ALMA Overview. Leonardo Testi (European Southern Observatory)

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1 ALMA Overview Leonardo Testi (European Southern Observatory) The ALMA Project Status Timeline towards Early and Full Science Operations Future Developments

2 Atacama Large Millimeter Array At least 50x12m Antennas Frequency range GHz (0.3-10mm) 18km max baseline (<10mas) ALMA Compact Array (4x12m and 12x7m) 1. Detect and map CO and [C II] in a Milky Way galaxy at z=3 in less than 24 hours of observation 2. Map dust emission and gas kinematics in protoplanetary disks 3. Provide high fidelity imaging in the (sub)millimeter at 0.1 arcsec resolution

Detect and map CO and [C II] in a Milky Way galaxy at z=3 in less than 24 hours of observation 2.

3 ALMA Major Elements Partners: ESO US/Canada Japan Chile Taiwan Array Operations Site AOS Operations Support Facility OSF Santiago Central Offices SCO ALMA Regional Centers ARCs + ARClets During full operation, the estimated flow of int/sd data into archive ~ 100 TB per year: proposal, u-v data, a reference image with pipeline processing history, calibration data modern radio astronomy

ARClets During full operation, the estimated flow of int/sd data into archive ~ 100 TB per year:

4 ALMA Science Requirements High Fidelity Imaging. Precise Imaging at 0.1 Resolution. Routine sub-mjy Continuum Sensitivity. Routine mk Spectral Sensitivity. Wideband Frequency Coverage. Wide Field Imaging Mosaicing. Submillimeter Receiver System. Full Polarization Capability. System Flexibility.

Routine mk Spectral Sensitivity. Wideband Frequency Coverage.

5 ALMA Science Star Formation, Proto-planets in nearby disks Astrochemistry Interstellar medium (Galaxy, Local Group) High-redshift deep fields +130 projects in first 3yrs DRSP ALMA Science is for everyone High resolution/sensitivity 3D instrument at mm-wl 100% service observing with full dynamic scheduling Complete e2e data flow system Science quality images (cubes) delivered to the users Raw, calibrations, pipeline processed data and recipes in archive Friendly and widespread User Support through ARCs

shtml ALMA Science is for everyone High resolution/sensitivity 3D instrument at mm-wl 100% service observing with full dynamic scheduling

6 Technical Specifications m antennas, 12 7-m antennas, at 5000 m site Surface accuracy ±25 µm, 0.6 reference pointing in 9m/s wind, 2 absolute pointing all-sky. Array configurations between 150m to ~18km. 10 bands in GHz GHz WVR. 8 GHz BW, dual polarization. Flux sens. 0.2 mjy in 1 min at 345 GHz (median cond.). Interferometry, mosaicing & total-power observing. Correlator: 4096 channels/if (multi-if), full Stokes. Data rate: 6MB/s average; peak MB/s. All data archived (raw + images), pipeline processing.

10 bands in 31-950 GHz + 183 GHz WVR. 8 GHz BW, dual polarization. Flux sens. 0.2 mjy in 1 min at 345 GHz (median cond.).

7 Chajnantor Plateau m Y + Antenna locations V. Licancabur Pampa La Bola ASAC Lascar Volcano AOS Tech Bldg Center of Array

8 AOS Technical Building Jan 2008

9 Operations Support Facility m 9

12 ALMA Test Facility Testing Defining Procedures for Commissioning Testing/Debugging Software Leonardo Testi: Science, ESAC 2008 Apr 15

13 ALMA Test Facility Testing Defining Procedures for Commissioning Testing/Debugging Software First Fringes (Mar07), Dyn. Fringes (Nov07), Int. Spec. (Jan08), TFB spectra (Apr08) Dynamical Fringes on 3C454.4 Continuum mode spec of Orion Leonardo Testi: Science, ESAC 2008 Apr 15

14 ALMA CSV, Early and Full Science CSV Team Sci IPT plus Ops Astr. Community involvement - ESO supported stays in Chile SV is NOT an early opportunity to do science with ALMA Early Science: 16 ants, at least 4 receiver bands, limited time Full Science Operations in 2012/

early opportunity to do science with ALMA Early Science: 16 ants, at

15 Your proposal here 2010

16 ALMA beyond ALMA ALMA will allow transformational science thanks to the sensitivity, angular resolution, spectral coverage and image fidelity, but... The baseline ALMA project will only achieve a fraction of the full potential of the site and instrument Incomplete Receiver Complement Limited Wide Field Capabilities Limited Correlator and Data Rate Capabilities Advanced Calibration, Software... 16

$.. The baseline ALMA project will only achieve a fraction of the full potential of the site and$

17 Examples of Scientific Limitations Limited Band 5 Complement Eu FP6 6 B5: just a glimpse at B5 Water in the Universe [CII] in the range 7 < z < 10 No Band 1 & 2 High-z low excitation CO Sunyaev-Zeldʼovich effect Dust Evolution in Protoplanetary Disks Limited correlator capabilities Line surveys, chemistry studies very time consuming Continuum Wide Field Mapping Efficiency SZ and Molecular Clouds applications very time consuming 17

Evolution in Protoplanetary Disks Limited correlator capabilities Line surveys, chemistry studies very time

18 The ALMA Development Program ALMA development budget is proposed to ramp up starting in 2013 to reach ~10M$/yr from ~2015 The ALMA Board has initiated a process to plan the development program ASAC and Project Scientist in charge of preparing a preliminary report for the science with ALMA in 2020 Working Groups are being formed to work on science topics From science report to development plan Process to be completed on a 2 years timescale 18

charge of preparing a preliminary report for the science with ALMA in 2020 Working Groups are being formed to

19 Feb 2008 Atacama Large Millimeter/submillimeter Array 19 77

ALMA: Stato, Early Science,, ARC

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