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Project status and specifications Douglas Bock Project Manager. 1. Berkeley-Illinois-Maryland Assn. array 10 6.1-m diameter antennas. Caltech array 6 10.4-m antennas. + UChicago SZA 8 3.5-m antennas. 2. BIMA mosaic of M33. CO 1-0 115 GHz
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Project status and specifications Douglas Bock Project Manager 1
Berkeley-Illinois-Maryland Assn. array 10 6.1-m diameter antennas Caltech array 6 10.4-m antennas + UChicago SZA 8 3.5-m antennas 2
BIMA mosaic of M33 • CO 1-0 115 GHz • 759 pointing centers 3
BIMA mosaic of M33(Engargiola et al. 2003) • 148 GMCs detected • overlie HI filaments (HI image: Deul & van der Hulst 1987) 4
MM Wavelength T Tauri Outburst in Orion • 2nd most luminous stellar radio outburst • Briefly, brightest object in nebula • Required long baselines for detection • Magnetized T Tauri outburst • Contemporaneous with X-ray outburst BIMA A configuration images (Bower, Plambeck, Bolatto et al.) 5
antennas 3 different antenna diameters - a heterogeneous array • sensitive to wide range of spatial frequencies; image large objects, search large areas • FOV of 8-m equivalent antenna (BIMA+OVRO) is 1.3’ at 100 GHz and 0.6’ at 230 GHz • SZA FOV more than twice as large • OVRO drive upgrade within next year to allow rapid source switching 15
sensitivity Line: 1 km/sec Continuum Factor of 5 to 20 better than present performance 16
receivers for the 1mm and 3mm bands: • 4 GHz bandwidth, 1 polarization • continuum sensitivity: 2-3 mJy/beam, in 1 minute • 230 GHz brightness sensitivity: 1 K for 1 km/sec channel, 1'' beam, in 1 hour 17
A-array synthesized beam, declination –30 0.26 × 0.14" FWHM 5% contours 19
first light correlator • uses COBRA hardware design • 15 telescopes, 105 baselines • 8 independent sections: • may be positioned anywhere in 4 GHz IF band • choose 2, 8, 31, 62, 125, 250, or 500 MHz bandwidth • velocity resolution 0.04 to 40 km s-1/ channel at 1.3 mm • 0.5 second integrations separateSZA correlator: 8 antennas, 28 baselines, 8 GHz bandwidth 20
timeline 21