CARMA Combined Array for Research in Millimeter-wave Astronomy

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CARMA Combined Array for Research in
Millimeter-wave Astronomy
Stuart Vogel ALMA Workshop May2004
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OVRO
Caltech Six 10.4 m dishes
Berkeley Illinois Maryland Nine 6.1 m dishes
BIMA
Chicago Eight 3.5 m dishes
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Rick Forster
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Inyo National Forest Cedar Flat 7300
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Timeline

• Cedar Flat permit
• Shut down BIMA OVRO
• Roads, pads, buildings
• Move BIMA OVRO
• First light Operations

• 2003 December
• 2004 June
• 2004 Summer
• 2004 Fall
• 2005 Fall

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BIMA Relocation
OVRO Relocation
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D Array
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SZA

• Carlstrom Chicago
• Built to CARMA standard

• Eight x 3.5 m dishes
• 30 90 230 GHz

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Heterogeneous Array
10.4 m OVRO 6.1 m BIMA D Array
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Cedar Flat View from South 15 OVRO BIMA
dishes SZA not shown
D 1.9 _at_1mm
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Cedar Flat View from South 15 OVRO BIMA
dishes SZA not shown
C 0.8 _at_1mm
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Cedar Flat View from South 15 OVRO BIMA
dishes SZA not shown
B 0.3 _at_1mm
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Cedar Flat View from South 15 OVRO BIMA
dishes SZA not shown
A 0.12 _at_1mm
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Antenna Transporter
Transporter
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OVRO Cedar Flat Juniper Flat
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CARMA Sensitivity
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
Continuum
Factor of 5 to 20 better
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• Caltech COBRA correlator
• FPGAs, not custom correlator chips
• 4 GHz bandwidth
• 256 20 Mhz channels
• 6 station

• For CARMA
• Reprogram FPGAs
• Spectral downconverters

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CARMA Correlators
8 antennas 8 GHz 256 channels
15 antennas 4 GHz 8 x 2 500MHz tunable
bands 64 512 channels
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Other CARMA Development

• New LO/IF system ? HEMT/SIS/MMIC
• New computing system reuse
• Upgrade antenna drives, cryogenics, telemetry
• Post first-light single-dish, polarization, WVR

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Large bandwidth, high sensitivity
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• Multiply-imaged SMM1-A2218
• CO (3-2) from z2.5165
• All three lensed images seen
• ?Sco Dv 5.4 Jy km/s (0.8, 3.1, 1.4)
• Dv 530 km/s
• Unlensed CO mass 6 x 109 M?
• No offset between optical and CO
• SFR 100-500 solar masses/yr
• Could be a circumnuclear ring (velocity
  structure) ?
• Witnessing a circumnuclear starburst w/ lifetime
  107 years?

z2.52 High resolution High sensitivity
Sheth, Blain, Kneib Frayer 04
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High resolutionHigh sensitivity
2 km baselines 0.12 _at_1mm
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Heterogeneous imaging, mosaics
Horsehead 29 fields
CO 1-0 Pound et al 2003
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Heterogeneous imaging, mosaics
L1551 C18O 220 fields
Swift 2004
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Heterogeneous imaging, mosaics
L1551 13CO 220 fields
Swift 2004
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M33 in Ha
H? Cheng et al. (1993)
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BIMA M33 GMC Survey

• CO 1-0
• 759 mosaic fields
• 135 total hours
• 10 minutes per field

CO Engargiola et al. (2003)
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GMCs in M33

• 148 GMCs
• Complete to 1.5 x 105 Msun
• Mass spectrum dN/dM?M-2.6
• Characteristic mass 7 x 104 Msun
• Nearly all HII regions near GMCs

CO Engargiola et al. (2003)
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Correlation with HI

• In M33, GMCs form from HI with N(HI)gt5x1020
  cm-2

HI Deul van der Hulst (1987)
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Andromeda
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Barred galaxies
NGC 2903
NGC 3627
NGC 3953
NGC 4303
CO
R
H?
BIMA SONG
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Barred galaxies
NGC 4321
NGC 4535
NGC 5457
NGC 6946
CO
R
H?
BIMA SONG
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Unbarred galaxies
NGC 0628
NGC 3938
NGC 4414
NGC 4736
CO
R
H?
BIMA SONG
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Unbarred galaxies
NGC 4826
NGC 5055
NGC 5194
NGC 7331
CO
R
H?
BIMA SONG
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Exclude inner ring galaxies
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Sunyaev-Zeldovich Effect
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CARMA

• Best array at 1 3 mm for resolution,
  sensitivity, fidelity, bandwidth (until ALMA
  up to speed)
• Northern hemisphere complement to ALMA (and
  Spitzer, SOFIA, JWST, etc)
• Heterogeneous mosaics, surveys
• Development (WVR, focal plane arrays)
• Hands-on student postdoc training
• Building the mm-wave community

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