Astronomia no Brasil

1
Astronomia no Brasil
2
Observatório Astrofísico Brasileiro 1980
Telescópio de 1,6 m de diâmetro em Brasópolis, MG
3
LNA - Observatório do Pico dos Dias
4
Telescópio 1,6 m Perkin-Elmer
1981
5
Telescópio 0,6 m Zeiss
1983
6
Telescópio 0,6 m Boller Chivens IAGUSP
1992 no OPD
7
INPE
Radiotelescópio GEM (Galactic Emission Mapping).
Desde 1998 em Cachoeira Paulista 408 MHz, 1.465
GHz, 2.3 GHz, 5 GHz e 10 GHz.
8
Experimentos do INPE
Telescópio BEAST (Background Emission Anisotropy
Scanning Telescope), que tem como objetivo mapear
anisotropias e Polarização na Radiação Cósmica de
Fundo em microondas.
Telescópio imageador de raios-X e gama MASCO
(MAScara COdificada). Opera entre 50 keV e 1.8
MeV.
9
Gemini 2 telescópios de 8m (Brasil tem 2,5)
Mauna Kea Hawaii 2000
Cerro Pachon Chile 2001
10
Gemini 8m - 2,5 do Brasil
Chile
Hawaii
11
Gemini Norte
12
Interior do Gemini Norte
Plutão e Caronte, com resolução de 0,08
13
SOuthern Astrophysical Research telescope
Brasil tem 30 do telescópio de 4,2 metros de
diâmetro
2003
14
SOAR
15
SOAR
João Evangelhista Steiner
16
SOAR
17
Cerro Pachon Gemini e Soar
18
(No Transcript)
19
200 doutores 250 estudantes de mestrado e
doutorado

• IF-UFRGS 9 doutores 4 PD 18 PG 12 IC
• 
  (1983-gt 41M e 18D)
• IAG-USP 35 doutores prof 14 PD e visitantes
  50 PG
• 
  (30
  anos149M109D)
• ON-Rio 22 doutores 7 PD e visitantes 20 PG
• INPE 18 doutores 7 PD e visitantes 28 PG
• UFRJ 17 doutores (graduação já formou 120 alunos)
• UFRN 7 doutores 10 PG
• UFMG 6 doutores 5 PG
• UFSM 4 doutores
• UFSC 3 doutores 2 PG
• LNA 7 doutores
• UEFS-Bahia 2 doutores
• UFES - 2 doutores
• Londrina, Curitiba, São Carlos, UCS, UEG,...

20
Instrumentation Program
21
Optical Imager Science

• Capabilities
• Small field (5.5 x 5.5 arc min)
• 4K UV-blue optimized Lincoln Labs CCDs
• UV optimized optics
• tip-tilt guider
• Filters
• Johnson-Cousins UBVRI
• SDSS uvgri
• Stromgren uvby filter sets
• narrow band shared with CTIO
• Science niche
• High resolution, high precision photometry
• Efficient fast readout (lt 10s) helps.
• Competitors
• Blanco
• 10 x faster than Blanco Mosaic to given S/N in U
  band, factor 3 in BVRI under median seeing
  conditions, another factor 2 in 25 percentile
  seeing
• Gemini
• GMOS same field, similar scale, 40 surfaces cf
  14, poor in UV
• HST WFC3

22
OSIRIS
Early Science Instrument

• Ohio State InfraRed Imager/Spectrometer) imager
  (JHKKs22000A)
• spectrometer (R1200 or 3000).
• l0.9 to 2.4 microns
• 1024x1024 HAWAII HgCdTe array

Already a scientifically productive instrument.
Will be fully integrated with SOAR before 1st
(Nasmyth) Light
23
Phoenix

• Installed working on Gemini-S
• Successful Engineering Demo science runs in Dec
  01 and Jan 02
• Scheduled for regular science use 02/02 - 05/02

• Largely independent installation at SOAR
• Electronics Control
• Components exist to for dedicated data system
• Mechanical modifications
• Just a simple 1 thick adapter plate
• Cryogenics
• He Lines installed in facility per specification
• spare CTIO cryo-cooler pump checked out
• All this will be checked out in advance during
  Science First period

Possible Early Science Instrument Available to
SOAR 02/03 05/03
24
Phoenix Science

• The First High Resolution IR Spectrometer in the
  South
• On Gemini-S
• Stars with K lt 10 require a few minutes
  integration ..
• . but 30m of set up time !!!!
• Set up time dominates
• There are many BRIGHT southern targets needing
  high resolution spectroscopy
• Done more efficiently on SOAR
• Joint Programs
• SOAR does the bright objects
• Gemini the faint

• Example Science Projects
• Orbits Line profiles of Pre-Main Sequence Stars
• Line profiles of interacting binaries
• Abundances
• field stars
• LMC/SMC supergiants, Carbon Stars, Post-AGB stars
• Galactic center stars (K7)
• ISM e.g H2, C/O isotopes
• Comets (Gemini cant move fast enough)
• Kinematic studies of variable stars
• Mapping of circumstellar shells
• CO can be detected off the star the mass
  distribution mapped

25
Goodman HTS Status

• Optics
• Final optical design delivered, at long last, by
  Epps
• Fabrication by Coastal Optical underway
• Delivery scheduled for 09/02
• Restarting efforts on ADC design . slowly
• Mechanical
• Assemblies for gratings, moving camera, filter
  wheels, camera focus, collimator focus all
  finished or near finished
• Dewar design finished, not yet constructed
• Design of slit mask changer underway
• Detector integration
• Out contracting to CTIO
• CCD mounting
• Integration with SDSU-II controller, test
  optimization

26
IFU Spectrometer Status

• Integral Field Unit
• 1500 fibers

27
Spartan IR Camera Performance

• Optical quality Instrument degrades Strehl by 2
  _at_ H
• Detectors
• 2 at first light
• f/21 1.53.0 with 0.043 pixel
• f/12 2.5 5.0 with 0.073 pixel
• Brazilians will purchase 3rd

28
Spartan IR Camera Science

• Fornax Globular Clusters and the Formation of the
  Halo (H Smith)
• The Milky Way halo, including its globular
  clusters, may be made partially of accreted
  dwarf galaxies. Are globular clusters in Fornax
  and MW similar?
• IR and optical photometry will be used to
  determine the properties of RR Lyrae stars in the
  Fornax globular clusters, whose core radii ?5.
• Number density and physical characteristics of
  very red galaxies (S Zepf)
• What is the formation epoch of elliptical
  galaxies?
• Absence of young stars or presence of dust ? red
  galaxy. Image quality of SOAR can distinguish
  between old and newly formed, dusty, and
  irregular galaxies.
• At depth approaching the formation epoch, density
  of red galaxies with regular morphology should
  decline, and density of red, irregular galaxies
  should increase.

• Supernovae at z2 (E Loh)
• Are supernovae at z ? 0.5 and 2 alike?
• Number of SN is larger in the IR than in the
  visible because vol ? z3
• z(J band)/z(R band)3(2.7)320
• In 8hr, expect 4 SN with zgt1 for (?,L)(0.2,0.8)
• Spectra are feasible with AO on 8-m telescope

29
MIT/LL CCD procurement

• MBE process
• 7 potential Science grade devices so far, with 3
  more in pipeline, from 10 wafers finished so far.
  
• Will be mounted characterized at UH over next
  month
• First distribution should take place by end of
  April
• We may get 1 device from this batch
• All MBE wafers so far have Real Teal red AR
  coating
• Lower UV QE (but better than BIV), no fringing
  in red ? IFU
• Final lot in MBE processing now
• Some of these will have blue/UV optimized
  coatings ? imager and HTS

Engineering Grade CCD
If yield holds will provide the CCDs we need
30
Seeing All Sky Monitors

• Seeing Monitors (DIMMs)
• Key tool for commissioning efficient science
  operations
• CTIO copy now in routine service
• Fully automatic operation
• Attacking low level unreliability issues
• Building 2 copies for SOAR
• One fixed ? site seeing monitor for CP
• One portable for inside/outside comparisons
• Installed once heavy construction activity on
  site is over

• All Sky Camera
• Key tool for efficient science operations
• CTIO copy now in routine service
• FLI 1k² CCD camera Nikon f/2.8 8mm 180 fisheye
  lens
• All sky image every 20s (1800 frames/night)
• Detects clouds, airglow, aircraft .
• SOAR copy
• CCD camera wide angle lens in hand
• Installed once heavy construction activity is
  over

31
Rede de dados

• Observação remota necessita de transferência de
  imagens em tempo real, tanto de controle de
  telescópio, condições climáticas e instrumentais,
  quanto de imagens científicas.

32
Projetos Corot

• COnvection ROtation and
• planetary Transits
• Satélite Frances a ser lançado em 2006,
  colaboração com Brasil.
• Busca de planetas extraterrestres
• Asterosismologia

33
Projetos SKA

• Square Kilometer Array
• Custo 1 bilhão de dólares
• 15 países

Parâmetro Projeto
Área efetiva/Temperatura do sistema 2 x 104 m2/K
Freqüências de operação 0.15 - 20 GHz
Campo de visão 1 grau2 _at_ 1.4GHz
Resolução angular 0.1 seg. arco _at_ 1.4GHz 
Número de canais espectrais 104
Range dinâmico 106 _at_ 1.4 GHz
Pureza de polarização -40 dB 
34
Projetos ligar ROEN a eVLBI
14,2m Fortaleza
35
ROEN

• A tecnologia utilizada é rádio-astronômica. Os
  quasares, situados a bilhões de anos-luz de
  distância, constituem fontes de rádio de
  referência. Com dois ou mais rádio-telescópios de
  uma rede observando simultaneamente, obtêm-se a
  interferência das ondas de rádio. A observação
  destes objetos ou "balisas" celestes por vários
  rádio-telescópios de uma rede de milhares de
  quilômetros permite a determinação de posições
  absolutas na superfície da Terra, com precisão
  inferior a um centímetro. Dadas as grandes
  distâncias que separam os terminais desta rede,
  denomina-se o método de VLBI (de "very long
  baseline interferometry" interferometria de
  muito longa linha de base). A base de tempo é
  maser de H.
• A European VLBI correlaciona os dados
  diretamente, sem armazenar em disco. Primeira
  imagem em 28 abril/2004, de uma lente
  gravitacional. Uma banda em 5 GHz, com 2 bits,
  resultou em uma taxa de transferência de 32Mb/s,
  por 2h.
• Projeto 1 Gbps até 2004 e 30 Gbps por telescópio
  até 2007