ALMA: Stato, Early Science,, ARC

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1 ALMA: Stato, Early Science,, ARC Leonardo Testi INAF Osservatorio Astrofisico di Arcetri Il progetto ALMA Stato attuale e schedula Piani per Early Science e Science Operations Supporto utenti: Alma Regional Centers

2 Atacama Large Millimeter Array 64x12m Antennas Frequency range GHz (0.3-10mm) 14km max baseline (<10mas) ALMA Compact Array (short spacing and total power) 1. Detecting CO and [C II] in a Milky Way galaxy at z=3 in less than 24 hours of observation 2. To map dust emission and gas kinematics in protoplanetary disks 3. 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

3 Joint ALMA Observatory Array Operations Site (AOS) Main Array+ALMA Compact Array,, Altopiano Chajnantor 5000m Operations Support Facility (OSF) Technical support, array operations center 2800m Santiago Central Office (SCO) Master Archive,, Pipeline Operations, Offices for admin and science staff ALMA Regional Centers (ARC) User and Science Support (Europe, North America, Japan)

4 ALMA Site

5 ALMA Site Development

6 ALMA Site Development OSF oggi e domani

7 ALMA Site Development AOS oggi

8 ALMA Site Development AOS oggi e domani

9 ALMA Prototype Antennas VLA Mitsubishi Alcatel-EIE Evaluation process still underway Vertex

10 ALMA Receivers

11 ALMA Receivers ALMA Cryostat Designed to host all 10 receiver cartdriges

12 ALMA Receivers Band 3 ( 3mm( 3mm ) Band 7 ( 850( 850µm ) Band 6 ( 1mm( 1mm ) Band 9 ( 450µm )

13 ALMA Correlator

14 ALMA Office in Santiago Master ALMA Archive Quality Control Pipeline Managment Science Staff

15 Project schedule towards ES

16 Science Operations Plan

17 The Camera Goal ALMA delivers images The astronomer specifies the science requirements: angular resolution field of view Image fidelity required Spectral configuration and calibration precision The observing preparation tools derive the observation Stringency Stringency concept: (inverse of the) Fraction of time in which the observing conditions are better than required to perform the project. Full service observing with dynamic scheduling The ALMA imaging pipeline ensures optimal (within current knowledge) data processing to produce the image ESO Garching Leonardo / Nov 2002Testi, INAF - Osservatorio Astrofisico ALMA di Arcetri, Status Users Expectations from the ALMA Software 8

18 The Camera Goal Remaining difficulties for Astronomers Proper definition of the science requirements Compromise Sensitivity / Angular Resolution The spectral correlator configuration definition (the correlator is very flexible...) a minimum understanding interferometry may still be important. High fidelity or very wide field images may require post-processing. Full polarization imaging may require post-processing Special observations (e.g. moving targets,...)... ESO Garching Leonardo / Nov 2002Testi, INAF - Osservatorio Astrofisico ALMA di Arcetri, Status Users Expectations from the ALMA Software 9

19 The ALMA software system Developed by the Computing IPT (B. Glendenning & G. Raffi) Designed to meet a set of Science Requirements prepared by the Science Software Requirements Commettee (R. Lucas) Subsystems Scientists (SSR members) ) are responsible for supporting the developers teams and ensure that each subsystem will meet the scientific requirements. Observation Preparation (Leonardo Testi) Offline Data Reduction (Debra Shepherd) (Science)) Pipeline (Christine Wilson)

20 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

21 Ruolo degli ARC Core Functions

22 Ruolo degli ARC Science Support Functions

23 Struttura degli ARC

24 Euro ARC

25 Euro ARC

26 Risposte alla Call di ESO per ARC Nodes Germania (UniBonn( UniBonn, MPIfR, UniKoeln, UniBochum) IRAM (Francia, Germania-MPG MPG,, Spagna) Italia (INAF( INAF-IstitutoIstituto di Radioastronomia) Paesi Bassi (Leiden( Leiden,, + probabilmente Belgio) NORDIC-Onsala Onsala (Svezia, Danimarca, Finlandia, + ) + UK (Jodrell( Jodrell, Edinburgh,, Cambridge, + ) + (Portogallo & Svizzera) Riunione in Gennaio/Febbraio con ESO

27 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 ALMA Subscribe to the ESO-ALMA Newsletter