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ALMA Atacama Large Millimeter Array NRAO, ESO, Japan,… alma

ALMA Atacama Large Millimeter Array NRAO, ESO, Japan,… www.alma.info. Uncited content taken from “Science with ALMA” http://www.eso.org/projects/alma/science/alma-science.pdf. Millimeter/submillimeter wavelength interferometer located in the Atacama desert in Chile

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ALMA Atacama Large Millimeter Array NRAO, ESO, Japan,… alma

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  1. ALMAAtacama Large Millimeter Array NRAO, ESO, Japan,…www.alma.info Uncited content taken from “Science with ALMA” http://www.eso.org/projects/alma/science/alma-science.pdf

  2. Millimeter/submillimeter wavelength interferometer located in the Atacama desert in Chile • 5000m altitude, good atmospheric transmission • “Public use” instrument • 2010 First science, 2012 “Full” capacity (4 bands?)

  3. Prototype 12m antennas from Japan, US, Europe 64 12 m antennas, baseline up to 14km Huge baseline, collecting area = huge resolution, sensitivity, cost Total Budget: ~1 Billion Euros

  4. ALMA bands Red: Band in the bilateral ALMA plan Blue: Will be delivered by Japan. Bands 4 and 8 are certain; Band 10 is more difficult and will come later Purple: Financed by the EU and only for a limited number of antennas Yellow: Not in the current planning.

  5. Receivers • One large receiver per antenna, each band contained in a modular cartridge • 10 dual polarization bands share the focal plane (no switching mirror) (ALMA memo 362) • Near quantum limit heterodyne detectors (SIS/HEMT) • Mechanical closed cycle cooler to 4K (GM)

  6. Band 9 cartridge (SRON) http://www.sron.rug.nl/alma/

  7. ALMA correlator (one quadrant of 4, 2nd under construction) From T. Beasley “ALMA status and upcoming events” Jan 2007

  8. SCIENCE • The ALMA “Level one design goals” • to detect CO in an Milky Way-like galaxy at z=3 in ~day • to image molecular lines in a protoplanetary disk with • a resolution of 1 AU out to a distance of 150 pc • 3) to obtain high fidelity imaging to match HST, JWST, or AO imaging. • Design reference science plan (118 pages) • http://www.strw.leidenuniv.nl/~alma/drsp10.shtml

  9. Cosmic Microwave Background • Multipole l ~ 2,500 25,000 • Probe high l CMB effects (test reionization models, etc.) • High resolution imaging of SZ effect in clusters to understand gas dynamics (survey followup?) Left: hydrodynamical model of z~1 2.5 x 1014 galaxy cluster Center: simulated ALMA observation Right: Smoothed simulated observation.

  10. Imaging galaxy clusters SCUBA 850um contours over optical image Cluster A1835 (central galaxy z~0.25) Submm reveals unseen galaxies (high z obscured galaxy on right) ALMA resolution better than the optical image Ivison et al., astro-ph/9911069

  11. Protoplanetary Disks High resolution imaging of thermal emission of cold, optically thin disks (no scattered visible/near IR) Ability to detect gaps due to Jupiter-like planets at 150 pc (Detected exoplanets <~ 100pc http://exoplanets.org/cne.pdf) Study chemical composition of disks, important to planet formation Study evolution of “debris disks” around older stars Integration time ~ 4 hours

  12. Our solar system • Outermost planet thermal emission – Pluto ~38K Turner & Wootten, astro-ph/0611639 • Planetary atmospheres • Solar flares (synchrotron)

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