1. New Results from the Recent HST Surveys: COSMOS, GOODS, UDF

2. Plan of the talk: Density-Morphology relation Discovery of a post-starburst galaxy at z ~7 Photometric redshift estimates Evolution of LF of galaxies to z~2 Narrow-band searches for high-z galaxies with Subaru

4. AIMS (COSMOS) evolution of galaxy morphology, SFR, merging, LF, correlation function as a function of LSS and redshift Assembly of galaxies, clusters and dark matter up to 10 14 M sun scales Reconstruction of dark matter distribution up to z >1

5. AIMS (UDF) Search for galaxies out to re-ionization epoch Extend study of star formation rate in galaxies to z ~ 6 Study rest-frame optical properties of galaxies to high redshifts Estimate the luminosity function of galaxies at z ~ 6

6. AIMS (GOODS) Study of the mass assembly rate and star formation in galaxies Explore rest-frame morphologies of galaxies and their evolution with redshift Provide multi-waveband data to address fundamental questions regarding the formation and evolution of galaxies

7. COSMOS: Morphology-Density Relation Bahram Mobasher Capak, Mobasher, Ellis, Scoville, Sheth, Abraham, ApJL 2005

8. Motivation: Role of environment in shaping Hubble sequence 0<z<1 Ingredients: ACS morphologies (+ proxies from photo-z/spectra)  Photometric redshifts (for slices)  Density estimates (  gals. Mpc -2, lensing  ….) Stellar masses (requires deeper K-band) Progress/issues: Auto/visual morphologies & photo-z tested in 3 x 3 inner field Robustness of 2-D  as a tracer of 3-D density is an issue Morphology-Density Relation: Progress & Issues

9. Evolution of the T-  relation 0 < z < 1 Environmental density  plays key role in governing morphological mix: - Continued growth in high  but delay for lower  regions - Slower conversion of spirals to S0s with only Es at z > 1? Smith et al 2004 (astro-ph/0403455) f E/S0

10. Evolution of the T-  relation ACS clusters Holland et al 2004 (astro-ph/0408165) Explores the high  end in more detail via GTO cluster sample (N=7, E:S0) Illustrates the advantage of combining COSMOS with cluster datasets? f E/S0  COSMOS

11. Morphological Catalog (Abraham, Sheth + RSE) Morph-cat (RGA): -based on earlier MDS, HDF precepts to I(AB)=24 - Asymm, Conc, Gini-C,  - N ~ ? Reality check (RSE/KS): - visual catalog I(AB)=22.5 in inner 3  3 g+I zone - typed according to precepts used in MDS, HDF, GOODS - N~700 Extension to full area: N(tot) ~ ?

12. COSMOS T=5 Sc(d)m I AB <22.5

13. COSMOS T=1 E/S0 I AB <22.5

16. What limit for automated morphologies? Robustness of “classic” parameters (A-C test): I(AB)=22.5 (COSMOS) is broadly equivalent to I(AB)=24 (HDF)

17. But how reliable is a projected 2-D density? Measured  in a photo-z slice   True spatial density  /  Fidelity of using  will depend on photo-z  z, error and itself (Benson VIRGO simulations)

20. Results Density-morphology relation was already in place at z~1 We see a steady increase in the fraction of elliptical galaxies with decreasing redshift from z=1.2 to present The strength of this trend depends on the local density

21. Merging Photo-z & Morph-cats in the inner region V-I Photo-z Independent demonstration of robustness of photo-z’s

22. Search for the highest redshift galaxies B. Mobasher, M. Dickinson, H. C. Ferguson, M. Giavalisco, T. Wiklind, R. S. Ellis, M. Fall N. Grogin, L. Moustakas, N. Panagia D. Stark, M. Sossy, M. Stiavelli E. Bergeron, S. Casertano, A. Koekemoer, M. Livio, C. Scaralata Mobasher et al (2005) submitted

23. Hubble Ultra-Deep Field A sub-area of the GOODS-S (CDF-S)  CS Area: 3’ x 3’ m AB (z 850LP ) = 28.4 mag (10  for extended source over 0.2 arcsec 2 aperture) NICMOS Area: 2.5’ x 2.5’ m AB (F160W) = 25.1 mag. (10  for extended source)

24. GOODS-South HUDF is fully covered By Spitzer

25. HUDF+GOODS-S ACS: B 435 V 606 i 775 z 850LP NICMOS: J 110 H 160 ISAAC: K s Spitzer: IRAC (3.6-8.0 micron) MIPS: 24 micron Radio 1.4 GHz (ATCA, VLA) X-ray (Chandra) Ground-based UBVRIJHK images Photometric Redshifts -10% accurate

26. High-z selection Sources with (J – H) AB > 1.3 and no detection in optical-ACS bands were selected. Two sources were identified. One close to an X-ray source (likely an AGN) while the other is not associated with any X-ray (or radio) source- UDF033238.7-274839

28. Spectral Energy Distributions Simultaneously optimizing model parameters consisting of redshift (z), extinction (E(B-V)), starburst age (t sb ) and metallicity (Z) Population synthesis models: STARBURST99 (Vazquez & Leitherer 2005) Bruzual & Charlot 2003

30. Associated with an X-ray source

36. Model Parameters Parameter range: Redshift 0 < z < 12 Extinction 0 < E(B-V) < 1 Starburst age 0.1 < t sb < 5 Gyrs Metallicity 0.004, 0.008, 0.02, 0.04 Calzetti extinction law Salpeter IMF 0.1 < M < 100 M sun

37. Star formation laws Continuous SF mode Instantaneous SF- single SF burst follwed by a decrease for t sb yrs Exponentially decreasing SFR with e-folding time scale  0,100,200,300,400 Myrs

38. Best SED Fits STARBURST99 Instantaneous star formation burst z=7.2; E B-V =0.05; t sb =600 Myrs Z=0.004 Bruzual & Charlot Exponentially decreasing SFR with  0 z=7.0; E B-V =0.15; t sb =400 Myrs Z=0.008

40. Degeneracies It is possible that different combinations of parameters could Produce equally acceptable fits. low metallicity SED and high age or extinction could mimic an SED with higher metallicity and lower age/extinction

41. Every single combination of age (0.1-5 Gyrs) Metallicity (0.2-2.5 solar) Extinction (0 < E(B-V) < 1) Redshift (0 < z < 12) e-folding SFR (  0-500) is considered

43. It is possible that the observed SED is caused by: Contribution from old stellar population at z ~ 2-4 heavily obscured starburst at lower redshifts Complicated degeneracy between redshift, extinction, metallicity, age

44. An old population SED was simulated by fixing the age to 1-2 Gyr and fitting the rest of the parameters- no acceptable fit to the observed SED (at the > 5  level) was found at any redshift. To fit the observed SED with a heavily reddened object, one needs E(B-V) > 0.5 and a MUCH reduced likelihood.

49. Spectroscopic Campaign Keck vs. Gemini Gemini vs. VLT VLT vs. Keck

50. Keck NIR Spectrum R. S. Ellis & D. Stark

51. Results High stellar mass of 8 x 10 10 M sun  Galaxy formed the bulk of its stars very rapidly, entering a significant quiescent phase  Formed today’s of Milky way mass when the Universe was 200-400 Myr old (z=12-20)  Evidence for monolitic formation of galaxies ?  Its SED is different from LBGs  JWST target ?

52. GOODS Photometric redshift measurement Evolution of rest-frame galaxy LF to z ~ 2 Narrow-band survey and nature of LAEs at z = 5.7- their Spitzer properties

53. GOODS Phot-z Measurement Mobasher et al 2004, 2005 six templates used Luminosity function used as prior Cosmic opacity from Madau et al. Extinction allowed as a free parameter, estimating E(B-V) for each galaxy Interpolates the spectral types Easily extended to other bands (ie IRAC, GALEX etc)

57. Input: Galaxy magnitudes, magnitude errors, templates, filter response functions Output: z(phot), spectral types, redshift probability distribution, conventional and prior-based redshifts, extinction COSMOS phot-z’s: UBVRizK bands, E, Sa, Sb, Sc, Im, Starburst templates

60. Luminosity functions are calculated using * 1/Vmax method * Maximum likelihood method Traditionally (ideally): each galaxy has one redshift -> one absolute magnitude -> one galaxy added to magnitude bin in LF Using phot-z's: Phot-z's have relatively large errors Each galaxy is represented by a redshift distribution

61. Evolution of rest-frame LFs T.Dahlen, B.Mobasher,R.Somerville, L.Moustakas, M.Dickinson, H.C. Ferguson, M.Giavalisco ApJ 2005 Combine 1100 arcmin 2 optical (UBVRI)- (RAB < 24.5) and 130 arcmin 2 near-IR (JHK)- (KAB < 23.2) surveys

62. Advantages… Deep and wide area near-IR data allow study of rest-frame optical LF to z~2 Near-IR data allow us to probe deeper in the rest- frame optical LFs in the range z~1-2 Allows study of rest-frame J-band LF (mass function) to z=1 Allow measurement of SFR to z~2.2, using rest- frame 2800A measurements- compare to GALEX

66. LF Results The shape of the LFs vary significantly between different spectral types. Early-type galaxy show a near gaussian LF Starburst LFs have steep faint-end slopes

71. Dimming of 0.6 mag in M* J between z=0.1 and 1

73. Results- evolution of rest-frame LFs Evolution of rest-frame U, B & R-band LFs are considered in six equal comoving volumes to z~2 M* brightens by 2.1 (U), 0.8 (B) and 0.7 (R) mag between z~0.1 and z~2. There is a strong decline in  * with redshift in U-band Rest-frame J-band LF shows a dimming between z~0.4 and 0.9  mean stellar mass was lower in the past There is strong evolution with redshift in the relative contribution from different spec. types to the luminosity density

75. SFR from rest-frame 2800A Mobasher et al 2005

76. Structure and Evolution of Starburst Galaxies Mobasher et al (2004) Aims: How different is the morphology of starburst and normal galaxies ? How significant is the effect of galaxy interactions on SFR ? Sample selection: Sample of SB galaxies is selected based on their spectral types (from SED fitting). A Control sample of normal (E,Sp) galaxies was also selected in the same way. Rest-frame B-band morphologies were determined, using BViz band ACS images and photometric redshifts

78. Concentration Most z<=1 optically selected starbursts have concentration indices which are significantly smaller than most early types C>0.3 : 12 % SB, 18% Late, 73% E/Sa Komogorov-Smirnov ( K-S) test - SB vs Early type : 7e-7 (> 99.9%) - SB vs Late-type : 0.53 Large C & galfit Sersic n=3-4 correlate AGN fraction : CDF-S X-ray catalog : 2% of SB host AGN vs >25% of Early types

79. Asymmetry in rest frame B 55 % of z 0.3) compared to lower fractions in late (20% ) and early (12%). K-S test on A B - SB vs Early type : 1e-10 - SB vs Late-type : 3e-4 ABAB Large A B : highly asymmetric distribution of massive SF (no m=2 symmetry) - Externally triggered : tidal interactions, mergers

81. Narrow-band search for high-z galaxies A survey in NB816 over the GOODS-ACS area NB816 < 25 I – NB816 > 0.7 Not detected in B and V-bands 29 sources identified over the GOODS area

82. Rest-frame Properties of LAEs Mobasher, Taniguchi, Ajiki 2005 75% of narrow-band selected LAEs have spect. Confirmation at z =5.7 (Rhoads et al 2003) No Spect. Data is yet available for our sample (BIG ASSUMPTION!) 18 (>60%) of the LAEs detected by IRAC

84. Sersic n dist. in rest-frame UV

85. rest-optical & -IR at z=5.8 SST IRAC detections of z~6 galaxies => stellar population & dust fitting possible Dickinson et al in prep ch1, 3.6  m rest =5300A ch2, 4.5  m rest =6600A

88. SFR vs. Mass

90. Nature of LAEs Dominated by disk systems Varied morphological types SFR ~ 20 – 40 M(sun)/yr (estimated from Ha line) How is the LAEs SEDs compared to that of the LBGs ? ACS (iz) ISAAC (JHK) IRAC data available