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CARMA C ombined A rray for R esearch in M illimeter-wave A stronomy. Stuart Vogel ALMA Workshop– May2004. OVRO. Caltech Six 10.4 m dishes. Berkeley – Illinois – Maryland Nine 6.1 m dishes. BIMA. Chicago Eight 3.5 m dishes. Rick Forster. Inyo National Forest Cedar Flat – 7300’.

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carma c ombined a rray for r esearch in m illimeter wave a stronomy
CARMACombined Array for Research in Millimeter-wave Astronomy

Stuart Vogel

ALMA Workshop– May2004

slide2

OVRO

Caltech

Six 10.4 m dishes

Berkeley – Illinois – Maryland

Nine 6.1 m dishes

BIMA

Chicago

Eight 3.5 m dishes

slide4

Inyo National Forest

Cedar 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

Timeline
slide6

BIMA Relocation

OVRO Relocation

slide8
Carlstrom – Chicago

Built to CARMA standard

Eight x 3.5 m dishes

30 – 90 – 230 GHz

SZA
slide9

+

3.5 m SZA

Heterogeneous

Array

10.4 m OVRO 6.1 m BIMA

D Array

slide10

Cedar Flat: View from South

15 OVRO & BIMA dishes;

SZA not shown

D 1.9” @1mm

slide11

Cedar Flat: View from South

15 OVRO & BIMA dishes;

SZA not shown

C 0.8” @1mm

slide12

Cedar Flat: View from South

15 OVRO & BIMA dishes;

SZA not shown

B 0.3” @1mm

slide13

Cedar Flat: View from South

15 OVRO & BIMA dishes;

SZA not shown

A 0.12” @1mm

slide15

OVRO

Cedar Flat

Juniper Flat

carma sensitivity
CARMA Sensitivity

Line:

1 km/sec

Continuum

Factor of 5 to 20 better

slide18
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
CARMA Correlators

8 antennas

8 GHz

256 channels

15 antennas

4 GHz

8 x 2– 500MHz

tunable bands

64 – 512 channels

other carma development
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
slide22

Multiply-imaged SMM1-A2218

  • CO (3-2) from z=2.5165
  • 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?

z=2.52

High resolution

High sensitivity

Sheth, Blain, Kneib & Frayer ‘04

high resolution high sensitivity
High resolutionHigh sensitivity

2km baselines – 0.12” @1mm

heterogeneous imaging mosaics
Heterogeneous imaging, mosaics

Horsehead

29 fields

CO 1-0

Pound et al 2003

slide25

Heterogeneous imaging, mosaics

L1551

C18O

220 fields

Swift 2004

slide26

Heterogeneous imaging, mosaics

L1551

13CO

220 fields

Swift 2004

m33 in h a
M33 in Ha

H: Cheng et al. (1993)

bima m33 gmc survey
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
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)

correlation with h i
Correlation with HI
  • In M33, GMCs form from HI with N(HI)>5x1020 cm-2

HI: Deul & van der Hulst (1987)

slide32

Barredgalaxies

Central kpc

NGC 2903

NGC 3627

NGC 3953

NGC 4303

CO

R

H

BIMASONG

slide33

Barredgalaxies

Central kpc

NGC 4321

NGC 4535

NGC 5457

NGC 6946

CO

R

H

BIMASONG

slide34

Unbarredgalaxies

Central kpc

NGC 0628

NGC 3938

NGC 4414

NGC 4736

CO

R

H

BIMASONG

slide35

Unbarredgalaxies

Central kpc

NGC 4826

NGC 5055

NGC 5194

NGC 7331

CO

R

H

BIMASONG

slide36

Secular Evolution

Early Barred

Late Barred

Nuc

(Mo pc-2)

Early Unbarred

Late Unbarred

Disk (Mo pc-2)

slide37

Secular Evolution

Early Barred

Nuc

(Mo pc-2)

Early Unbarred

Disk (Mo pc-2)

Exclude inner ring galaxies

carma
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