Project status and specifications

Douglas Bock

Project Manager1

+ 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

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BIMA mosaic of M33

• CO 1-0 115 GHz

• 759 pointing centers

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BIMA mosaic of M33(Engargiola et

al. 2003)

• 148 GMCs detected

• overlie HI filaments (HI image: Deul & van der Hulst

1987)

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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.)

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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

CARMA CARMA + SZA

# antennas 15 23

# baselines 105 253

collecting area 773 m2 850 m2

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100 GHz 230 GHz

Array Beam 1-min 5-hr Beam 1-min 5-hr

D 6.3” 0.3 K 0.02 K 2.7” 0.4 K 0.02 K

C 2.5” 2.0 K 0.1 K 1.1” 2.2 K 0.13 K

B 1.0” 12 K 0.7 K 0.4” 17 K 1.0 K

A 0.4” 77 K 4.5 K 0.2” 67 K 4 K

Line: 1 km/sec

100 GHz 230 GHz

1-min 5-hr 1-min 5-hr

0.7 mJy 0.04 mJy 1.1 mJy 0.07 mJy

sensitivity

Continuum

Factor of 5 to 20 better than present performance16

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) OVRO BIMA SZA210-270 SIS SIS

85-116 SIS SIS (70-116) MMIC

29-37 HEMT HEMT

22 MMIC

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

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A-array synthesized beam, declination –30 0.26 × 0.14" FWHM

5% contours

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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

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timeline

June 2004 Site construction began

Sep 2004 BIMA antennas moved

May 2005 Buildings, power station complete

Mar & June 2005 OVRO antennas moved

Dec 2005 Shared-risk science, 1.5 GHz correlator

Mid 2006 Routine science with 4 GHz correlator

End 2006 High resolution (sub-arcsecond) observations

2008 Dual polarization at 1 mm, wideband MMICs at 3 mm

2009+ New correlator, array receivers21