Astronomia no Brasil

Observatório Astrofísico Brasileiro 1980

Telescópio de 1,6 m de diâmetro em Brasópolis, MGTelescópio de 1,6 m de diâmetro em Brasópolis, MG

LNA - Observatório do Pico dos Dias

Telescópio 1,6 m Perkin-Elmer

1981

Telescópio 0,6 m Zeiss

1983

Telescópio 0,6 m Boller & Chivens IAGUSP

1992 no OPD

INPE

Radiotelescópio GEM (Galactic Emission Mapping). Desde 1998 em Cachoeira Paulista: 408 MHz, 1.465 GHz, 2.3 GHz, 5 GHz e

10 GHz.

Experimentos do INPETelescópio 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.

Gemini: 2 telescópios de 8m (Brasil tem 2,5%)2 telescópios de 8m (Brasil tem 2,5%)

Mauna Kea: HawaiiMauna Kea: Hawaii20002000

Cerro Pachon: ChileCerro Pachon: Chile 20012001

Gemini 8m - 2,5% do Brasil

HawaiiHawaiiChileChile

Gemini Norte

Interior do Gemini Norte

PlutãoPlutãoe Caronte, com e Caronte, com

resolução de 0,08”resolução de 0,08”

SOuthern Astrophysical Research telescope

Brasil tem 30% do telescópio de 4,2 metros de diâmetro

2003

SOAR

SOAR

João Evangelhista Steiner

SOAR

Cerro Pachon: Gemini e Soar

200 doutores + 250 estudantes de mestrado e doutorado

IF-UFRGS 9 doutores + 4 PDIF-UFRGS 9 doutores + 4 PD + 18 PG + 12 IC+ 18 PG + 12 IC (1983-> 41M e 18D)(1983-> 41M e 18D) IAG-USP 35 doutores prof + 14 PD e visitantes + 50 PG IAG-USP 35 doutores prof + 14 PD e visitantes + 50 PG (30 anos:149M+109D)(30 anos:149M+109D) ON-Rio 22 doutores + 7 PD e visitantes + 20 PGON-Rio 22 doutores + 7 PD e visitantes + 20 PG INPE 18 doutores + 7 PD e visitantes + 28 PGINPE 18 doutores + 7 PD e visitantes + 28 PG UFRJ 17 doutores (graduação já formou 120 alunos)UFRJ 17 doutores (graduação já formou 120 alunos) UFRN 7 doutores + 10 PGUFRN 7 doutores + 10 PG UFMG 6 doutores + 5 PGUFMG 6 doutores + 5 PG UFSM 4 doutoresUFSM 4 doutores UFSC 3 doutores + 2 PGUFSC 3 doutores + 2 PG

LNA 7 doutoresLNA 7 doutores UEFS-Bahia 2 doutoresUEFS-Bahia 2 doutores UFES - 2 doutoresUFES - 2 doutores Londrina, Curitiba, São Carlos, UCS, UEG,...Londrina, Curitiba, São Carlos, UCS, UEG,...

Optical Imager – Science Capabilities:Capabilities:

Small field (5.5 x 5.5 arc min) Small field (5.5 x 5.5 arc min) 4K UV-blue optimized Lincoln Labs CCDs4K UV-blue optimized Lincoln Labs CCDs UV optimized opticsUV optimized optics tip-tilt guidertip-tilt guider FiltersFilters

Johnson-Cousins UBVRIJohnson-Cousins UBVRI SDSS uvgriSDSS uvgri Stromgren uvby filter setsStromgren uvby filter sets narrow band shared with CTIO narrow band shared with CTIO

Science niche:Science niche: High resolution, high precision photometryHigh resolution, high precision photometry Efficient – fast readout (< 10s) helps. Efficient – fast readout (< 10s) helps.

Competitors:Competitors: Blanco:Blanco:

10 x faster than Blanco Mosaic to given S/N 10 x faster than Blanco Mosaic to given S/N in U band, factor 3 in BVRI under median in U band, factor 3 in BVRI under median seeing conditions, another factor 2 in 25 seeing conditions, another factor 2 in 25 percentile seeingpercentile seeing

GeminiGemini GMOS same field, similar scale, 40 surfaces GMOS same field, similar scale, 40 surfaces

cf 14, poor in UVcf 14, poor in UV HST WFC3HST WFC3

FOV 0.25 x SOI, 0.04” pixels, also UV-FOV 0.25 x SOI, 0.04” pixels, also UV-optimizedoptimized

OSIRIS

- Ohio State InfraRed Ohio State InfraRed Imager/Spectrometer) Imager/Spectrometer) imager (JHKKimager (JHKKs22000As22000A))

spectrometer (R~1200 or spectrometer (R~1200 or 3000).3000).

0.9 to 2.4 microns 0.9 to 2.4 microns

1024x1024 HAWAII 1024x1024 HAWAII HgCdTe arrayHgCdTe array

Early Science Instrument

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

Phoenix Installed & working on Gemini-SInstalled & working on Gemini-S

Successful Engineering & Demo science runs Successful Engineering & Demo science runs in Dec 01 and Jan 02in Dec 01 and Jan 02

Scheduled for regular science use 02/02 - 05/02Scheduled for regular science use 02/02 - 05/02

Largely independent installation at SOARLargely independent installation at SOAR Electronics & ControlElectronics & Control

Components exist to for dedicated data systemComponents exist to for dedicated data system Mechanical modificationsMechanical modifications

Just a simple 1” thick adapter plateJust a simple 1” thick adapter plate CryogenicsCryogenics

He Lines installed in facility per specificationHe Lines installed in facility per specification““spare” CTIO cryo-cooler pump checked out spare” CTIO cryo-cooler pump checked out

All this will be checked out in advance during All this will be checked out in advance during “Science First” period“Science First” period

Possible Early Science Instrument

Available to SOAR 02/03 – 05/03

Phoenix Science The First High Resolution IR The First High Resolution IR

Spectrometer in the SouthSpectrometer in the South On Gemini-SOn Gemini-S

Stars with K < 10 require a few Stars with K < 10 require a few minutes integration …..minutes integration …..

……. but 30m of set up time !!!!. but 30m of set up time !!!! Set up time dominatesSet up time dominates

There are many BRIGHT southern There are many BRIGHT southern targets needing high resolution targets needing high resolution spectroscopyspectroscopy Done more efficiently on SOARDone more efficiently on SOAR

Joint ProgramsJoint Programs SOAR does the bright objectsSOAR does the bright objects Gemini the faintGemini the faint

Example Science ProjectsExample Science Projects Orbits & Line profiles of Pre-Main Orbits & Line profiles of Pre-Main

Sequence StarsSequence Stars Line profiles of interacting binariesLine profiles of interacting binaries AbundancesAbundances

field starsfield starsLMC/SMC supergiants, Carbon Stars, LMC/SMC supergiants, Carbon Stars,

Post-AGB starsPost-AGB starsGalactic center stars (K~7)Galactic center stars (K~7)ISM – e.g HISM – e.g H22, C/O isotopes, C/O isotopesComets (Gemini can’t move fast Comets (Gemini can’t move fast

enough)enough) Kinematic studies of variable starsKinematic studies of variable stars Mapping of circumstellar shellsMapping of circumstellar shells

CO can be detected off the star & the CO can be detected off the star & the mass distribution mappedmass distribution mapped

Goodman HTS – Status OpticsOptics

Final optical design delivered, at long last, by Epps Final optical design delivered, at long last, by Epps Fabrication by Coastal Optical underwayFabrication by Coastal Optical underway

Delivery scheduled for 09/02Delivery scheduled for 09/02 Restarting efforts on ADC design …. slowlyRestarting efforts on ADC design …. slowly

Mechanical Mechanical Assemblies for gratings, moving camera, filter Assemblies for gratings, moving camera, filter

wheels, camera focus, collimator focus all finished wheels, camera focus, collimator focus all finished or near finishedor near finished

Dewar design finished, not yet constructedDewar design finished, not yet constructed Design of slit mask changer underwayDesign of slit mask changer underway

Detector integrationDetector integration Out contracting to CTIOOut contracting to CTIO

CCD mountingCCD mounting Integration with SDSU-II controller, test & Integration with SDSU-II controller, test &

optimizationoptimization

IFU Spectrometer – StatusIntegral Field Unit Integral Field Unit

1500 fibers1500 fibers

Spartan IR Camera — Performance Optical quality: Instrument degrades Strehl Optical quality: Instrument degrades Strehl

by 2% @ Hby 2% @ H DetectorsDetectors

2 at first light2 at first lightf/21: 1.5’f/21: 1.5’×3.0’ with 0.043” pixel×3.0’ with 0.043” pixelf/12: 2.5 f/12: 2.5 ’’×5.0’ with 0.073” pixel×5.0’ with 0.073” pixel

Brazilians will purchase 3Brazilians will purchase 3rdrd

0 0.05 0.1 0.15 0.2 0.25 0.3q [arcsec]

0

5

10

15

20

ytisnetnI

[cescra

-2]

K-tt

H-tt

J-tt

V-tt

PSF w/ Median Seeing

0.5 1 1.5 2 2.5wavelength [m]

0

0.1

0.2

0.3

0.4

0.5

MHWF

[cescra

]

Diffraction

TT/top quartileTT/median

Natural/top quartile

Natural/median

Image Size

Spartan IR Camera — Science Fornax Globular Clusters and the Formation Fornax Globular Clusters and the Formation

of the Halo (H Smith)of the Halo (H Smith) The Milky Way halo, including its The Milky Way halo, including its

globular clusters, may be made partially globular clusters, may be made partially of accreted dwarf galaxies. Are globular of accreted dwarf galaxies. Are globular clusters in Fornax and MW similar?clusters in Fornax and MW similar?

IR and optical photometry will be used to IR and optical photometry will be used to determine the properties of RR Lyrae stars determine the properties of RR Lyrae stars in the Fornax globular clusters, whose in the Fornax globular clusters, whose core radii core radii 5”.5”.

Number density and physical characteristics Number density and physical characteristics of very red galaxies (S Zepf)of very red galaxies (S Zepf) What is the formation epoch of elliptical What is the formation epoch of elliptical

galaxies?galaxies? Absence of young stars or presence of dust Absence of young stars or presence of dust

red galaxy. Image quality of SOAR can red galaxy. Image quality of SOAR can distinguish between old and newly distinguish between old and newly formed, dusty, and formed, dusty, and irregularirregular galaxies. galaxies.

At depth approaching the formation At depth approaching the formation epoch, density of red galaxies with regular epoch, density of red galaxies with regular morphology should decline, and density of morphology should decline, and density of red, irregular galaxies should increase.red, irregular galaxies should increase.

Supernovae at z=2 (E Loh)Supernovae at z=2 (E Loh) Are supernovae at z Are supernovae at z 0.5 and 2 alike? 0.5 and 2 alike? Number of SN is larger in the IR than in the Number of SN is larger in the IR than in the

visible because vol visible because vol z z33

[z(J band)/z(R band)][z(J band)/z(R band)]33=(2.7)=(2.7)33=20=20 In 8In 8hrhr, expect 4 SN with z>1 for , expect 4 SN with z>1 for

(()=(0.2,0.8))=(0.2,0.8) Spectra are feasible with AO on 8-m telescope Spectra are feasible with AO on 8-m telescope

0 0.5 1 1.5 2 2.5z

0

0.5

1

1.5

22.5

3

N(<z)

(0.2,0)

(1,0)

(Wm,WL)=(0.2,0.8)

Number of SN in a 4-hr Exposure with 4-detector Camera

MIT/LL CCD procurement MBE processMBE process

7 potential Science grade devices so far, 7 potential Science grade devices so far, with 3 more in pipeline, from 10 wafers with 3 more in pipeline, from 10 wafers finished so far. finished so far. Will be mounted & characterized at UH Will be mounted & characterized at UH

over next monthover next month First distribution First distribution shouldshould take place by end of take place by end of

April April We may get 1 device from this batchWe may get 1 device from this batch

All MBE wafers so far have All MBE wafers so far have “Real Teal” red“Real Teal” red AR coatingAR coatingLower UV QE (but better than BIV), no Lower UV QE (but better than BIV), no

fringing in red fringing in red IFU IFU Final lot in MBE processing nowFinal lot in MBE processing now

Some of these will have Some of these will have blue/UVblue/UV optimized coatings optimized coatings imager and HTS imager and HTS

Engineering Grade CCD

If yield holds will provide the CCDs we need

Rede de dados

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

Projetos: Corot

COnvection ROtation and COnvection ROtation and

planetary Transits planetary Transits Satélite Frances a ser lançado em 2006, Satélite Frances a ser lançado em 2006,

colaboração com Brasil.colaboração com Brasil. Busca de planetas extraterrestresBusca de planetas extraterrestres AsterosismologiaAsterosismologia

Projetos: SKA Square Kilometer ArraySquare Kilometer Array Custo: 1 bilhão de dólaresCusto: 1 bilhão de dólares 15 países15 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 @ 1.4GHz

Resolução angular 0.1 seg. arco @ 1.4GHz 

Número de canais espectrais 104

Range dinâmico 106 @ 1.4 GHz

Pureza de polarização -40 dB 

Projetos: ligar ROEN a eVLBI

14,2m Fortaleza

ROEN A tecnologia utilizada é rádio-astronômica. Os quasares, situados a bilhões de 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 anos-luz de distância, constituem fontes de rádio de referência. Com dois ou mais rádio-telescópios de uma rede observando simultaneamente, obtêm-se a mais rádio-telescópios de uma rede observando simultaneamente, obtêm-se a interferência das ondas de rádio. A observação destes objetos ou "balisas" interferência das ondas de rádio. A observação destes objetos ou "balisas" celestes por vários rádio-telescópios de uma rede de milhares de quilômetros celestes por vários rádio-telescópios de uma rede de milhares de quilômetros permite a determinação de posições absolutas na superfície da Terra, com permite a determinação de posições absolutas na superfície da Terra, com precisão inferior a um centímetro. Dadas as grandes distâncias que separam os 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 terminais desta rede, denomina-se o método de VLBI (de "very long baseline interferometry": interferometria de muito longa linha de base). A base de interferometry": interferometria de muito longa linha de base). A base de tempo é maser de H.tempo é maser de H.

A European VLBI correlaciona os dados diretamente, sem armazenar em A European VLBI correlaciona os dados diretamente, sem armazenar em disco. Primeira imagem em 28 abril/2004, de uma lente gravitacional. Uma 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 banda em 5 GHz, com 2 bits, resultou em uma taxa de transferência de 32Mb/s, por 2h.32Mb/s, por 2h.

Projeto: 1 Gbps até 2004 e 30 Gbps por telescópio até 2007Projeto: 1 Gbps até 2004 e 30 Gbps por telescópio até 2007