GMTIFS – An AO-Corrected Integral-Field

Spectrograph and Imager for GMT

Peter McGregorThe Australian National University

1IFUs in the Era of JWST - October 2010

GIANT MAGELLAN TELESCOPE

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GMT – Seven 8.4-m Segments

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Instrument Function l range(microns)

ResolvingPower

FOV

GMACS Optical Multi-ObjectSpectrometer

0.35-1.0 250-4000 64-200arcmin2

NIRMOS Near-IR Multi-ObjectSpectrometer

1.0-2.5 Up to ~4000 49arcmin2

G-CLEF Optical High Resolution(Doppler) Spectrometer

0.4-0.7 150K 7 x 1” fibers

GMTNIRS Near-IR High-ResolutionSpectrometer

1.2- 5.0 25K-100K Single object

GMTIFS NIR AO-fed IFU+Imager 0.9-2.5 5000-10000 <5”

TIGER Mid-IR ImagingSpectrometer

3.0-25.0 1500 30”

GMT First-Light Instrument Studies

Wide-field instruments LTAO instruments

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Timeline

• Sept 2011: Six Conceptual Design Reviews• Oct 2011: Down select to 2-3 first-light instruments

• 2020: GMT first light

What will we want to be doing in 10 yr time?

LASER TOMOGRAPHY ADAPTIVE OPTICS

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Laser Tomography Adaptive OpticsLTAO in the H band, Antennae at z=1.4

12 mas FWHM at 1.2 μm16 mas FWHM at 1.6 μm22 mas FWHM at 2.2 μm

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Adaptive Secondary Mirror (ASM)

Hexapod

Interface

Telescope structure

Controller

Wind shield

DM assembly• Cold plate• Reference

Body• Face sheet

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LTAO System LayoutLGS Projector

Laser beam relay

Laser house

Adaptive secondary mirror (ASM)

AO Focal Plane Assembly (FPA)

• Tertiary mirror• AO instruments• Optical TTF + Truth WFS• LGS wave-front sensors• Phasing camera

top view

GMTIFS SUMMARY

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Motivations

• AO-corrected integral-field spectroscopy allows study of • Kinematics• Excitation

• GMT provides higher angular resolution for diffraction-limited science• Black-hole masses, protoplanetary disks• ~22 mas FWHM at 2.2 μm

• GMT provides larger collecting area for faint-object science• Galaxy dynamics at high redshift• 50 mas sampling, 4.5x2.24 arcsec FOV

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Physical processes

GMTIFS – Overview

• Near-infrared; 1-2.5 μm + LTAO• Primary science instrument

• Single-object, LTAO-corrected, integral-field spectroscopy• Two spectral resolutions: R = 5000 (Δv = 60 km/s) & 10000 (Δv = 30 km/s) • Range of spatial sampling and fields of view:

• Secondary science instrument • Narrow-field, LTAO-corrected, imaging camera• 5 mas/pixel, 20.4× 20.4 arcsec FOV• Acquisition camera for IFS

• NIR AO-corrected tip-tilt WFS• 180 arcsec diameter guide field

• Flat-field and wavelength calibrationIFUs in the Era of JWST - October 2010 12

Spaxel size (mas) 6 12 25 50

Field of view (arcsec) 0.54×0.27 1.08×0.54 2.25×1.13 4.5×2.25

Guide Field Geometry

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SCIENCE DRIVER The Formation of Disk Galaxies at High Redshift

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High-z Disk Galaxies

IFUs in the Era of JWST - October 2010 15Elmegreen et al. (2009)

ClumpCluster

EarlyBulge

FlocculentSpiral

MatureSpiral

Natascha Förster-Schreiber

Marie Lemonie-Busserolle

Shelley Wright

Andy Green

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Gravitationally Lensed Galaxies

MACS J2135-0102, z = 3.075

Stark et al. 2008, Nature, 455, 775

Tucker Jones

SCIENCE DRIVER “AGN” Feedback at High Redshift

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[O III] in Radio Galaxies & ULIRGS

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Nesvadba 2009; z ~ 2 radio galaxies

Alexander et al. 2010; z ~ 2 ULIRG SMM J1237+6203

SCIENCE DRIVER Massive Nuclear Black Holes

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Nuclear Black Holes

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Nuclear Black Holes• High spatial resolution is required at high-mass end

• R = GMBH/σ2 ~ 10.8 pc (MBH/108 M☼)(σ/200 km/s)-2

~ 35.3 pc (MBH/109 M☼)(σ/350 km/s)-2

• H-band diffraction limit ~ 16 mas• 10 pc @ z = 0.04• 35 pc @ z = 0.15

• > 5×109 M☼ can be resolved at any distance

• High spectral resolution is required at low-mass end• Probe 104-106 M☼ black holes in clusters• Velocity dispersions ~ 20-60 km/s => FWHM ~ 40-140 km/s• Requires R ~ 10,000 (Δv ~ 30 km/s) to detect presence of

black hole

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Massive Nuclear Black Holes

• Stellar kinematics of quasar host galaxies?• QSO PG1426+0.15 with NIFS (Watson et al. 2008, ApJ,

682, L21)

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Nuclear Star Clusters

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5"

SCIENCE DRIVER Active Galactic Nuclei

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NGC 4151 - Seyfert 1 Galaxy

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[Fe II] 1.644 μm H2 1-0 S(1) 2.122 μm

H I Brγ 2.166 μm [Ca VIII] 2.321 μmThaisa Storchi-Bergmann

João Steiner

SCIENCE DRIVER Protoplanetary Disks and Outflows from Young Stars

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Protostellar Disks and Outflows

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Tracy Beck

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DG Tau – Integrated [Fe II] (2005)

• NIFS H band

• Inclination ~ 60°• > 5:1 jet aspect

ratio

• Launch radius expected to be ~ 1 AU

• 20 AU resolution with NIFS

• 4 AU resn. with GMT at diffraction limit

100 AU

1 yr at 200 km/s

20 AU

INSTRUMENT DESIGN

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LGS WFS

NGS WFS

GMTIFS Light Paths

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AO WFSs GMTIFS

NIR NGS WFS

IFS

F-converters

Imager

Calibration Dichroic

OptLGSNIR

ADC

Optics – Trimetric View

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Calibration system

Tertiary mirror

Imager

Spectrograph

First Satisfied Observer!

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LTAO wave-front sensors

GMTIFS calibration system GMTIFS cryostat

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GMTIFS on Instrument Platform

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SYNERGIES

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JWST Comparison

• Integral-Field Spectroscopy:• GMTIFS will have higher spectral resolution (R = 5000-10000 vs

2700)• AND higher spatial resolution (≤ 50 mas vs 100 mas)

• GMTIFS will address broader science

• Imaging:• JWST will out-perform GMTIFS for imaging targets with 6.5 m

diffraction-limited resolution (85 mas @ K)• GMTIFS’s advantage is in observations requiring higher spatial

resolution (22 mas @ K)• Crowded fields, morphology, size measurement

• GMTIFS will do different science

1 1.2 1.4 1.6 1.8 2 2.2 2.4-20.00

-19.00

-18.00

-17.00

-16.00

-15.00

-14.00

-13.00

Wavelength [microns]

Continuum Sensitivity: 10:1 in 10,000s

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6 mas; R=10000

6 mas; R=5000

12 mas; R=10000

12 mas; R=5000

25 mas; R=1000025 mas; R=500050 mas; R=1000050 mas; R=5000

JWST; R=2700

AB mag/arcsec2

NIFS; R=5000

1 1.2 1.4 1.6 1.8 2 2.2 2.4

3.33E-17

3.33E-16

3.33E-15

Wavelength [microns]

Line Sensitivity: 200 km/s,10:1 in 10,000s

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JWST; R=2700

6 mas; R=100006 mas; R=5000

12 mas; R=1000012 mas; R=500025 mas; R=1000025 mas; R=500050 mas; R=1000050 mas; R=5000

erg/s/cm2/arcsec2

NIFS; R=5000

Summary

• GMTIFS will be a general-purpose AO instrument for GMT

• It will address many of the key science drivers for GMT

• It will be competitive with similar instruments on other ELTs• (within certain caveats)

• It will fully utilize the LTAO capabilities of GMT

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