High -Redshift Quasars and Galaxies at the Epoch of Cosmic Reionization
Extremely Large Telescopes and the Epoch of Reionization Xiaohui Fan(Arizona) with help from Pat...
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Transcript of Extremely Large Telescopes and the Epoch of Reionization Xiaohui Fan(Arizona) with help from Pat...
Extremely Large Extremely Large Telescopes and the Epoch Telescopes and the Epoch
of Reionizationof Reionization
Xiaohui Fan(Arizona)
with help from Pat McCarthy andGMT Science Working Group
July 11, 2008, KIAA-PKU
TMT
30m Aperture
738 segments
3 mirror
f/1 primary
f/15 foci
First light ~2018
Site: MK/Chile
Caltech
Canada
U. California
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
Telescope Concept
Seven x 1.1m segmented
secondary mirror (3.2 m Φ)
Seven x 8.4 m segmented borosilicate
primary mirror
Alt-az mount
Laser housing
Pier
Telescope stats
Height: 38.7 meters
1,125 metric tons
Lowest Mode: 4.5 Hz
(4.3 Hz with pier)
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.
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
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?
Evolution of IGM Metals• 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
OI system at z=6.26
Becker et al. 2006
Ryan-Weber et al.
Evolution of CIV systems
Iye et al. 2006Kashikawa et al. 2006Ota et al. 2007
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
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 emittersover 3’x3’ FOV
McQuinn et al.Angular correlation of Ly emitters
Neutral Ionized
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
Pho
tons
/sec
/cm
2~ IOK-1
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
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
Ly alpha image with
GMT GLAO
R=3000 filter
20% escape fraction
8 hour exposure
Laser Tomography
AO
Ly HeII 1640
Structure at z ~ 10
Very top-heavy IMF!
ELT SCIENCE: CONTEXT & SYNERGY
JWSTALMA
LSST
SKA
Broad Synergy Across Wavelength, Spatial and Time Domains
Magellan
Physical DiagnosticsDeep/Wide Surveys
High-resolution imagingHigh SNR & Res. Spectroscopy
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