Giant Magellan Telescope Project: Current Statusastro1.snu.ac.kr/eama10/20160928_EAMA10/2....

Giant Magellan Telescope Project:Current Status

Byeong-Gon Park

2016. Sep. 28.

Telescope Overview

Optical Characteristics

Seven 8.4m primary segments

Total diameter : 25.4m (area equiv. to 22m)

Seven 1.06m secondary segments

Total diameter : 3.2m

Two sets of secondary mirror systems

• Fast Steering Mirrors

• Adaptive Secondary Mirrors

Gregorian Focus

f/8, FOV ~ 20 arcmin

Plate scale – 1.0mm/arcsec

Alt-Azimuth Mount

Site : Las Campanas Peak, Chile

Major Gains Angular Resolution : 0.01 arsec at 1μm , 10 x HST

Collecting Power : 380 sq. meter, 10 x Magellan

EAMA 10 - The 10th East Asian Meeting on Astronomy, Sep. 26-30, 2016, SNU

Galaxies in the Early Universe

From Harvard MagazineEAMA 10 - The 10th East Asian Meeting on Astronomy, Sep. 26-30, 2016, SNU

GMT - Partners

Korea

Sao Paulo, Brazil

Texas A&M

Arizona


GMT - Partners


HarvardCarnegie

Texas A&M

ANU

KASI U. Arizona

LCO

SAO

U. Texas Austin

AALSan Paulo

Chicago

Staged Implementation Plan

Conceptual Design Phase : 2003 ~ 2007

Design Development Phase : 2008 ~ 2015

2009 : KASI joined GMT project

Construction and Commissioning Phase : 2016 ~

First Light & Early Science Operation with 4 mirrors : 2022 ~

Full Operation with 7 mirrors : 2025 ~


CURRENT STATUS

Current Status

Entering Construction and Commissioning Phase

Groundbreaking Ceremony, Nov. 11th, 2015

Site Development Activities

Primary Mirror Production

Telescope Mount Procurement

Ground Breaking in Chile


Site Layout


Site Development


Site work focused on construction readiness

Road widening and grading

Power, water and data to summit and support sites

Housing for ~200 person construction crew

Construction offices for staff and contractors

Completion expected by late 2016

Ready for excavation and concrete work in 2017

Site Development for Construction


First Housing Units on the Mountain


Summit Construction Offices


Primary Mirror Segments – A Critical Path of the Project -

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Spin-cast at Richard F. Caris Mirror Lab (RFCML) in University of Arizona

#1 : Finished in Jan. 2012 #2 : Cast in Jan. 2012 – front processing

#3 : Cast in Aug. 2013 – back processing #4 : cast in Sep. 18th. 2015


Telescope Final Design and Fabrication

Telescope Mount Procurement

Competitive procurement

World-wide sourcing, open to qualified vendors

Contract structure: design with option to build

Potential for more than one design phase contract

Bidders Conference/Industry Day in California

September 21st – 22nd

19 companies from 9 countries attended by invitation

Request for Proposals/Request for Tender

Before the end of Calendar Year


FIRST GENERATION INSTRUMENTS

1st Generation Instruments: Summary

Instrument / Mode Capabilities λ Range, μm Resolution Field of View

G-CLEF / NS, GLAO Optical High Resolution Spectrograph / PRV

0.35 – 0.95 20 – 100K 7 x 0.7,1.2” fibers

GMTIFS / LTAO, NGSAO NIR AO-fed IFS / Imager 0.9 – 2.5 5,000 & 10,000 10 / 400 arcsec2

GMACS / NS, GLAO Wide-Field Optical Multi-Object Spectrograph

0.36 – 1.01,500 – 4,000

(10K with MANIFEST)40-60 arcmin2

GMTNIRS / NGSAO, LTAOJHKLM AO-fed High Resolution Spectrograph

1.2 – 5.0 50K, 100K 1.2” long-slit

MANIFEST* / NS, GLAO Facility Robotic Fiber Feed 0.36 – 1.0 20’ diameter

Starting Critical Design

Developing Large Immersion Grating

2nd Stage Conceptual Design Study

Prototyping being finished

*MANIFEST is a robotic fiber feed for G-CLEF and GMACS, not an instrument


Gregorian Instrument Rotator (GIR)

Folded Ports

• Medium-Size Instruments (G-CLEF, GMTIFS, GMTNIRS)

• GLAO Assembly

• Guider Assembly

• Tertiary Mirror Assembly

Direct Gregorian Focus• Four Science Instrument bays• GMACS• MANIFEST


G-CLEF Location on GMT

Spectrograph in Thermal Enclosure(Gravity Invariant Station)

Fiber Run

Front End Assemblies


Summary Schedule


KOREAN GMT PROJECTEAMA 10 - The 10th East Asian Meeting on Astronomy, Sep. 26-30, 2016, SNU

Scientific Activities

K-GMT Science and Instrument Working Group Bridge between K-GMT project team and Korean community

Composed of 15 members from the project and universities

Current chair : Prof. Changbom Park (KIAS)

Usage of 6m-8m Telescopes Strategic planning conducted and report published

MOU extended for MMT/Magellan with Univ. of Arizona

MOU extended for Gemini with AURA

Joint Fellowship MOU signed with Univ. of Arizona

AAS Job announcement to be released on Oct. 1st

Participation in Survey Projects Continued participation in SDSS4, DESI

MOA signed with LSSTC for operation of the LSST

Publication of the Korean GMT Science book Science cases with G-CLEF & GMACS

6th Annual GMT Summer School Aug. 22-26 for graduate students and postdocs


Technical Activities

Development of the GMT Secondary Mirror System (FSM)

KASI team composed of KASI-KRISS-IAE-NOAO-UA in

collaboration with GMTO M2 team

Phase 0 – Project definition study completed in April

Phase 1 – delta PDR study will begin soon in this year

Development of G-CLEF

KASI in collaboration with SAO

KASI role – guider, calibration, dichroic

Critical design study under progress

Development of GMTNIRS

Based on the success of IGRINS development

KASI in collaboration with Univ. of Texas at Austin

Large Immersion Grating development done

KASI role – spectrograph, detector, calibration

Preliminary Design Study will follow


THANKS!!

BACKUP SLIDES

MANIFEST: MANy Instrument FibEr SysTem

~2000 moving Starbugs

Covers the GMT’s full 20’ diameter field

Single-fibre/image-slicer/IFU feeds for NIRMOS/GMACS/G-CLEF

Higher target multiplex and/or higher spectral resolution

Configuration time < 3 min

Object spacing > 10 arcsec

Telescope+Instrument Diam (m) D2 AΩ

GMT+MANIFEST 25.4 =1 =1

TMT+WFOS 30 1.4 0.23

E-ELT+DIORAMAS 39.3 2.4 0.39


G-CLEF

Gmt-Consortium Large Earth Finder :

CfA, OCIW, KASI, Catholica Univ.(Chile)

“THE First Light” instrument of GMT : working on 2020 ~ with 4 mirrors)

Fiber-fed high resolution optical spectrograph

λλ 0.35 ~ 1.0 μm, R 25k ~ 100k

RV Precisional Goal ~ 10 cm/sec (cf. HARPS ~ 70 cm/sec)

PDR successfully passed in April 2015

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G-CLEF

KASI’s main responsibilities in the G-CLEF development

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Mangin-Mirror

Dichroic Optics + Mount

Calibration System Guide Camera System

370x240x30mm Toroidal second surface mirror

GMTNIRS

What is GMTNIRS?

GMT Near-Infrared Spectrograph, UT-KASI-KHU collaboration

One of four GMT 1st generation instruments

High resolution AO-fed spectrograph

Covers all 1.12-5.3 um range in a single exposure

R= 50,000 at JHK and 100,000 at LM

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GMTNIRS

KASI’s role in the GMTNIRS project

Spectrograph : mechanics + optomechanics + cryogenics

Detector electronics + control system

Calibration unit : optics + mechanics + control system

Systems Engineering

Current Status

UT is developing large immersion grating for GMTNIRS

Starting of Preliminary Design Study expected in 2017

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Colored boxes representspace for AO componentsand GMTNIRS cal system

Giant Magellan Telescope Project: Current Statusastro1.snu.ac.kr/eama10/20160928_EAMA10/2....

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