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.
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