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Microwave Background

Searching for Lyman  Beyond Reionization Betsy Barton (UC Irvine). Image from Space Telescope Science Institute. Microwave Background. What reionized the universe?. Recent reionization results. Wilkinson Microwave Anisotropy Probe (WMAP) :

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Microwave Background

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

  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 How can we find these galaxies? STAR-FORMING GALAXIES! (see Tinsley 1973)

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

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

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

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

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

  8. Adopted Lyman  scenarios

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

  10. z=8.2 galaxies “optimistic” scenario simulation 48 hour obs. 1.122mm 20% throughput R=125 filter 0.35-arcsec seeing Springel & Hernquist (2003) model (Barton et al. 2004) 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 Gemini-South FLAMINGOS 2: 6.1’ FOV Keck MOSFIRE: 6.2’ 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 Al Scott COMDEV Betsy Barton UC Irvine Mike Gladders U.Chicago Nick Raines U.Florida Matt Bershady U. Wisconsin Jeff Julian U.Florida Neil Rowlands COMDEV Joss Bland-Hawthorn AAO Roger Julian U.Florida JD Smith U.Arizona David Crampton HIA, Victoria Dave Loop HIA, Victoria René Doyon U de Montréal Jean-Paul Kneib Marseilles

  15. Gemini F2T2 JWST TFI 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. 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. First light ~2014 Early 2007 800+ (wing suppressed) Spectral resolution 100 30% of the range 1.0µm – 1.35µm Wavelength range 1.5µm – 3.5µm Field of view ~50” ~2.5’ Image quality MCAO Diffraction limited P.I. R. Doyon (Montreal) R. Abraham (Toronto)

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

  17. The Future 30m • 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

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

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

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

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

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