Workshop for evaluation of the

Long Latin American Arrayproject

FAPESP, August 2011

www.astro.iag.usp.br/~nara

Thanks

To all of you: Dr. Brito, Dr, de Graauw, Dr. Marta Rovira, Dr.Monica Rubio

to all the bright scientists who prepared talks to show our capacity ofgiving full use of LLAMA

to the other bright scientist present here that could not be invited to give a talk

to the members of the LLAMA team who worked so hard to reach this moment

Nota del Prof. Richard T. Schilizzi, Director SKANota del Dr. Tim de Zeeuw, Director General European Southern Observatory (ESO)Nota de la Dra. Catherine Cesarsky, ex Presidente de la IAU .Nota del Prof. W. Miller Goss, ex Director VLA – VLBANota del Prof Yasuo Fukui, Director Nagoya University Southern ObservatoriesNota del Dr. José Franco, Director del Instituto de Astronomía, Observatorio Astronómico . . Nacional, UNAM, MéxicoNota enviada por e-mail del Dr. Jay Gallagher, Editor-in-Chief of the Astronomical JournalNota del Dr. Luis Felipe Rodríguez, investigador de la UNAMNota del Dr. Thomas Krichbaum, Max-Planck Intitute fur Radioastronomie, AlemaniaNota del Dr. Josep Martí, Catedrático de la Universidad de Jaén, EspañaNota del Dr. Josep M. Paredes, Catedrático de la Universidad de Barcelona, EspañaNota de Prof. Anne J. Green, Sydney Institute for Astronomy, Australia

to approve the LLAMA project the Ministry of Science of Argentina asked for letters of support

Summary

LLAMA (Long Latin American Milimetric Array): what is it?

The Latin-American connections and network

technology associated with LLAMA

science with LLAMA

Brazilian radioastronomy context

Our previous interaction with Argentinean radioastronomers:the SKA proposal

APEX can give us an idea of whatLLAMA will look like

But LLAMA is not just “one more” APEX !!

APEX= Atacama Pathfinder Experiment

APEXSingle dish operation very similar to our future LLAMA

containers

High altitude site: antenna, containers for control room, small lab,

storage of spare parts, a number of vehicles is needed

Control room - only simple computers

A CO line at 691 GHz being observed

Oxygen concentrator

rises the %

of oxygen in air

from 21 to 24%

Inside the antenna: system controlling the Gunoscillators, and part of a bolometric array

National Observatory of JapanUniversity of Tokyo, Nagoya Universityand Osaka Prefecture University,

ASTE radiotelescopeAtacama Submillimeter Telescope Experiment10 m. MitsubishiPampa La Bola near ALMA

APEX is close to ALMA so that VLBI with ALMA will not increase muchthe angular resolution of ALMA

LLAMA -ALMA- APEX-ASTE- offers much more convenient opportunities for VLBI

LLAMA is the seed for a true Long Latin-American Array. Can start with lower frequency VLBI without waiting for a second antennas

ALMAband GHz mm

1 31-45 7

3 84-116 3

6 211-275 1

7 275-373 0,85

9 602-720 0,45

The initial ALMA bands will benumbers 3,6,7,9

we would like to start also withband 1

Sicaya

Itapetinga

SEST

LLAMA

LLAMA could work at 43 GHz and even at 22 GHz Itapetinga: 22GHz and 43 GHzSicaya: will have a receiver at 22GHz SEST: could be reactivated, 22GHz and 43 GHz

ALMA

ESA Malargüe 32GHz

What angular resolution can be achieved?

• LAMA-Itapetinga about 2000 km at 7 mm

1.2 λ/D = 3.5 10-9 radians= 0.8 milliarcsecond(mas)

• Sicaya-Itapetinga 3000 km 13.5 mm 22 GHz

1.1 mas

• LLAMA-ALMA 200km 1 mm 300 GHz

1.2 mas

For comparison: the rotation of the solar system around the Galactic Center producesa change of direction of the Center of 6 mas/year

• LLAMA will take the lead in a global project that the central countries would start to fund not earlier than 2015. It would place the countries of the region in an advantageous position to participate in an extended version of ALMA

• In the long run, extended ALMA will require the installation of antennae in several countries of the region. LLAMA will serve as a starter of regional scientific-technological integrations, in a progressive way

LLAMA is a seed of a Latin-American network:

High frequency, high sensivity receivers, criogenic cooling of receivers,corrugated horns, lenses for microwaveswe could construct our 45 GHz receivers in collaboration withUniversidad de ChileApplications in future: remote sensing with satellites, satellite links, communications

Technology associated with LLAMA-like projects

Antenna tecnology: high accuracy surfaces using carbon fiber, holographic method to adjust the pannels, high accuracy encoders andcontrol systems for pointing the antennas

we should stimulate the construction of radiotelescopes in Brazil to installmore antennas for a VLBI networkmicrowave holography has been proposed for investigation of breast tumor.many possible applications

carbon fiber sectors of VERTEX dishestower with radio emitter for holography

Signal processing, Fast Fourier transform spectrometers, correlators using FGPAtechnology

when used as a clock, it willgain or lose a second in63 million years

Cesar Strauss here in Brazil and Ricaro Finger at Universidad de Chile are developping suchboards.. Many applications.

Hydrogen maser clocks are neededfor VLBI experiments

Hydrogen maser

• Two kinds of science: single dish and VLBI

• Strong case for VLBI: for each important resultobtained by ALMA that would require an angular

resolution 10 x better to further investigate theobject, LLAMA will be there!

This will generate the kind of results to be publishedin Nature and Science

• But VLBI will also generate fundamental long term work, that do notproduce immediate results but are important for future. Oneexample is astrometry which will refine the connection betweenoptical and radio frames of reference (R.Teixeira)

LLAMA scientific objectives

• VLBI images of regions a few times the horizon size of super-massive black holes (e.g. Sgr A*, Cen A, etc.).

• Galaxy Formation in the Early Universe• How relativistic jets are released, accelerated & collimated.• Extragalactic megamasers of water molecules• Masers of recombination lines of the hydrogen atom.• Masers in stellar forming regions & stellar envelopes• Spiral structure of the Galaxy and other galaxies• Molecular absorption in front of quasars at very high Zs• Non-thermal processes in stellar magneto-spheres• Extra-solar planets and proto-planetary disks• Polarimetry of radio sources and of the Interstellar Medium• Solar Physics• Applications in Geophysics (e.g. relax time after an earthquake)

with LLAMA we will supervise master and PhD theses in radioastronomy

The bar of our Galaxy: most of the astronomers believe that the bar rotates about 3times faster than the “normal” spiral structure. I will show that they are wrong by analysingthe proper motion of SiO masers of AGB stars associated with the extremty of the bar.

Map of the plane of our Galaxy based on CS sources

My science case

Radio Astronomy in Brazil(we are prepared for LLAMA!)

• Radioastronomy had a strong increase in scientificproduction after the installation of the Itapetinga 14 mradiotelescope in 1972, by the CRAAM.

• The discovery and investigation of many H2O and SiO masersources, including the first extragalactic megamaser, werereported

• A number of VLBI experiments in conjunction with Northernobservatories were performed

Itapetinga Radio Observatory ROI

• 13.7 m radome enclosed antenna

• Continuum at 22, 30, 43, 48, and 90 GHz

• Spectrometers operating at

22 and 44 GHz

• Criogenic radiometer

21.7 to 24.1 GHz

( molecular lines)

• Located at Atibaia (SP)

Submillimeter Solar Telescope SST

• Submillimetric (212 and 405 GHz) telescope for solar observations

• operated by CRAAM (Mackenzie University)

• located at El LeoncitoObservatory, in Argentina

• Operating since 1999.

Background Emission Anisotropy Scanning TelescopeBEAST

• The BEAST experiment is

designed to measure the Cosmic

Microwave Background

Radiation at 30 e 41 GHz;

• 2.2 m dish with spatial resolution of

30 arcmin;

• Launched by balloons (2000-2005)

• INPE

• Cost: US$ 0.6 Mi (FAPESP)

Galactic Emission Mapping GEM

• 5.5 m radio antenna

• Determine the spatial distribution andabsolute intensity of the microwavespectrum of the radiation emitted bythe Milky Way galaxy and by theunresolved blend of external galaxies.

• 0.408, 1.465, 2.3 and 5 GHz;

• Prototype at 10 GHz

• Cachoeira Paulista,SP, since 1998

• INPE

• Cost: US$ 50,000 (FAPESP)

Brazilian Solar Spectroscope BSS

• In operation at INPE since 1998;

• 9 meter antenna

• Dedicated to solar spectralobservations in decimetric band(200-2500 MHz) with high time (10-1000 ms) and spectral (3 MHz) resolutions.

Brazilian Decimetric Array - BDA

• Interferometer of 32dishes with 4 meter diameter;

• Observes the Sun atfrequencies of 1.4, 2.7 and5 GHz.

PI: Hanumar Sawant

Cachoeira Paulista, SPINPE in collaboration with India.

BrSKA team:Jacques Lépine (IAG/USP) – chair, Adriana V. R. Silva (CRAAM/Mackenzie) vice-chair, Abraham Chian (INPE),Carlos Guillermo Gimenez de Castro(CRAAM/Mackenzie), César Strauss (IAG/USP), Elisabete Dal Pino (IAG-USP), FábioSantos Lobão (ANATEL), Hanumant Sawant (DAS/INPE), Joaquim E. R. Costa(CRAAM/INPE), José Ângelo Amado (ANATEL), José Ângelo Néri (DAS/INPE),, JoséWilliams Vilas Boas (DAS/INPE), Jorge Ducati (UFRGS), Mauro Prado (INPE), MilitãoFigueredo (IAG-USP), Sergio Scarano Jr (IAG-USP), Thyrso Villela (DAS/INPE),Zulema Abraham (IAG/USP)

ArSKA teamGloria Dubner (IAFE)- chair , Marcelo Arnal (IAR), Ricardo Morras (IAR), Elza Giacanni (IAFE), Estela Reynoso. Hugo Levato (Observatório El Leoncito)

Argentine-Brazlian joint proposal to host SKA:(we are able to work together!)

2004- pure Brazilian and pure Argentinean proposals rejected

2005 – SKA maintained 4 proposals for further studies: China, Austrlalia, South-Africa and Argentine+ Brazil