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Comprehensive Overview of the BIMA and SZA Radio Antenna Arrays for Astrophysical Observations

This project outlines the specifications and status of the BIMA and SZA radio telescope arrays utilized in astrophysical research. The highlighted parameters include the array configurations featuring various antenna diameters, recent upgrades, sensitivity improvements, and capabilities for wide field imaging. Notably, the arrays allow for the detection of cosmic phenomena such as the T Tauri outburst and facilitate extensive surveys of galactic structures. The project emphasizes advanced data collection techniques and the future direction for radio astronomy advancements.

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Comprehensive Overview of the BIMA and SZA Radio Antenna Arrays for Astrophysical Observations

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  1. Project status and specifications Douglas Bock Project Manager 1

  2. 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

  3. BIMA mosaic of M33 • CO 1-0 115 GHz • 759 pointing centers 3

  4. BIMA mosaic of M33(Engargiola et al. 2003) • 148 GMCs detected • overlie HI filaments (HI image: Deul & van der Hulst 1987) 4

  5. 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

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  15. 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

  16. sensitivity Line: 1 km/sec Continuum Factor of 5 to 20 better than present performance 16

  17. 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

  18. u,v coverage for declination –30 4-hr observing track 18

  19. A-array synthesized beam, declination –30 0.26 × 0.14" FWHM 5% contours 19

  20. 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

  21. timeline 21

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