Evolution of Galaxy Properties from High Redshift to Today

1. Evolution of Galaxy Properties from High Redshift to Today

2. AGNs: Where do they live? Kauffmann et al 2003 • In M*>1010M. • Morphologically similar to early-types. • OTOH, recent SF similar to late-types (esp. in strong AGN).

3. Kauffmann et al 2004 AGNs and the red sequence • AGNs roughly occupy “green valley”. • Black hole growth occuring in M*~1010.5-1011 M galaxies. • Same M* as transition in colors, SFRs, etc. • Cause or effect?

4. Norberg et al 2001 Clustering: 2PCF • x=(r/r0)-g, g~1.8 and r0~5 Mpc/h. • Departs significantly from pure power law. • Red galaxies have steeper x slope. • Mild luminosity dependence, strongest at luminous end. Zehavi et al. 2003, 2004

5. Yang et al 2004 Halo Occupation Distribution Zehavi et al 2003 • HOD = P(Ng,Mh). • x made up of “1-halo” and “2-halo” terms. • From this, get bias: b≡(xgg/xmm)1/2. • <N(M)> has character-istic shape; can derive by matching x(r).

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

7. Evolution of Galaxy Properties from High Redshift to Today

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

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

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

11. 0 < z < 1 : Red sequence, blue cloud, green valley ? Franzetti et al. 2006 (VVDS) Late-type 0.6<z<0.8 Early-type 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) Cirasuolo et al. 2006 (UKIDSS)

12. Beyond z ~ 1 : optical selections 1 < z < 4+ < log M(stars)/Msun > = 10.3 ± 0.5 < SFR > = 30 ± 20 Msun/yr 0 < 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) Color-selected BM/BX/LBG Pure flux-limited optical selection 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) No color cuts

13. Beyond z ~ 1 : NIR-selected star-forming galaxies Dusty EROs Star-forming BzKs (sBzK) B z K 1 < z < 3 SFR up to ~ 200+ Msun/yr Most sBzKs and some DRGs are ULIRGs Stellar masses up to ~ 1011 Msun High specific SFR Nearly solar metallicity Merger morphology in rest-frame UV sBzK & DRGs strongly clustered (r0 ~ 8-11 h-1 Mpc) DRGs 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. 2004 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. 2006

14. Beyond z ~ 1 : NIR-selected old/passive systems to z ~ 2.5 Passive systems 0.5 - 3 Gyr old SFH : z(SF onset) > 2-3 + starburst M(stars) > 1011 Msun Strongly clustered McCarthy et al. 2004, Daddi et al. 2005, Saracco et al. 2005 Longhetti 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 Kriek et al. 2006

15. Example : BM/BX vs BzK (1.4<z<2.5) Optical color -selected (BM/BX, R < 25.5) K-selected (K < 20, Vega) Star forming Passive 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)

16. NEAR-IR SELECTION Narrow-band & Slitless OPTICAL SELECTION

17. 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. 2006 • Borch et al. 2006… Bundy et al. 2006 (DEEP2 + K) Drory et al. 2005 Caveat on TP-AGB stars (Maraston)

18. Morphology evolution Cassata et al. 2005 (K20+GOODS) Hubble sequence and morphological fractions already in place at z~1 (HDF, MDS, GOODS, HUDF…) (Griffith et al., Abraham et al, Conselice et al,…) Rapid increase of mergers with redshift Early and rapid merging (z>1.5) : formation mechanism of massive galaxies (Conselice 2006)

19. The role of environment (0<z<1.5) Color-density relation Cucciati et al. 2006 (VVDS) Stellar mass function Bundy et al. 2006 (DEEP2 + K) Downsizing more pronounced in the highest density environments 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. 2006