1. 64th International Symposium on Molecular Spectroscopy June 22 - 26, 2009 – Columbus, Ohio MOLECULAR SPECTROSCOPY AND THE ATACAMA LARGE MILLIMETER/SUBMILLIMETER ARRAY (ALMA) Anthony J. Remijan (Commissioning Liaison/NAASC)

2. ALMA Outline: Review the ALMA Progress including Scientific Support at the NAASC Overview of the ALMA Correlator and Examples of Observing Modes – along with a warning! Discuss the NAASC effort and vision for a Molecular Spectroscopy Database (Splatalogue) Do this all in 13 mins!

3. ALMA The ALMA Partnership ALMA is a global partnership in astronomy to deliver a truly transformational instrument – North America (US, Canada, Taiwan) – Europe (via ESO) – East Asia (Japan, Taiwan) Located on the Chajnantor plain of the Chilean Andes at 16500’ ALMA will be operated as a single Observatory with scientific access via regional centers – North American ALMA Science Center (NAASC) is in Charlottesville, VA The NSB approved budget for ALMA is $499.3M – Total Global Budget ~$1.3B 3

4. ALMA ALMA Funding:

5. ALMA Push to Early Science Interferometry at 2900m June 2009 and onwards – Move past accomplishments at the ATF – Production equipment, for the most part – Still one baseline Antennas exiting AIV phases moved to 5000m Aug/Sep 2009 Interferometry at 5000m Nov/Dec 2009 – Beginning of Commissioning and Science Verification – First use of LO, correlators, B8, B9 and eventually B10 Call for Early Science Proposals Dec 2010 Early Science Q4 FY2011 5

6. ALMA Requirements Buildings/Roads/Foundations 3 Antennas Transporter 3 Front Ends 3 Back Ends LO Correlator Software End to End Connectivity 6

7. ALMA Requirements Buildings/Roads/Foundations 3 Antennas Transporter 3 Front Ends 3 Back Ends LO Correlator Software End to End Connectivity 7

8. ALMA OSF 8

9. ALMA AOS 9

10. ALMA Requirements Buildings/Roads/Foundations 3 Antennas Transporter 3 Front Ends 3 Back Ends LO Correlator Software End to End Connectivity 10

11. ALMA Four MELCO Antennas being tested (non-interferometrically!) 11

12. ALMA Two Vertex Antennas under test – Seven more being assembled 12

13. ALMA EU Antennas 13

14. ALMA Requirements Buildings/Roads/Foundations 3 Antennas Transporter 3 Front Ends 3 Back Ends LO Correlator Software End to End Connectivity 14

15. ALMA 15 Transporters coming past the valley of moon

16. ALMA 16

17. ALMA Requirements Buildings/Roads/Foundations 3 Antennas Transporter 3 Front Ends 3 Back Ends LO Correlator Software End to End Connectivity 17

18. ALMA Bands 3 (84-116 GHz), 6 (211-275 GHz), 7 (275-373 GHz), and 9 (602-720 GHz) 18

19. ALMA Band 10 Cartridge Pre-prototype Cartridge (Engineering model) Successfully achieved the ALMA specifications!! 19

20. ALMA Requirements Buildings/Roads/Foundations 3 Antennas Transporter 3 Front Ends 3 Back Ends LO Correlator Software End to End Connectivity 20

21. ALMA Correlator 2 Antenna Correlator used at ATF, now installed at OSF ACA correlator installed at AOS Q1 of the bilateral correlator at the AOS

22. ALMA Correlator Modes - baseband pairs from antennas are 2 GHz wide - 4 baseband pairs are independently tunable 4 GHz8 GHz4 GHz e.g., Band 3: LSBUSB 1 2 3 4 o LO1

23. ALMA Correlator Modes The ALMA Correlator: - 32 main racks with 3,000 printed circuit cards - 32 main racks with 3,000 printed circuit cards - a total of 135,000 complex integrated circuits - a total of 135,000 complex integrated circuits - factor of 15,000 larger than the VLA correlator - factor of 15,000 larger than the VLA correlator - overall system dissipation: 170,000 W - overall system dissipation: 170,000 W one quadrant station rackcorrelator rack power supply computer

24. ALMA Correlator Modes

25. ALMA Correlator Modes

26. ALMA Correlator Modes

27. ALMA Correlator Modes (Examples) Example of Time Division Modes (Band 6): - 1 quadrant observes 2 GHz of LSB (230-232 GHz), 2 polzns, 2-bit, Nyq., get 128 spectral points each 15.6 MHz wide - 1 quadrant observes 2 GHz of LSB (232-234 GHz), 4 polzns, 2-bit, Nyq., get 64 spectral points each 31.25 MHz wide - 1 quadrant observes 2 GHz of USB (246-248 GHz), 2 polzns, 2-bit, Nyq., get 128 spectral points each 15.6 MHz wide - 1 quadrant observes 2 GHz of USB (248-250 GHz), 4 polzns, 2-bit, Nyq., get 64 spectral points each 31.25 MHz wide

28. ALMA Correlator Modes Example of Frequency Division Modes (Band 6): - 1 quadrant observes (in USB) CO 2-1 at 230.538 GHz over 125 MHz; mode 61 yields 512 spectral points with 0.32 125 MHz; mode 61 yields 512 spectral points with 0.32 km s -1 resolution, 2 polzns, 4-bit, 2 x Nyq. km s -1 resolution, 2 polzns, 4-bit, 2 x Nyq. - 1 quadrant observes (in LSB) C 18 O 2-1 at 219.560 GHz over 31.25 MHz; mode 63 yields 1024 spectral points with 0.04 31.25 MHz; mode 63 yields 1024 spectral points with 0.04 km s -1 resolution, 2 polzns, 4-bin, 2 x Nyq. km s -1 resolution, 2 polzns, 4-bin, 2 x Nyq. - 2 quadrants observe continuum over 2 GHz each (one in USB, one in LSB) in time division mode; mode 69 yields 128 USB, one in LSB) in time division mode; mode 69 yields 128 spectral points, 20.4 km s -1 resolution, 2 polzns, 2-bit, Nyq. spectral points, 20.4 km s -1 resolution, 2 polzns, 2-bit, Nyq.

29. ALMA Correlator Modes Example of Multiple Region Modes (Band 6): - 1 quadrant observes (in USB) uses mode 47, 125 GHz BW, 1024 spectral points at 0.16 km s -1 SR, 2 polzns, 4-bit, Nyq.: 1024 spectral points at 0.16 km s -1 SR, 2 polzns, 4-bit, Nyq.: 1/4 for CO 2-1 at 230.5 GHz, 1/4 for CO 2-1 at 230.5 GHz, 1/4 for N 2 D+ 3-2 at 231.3 GHz, 1/4 for N 2 D+ 3-2 at 231.3 GHz, 1/4 for CH 3 OH 8 -1 -7 0 E at 229.8 GHz, 1/4 for CH 3 OH 8 -1 -7 0 E at 229.8 GHz, 1/4 for SO 2 11(5,7) - 12(4,8) at 229.3 GHz, 1/4 for SO 2 11(5,7) - 12(4,8) at 229.3 GHz, for 4 windows each with 256 spectral points (BW: 164 km s -1 ) for 4 windows each with 256 spectral points (BW: 164 km s -1 ) - 1 quadrant observes (in LSB) C 18 O 2-1, 13 CO 2-1, SO 5 6 -4 5 and CH 3 OH 8 0 -7 1 E also in mode 47, as above CH 3 OH 8 0 -7 1 E also in mode 47, as above - 2 quadrants: LSB/USB continuum in time division mode (69)

30. ALMA This is all very challenging, but it is important to figure it all out before proposals are written! “I think anyone who does not take full advantage of the correlator deserves to be publicly ridiculed.” - Anonymous

31. ALMA ALMA Operations: Three ALMA Regional Centers - ARCs Joint ALMA Observatory (Chile) EU ARC (ESO) EA ARC (NAOJ + ASIAA) ARCs provide basic user interface, as well as basic archive, software, and hardware maintenance and development EU ARC nodes NAASC Full Science Support Services Full Science Support is needed to provide advanced user support, algorithm development, student programs, EPO, etc NA ARC (NRAO+ NRC + ASIAA)

32. ALMA NA ARC Core support Proposal and Scheduling Functions: –Review and evaluate the Observing Tool –Issue call for proposals and assist proposers –Support JAO with international proposal review process –Provide assistance to users in generating observe files –Verify and correct schedule blocks –Provide user-friendly documentation User Science Support: –Participate in Commissioning and Science Verification –Review and evaluate the pipeline and off-line data reduction software, cookbooks, and web pages –OSF staffing: “Astronomer-on-Duty” –Quality assurance and user feedback to OSF –Post-observation user support via helpdesk Archive support: –Operate NA ALMA Archive (>180 Tbytes per year) –Distribute full uv data sets and pipeline products to user –Operate regional pipeline –Provide interface to the VO

33. ALMA NAASC additional functions: Coordination of Canadian and Taiwanese contributions to NA ALMA operations Scientific Workshops – venues to explore future directions for ALMA NA ALMA EPO Science support development activities –Splatalogue –Enhanced simulations Advanced data processing and data analysis user support Enhanced science archive / IVOA functionality Special development projects –Support of UVa Microfabrication Laboratory for high-frequency SIS mixer design & fabrication

34. ALMA –The concept for Splatalogue was built on a need for specifically ALMA to have the most up-to-date and complete spectral line catalog. –The current way telescopes include catalogs is to download a publicly available line list and import it into Observing tool Proposal tool Data reduction tool (GBDish, GBTIDL, CASA, MIRIAD) –This is problematic because there are pros and cons associated with each list (e.g. Lovas NIST only observed lines). So, why not include all of them all AND lists from others around the world? –More often than not, there is very little management of the catalogs by the developers of these tools.

35. ALMA The molecular spectral line data that are currently “inside” Splatalogue are those which are made publically available and maintained by the following 3 groups: – The Jet Propulsion Laboratory Molecular Spectroscopy: http://spec.jpl.nasa.gov/ – The Cologne Database of Molecular Spectroscopy: http://www.ph1.uni-koeln.de/vorhersagen/ – The National Institute of Standards and Technology Lovas List: http://physics.nist.gov/cgi-bin/micro/table5/start.pl In addition, Frank Lovas has contributed his “Spectral Line Database of Interstellar Molecules” (SLAIM) list. Future updates to SLAIM or to the Lovas/NIST list will be available only through Splatalogue. Point to emphasize – this tool would not be available/possible without the efforts of these and similar laboratory efforts!

36. ALMA Splatalogue: CO example

37. ALMA Splatalogue: frequency search

38. ALMA JPL Splatalogue CDMS Lovas/NIST SLAIM Recomb ToyaMA WWW JPL+ CDMS+ WWW Currently Available Public Molecular Spectral Line Databases & Interfaces ToyaMA+ NRAO Rec Freq Other Apps API Software applications ALMA Archive SLAP protocol ALMA OT Astronomers

39. ALMA Splatalogue in the ALMA OT

40. ALMA JPL Splatalogue CDMS Lovas/ NIST SLAIM Recomb ToyaMA WWW NRAO Rec Freq Other Apps JPL+ CDMS+ WWW Molecular Spectral Line Databases & Interfaces in the VO Era (A model) VO applications e.g.: NRAO Rec Freq VO app VO Queries (Users or applications) (requires VO spectral line standard) ToyaMA+ API NRAO Rec Freq ALMA/Herschel Generated Databases Astronomers Software applications ALMA ArchiveALMA OT ALMA/Herschel Generated Databases ALMA/Herschel Generated Databases

41. ALMA Advanced Tools for Lab Spectroscopy Advanced Tools for Astronomy Lab Spectroscopy Spectral Line Database(s) Collisional Cross Sections Radiative Transfer Molecular Theory Source Editor (geometry, structure) VO Queries (Users or applications)

42. ALMA Future efforts and action items: – Splatalogue v2.0 will be available ~July 1, 2009. Updates to the database will include The Toyama Microwave Atlas. Special Thanks to Kaori Kobayashi! An API to allow programs to access the database Full VO compliance via the SLAP standard. Working with the developers of the VO to enhance the SLAP protocol. Want to track/see the changes? – easy access to v1.0. – The ALMA OT and CASA will need an “offline” version. Need to decide on: Carry only detected transitions? Carry only transitions of known molecules? Other ideas? To provide input or contribute to the effort contact: Anthony Remijan – aremijan@nrao.eduaremijan@nrao.edu Andrew Markwick – Andrew.Markwick-kemper@manchester.ac.ukAndrew.Markwick-kemper@manchester.ac.uk

43. ALMA ALMA is nearly here! Are we Ready? D. Barkats