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

European ELT Program

42m baseline

5 mirror system

850M€ budget

(~ $1.1B)

First light 2017+

Thirty Meter Telescope

TMT

30m Aperture

738 segments

3 mirror

f/1 primary

f/15 foci

First light ~2018

Site: MK/Chile

Caltech

Canada

U. California

The Giant Magellan Telescope ProjectThe Giant Magellan Telescope Project

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)

M1 Fold sphere & GMT1

Jan 2008

3.8 m Fold sphere

GMT1

GMT1 Completion April 2009

GMT & LBT Comparison

Las Campanas Observatory

Magellan (Manqui) Campanas Pk.

Alcaino Pk.

Ridge (Manquis)

Probing Reionization History

Fan, Carilli & Keating 2006

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?

Reionization History

X. Fan

Z=9.4 QSO

Magellan 8hrs

GMT 8hrs

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

Structure at z ~ 10

Numerical simulation of gas cooling at z = 10

Dave’, Katz & Weinberg

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

Probing Reionization History

JWST, ELT21cm, GRB, ALMA

Fan, Carilli, Keating 2006