CARMA Combined Array for Research in

Millimeter-wave Astronomy

Stuart VogelALMA Workshop– May2004

OVRO

BIMA

CaltechSix 10.4 m dishes

Berkeley – Illinois – MarylandNine 6.1 m dishes

ChicagoEight 3.5 m dishes

Rick Forster

Inyo National ForestCedar Flat – 7300’

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

BIMA Relocation

OVRO Relocation

D Array + SZA

SZA

• Carlstrom – Chicago

• Built to CARMA standard

• Eight x 3.5 m dishes

• 30 – 90 – 230 GHz

+3.5 m SZA

10.4 m OVRO 6.1 m BIMAD Array

Heterogeneous Array

D 1.9” @1mm

Cedar Flat: View from South15 OVRO & BIMA dishes; SZA not shown

C 0.8” @1mm

Cedar Flat: View from South15 OVRO & BIMA dishes; SZA not shown

B 0.3” @1mm

Cedar Flat: View from South15 OVRO & BIMA dishes; SZA not shown

A 0.12” @1mm

Cedar Flat: View from South15 OVRO & BIMA dishes; SZA not shown

Transporter

Antenna Transporter

OVROCedar FlatJuniper Flat

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

CARMA Sensitivity

Continuum

Factor of 5 to 20 better

Caltech COBRA correlator

• FPGAs, not custom correlator chips

• 4 GHz bandwidth

• 256 20 Mhz channels

• 6 station

For CARMA

• Reprogram FPGAs

• Spectral downconverters

CARMA Correlators

8 antennas8 GHz256 channels

15 antennas4 GHz8 x 2– 500MHz tunable bands64 – 512 channels

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

Large bandwidth, high sensitivity

QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.

•Multiply-imaged SMM1-A2218

• CO (3-2) from z=2.5165

• All three lensed images seen

• ∫Sco v ~ 5.4 Jy km/s (0.8, 3.1, 1.4)

• v ~ 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?

Sheth, Blain, Kneib & Frayer ‘04

z=2.52

High resolutionHigh sensitivity

High resolutionHigh sensitivity

2 km baselines – 0.12” @1mm

Horsehead

29 fields

CO 1-0Pound et al

2003

Heterogeneous imaging, mosaics

Swift 2004

Heterogeneous imaging, mosaics

L1551C18O220 fields

Swift 2004

Heterogeneous imaging, mosaics

L155113CO220 fields

H: Cheng et al. (1993)

M33 in H

BIMA M33 GMC Survey

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

CO: Engargiola et al. (2003)

GMCs in M33• 148 GMCs• Complete to

1.5 x 105 Msun

• Mass spectrum: dN/dM

• Characteristic mass: 7 x 104 Msun

• Nearly all HII regions near GMCs

CO: Engargiola et al. (2003)

Correlation with HI

• In M33, GMCs form from HI with N(HI)>5x1020

cm-2

HI: Deul & van der Hulst (1987)

Andromeda

CO

R

H

BIMA SONG

NGC 2903 NGC 3627 NGC 3953 NGC 4303Barred galaxies

Central kpc

CO

R

H

BIMA SONG

NGC 4321 NGC 4535 NGC 5457 NGC 6946Barred galaxies

Central kpc

CO

R

H

BIMA SONG

NGC 0628 NGC 3938 NGC 4414 NGC 4736Unbarred galaxies

Central kpc

CO

R

H

BIMA SONG

NGC 4826 NGC 5055 NGC 5194 NGC 7331Unbarred galaxies

Central kpc

Secular Evolution

Nuc

(Mo pc-2)

Disk (Mo pc-2)

Early Barred

Early Unbarred

Late Barred

Late Unbarred

Secular Evolution

Nuc

(Mo pc-2)

Disk (Mo pc-2)

Early Barred

Early Unbarred

Exclude inner ring galaxies

Sunyaev-Zel’dovich Effect

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