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Extremely Large Telescopes and the Epoch of Reionization

Extremely Large Telescopes and the Epoch of Reionization. Xiaohui Fan(Arizona) with help from Pat McCarthy and GMT Science Working Group July 11, 2008, KIAA-PKU. European ELT Program. 42m baseline 5 mirror system 850M€ budget (~ $1.1B) First light 2017+. Thirty Meter Telescope. TMT.

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Extremely Large Telescopes and the Epoch of Reionization

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  1. Extremely Large Telescopes and the Epoch of Reionization Xiaohui Fan(Arizona) with help from Pat McCarthy and GMT Science Working Group July 11, 2008, KIAA-PKU

  2. European ELT Program 42m baseline 5 mirror system 850M€ budget (~ $1.1B) First light 2017+

  3. Thirty Meter Telescope

  4. TMT Caltech Canada U. California 30m Aperture 738 segments 3 mirror f/1 primary f/15 foci First light ~2018 Site: MK/Chile

  5. The Giant Magellan Telescope Project

  6. GMT Partners Astronomy Australia Limited Australian National University Carnegie Institution of Washington Harvard University Smithsonian Institution Texas A&M University U. of Arizona U. of Texas at Austin Joining: Korea Astronomy & Space Science Institute Site: Las Campanas, Chile First light ~2018

  7. Telescope Concept Seven x 1.1m segmented secondary mirror (3.2 m Φ) Alt-az mount Seven x 8.4 m segmented borosilicate primary mirror Laser housing Telescope stats Height: 38.7 meters 1,125 metric tons Lowest Mode: 4.5 Hz (4.3 Hz with pier) Pier

  8. M1 Fold sphere & GMT1 GMT1 Completion April 2009 GMT1 3.8 m Fold sphere Jan 2008

  9. GMT & LBT Comparison

  10. Magellan (Manqui) Campanas Pk. Alcaino Pk. Ridge (Manquis) Las Campanas Observatory

  11. Probing Reionization History Fan, Carilli & Keating 2006

  12. Relevant Instrumentation IGM and Reionization studies need high resolution spectroscopy, multiplexed survey spectroscopy and near-IR AO-fed IFUs All three ELT projects are looking at MOS systems in the visible and near-IR and echelle spectrographs and IFUs in the near-IR with a view towards early universe studies.

  13. NIRMOS - An Example near-IR MOS • Wavelength range: 0.85 – 2.5 μm • Imaging Mode: • 7 x 7 arcmin field of view • 0.067 arcsec/pixel • 6kx6k detector • Spectroscopy Mode: • Multi-slits: 140 x 3 arcsec long, full wavelength coverage • 5 x 7 arcmin field of view • R ~ 3000 with 0.5 arcsec slits • Augmented by GLAO

  14. Reionization Probes with the ELTs • Gunn-Peterson effect • “Dark” GRBs ? • Evolution of Ly luminosity density and spatial distribution of LAEs • HeII emission from z>8 Galaxies • Ly florescence from boundary regions • Abundance in extremely metal poor stars How can ELTs explore the end of the Dark Ages?

  15. Reionization History Z=9.4 QSO Magellan 8hrs GMT 8hrs X. Fan

  16. Evolution of IGM Metals Evolution of CIV systems • Early Enrichment of the IGM by First stars • Lack of evolution in metal line density up to z~6 • OI Forest (Oh 2002) • OI and H have almost identical ionization potentials • In charge exchange equilibrium with H but much lower abundance • Fluctuating OI forest during neutral era to probe ionization topology and metal pollution in the IGM Ryan-Weber et al. OI system at z=6.26 Becker et al. 2006

  17. Ly  Galaxy LF at z>6 • Neutral IGM has extended GP damping wing  attenuates Ly  emission line • New Subaru results • Declining density at z~6-7 (2-3 result) • Reionization not completed by z~6.5 • fHI ~ 0.3 - 0.6 at z~7 • Overlapping at z=6-7? • cf. Malhotra & Rhoads, Hu et al.: lack of evolution in Ly  galaxy density Iye et al. 2006 Kashikawa et al. 2006 Ota et al. 2007

  18. Reionization Topology with Ly Emitters • Ly  emitter could provide sensitive probe to reionization history, especially during overlapping • Evolution of LF (constrain fHI) • Clustering • genus numbers Distribution of Ly emitters over 3’x3’ FOV Neutral  Ionized Angular correlation of Ly emitters McQuinn et al.

  19. Ly Spectroscopy in the Near-IR Ly at z = 8.7 in the J-band NIRMOS Properties with current Near-IR detectors 200 km/sec line widths 25 hour exposures 7 x 7 field of view ~ IOK-1 Photons/sec/cm2

  20. Ly Spectroscopy in the Near-IR NIRMOS Properties with OH Suppression and low-noise Near-IR detectors 200 km/sec line widths 25 hour exposures 7 x 7 field of view With OH suppression

  21. Ly Spectroscopy in the Near-IR NIRMOS Properties with OH Suppression and low-noise Near-IR detectors 200 km/sec line widths 25 hour exposures 7 x 7 field of view With OH suppression

  22. Structure at z ~ 10 Numerical simulation of gas cooling at z = 10 Dave’, Katz & Weinberg

  23. Structure at z ~ 10 Ly alpha image with GMT GLAO R=3000 filter 20% escape fraction 8 hour exposure Laser Tomography AO Ly HeII 1640 Very top-heavy IMF!

  24. ELT SCIENCE: CONTEXT & SYNERGY Physical Diagnostics Deep/Wide Surveys High-resolution imaging High SNR & Res. Spectroscopy Broad Synergy Across Wavelength, Spatial and Time Domains JWST ALMA LSST Magellan SKA

  25. Reionization Probes: ELT vs. JWST • ELT: • Narrow-band imaging in the near-IR (YJH bands): LAE surveys • High resolution IR spectroscopy (R>3000): first metals in the IGM • High resolution optical spectroscopy: first stars • OH suppression and Ground-Layer AO crucial • JWST: • Continuum-based surveys: reionization sources • Tunable filter narrow-band surveys (>1.5 micron): LAEs • Low-resolution spectroscopy: high-z quasars and GRBs

  26. Probing Reionization History JWST, ELT 21cm, GRB, ALMA Fan, Carilli, Keating 2006

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