O GMT, a perspectiva da Astronomia Brasileira e participação industrial

João Steiner

Instituto de Astronomia, Geofísica e Ciências Atmosféricas

Universidade de São Paulo

Brazilian Astronomy: papers

The Pico dos Dias Observatory (OPD)

The Gemini and SOAR Telescopes

Cerro Pachón - Chile

The SOAR telescope: mirror with 4.1 m x 10 cm

Active optics

The SOAR telescope primary mirror cell: 220 opto-

mechanical actuators

Telescópios órbita x solo

Imagem limitada pela: optica X atmosfera

Óptica Adaptativa:

alisando as ondas luminosas

onda

corrigida

Luz do

astro

espelho

auxiliar

sensor de frente de onda

Imagem

nítida

onda

corrigida

Atuadores moldam o espelho terciário

Óptica Adaptativa

guiada a laser

Estrela de laser para mapear as irregularidades atmosféricas

SOAR Dome Fabrication

●Dome Steel Work – Brazil

○Equatorial Sistemas (S.J. Campos)

○Fibraforte (S. J. Campos)

○Santim (Piracicaba)

○ATLAS Metalúrgica (S. Paulo)

STELES and BTFI spectrographs

Participation of industries in the SOAR instrumentation program

●Solumnia (eletrônica) Araraquara

●Metalcard (mecânica fina) São José dos Campos

●OIO (Fibras ópticas) Itajubá

●Equitecs (Usinagem mecânica) São Carlos

●Erominas (Usinagem Mecânica) Itajubá

●Anodont (anodização) Ribeirão Preto

●Cirvale (circuitos impressos) Santa Rita do Sapucaí

●ZetaLabs Brasil (vibração, RAMS, modelagem) Itajubá

●Usinagem Moabe (usinagem mecânica, fibra de vidro) Itajubá

Papers + Theses per Biennium

●Telescopes managed by LNA

●OPD = Observatório do Pico dos Dias

●Gemini+SOAR publications: growing 17% per year

0.6” H-band

Integral to the telescope: No extra reflections, no extra background

Adaptive Secondary (7x 1.1m): voice coil

Adaptive Optics Modes:

- Natural guide star high-Strehl (95% Strehl)

- Laser guide star high sky coverage

- Ground layer (GLAO) correction with natural guide stars

HST JWST GMT

Founding Partners

Astronomy Australia Ltd.The Australian National UniversityCarnegie Institution of ScienceFundação de Amparo à Pesquisa do Estado de São PauloHarvard UniversityKorean Astronomy and Space Science InstituteSmithsonian InstituteUniversity of Texas at AustinTexas A&M UniversityUniversity of ArizonaUniversity of Chicago

The GMT – Giant Magellan Telescope

Thank you

The GMT and the perspective of Brazilian Astronomy

João Steiner

Instituto de Astronomia, Geofísica e Ciências Atmosféricas

Universidade de São Paulo

Observatório Nacional (founded in 1827)

The Itapetinga radiotelescope

Modern telescopes

●Active optics

●Adaptive optics

SIFS Spectrograph

GMT Scientific Motivation: top-level areas

26

LSST ALMA

JWSTVISTA

SKA

• Extrasolar planets

• Stellar Populations and Chemistry

• Galaxy Building

• Black Hole Growth

• Cosmological Physics

• First-Light & Reionization

Extra-solar planets

Stellar populations and Chemistry

Galaxy building

Black hole growth

Cosmological physics

First light & reionization

First generation Instruments

●GCLEF – High stability spectrograph; R = 25K a 120K

●GMACS – Multi-object spectrograph

●GMTIFS – NIR IFU from .9 to 2.5 micron and R=5K-10K

●GMTNIRS – NIR-Echelle 1-5 micron and R=50K-100K

●MANIFEST - Facility fiber positioning system for 20 arcmin

A high throughput, general purpose multi-object spectrograph optimized forobservations of very faint objects. GMACS will be used for studies of galaxyevolution, evolution of the IGM and circumstellar matter, and studies ofresolved stellar populations, among other applications.

G-CLEF

●3 resolutions (R= 25 000, 40 000 e 120 000)

●δVr < 10 cm/s

The GMT integral field spectrograph (GMTIFS) builds on the legacy of theNIFS instrument on Gemini. It uses an image slicing micro-mirror system toreformat the focal plane onto the detector. Spaxel scales from 8 to 50mas areprovided and all feed an R = 5000 spectrograph that can cover any one of theJ, H, or K-bands in a single setting. The instrument also has an imagingchannel that will cover the laser tomography AO (LTAO) field while criticallysampling the PSF in the J-band.

The GMT Near-IR spectrometer (GMTNIRS) is a 1.2 – 5 micron echelle optimized for studiesof young stellar objects, debris disks, and protoplanetary systems. It will use Siliconimmersion gratings to achieve high spectral resolution in a compact format. Using slits wellmatched to the diffraction-limited image size from a single segment, GMTNIRS will deliverR = 50 – 100k spectra over 5 (JHKLM) atmospheric windows in a single observation. Thisrepresents an enormous gain in observing efficiency compared to current spectrographsthat sample only a fraction of a band in a single setting.

●Localização: Las Campanas – Chile

●Custo: 1.05 bilhão de dólares

●Contribuição da FAPESP: US$ 40 milhões

●Fração de uso para São Paulo: 4%

●Reserva técnica institucional e de projeto

GMT SP-packages

●1. Site Work and Foundations

●2. Fabrication and shipment of the structural steel

●3. Fabrication and Shipment of the Mechanisms

●4. Erection of the Structural Steel, Roof and Wall Panels

●5. Completion of the Architectural, Electrical and Mechanical Systems and Comissioning of Motion Control systems

SPANet – São Paulo Astronomy Network

●Science – transform S.Paulo in a Hub of observational

astronomy and Cosmology

●Education (all levels) and outreach

●Instrumentation and industrial participation

Bench made out of carbon fiber

Thermal enclosure

Projeto temático FAPESP

PI: 1) João Steiner

MI: 2) Laerte Sodré

MI: 3) Augusto Damineli

MI: 4) Cláudia Mendes de Oliveira

5) L. R. Abramo 6) Francisco Jablonski 7) F. d’Amico

8) E. Cypriano 9) Vera Jatenco 10) Élcio Abdala

11) Marcos Lima 12) Gastão Lima Neto 13) Reuven Opher

14) Cássio Barbosa 15) Alexandre Oliveira 16) Irapuan Rodrigues

17) Angela Krabbe 18) Oli Dors 19) Sérgio Pilling

20) J. Ademir S. Lima 21) Rose C. Santos 22) Francisco Fernandes

23) Deonísio Cieslinski 24) Nelson Leister 25) Alex Carciofi

26) Jacques Lepine 27) Roberto Costa

GCLEF

SP Participation

●1 - AO

●2 - Vibration isolation system

●3 - Bench made out of carbon fiber

●4 - Assembly tooling

●5 - Mechanical parts fabrication

●6 - Thermal enclosure

●7 – Design of specific parts

The GMT – CfA Large Earth Finder (G-CLEF) is a general purpose visible echellespectrograph that also provides precision radial velocity capabilities. G-CLEF will reside in agravity invariant and temperature controlled environment on the azimuth disk of thetelescope. An optical and fiber relay system will transfer light from the telescope to G-CLEFand will scramble the light within each of the seven sub-apertures in the process. Theinstrument will support several observing modes with a range of spectral resolutions andinput aperture sizes.