Atacama Large Millimeter Array

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Atacama Large Millimeter Array

• 64x12m Antennas
• Frequency range 30-1000 GHz (0.3-10mm)
• 14km max baseline (lt10mas)
• ALMA Compact Array (short spacing and total power)

• Detecting CO and C II in a Milky Way galaxy at
  z3 in less than 24 hours of observation
• To map dust emission and gas kinematics in
  protoplanetary disks
• The ability to provide high-quality and high
  resolution imaging in the millimeter and
  submillimeter bands to match that of HST and
  ground-based AO-equipped telescopes

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Alma sensitivity

• Observing thermal sources, there is no point
  having angular resolution without sensitivity to
  low brightness temperature
• Alma allows 30 K rms with 30 mas res. at 1mm

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Red shifted CII and OI lines
CO at z6.4 is already seen

• With ALMA one will see the fine structure lines
  of CII(157 micron) and O I(63 micron) (for zgt 2
  (CII) and zgt5(OI)), so one can measure the
  cooling directly.

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ALMA Site
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Trasparenza Atmosferica
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ALMA Receivers
? Japanese contribution all telescopes plus ACA ?
EC funded 8 receivers ALMA-Herschel sinergy
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ALMA Receivers
Band 3 (3mm)
Band 7 (850µm)
Band 6 (1mm)
Band 9 (450µm)
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Milky Way galaxy at high redshift
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ALMA Compact Array

• ACA è il contributo più rilevante portato dal
  Giappone, assieme alle bande 4, 8 e 10.

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Comparing CO and optical image

• Antennae Galaxy (HST and OVRO)

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Project schedule towards ES
Will be revised soon
Early Science
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Science Operations Plan
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ALMA SW Expectation for Early Science

• Observation Preparation
• All modes offered to the users will be supported
  from the Novice to the Expert levels.
• At the very beginning of Early Science, the
  Novice mode behaviour will be mostly based on
  expectation from simulation and initial testing
  rather than on a solid experience with ALMA
• Science Pipeline
• Not available to the users for Early Science (it
  will be in the heuristics learnig phase)
• Offline Data Reduction Package (AIPS)
• All modes offered will have been fully tested and
  supported
• No Graphical User Interface will be available for
  Early science
• A solid well tested User Interface and scripting
  language based on Python will be available

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Ruolo degli ARC Core Functions
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Ruolo degli ARC Science Support Functions
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Struttura degli ARC
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Euro ARC
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Risposte alla Call di ESO per ARC Nodes

• Germania (UniBonn, MPIfR, UniKoeln, UniBochum)
• IRAM (Francia, Germania-MPG, Spagna)
• Italia (INAF-Istituto di Radioastronomia)
• Paesi Bassi (Leiden, probabilmente Belgio)
• NORDIC-Onsala (Svezia, Danimarca, Finlandia, )
• UK (Jodrell, Edinburgh, Cambridge, )
• (Portogallo Svizzera)
• Ogni nodo fornisce servizi di base e servizi
  specializzati (per tutta la comunità Europea)

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Where is italian mm astronomy

• Disadvantaged rel. to IRAM countries but with
  interest in certain areas
• Quite a few theoretical groups (esp. Cosmology)
• Stellar (circumstellar) groups absent

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Per saperne di più

• Gianni Tofani
• European ALMA Board
• Leonardo Testi
• European Science Advisory Committee
• Bilateral ALMA Science Advisory Committee
• LT, Gianfranco De Zotti, Karl-Heinz Mack,
  Antonella Natta, Mauro Pucillo
• Gruppo di lavoro INAF-ALMA
• Subscribe to the ESO-ALMA Newsletter
• http//www.eso.org/projects/alma/newsletter/