1. Project status and specifications Douglas Bock Project Manager 1

2. + UChicago SZA 8 3.5-m antennas Berkeley-Illinois-Maryland Assn. array 10 6.1-m diameter antennas Caltech array 6 10.4-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 2 nd 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 CARMACARMA + SZA # antennas1523 # baselines105253 collecting area773 m 2 850 m 2 15

16. 100GHz230GHz ArrayBeam1-min5-hrBeam1-min5-hr D6.3”0.3 K0.02 K2.7”0.4 K0.02 K C2.5”2.0 K0.1 K1.1”2.2 K0.13 K B1.0”12 K0.7 K0.4”17 K1.0 K A0.4”77 K4.5 K0.2”67 K4 K Line: 1 km/sec 100GHz230GHz 1-min5-hr1-min5-hr 0.7 mJy0.04 mJy1.1 mJy0.07 mJy sensitivity 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 freq (GHz)OVROBIMASZA 210-270SIS 85-116SISSIS (70-116)MMIC 29-37HEMT 22MMIC 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 separate SZA correlator: 8 antennas, 28 baselines, 8 GHz bandwidth 20

21. timeline June 2004Site construction began Sep 2004BIMA antennas moved May 2005Buildings, power station complete Mar & June 2005OVRO antennas moved Dec 2005Shared-risk science, 1.5 GHz correlator Mid 2006Routine science with 4 GHz correlator End 2006High resolution (sub-arcsecond) observations 2008Dual polarization at 1 mm, wideband MMICs at 3 mm 2009+New correlator, array receivers 21