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Giant Telescopes

&

OIR Astronomy in the 2020’s

1

GMT Overview | Sept 23, 2016 | Ohio University

Winter Solstice 2017

Nicholas B Suntzeff

Texas A&M University

GMT Overview | Sept 23, 2016 | Ohio University 2

I would like to thank Dr. Pat McCarthy and

the GMT project for use of these slides. I

have added my own slides which reflect my

opinion and may not reflect that of the GMT

Board.


GMT Founder Institutions

New partners are welcome

Korea

Sao Paulo, Brazil

Texas A&M

Arizona

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Ground Breaking in Chile


The Giant Magellan Telescope

5GMT Overview | Sept 23, 2016 | Ohio University

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19th and Early 20th Century Observatories

Harvard

CarnegieUT Austin

Australia

Chicago


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Telescopes Double in Size Every 40 Years


The telescope I built in

high school

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The Challenge

Magellan 6.5m Telescopes

Giant Magellan Telescope

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Optics

50,000,000 wavelengths of light!

Polished to an accuracy of 1/20 a wave

1 part in a billion!

82 Feet

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Center Segment Casting – Sept 2015

Glass from Ohara of Japan

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Mirror #4

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Mirror #4

Mirror #1 Mirror #2

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Coring the mountain

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Single Friction Pendulum

standard in the industry

Seismic Base Isolation

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Modeling the Airflow Over the Site

Boeing computing division (St. Louis)

Used to optimize enclosure venting and base structure

Enclosure final design underwayProcurement to be launched in mid/late 2017

Open bidding – potential vendors in North America, Europe, Asia, Brazil, Chile

Summary Schedule(no schedule margin included)

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Upcoming Schedule Milestones

• Telescope Design/Build Contract Award Aug 2017

• Enclosure Bid Packages Released Sep 2017

• Start of Summit Concrete work Late 2017

• Enclosure Closed to Weather Mid 2020

• Delivery of telescope to site Early 2021

• Installation of First Primary Mirrors Mid 2022

• Engineering First-Light with Subset of Mirrors 2023

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Science Goals


Top-Level Science Areas

• Extra-solar planets

• Stellar Populations and Chemistry

• Galaxy Building

• Black Hole Growth

• Cosmological Physics

• First-Light & Reionization

Giant Magellan TelescopeScientific

Promise and Opportunities



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Science Goals


What’s New?

• Earth-like planets, visible AO…

• 2000+ Exoplanets, TESS in 2018

• Stars with [Fe/H] < -7

• Black holes with M > 1010Msun

• FRBs and other new transients

• JWST 2 years away

• LSST to start in 2020+

• …...





Potentially Habitable Worlds

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Low Mass Exoplanet Detections

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Radial Velocity Detections

- Rely on reflex motion of star

- Current precision limits < 1m/s

- Typical precision ~ 3-4 m/s

- Requires high stability

- Requires carefully planned

observing program

GMT Goals

- 1 – 2 ME planets

- In habitable zone

- G-M type stars

- 10 cm/s precision


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Exoplanet Science


Planets around M stars!


Proxima Cen b – Strong signal!

Simulated GMT Imaging of Exoplanets

GMT will image giant planets to ≈150 pc and Earth analogs at

< 10pc


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Current TechnologyGMT

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How will we Search for Life

on Extrasolar Planets ?

Image: Tanja Bosak Lab (MIT)

Oxygen gasCyanobacteria

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Image: Tanja Bosak Lab (MIT)

We will be able to

detect O2, O3, CH4, …in

an exoplanet

atmosphere with the

GMT

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Exoplanet Atmosphere Detections

Detection of Potassium in the Hot Jupiter in XO-2b (Sing et al. 2010)

> 3 detection

Detection of Sodium in the Hot Jupiters in HD209458b (Charbonneau et al. 2002) and HD198733b (Redfield et al. 2008)

Transmission spectroscopy has proven successful in about

a dozen planets, with the detection of e.g. H2O, CH4 , CO, Na I and K I

in their atmospheres.


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Imaging the Galactic Center Black Hole

GMT AAS OPEN HOUSE - JAN 5, 2017

Current TechnologyGMT

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Simulated AO Images


Globular Cluster around Cen A 3.8Mpc 3pc core radius H-band

0.5

Gemini 8m GMT 25m

GMT Image Simulations

Current Telescopes

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Hubble Space Telescope

James Webb GMT w/Adaptive Optics

GMT with Adaptive Optics

Extreme Metal Poor Stars

Detection of heavy neutron capture elements in metal poor stars


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“Ultra Faint” Dwarf Galaxies

Current Limit

4 mirror GMT limit

GMT Limit

Fornax Sculptor Leo I

Segue 1 CVn I

Sextans

ComBer Leo IV

Key Question: Are ultra-low mass galaxies “closed box” systems or

are they cleared of gas and metals during bursts or star formation?

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Probing Cosmic Dawn

Galaxy seen when the

Universe was 400

Million Years old

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Focal Stations


Instrument Mount Locations

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Folded Ports (4)

Direct Gregorian Ports

(4)

Gravity Invariant (1)

Instrument Platform

Auxiliary Ports (2)

(not shown)


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GMT FOCAL PLANE – 2 meters in diameter!


Natural Seeing Optical (350-950 nm) Spectrographs

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2.4

m

2.3

m

4.5m

5.2

m

GMACSDarren DePoy (Texas A&M)

Multi-object, dual channel

R = 1,000 – 6,000

7.5’ diameter FoV spectroscopy / imager

• Stellar evolution & abundances

• ISM & sIGM abundances

• Galaxy chemical evolution, Lyα systems

G-CLEFAndrew Szentgyorgyi (Harvard/SAO)

Stabilized, fiber-fed, dual channel echelle

R = 19,000, 35,000, 108,000

<50 cm/s per observation

• Exoplanets PRV (<10 cm/s) & chemistry

• Stellar abundances

• Dark matter distribution in dwarf galaxies


Facility Fiber Feed to Spectrographs

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MANIFESTJon Lawrence (AAO) / Matthew Colless (ANU)

Robotic fiber-feeds – 2-3 min config time

Single fiber, IFUs, Image slicer

Extendable to thousands of fibers

Feeds multiple instruments (G-CLEF, GMACS, future IR MOS)

• Extends/Adds MOS capability over 20’ FoV

• Enables very high A-Ω survey science (RV, stellar abundances)

• Allows simultaneous observing with multiple instrument (“parallels”)


AO-Fed Spectrographs

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GMTNIRSDan Jaffe (Univ of Texas Austin)

Near-diffraction limited JHKLM echelle

Full 5 band coverage simultaneously

R = 50,000 (JHK) – 75,000 (LM)

• Exoplanet structure and atmospheres

• Star and planet formation

• Composition of stars & nebulae

• Galaxy chemical evolution history

GMTIFSRob Sharp (ANU)

Diffraction-limited yJHK IFU / imager (20.4”)

R = 5,000, 10,000

Spaxels: 6, 12, 25, 50 mas

• Galaxy chemical enrichment history

• First galaxy structure and assembly

• Black hole masses

• IGM at high redshift


ELT

8m

4m


Comparing the ELTs

Increasing collecting area & angular resolution

2 reflections

f/8

1.0mm/arcsec

1.2m

3 reflections

f/15

2.2mm/arcsec

2.6m

5 reflections

f/17.7

3.6mm/arcsec

4.3mGMT Overview | Sept 23, 2016 | Ohio University 51

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The following is my opinion, and I represent no group – only my experience of 40 years in astronomy and physics.

Now let me speak frankly


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We must admit we are building the smallest giant telescope. While this is a slight disadvantage, we have one HUGE advantage. If we keep the project on track, we will be on the sky 3-5 years before any of the other two telescopes. Let’s grab that opportunity!

We must take a cue from our physicist friends and agree upon one major science goal and devote the first ~3 years to this project. The grandest project to work on, in fact, the grandest discovery that can me made in the history of science, is to find life on other planets.

Let’s take the challenge of doing one experiment – something like the LHC and the discovery of the Higgs – and unite our project to do this one experiment – find life elsewhere in the Universe. We will be the only telescope on the sky. If there is life to be found, we can be the ones that will do it, and be the ones who will have made the greatest discovery science.


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