Fardal et al 2006

0 < z < 1 : Red sequence, blue cloud, green valley ? Cirasuolo et al (UKIDSS) Franzetti et al (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 selections 1 < z < 4+ = 10.3 ± 0.5 = 30 ± 20 Msun/yr 0 < E(B-V) < 0.3  by construction 1/3 < Z/Zsun < 1 r 0 ~ 3-5 h -1 Mpc (Steidel et al , 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 galaxies 1 < z < 4 Wider range of colors (ages/dust) Larger surface density (e.g. I < 24; Le Fèvre et al. 2005) Pure flux-limited optical selection No color cuts

Beyond z ~ 1 : NIR-selected star-forming galaxies 1 < z < 3 SFR up to ~ 200+ Msun/yr Most sBzKs and some DRGs are ULIRGs Stellar masses up to ~ Msun High specific SFR Nearly solar metallicity Merger morphology in rest-frame UV sBzK & DRGs strongly clustered (r 0 ~ 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 van 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 Dusty EROs Star-forming BzKs (sBzK) BzKBzK DRGs

Passive systems Gyr old SFH : z(SF onset) > starburst M(stars) > Msun Strongly clustered McCarthy et al. 2004, Daddi et al. 2005, Saracco et al Longhetti et al. 2005, Kong et al. 2006, Kriek et al 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 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 21, Reddy et al. 2005) BM/BX selects 3% (23%) with M>10 11 (>5x10 10 ) 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) Passive Star forming

OPTICAL SELECTION NEAR-IR SELECTION Narrow-band & 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 Borch et al. 2006… Drory et al Bundy et al (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 morphological fractions already in place at z~1 (HDF, MDS, GOODS, HUDF…) (Griffith et al., Abraham et al, Conselice et al,…) Cassata et al (K20+GOODS)

The role of environment (0<z<1.5) Downsizing more pronounced in the highest density environments Color-density relation Cucciati et al (VVDS) Bundy et al (DEEP2 + K) C-D relation stronger for high luminosity C-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 Stellar mass function