Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Atacama Large Millimeter ArrayAtacama Large Millimeter Array

1.1. Detecting CO and [C II] in a Milky Way galaxy at z=3 in less Detecting CO and [C II] in a Milky Way galaxy at z=3 in less than 24 hours of observationthan 24 hours of observation

2.2. To map dust emission and gas kinematics in protoplanetary To map dust emission and gas kinematics in protoplanetary disksdisks

3.3. The ability to provide high-quality and high resolution The ability to provide high-quality and high resolution imaging in the millimeter and submillimeter bands to match imaging in the millimeter and submillimeter bands to match that of HST and ground-based AO-equipped telescopesthat of HST and ground-based AO-equipped telescopes

• 64x12m Antennas 64x12m Antennas

• Frequency range 30-1000 Frequency range 30-1000 GHz (0.3-10mm)GHz (0.3-10mm)

• 14km max baseline 14km max baseline (<10mas)(<10mas)

• ALMA Compact Array (short ALMA Compact Array (short spacing and total power)spacing and total power)

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Alma sensitivityAlma sensitivity

• Observing thermal sources, there is no point Observing thermal sources, there is no point having angular resolution without sensitivity to having angular resolution without sensitivity to low brightness temperaturelow brightness temperature

• Alma allows 30 K rms with 30 mas res. at 1mmAlma allows 30 K rms with 30 mas res. at 1mm

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Red shifted CII and OI linesRed shifted CII and OI lines

• With ALMA one will see the fine structure lines of With ALMA one will see the fine structure lines of CII(157 micron) and O I(63 micron) (for z> 2 (CII) CII(157 micron) and O I(63 micron) (for z> 2 (CII) and z>5(OI)), so one can measure the cooling and z>5(OI)), so one can measure the cooling directly.directly.

CO at z=6.4is already seen

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

ALMA SiteALMA Site

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Trasparenza AtmosfericaTrasparenza Atmosferica

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

ALMA ReceiversALMA Receivers

★ ★ Japanese contribution all telescopes plus ACAJapanese contribution all telescopes plus ACA★ ★ EC funded 8 receivers ALMA-Herschel sinergyEC funded 8 receivers ALMA-Herschel sinergy

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

ALMA ReceiversALMA Receivers

Band 3 (“3mm”)Band 3 (“3mm”)

Band 6 (“1mm”)Band 6 (“1mm”)

Band 7 (“850Band 7 (“850μμm”)m”)

Band 9 (“450Band 9 (“450μμm”)m”)

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Milky Way galaxy at high redshiftMilky Way galaxy at high redshift

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

ALMA Compact ArrayALMA Compact Array

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

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Comparing CO and optical imageComparing CO and optical image

• Antennae Galaxy (HST and OVRO)Antennae Galaxy (HST and OVRO)

36th Liège International Astrophysical Colloquium: From Optical to Millimetric Interferometry Extragalactic Observations with ALMA

HST optical image HST optical image + CO contours

The “Antennae”

(CO : Wilson et al. 2000)(HST: Whitmore et al. 1999)

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Project schedule towards ESProject schedule towards ES

Will

be revise

d soon

Will

be revise

d soon

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Science Operations PlanScience Operations Plan

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

ALMA SW: Expectation for Early ALMA SW: Expectation for Early ScienceScience

• Observation PreparationObservation Preparation– All modes offered to the users will be supported from the Novice All modes offered to the users will be supported from the Novice

to the Expert levels.to the Expert levels.

– At the very beginning of Early Science, the Novice mode At the very beginning of Early Science, the Novice mode behaviour will be mostly based on expectation from simulation behaviour will be mostly based on expectation from simulation and initial testing rather than on a solid experience with ALMAand initial testing rather than on a solid experience with ALMA

• Science PipelineScience Pipeline– Not available to the users for Early ScienceNot available to the users for Early Science (it will be in the (it will be in the

heuristics “learnig phase”)heuristics “learnig phase”)

• Offline Data Reduction Package (AIPS++)Offline Data Reduction Package (AIPS++)– All modes offered will have been fully tested and supportedAll modes offered will have been fully tested and supported

– No Graphical User Interface will be available for Early scienceNo Graphical User Interface will be available for Early science

– A solid well tested User Interface and scripting language based A solid well tested User Interface and scripting language based on Python will be availableon Python will be available

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Ruolo degli ARC – Core FunctionsRuolo degli ARC – Core Functions

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Ruolo degli ARC – Science Support Ruolo degli ARC – Science Support FunctionsFunctions

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Struttura degli ARCStruttura degli ARC

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Euro ARCEuro ARC

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Risposte alla Call di ESO per ARC Risposte alla Call di ESO per ARC NodesNodes

• Germania (UniBonn, MPIfR, UniKoeln, UniBochum)Germania (UniBonn, MPIfR, UniKoeln, UniBochum)

• IRAM (Francia, Germania-MPG, Spagna)IRAM (Francia, Germania-MPG, Spagna)

• Italia (INAF-Istituto di Radioastronomia)Italia (INAF-Istituto di Radioastronomia)

• Paesi Bassi (Leiden, + probabilmente Belgio)Paesi Bassi (Leiden, + probabilmente Belgio)

• NORDIC-Onsala (Svezia, Danimarca, Finlandia, +NORDIC-Onsala (Svezia, Danimarca, Finlandia, +…)…)

• UK (Jodrell, Edinburgh, Cambridge, +…)UK (Jodrell, Edinburgh, Cambridge, +…)

• (Portogallo & Svizzera)(Portogallo & Svizzera)

• Ogni nodo fornisce servizi di base e servizi Ogni nodo fornisce servizi di base e servizi specializzati (per tutta la comunità Europea)specializzati (per tutta la comunità Europea)

Leonardo Testi, INAF - Osservatorio Astrofisico di Arcetri, ALMA

Where is italian mm astronomyWhere is italian mm astronomy

• Disadvantaged rel. to IRAM countries but with Disadvantaged rel. to IRAM countries but with interest in certain areasinterest in certain areas

• Quite a few “theoretical groups” (esp. Quite a few “theoretical groups” (esp. Cosmology)Cosmology)

• Stellar (circumstellar) groups absentStellar (circumstellar) groups absent