CARMA Combined Array for Research in Millimeterwave Astronomy
CARMA Combined Array for Research in Millimeter-wave Astronomy Stuart Vogel ALMA Workshop– May 2004
OVRO Caltech Six 10. 4 m dishes BIMA Berkeley – Illinois – Maryland Nine 6. 1 m dishes Chicago Eight 3. 5 m dishes
Rick Forster
Inyo National Forest Cedar Flat – 7300’
Timeline • • • Cedar Flat permit Shut down BIMA & OVRO Roads, pads, buildings Move BIMA & OVRO First light & Operations 2003 2004 2005 December June Summer 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
Heterogeneous Array 10. 4 m OVRO 6. 1 m BIMA D Array + 3. 5 m SZA
Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown D 1. 9” @1 mm
Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown C 0. 8” @1 mm
Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown B 0. 3” @1 mm
Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown A 0. 12” @1 mm
Transporter Antenna Transporter
OVRO Cedar Flat Juniper Flat
CARMA Sensitivity Line: 1 km/sec Continuum 100 GHz 230 GHz Array 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 100 GHz Beam 1 -min 5 -hr 230 GHz 1 -min 5 -hr 0. 7 m. Jy 0. 04 m. Jy 1. 1 m. Jy 0. 07 m. Jy 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 antennas 8 GHz 256 channels 15 antennas 4 GHz 8 x 2– 500 MHz tunable bands 64 – 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
• Multiply-imaged SMM 1 -A 2218 • 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 2 km baselines – 0. 12” @1 mm
Heterogeneous imaging, mosaics Horsehead 29 fields CO 1 -0 Pound et al 2003
Heterogeneous imaging, mosaics L 1551 C 18 O 220 fields Swift 2004
Heterogeneous imaging, mosaics L 1551 13 CO 220 fields Swift 2004
M 33 in Ha H : Cheng et al. (1993)
BIMA M 33 GMC Survey • • CO: Engargiola et al. (2003) CO 1 -0 759 mosaic fields 135 total hours 10 minutes per field
GMCs in M 33 • 148 GMCs • Complete to 1. 5 x 105 Msun • Mass spectrum: d. N/d. M M-2. 6 • Characteristic mass: 7 x 104 Msun • Nearly all HII regions near GMCs CO: Engargiola et al. (2003)
Correlation with HI • In M 33, GMCs form from HI with N(HI)>5 x 1020 cm-2 HI: Deul & van der Hulst (1987)
Andromeda
NGC 2903 Barred galaxies NGC 3627 NGC 3953 NGC 4303 CO R H Central kpc BIMA SONG
NGC 4321 Barred galaxies NGC 4535 NGC 5457 NGC 6946 CO R H Central kpc BIMA SONG
NGC 0628 Unbarred galaxies NGC 3938 NGC 4414 NGC 4736 CO R H Central kpc BIMA SONG
NGC 4826 Unbarred galaxies NGC 5055 NGC 5194 NGC 7331 CO R H Central kpc BIMA SONG
Secular Evolution Early Barred Late Barred Nuc Early Unbarred Late Unbarred (Mo pc-2) Disk (Mo pc-2)
Secular Evolution Early Barred Nuc Early Unbarred (Mo pc-2) Exclude inner ring galaxies Disk (Mo pc-2)
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
- Slides: 43