1. Microwave Background Image from Space Telescope Science Institute What reionized the universe? Searching for Lyman  Beyond Reionization Betsy Barton (UC Irvine)

2. Recent reionization results Wilkinson Microwave Anisotropy Probe (WMAP): –Reionization begins at 14 < z < 20 (Kogut et al. 2003) Becker et al. (2001); Djorgovski et al. (2001); Fan et al. (2002): –Absorption systems and Gunn-Peterson troughs in distant quasar spectra –Reionization ends near z ~ 6 Fan et al. (2001): –quasars not enough to reionize universe STAR-FORMING GALAXIES! (see Tinsley 1973) How can we find these galaxies?

3. Cosmological hydrodynamic simulations form “tiny” early seed galaxies (Davé, Katz, & Weinberg) z=8 Ly  star formation cooling radiation

4. Cosmological hydrodynamic simulations: the star formation history of the universe redshift global star formation rate (Springel & Hernquist 2003) Peak is near z=5 rate significant at extremely high redshifts

5. Finding “holes” in the night sky Atmospheric lines dominate At higher spectral resolution, observe between them

6. Window at z=8.227 Narrow-band filter (R=125) Noise down by factor of >10 from other Gemini/NIRI narrow-band filters transmission skyemission

7. The Production and Escape of High- redshift Lyman-  Photons { { stellar initial mass function star formation rate penetration through intergalactic medium escape of ionizing and Ly  photons partially neutral IGM (above z ~ 6.2)

8. Adopted Lyman  scenarios Scenario IMF (M O ) Metallicity (Z O ) f IGM f esc f Ly  Optimistic300-100001.00.352.1 x 10 43 Plausible50-50000.250.16.4 x 10 42 Heavy Salpeter 1-50010 -5 0.250.11.8 x 10 42 Salpeter1-1000.20.250.17.3 x 10 41

9. Lyman  Luminosity Function 8m 30+ hrs Models: Barton et al. (2004) Data: various sources compiled in Santos et al. (2004)

10. “optimistic” scenario simulation 48 hour obs. 1.122  m 20% throughput R=125 filter 0.35-arcsec seeing Springel & Hernquist (2003) model (Barton et al. 2004) z=8.2 galaxies 10 h -1 comoving Mpc=5.4 arcmin

11. Narrow-band filter Hubble Deep Field [OII] line emission at z=2.01, 15 hours with Gemini/NIRI

12. The Next Steps: FLAMINGOS 2 and MOSFIRE Keck MOSFIRE: 6.2’ FOV Gemini-South FLAMINGOS 2: 6.1’ FOV

13. F2T2 An engineering prototype for the JWST Tunable Filter Imager… F2T2 will be fed by a multi-conjugate adaptive optics system and be a facility-class instrument on Gemini next year.

14. The F2T2 Team Bob Abraham U. Toronto Steve Eikenberry U. Florida Nick Raines U.Florida Jeff Julian U.Florida Betsy Barton UC Irvine Dave Loop HIA, Victoria Al Scott COMDEV JD Smith U.Arizona David Crampton HIA, Victoria Joss Bland-Hawthorn AAO Mike Gladders U.Chicago Roger Julian U.Florida Neil Rowlands COMDEV Matt Bershady U. Wisconsin René Doyon U de Montréal Jean-Paul Kneib Marseilles

15. JWST TFI Gemini F2T2 First light Spectral resolution Wavelength range Field of view Image quality P.I. Prototype single etalon IR tunable filter for JWST. This opto-mechanical design is the basis for F2T2. Contributed by the Canadian Space Agency. Polished F2T2 optics. F2T2 will be inserted into Flamingos-2 and fed by the Gemini MCAO system. ~2014 100 1.5µm – 3.5µm ~2.5’ Diffraction limited R. Doyon (Montreal) Early 2007 800+ (wing suppressed) 30% of the range 1.0µm – 1.35µm ~50” R. Abraham (Toronto) MCAO JWST TFI and Gemini F2T2 share key optics and electronics. The biggest optical difference is that F2T2 is designed to work inside contaminating OH lines, and has two etalons running in series to suppress transmission profile wings.

16. New observatories will reveal the birth of galaxies Thirty Meter Telescope James Webb Space Telescope

17. The Future R >> 125 gives more sensitivity but less volume Maximum R set by intrinsic linewidths Need larger telescopes to study: IMF metallicity line profiles clustering 8m 30m

18. Penetrating the IGM with ionized bubbles Furlanetto & Oh (2005) Furlanetto, Zaldarriaga, & Hernquist (2004)

19. Penetrating the IGM with ionized bubbles Best places to find PopIII Ly  may be small galaxies inside these ionized bubbles Luminous sources already enriched (e.g., Davé, Finlator, & Oppenheimer 2005)

20. HeII (1640): signature of Pop III Pop III Pop II Only PopIII has detectable HeII (1640) emission Schaerer (2003) predicts high (>~ 20 Angstrom) equivalent widths for young, zero-metal bursts

21. Summary Ly  at z=8 may be detectable with present- day technology –high  e from WMAP suggests that conditions favorable –Gemini survey underway with NIRI Future will focus on luminosity function, topology of reionization, searches for PopIII