Evolution of the Highest Redshift Quasars

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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
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European ELT Program
OWL - 100 meter 14,000 tons 3048 segments 5
mirror system
Euro 50m 3,500 tons 618 segments 3 mirror system
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European ELT Program
42m baseline 5 mirror system 850M budget (
1.1B) First light 2017
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Thirty Meter Telescope
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TMT
Caltech Canada U. California
30m Aperture 738 segments 3 mirror f/1 primary
f/15 foci First light 2018 Site MK/Chile
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The Giant Magellan Telescope Project
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Giant Magellan Telescope Project
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GMT Partners
Astronomy Australia Limited Australian National
University Carnegie Institution of
Washington Harvard University Smithsonian
Institution Texas AM University U. of Arizona U.
of Texas at Austin Joining Korea Astronomy
Space Science Institute Site Las Campanas,
Chile First light 2018
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Telescope Concept
Seven x 1.1m segmented secondary mirror (3.2 m F)
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
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M1 Fold sphere GMT1
GMT1 Completion April 2009
GMT1
3.8 m Fold sphere
Jan 2008
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GMT LBT Comparison
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Las Campanas Observatory
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Cost Scaling Laws
ELTs
ELT projects must break past scaling laws to be
affordable!
D2.7
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GMT Science Case

• Planets and Their Formation
• Stellar Populations and Chemical Evolution
• Assembly of Galaxies
• Black Holes in the Universe
• The Accelerating Universe
• First Light and Reionization of the Universe

Science case www.gmto.org
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Probing Reionization History
Fan, Carilli Keating 2006
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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.

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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

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GMACS NIRMOS on the GMT
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Discovery Space
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mAB
Seeing Limited
-
2
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Adaptive Optics
-
1
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8m limit
Gain
5? 1hr Sensitivity (?Jy)
Spectroscopy
0
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-1
GMT limit
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-2
30
-3
0.3
0.5
1.0
2.0
3.0
5.0
10
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Wavelength (?m)
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Reionization Probes with the ELTs
How can ELTs explore the end of the Dark Ages?

• Gunn-Peterson effect
• Dark GRBs ?
• Evolution of Ly? luminosity density and spatial
  distribution of LAEs
• HeII emission from zgt8 Galaxies
• Ly? florescence from boundary regions
• Abundance in extremely metal poor stars

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Accelerated Evolution at zgt5.7

• Optical depth evolution accelerated
• zlt5.7 ? (1z)4.5
• zgt5.7 ? (1z)gt11
• End of reionization?
• Evolution of neutral fraction
• fHI gt 10-3 - 10-2 at z6
• Order of magnitude increase from z5
• G-P absorption saturates needs more sensitive
  tests

(1z)11
(1z)4.5
XF et al. 2006
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Reionization History
Z9.4 QSO
Magellan 8hrs
GMT 8hrs
X. Fan
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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 z6
• 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 z6.26
Becker et al. 2006
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Ly ? Galaxy LF at zgt6
Iye et al. 2006 Kashikawa et al. 2006 Ota et al.
2007

• Neutral IGM has extended GP damping wing ?
  attenuates Ly ? emission line
• New Subaru results
• Declining density at z6-7 (2-3? result)
• Reionization not completed by z6.5
• fHI 0.3 - 0.6 at z7
• Overlapping at z6-7?
• cf. Malhotra Rhoads, Hu et al. lack of
  evolution in Ly ? galaxy density

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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 3x3 FOV
Neutral ? Ionized
Angular correlation of Ly? emitters
McQuinn et al.
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Use Case Ly? Luminosity Function at z 6
500 km/s FWHM W? 100Å 30hr integration with
GMACS using 0.5 slits in 0.5 seeing 30
throughput Gemini sky spectrum Nod Shuffle sky
rejection R 5000 rebinned to R 1200,
Gaussian smoothing
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Mock Ly? Luminosity Function at z 6 with GMT
How do we extend this to z gt 8?
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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
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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
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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
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Ly? Emitter Surveys in ELT/JWST Era
intrinsic
observed

• Interpretation of Ly? emitters alone is highly
  model dependent
• Evolution of continuum LF
• Uncertainties in Ly?? radiative transfer
• Intrinsic clustering of galaxies etc.
• Requires surveys of continuum and SF selected
  samples

• Ly? selected
• ? continuum selected

Rhoads 2007
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Structure at z 10
Numerical simulation of gas cooling at z 10
Dave, Katz Weinberg
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Structure at z 10
Ly alpha image with GMT GLAO R3000 filter 20
escape fraction 8 hour exposure Laser Tomography
AO
Ly?
HeII 1640
Very top-heavy IMF!
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ELT SCIENCE CONTEXT SYNERGY
Physical Diagnostics Deep/Wide Surveys High-resolu
tion imaging High SNR Res. Spectroscopy
Broad Synergy Across Wavelength, Spatial and Time
Domains
JWST
ALMA
LSST
Magellan
SKA
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Reionization Probes ELT vs. JWST

• ELT
• Narrow-band imaging in the near-IR (YJH bands)
  LAE surveys
• High resolution IR spectroscopy (Rgt3000) 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 (gt1.5 micron)
  LAEs
• Low-resolution spectroscopy high-z quasars and
  GRBs

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