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CARMA C ombined A rray for R esearch in M illimeter-wave A stronomy

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

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  1. CARMACombined Array for Research in Millimeter-wave Astronomy Stuart Vogel ALMA Workshop– May2004

  2. OVRO Caltech Six 10.4 m dishes Berkeley – Illinois – Maryland Nine 6.1 m dishes BIMA Chicago Eight 3.5 m dishes

  3. Rick Forster

  4. Inyo National Forest Cedar Flat – 7300’

  5. 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

  6. BIMA Relocation OVRO Relocation

  7. + SZA D Array

  8. Carlstrom – Chicago Built to CARMA standard Eight x 3.5 m dishes 30 – 90 – 230 GHz SZA

  9. + 3.5 m SZA Heterogeneous Array 10.4 m OVRO 6.1 m BIMA D Array

  10. Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown D 1.9” @1mm

  11. Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown C 0.8” @1mm

  12. Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown B 0.3” @1mm

  13. Cedar Flat: View from South 15 OVRO & BIMA dishes; SZA not shown A 0.12” @1mm

  14. Transporter Antenna Transporter

  15. OVRO Cedar Flat Juniper Flat

  16. CARMA Sensitivity Line: 1 km/sec Continuum Factor of 5 to 20 better

  17. Caltech COBRA correlator • FPGAs, not custom correlator chips • 4 GHz bandwidth • 256 20 Mhz channels • 6 station • For CARMA • Reprogram FPGAs • Spectral downconverters

  18. CARMA Correlators 8 antennas 8 GHz 256 channels 15 antennas 4 GHz 8 x 2– 500MHz tunable bands 64 – 512 channels

  19. 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

  20. Large bandwidth, high sensitivity

  21. 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

  22. High resolutionHigh sensitivity 2km baselines – 0.12” @1mm

  23. Heterogeneous imaging, mosaics Horsehead 29 fields CO 1-0 Pound et al 2003

  24. Heterogeneous imaging, mosaics L1551 C18O 220 fields Swift 2004

  25. Heterogeneous imaging, mosaics L1551 13CO 220 fields Swift 2004

  26. M33 in Ha H: Cheng et al. (1993)

  27. BIMA M33 GMC Survey • CO 1-0 • 759 mosaic fields • 135 total hours • 10 minutes per field CO: Engargiola et al. (2003)

  28. 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)

  29. Correlation with HI • In M33, GMCs form from HI with N(HI)>5x1020 cm-2 HI: Deul & van der Hulst (1987)

  30. Andromeda

  31. Barredgalaxies Central kpc NGC 2903 NGC 3627 NGC 3953 NGC 4303 CO R H BIMASONG

  32. Barredgalaxies Central kpc NGC 4321 NGC 4535 NGC 5457 NGC 6946 CO R H BIMASONG

  33. Unbarredgalaxies Central kpc NGC 0628 NGC 3938 NGC 4414 NGC 4736 CO R H BIMASONG

  34. Unbarredgalaxies Central kpc NGC 4826 NGC 5055 NGC 5194 NGC 7331 CO R H BIMASONG

  35. Secular Evolution Early Barred Late Barred Nuc (Mo pc-2) Early Unbarred Late Unbarred Disk (Mo pc-2)

  36. Secular Evolution Early Barred Nuc (Mo pc-2) Early Unbarred Disk (Mo pc-2) Exclude inner ring galaxies

  37. Sunyaev-Zel’dovich Effect

  38. 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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