Future Instrumentation for Solar and Stellar Research at Radio ...

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CARMA Combine the six 10.4 m antennas at OVRO with the nine 6.1 m BIMA antennas . 772 m 2 collecting area (~0.1 ALMA) Frequency coverage: 115 GHz 230 GHz 345 GHz (planned) 4 configurations with up to 0.1” resolution OVRO BIMA
CARMA will be the best mm-λ array for a period of several years. After completion of ALMA, it will continue to provide access to the northern sky. The current timeline calls for site construction and moving the OVRO antennas in 2003. The BIMA array will be moved in 2004. The array will become operational in 2005. CARMA science will concentrate on detecting, identifying, and mapping emission from organic molecules in a variety of contexts (e.g., comets), protostellar and protoplanetary disks, star formation, emission from molecular gas and dust at high z, and the cosmic microwave background.
Page 1 and 2: Future Instrumentation for Solar an
Page 3 and 4: And Beyond … •SKA - Square Kilo
Page 5 and 6: By deploying N antennas over a two
Page 7: The EVLAThe EVLA (Phase 1) Point so
Page 10 and 11: Configurations Nested rings with di
Page 12 and 13: from R. Simon
Page 16 and 17: The Frequency Agile Solar Radiotele
Page 18 and 19: Strawman FASR Specifications Freque
Page 20 and 21: from J. Lee
Page 22 and 23: FASR Science • Nature & Evolution
Page 24 and 25: Noise storm Bastian et al. (2001)
Page 26 and 27: from Aschwanden & Benz 1997
Page 28 and 29: Status and Plans The NAS/NRC Astron
Page 30 and 31: The ATA The ATA is a project of the
Page 32 and 33: 6.1 m x 7.0 m Primary Log-periodic
Page 34 and 35: ATA Science • SETI - 100,000 FGK
Page 36 and 37: SM146 Concept (VLA Scientific Memor
Page 38 and 39: SM146 CAPABILITY SM146 SM146 SM146
Page 40 and 41: SKA Finally, it is worth mentioning
Page 42 and 43: Originally conceived as a “red sh

Future Instrumentation for Solar and Stellar Research at Radio ...

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