2. Exploring the High-z Frontier — Galaxies at z  6 and beyond Haojing Yan (Carnegie Observatories) Purple Mountain Observatory July 14, 2008 Haojing Yan (Carnegie Observatories) Purple Mountain Observatory July 14, 2008

3. Outline UV Luminosity Function of Galaxies at z  6 — LBG LF has a very steep faint-end slope Stellar Masses of Galaxies at z  6 — some high-mass, “old” galaxies already in place Implications for (HI) Reionization — dwarf galaxies did it! Unanswered Questions at z  6 — evolution of LF at the bright-end? Searching for Galaxies at z > 7-8

4. Part I LF of Galaxies at z  6 (5.5  z  6.5)

5. Reionization might have ended at z  6 (Fan et al. 2006, AJ, 132,117) ~ 1% is sufficient to create a complete GP-trough Practically, H still nearly fully ionized at z  6

6. Searching Techniques Lyman- Break Galaxy (LBG) “Dropout” Ly  Emitter (LAE)

7. Surface Density Expectation Assuming non-evolving M* (- 21.23) & faint-end slope  (-1.6) from z=3 Using the z=5.60 galaxy in the HDF-N (Weymann et al. 1999) to fix the normalization Yan et al. 2002, ApJ, 580, 725

8. Simple Prediction Seems to Work Well Consistent with all observations up to 2003, including new results from the HST/ACS Different groups emphasized different aspects: Yan et al. (2003) Bouwens et al. (2003) Bunker et al. (2004) Dickinson et al. (2004)

9. Source(s) of Reionization Yan & Windhorst 2004, ApJ, 600, L1 Critical value from Madau, Haardt & Rees 1999 Contribution from reionizing sources Galaxies can account for the necessary reionizing photons, if the LF has a steep faint-end slope; dwarf galaxies are important contributors. Galaxies can account for the necessary reionizing photons, if the LF has a steep faint-end slope; dwarf galaxies are important contributors.

10. To z<30 mag, 108 i-dropouts found in the HUDF (Yan & Windhorst 2004, ApJ, 612, L93; YW04) Note: ~ 1.5 mag deeper than Bunker et al. (2004; MNRAS, 355, 374)

11. By pushing to the very limit of the HUDF, we start to be able to address the LF faint-end slope at z~6.

12. i’ z’ z’=29.23 z’=29.97 Detection Reliability at z>28.5 mag Level

13. z=5.83; Dickinson et al. (2004) z=5.9; Malhotra et al. (2005)

14. ACS Grism Observations of HUDF (GRAPES; Malhotra et al. 2005) z=6.0 z=6.1 z=6.4 GRAPES: i-dropouts success rate of ~ 90% in the HUDF to z~27.5 mag

15. Our HUDF z  6 candidate sample supports a very steep UV LF faint-end slope: α = -1.8 to -1.9 Dwarf galaxies can provide sufficient (re)ionizing photons at z  6 YW04 Constrain to the UV LF at z  6

16. Recent Result Confirms the Steep Faint-end Slope (Bouwens et al. 2006) 506 i-drops: UDF, UDF-Pars, GOODS But compare to YW04: M* = -21.03,  * = 4.6x10 -4 /Mpc 3 4.6x10 -3 M sun /yr/Mpc 3 1.1x10 -2 M sun /yr/Mpc 3  SFR is still uncertain by 2x “Lilly-Madau Diagram”

17. Luminosity Function of z  6 LAE LAE : ~ 1/4 of the entire galaxy population (based on results at z~3), but still very important — easier to identify; current redshift record holder is the LAE at z=6.96 (Iye et al. 2006) LAE as probe of the reionization epoch : neutral IGM — Lya line suppressed — LAE number drop (e.g., Marilada-Escude 1998; Malhotra & Rhoads 2001) LAE at z  6 are usually selected at two narrow windows at z=5.7 & 6.5 in order to avoid strong night-sky lines

18. Evolution of LAE LF from z=5.7 t0 6.5 Malhotra & Rhoads (2004): no evolution seen; IGM ionized up to z=6.5 Haiman & Cen (2005): not necessarily; local HII bubble permits escape of Lya photons and the suppression is not as large; up to 25%

19. Better Statistics from Subaru Deep Field Shimasaku et al. (2006)Kashikawa et al. (2006) Kashikawa et al. (2006): strong evolution from z=5.7 to z=6.5 ! Significant fraction of HI at z=6.5 ?? WMAP z reion ~ 11.4?

20. Part II Stellar Masses of Galaxies at z  6

21. Stellar Mass Assembly History in Early Universe Stellar mass density & SFR density:   = ∫  SFR dt Need measurements at rest-frame optical (and beyond) to reduce biases caused by dust extinction and short-lived stars when converting light to mass Study at high-z made possible by Spitzer IRAC GOODS Spitzer Legacy Program has played an important role

22. HST Chandra Spitzer GOODS: Great Observatories Origins Deep Survey

23. Chandra Deep Field SouthChandra Deep Field North (HDF-N) 24’ 28’ (2 Million Seconds)(1 Million Seconds) GOODS Fields

24. CDF-SHDF-N 10’ 16.5’ 10’ 16.5’ (PI. Mauro Giavalisco) HST Treasury Program: ACS B, V, i, z (0.5 to 0.9μm) to near-HDF depth

25. CDF-S HDF-N (PI. Mark Dickinson) Spitzer Legacy Program: Deepest IRAC 3.6 – 8.0μm & MIPS 24μm

26. Extensive Supporting Observations

27.   3.6, 5.8, 4.5, 8.0µm   256x256 array   1.2”/pixel   5.12’x5.12’

28. 3.6 μ m4.5 μ m 5.6 μ m8.0 μ m z =5.83 galaxy IRAC Sees z ~ 6 Galaxies in HUDF

29. z=5.83 z=5.9 z p ~5.9 Three i-drops in HUDF securely detected by IRAC Yan et al. 2005, ApJ, 634, 109

30. Some high-mass (a few x 10 10 M sun ) galaxies were already in place by z  6 (age of Universe < 1.0 Gyr) A few hundred Myr old (formed at z>>6) Number density consistent with  CDM simulation from Nagamine et al. (2004) Some Major Conclusions from SED Fitting See also Eyles et al. (2005)

31. CDFS, 3.6 μ mHDFN, 3.6 μ m Extending to Entire GOODS (Yan et al. 2006, ApJ, 651, 24) IRAC-detected i-dropouts

32. CDFS, 3.6 μ m HDFN, 3.6 μ m IRAC-invisible i-dropouts

33. 274 i’-drops selected by GOODS ACS data (~12 spec-id’ed) Rejecting low-z contaminators --- IRAC-selected Extremely Red Objects (IEROs; Yan et al. 2004): ~17% among the non-blended i’-drops CDF-S HDF-N Sum detected 34 19 53 (“IRAC- detected”) invisible 45 34 79 (“IRAC- invisible”) blended 54 64 118 x 83% 98 (“Blended”) additional contamination due to photometric error 3/13~23% based on HUDF results Basic Statistics

34. Difficulty: no photometric info between z’ and IRAC 3.6 μ m Have to take a different, simplified approach (z’-3.6 μ m) color  age for a given SFH  M/L for a given SFH at this age  stellar mass; repeat for all SFH in the set, and take min, max, median

35. Stellar Mass Estimates Summarized IRAC-detected Sample M rep : 0.09 ~ 7.0x10 10 M sun (median 9.5x10 9 M sun ) T rep : 50 ~ 400 Myr (median 290 Myr) IRAC-invisible Sample, using 3.6  m upper limit Upper-limit of M max (median 4.9x10 9 M sun )

36. IRAC-invisible sample stackRandom stack 3.6 μ m 3.6 μ m mag = 27.44 median z’ mag = 27.00 M min = 1.5x10 8 M rep = 2.0x10 8 M sun M max = 5.9x10 9 Stacking of IRAC-invisible i-dropouts

37. Models courtesy of K. Nagamine; based on simulations of Nagamine et al. (2004) and Night et al. (2006) Implications (I): compare to simulation ΛCDM models seem to be capable of producing such high-mass galaxies by z  6

38. Implications (II): Global Stellar Mass Density Lower limit at z ~ 6: (1.0, 1.6, 6.5) x 10 6 M sun Mpc -3

39. Implications (III): Source of Reionization Critical SFR based on Madau et al. (1999) Progenitors of all IRAC- detected z  6 galaxies formed simultaneously with the same e-SFH: SFR  e -t/  The progenitors of high-mass galaxies alone CANNOT provide sufficient ionizing photons to sustain the reionization Dwarf (low-mass, low- luminosity) galaxies, which could be more numerous, must have played an important role

40. Part III Bright-end of LF at z  6

41. L* & Bright-end of LBG LF Bouwens et al. (2006): L*(z=6) = 0.6L*(z=3) Effect of large-scale structure ( “cosmic variance”)??

42. Need Degree-sized Surveys to Minimize Impact of “Cosmic Variance” at Bright-end (Millennium Simulation slice at z=5.7)

43. D1(2h-4d) (overlap SWIRE) D2 (10h+2d) (w/COSMOS) D3 D4 16.5’x10’ GOODS- Size Area Bright i-drops in 4-deg 2 CFHTLS Yan et al. (in prep)

44. u’ g’ r’ i’ z’ 3.6µm 4.5µm 5.8µm 8.0µm u’ g’ r’ i’ z’ 3.6µm 4.5µm 5.8µm 8.0µm z’-ch1≥3.25; IRAC-selected ERO (IERO; Yan et al. 2004); “red & dead” galaxies at z~2-3 IRAC to Screen Out Interlopers

45. D1 D2 D3 D4 z’<24.0 12 50 12 34 24.0≤z’<24.5 18 36 19 37 24.5≤z’<25.0 54 67 42 75 Total 72 103 61 112 75% 54 77 46 84 Yan & Windhorst 04: Bouwens et al. 06: 17.81 1.53 96.21 26.72 114/deg 2 28/deg 2   Much closer to YW04 prediction; the agreement is even better after counting the incompleteness correction at AB~25. Sample Statistics

46. Magellan High-z LAE Survey Yan, McCarthy & Windhorst

47. Survey Highlights Narrow-band imaging in 917nm & 971nm OH- free windows to search for LAE at z ≈ 6.5 & 7.0 Four IMACS f/2 fields (~ 0.9 deg 2 ); reducing cosmic variance with limited telescope time Survey depth (5-  ) AB=25.0 mag (2.45  10 -17 erg/s/cm 2 for pure-line sources; 7-8  10 -18 erg/s/cm 2 for continuum-detected sources) Aiming at bright-end of the luminosity function

48. 6.46 — 6.62 6.91 — 7.07 ~ 400 Mpc 3 /arcmin 2 (Before upgrading, SITe CCDs) o(917nm)p(971nm) Survey Design: Filters

49. Survey Design: Fields Use fields that have public, deep continuum images in multi-bands (especially in z’-band) Accessibility from Las Campanas CFHTLS Deep D1, D2 & D4 spreading out in RA

50. Survey Status 1-night in Feb. 2007 + 2-night in Mar. 2008, 1 IMACS pointing in COSMOS field (CFHTLS- D2), 20hr in o(917nm) 3-night in Jul. 2007, 1 IMACS pointing in CFHTLS-D4, 20 hr in o(917nm) Achieved desired depth

51. COSMOS CFHTLS-D4 1.48 o 1o1o 1o1o

52. 5-  source counts CFHTLSD4NW, 20hr in o

53. LAE Candidate Selection Continuum images from the T0003 release of CFHTLS-D4 z’-o>0.44 (f lin /f con >1.5) i’-z’>1.3 if detected in z’ non-detection in u’,g’ and r’ For now only discussing candidates invisible in z’

54. 3 candidates invisible in continuum o=23.88 o=24.39 o=25.49? (Now seeking time do spectroscopic identification)

55. Kashikawa et al. 2006 (in Subaru Deep Field) Rapid Evolution from z=5.7 to 6.6 or not?

56. Part IV Searching for Galaxies at z > 7-8 and beyond

57. Deep Space-based IR Imaging for LBG Bouwens & Illingworth (2006); Bouwens et al. (2008)

58. Space-based IR Imaging around Lensing Clusters for LBG Bradley et al. (2008) Abell 1689

59. Direct Slit-Spectroscopy around Lensing Clusters for LAE Stark et al. (2007)

60. Another Line of Thought There might be a much more luminous population at z>7; surface density as high as 0.01-0.05/arcmin 2 From Yan et al. (2006)

61. Wide-field near-IR Survey with WIRCam at CFHT PIs. Lihwai Lin & Luc Simard

62. CFHT WIRCam J, 26 hrs Candidates to be observed by NICMOS in Cy-16 soon (PI. Yan)

63. WFC3/HST Will Play a Critical Role in the Study of the High-z Universe

64. Programs with various depths & coverage WFC3 IR FOV 4.6 arcmin2 Ultra-deep program (HUDF- like) to probe the faint-end Wide program (GOODS-like) to probe the L* level Different sight-lines to beat down the cosmic variance — 200-orbit parallel program approved in Cycle- 17 (PI. Yan)

65. Summary UV Luminosity Function of Galaxies at z  6 — a very steep faint-end slope Stellar Masses of Galaxies at z  6 — some high-mass, “old” galaxies already in place Implications for (HI) Reionization — dwarf galaxies did it! Unanswered Questions at z  6: Bright-end of LF (LBG/LAE) — degree-sized surveys needed to reduce “cosmic variance” Searching for Galaxies at z > 7-8 — very wide-field IR survey from the ground and deep surveys from the space (wait for WFC3!)