1. Charlottesville, November 2010 1 ALMA CSV Update Alison Peck Current status

2. Charlottesville, November 2010 2 Current Shape of the OSF Seen from the holography tower MElCo Camp Vertex Camp Construction Camp Staff cafeteria and dorms AEM Camp Technical Facility Offices and Labs Antenna Test Stations

3. Charlottesville, November 2010 3 Demographics of CSV Team Santiago-based CSV Scientists (100% toward CSV) Operations Astronomers (30% toward CSV) NAOJ in kind contribution (100%) ALMA Regional Center (ARC) Liaisons (100% - shortest trip ~3 months) Secondments (ie IRAM) (100% - shortest trip ~3 months) Visitors Program (100% - shortest trip ~3 months) Additional specialized ARC staff (2-3 turnos per trip) ESO (and other?) Fellows (3 turnos per trip) In order to have 6-8 people at the OSF at any given time, we need 24-32 people on the Science Team in Santiago at any given time. These are comprised of:

4. Charlottesville, November 2010 4 CSV Group Structure Groups are (with abbreviated lists of topics): Antenna – final test and characterization at high site, monitoring Calibration – phase, amplitude, bandpass, polarization Correlator – hardware & software 64-in and ACA up to Archive Documentation – quality & organization of reports, procedures, records Imaging – data reduction, configuration planning, ancillary (weather, etc) Observing Modes – end-to-end test, Observing Tool, science verification System – covers signal path from input to front-end to arrival at correlator We have dedicated groups for different areas of testing. Each team of ~5 people is led by one of the CSV Scientists who coordinates the work, assigns tasks, collects reports, etc. Visitors are assigned to a group based on preference and need:

5. Charlottesville, November 2010 5 Interaction with ARCs and Nodes Several groups seek assistance from people at the Executives. In particular, Imaging and Observing Modes. How you can help: Imaging - reducing data taken at ALMA promptly to look for obvious problems, but also, reducing data very carefully and comparing notes with others to catch more subtle problems. Science Verification involves comparing results to those of other telescopes. Feedback also needed for Calibration group. Observing Modes - suggest targets or projects for Science Verification, help create Scheduling Blocks and check existing SBs in new software versions, provide feedback to software developers

6. Charlottesville, November 2010 6 Science Verification Starting Jan 2011 Goals: End to End Test of ALMA as a telescope before Early Science Provide data, images (and enthusiasm) to community Call for Suggestions Not full proposals, just a couple of paragraphs No full proposal review process, appropriate projects chosen by committee led by Project Scientist Data not proprietary Images released through EPO department Data available to any users who wish to try data reduction

7. Charlottesville, November 2010 7 Various types of Observations needed Discrete sources, continuum and spectral line: All bands, all correlator setups Single and multiple lines - is it easy to create complicated setups in the OT? Single and multiple sources per SB – can the system deal with different source redshifts and calibrate correctly? Bright and weak lines – weak lines need good bandpass Absorption and emission lines Narrow and broad lines High-resolution, narrow bandwidth correlator modes requiring wider bandwidth on calibrators (Mixed correlator modes – Q2 2011) (Compact & extended arrays - Q2 2011)

8. Charlottesville, November 2010 8 Science Verification Matrix (partial)

9. Charlottesville, November 2010 9 Science Verification Observing Modes: Galactic: High Velocity Outflows NGC1333 IRAS4B, band 7 Observed on September 16 7 antennas, band 7, high-velocity CO + SO + continuum emission SMA, 230 GHz, high-velocity CO + continuum emission Jorgensen 2007

10. Charlottesville, November 2010 10 Science Verification Observing Modes Extragalactic: Broad line, strong continuum NGC 253 – B3 – CO J=1-0 NGC 253 – B6 – CO J=2-1 NGC 253 – B7 – CO=3-2 (Sakamoto et al, 2006) NGC 253 – B9 – CO=6-5 4 antennas, 3 hrs on source

11. Charlottesville, November 2010 11 Science Verification Observing Modes: Galactic: “Line Forest” G34.26+0.15 Band 3 Single 2 GHz Spectral Window

12. Charlottesville, November 2010 12 Science Verification Observing Modes: Extragalactic: Faint Continuum (High z) Also testing multiple science targets in SB with single phase calibrator -- Oct 10, 2010 SHADES SDXF 850.1, 3 and 5 at 345 GHz

13. Charlottesville, November 2010 13 Science Verification Observing Modes: Extragalactic: High Redshift Line Sources C[II] line in BRI 0952 at z=4.4 Band 7 16 th Nov 2010 ↑ ← APEX

14. Charlottesville, November 2010 14 Science Verification Observing Modes: Galactic: Faint Continuum (Debris Disk)  Pictoris Herschel ↓ 70 microns ALMA Band 7 ↓ (11 th Nov)

15. Charlottesville, November 2010 15 What’s next?

16. Charlottesville, November 2010 16 Science Verification Process: Start with suggestions from users (you!) Create Scheduling Blocks using “Science Goals” in OT Run SBs in the most efficient way possible Fill data to CASA and reduce manually Determine whether appropriate sensitivity level reached Review calibration strategies Rerun if sensitivity not adequate or calibration needs improvement Tweak up control scripts as necessary to deal with new observing modes and calibration strategies Provide additional feedback to CIPT on OT and control scripts Discuss results and images with PS and Director Release approved images through the EPO Group Release approved data through ARCs

17. Charlottesville, November 2010 17 Early Science Requirements (“Cycle 0”) 16 x 12m antenna array, no ACA 18 - 250m baselines, 2 configurations Single field imaging Bands 3, 6, 7 & 9 (no bands 4 or 8) Full set of spectral modes Full Stokes parameters on axis, 1% calibration Mosaicing and/or zero-spacing possible No subarrays, no special modes

18. 18 Spectral modes for Cycle 0 The number in each cell shows the number of polarization products provided: 1 – single pol, 2 – both polarizations, 4 – Full Stokes. FDM modesResolution (kHz)→ Band-MHz7.615.330.561122244488977 width2000 124 ↓1000 124 500 124 250 124 125 124 62.5124 TDM modesResolution (MHz) → Band-MHz7.815.631.3 width2000124

19. 19 Best Efforts (shared risk) Limited set of capabilities Aim to complete projects with good u,v coverage, which may mean fewer projects started JAO will conduct Quality Assurance to a lesser extent than in full operations PIs will need to contribute to data processing and to Quality Assurance (Astronomers with little experience in millimeter interferometry are recommended to seek expert collaborators - help available at JAO as well as ARCs and nodes)

20. 20 Early Science Cycle 0 8 month initial cycle 500-700 hours array time for Early Science Expect around 100 successful proposals Average allocation per proposal likely to be 5-7 hours (with a wide range)

21. 21 Optimal projects for Cycle 0 Well matched to Cycle 0 capabilities Scientifically worthwhile & publishable outcomes from Cycle 0 observations Produce images/spectra from observations of ~8 hours or less Exploit ALMA’s unique capabilities

22. Charlottesville, November 2010 22 *Tentative* schedule 1Jan 2011Call for SV suggestions and Pre-announcement of ES 2Feb 2011 3Mar 201131-ish Call for Proposals 4Apr 2011 5May 2011 6Jun 20111-ish Opening of Archive 30-ish Deadline for Proposals 7Jul 2011 8Aug 2011 9Sep 201130 th Start Cycle 0 10Oct 2011Cycle 0 11Nov 2011Cycle 0 12Dec 2011Cycle 0 1Jan 2012Cycle 0 2Feb 2012Engineering shutdown? 1? : Call for Proposals Cycle 1 3Mar 2012Cycle 0 31?: Deadline for Proposals 4Apr 2012Cycle 0 5May 2012Cycle 0 6Jun 201230-ish End Cycle 0

23. Charlottesville, November 2010 23 The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan. ALMA construction and operations are led on behalf of Europe by ESO, on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.