64th International Symposium on Molecular Spectroscopy June 22 - 26, 2009 – Columbus, Ohio...

64th International Symposium on Molecular 64th International Symposium on Molecular SpectroscopySpectroscopy

June 22 - 26, 2009 – Columbus, Ohio

MOLECULAR SPECTROSCOPY AND THE ATACAMA LARGE MILLIMETER/SUBMILLIMETER ARRAY (ALMA)

Anthony J. Remijan (Commissioning Liaison/NAASC)

ALMAOutline:

• 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!

ALMAThe 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

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ALMAALMA Funding:

ALMAPush 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

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ALMARequirements

• Buildings/Roads/Foundations• 3 Antennas• Transporter• 3 Front Ends• 3 Back Ends• LO• Correlator• Software• End to End Connectivity

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ALMARequirements


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ALMAOSF

8

ALMAAOS

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ALMARequirements


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ALMAFour MELCO Antennas being tested (non-interferometrically!)

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ALMATwo Vertex Antennas under test – Seven more being assembled

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ALMAEU Antennas

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ALMARequirements


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ALMA

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Transporters coming past the valley of moon

ALMA

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ALMARequirements


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ALMABands 3 (84-116 GHz), 6 (211-275 GHz), 7 (275-373 GHz), and 9 (602-720 GHz)

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ALMABand 10 Cartridge

Pre-prototype Cartridge (Engineering model)

780 800 820 840 860 880 900 920 940 9600

50100150200250300350400450500550600

Unc

orre

cted

Trx

(K

)

LO frequency (GHz)

Measured Spec 100% Spec 80%

230 K

344 K

Successfully achieved the ALMA specifications!!19

ALMARequirements


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ALMACorrelator

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

ALMACorrelator ModesCorrelator Modes

- baseband pairs from antennas are 2 GHz widebaseband pairs from antennas are 2 GHz wide- 4 baseband pairs are independently tunable4 baseband pairs are independently tunable

4 GHz 8 GHz 4 GHz

e.g., Band 3:

LSB USB

12 3

4

o

LO1


The ALMA Correlator: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 rack correlator rackpowersupply computer

ALMACorrelator Modes (Examples)Correlator Modes (Examples)

Example of Time Division Modes (Band 6):Example of Time Division Modes (Band 6):

- 1 quadrant observes 2 GHz of LSB (230-232 GHz), 2 polzns, 2-bit, Nyq., 1 quadrant observes 2 GHz of LSB (230-232 GHz), 2 polzns, 2-bit, Nyq., get get 128 spectral points each 15.6 MHz wide128 spectral points each 15.6 MHz wide

- 1 quadrant observes 2 GHz of LSB (232-234 GHz), 4 polzns, 2-bit, Nyq., 1 quadrant observes 2 GHz of LSB (232-234 GHz), 4 polzns, 2-bit, Nyq., get get 64 spectral points each 31.25 MHz wide64 spectral points each 31.25 MHz wide

- 1 quadrant observes 2 GHz of USB (246-248 GHz), 2 polzns, 2-bit, Nyq., 1 quadrant observes 2 GHz of USB (246-248 GHz), 2 polzns, 2-bit, Nyq., get get 128 spectral points each 15.6 MHz wide128 spectral points each 15.6 MHz wide

- 1 quadrant observes 2 GHz of USB (248-250 GHz), 4 polzns, 2-bit, Nyq., 1 quadrant observes 2 GHz of USB (248-250 GHz), 4 polzns, 2-bit, Nyq., get get 64 spectral points each 31.25 MHz wide64 spectral points each 31.25 MHz wide


Example of Frequency Division Modes (Band 6):Example of Frequency Division Modes (Band 6):

- 1 quadrant observes (in USB) 1 quadrant observes (in USB) CO 2-1 at 230.538 GHzCO 2-1 at 230.538 GHz over over 125 MHz; mode 61 yields 512 spectral points with 0.32 125 MHz; mode 61 yields 512 spectral points with 0.32 km skm s-1-1 resolution, 2 polzns, 4-bit, 2 x Nyq. resolution, 2 polzns, 4-bit, 2 x Nyq.

- 1 quadrant observes (in LSB) 1 quadrant observes (in LSB) CC1818O 2-1 at 219.560 GHzO 2-1 at 219.560 GHz over 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 skm s-1-1 resolution, 2 polzns, 4-bin, 2 x Nyq. resolution, 2 polzns, 4-bin, 2 x Nyq.

- 2 quadrants observe 2 quadrants observe continuumcontinuum over 2 GHz each (one in 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 sspectral points, 20.4 km s-1-1 resolution, 2 polzns, 2-bit, Nyq. resolution, 2 polzns, 2-bit, Nyq.


Example of Multiple Region Modes (Band 6):Example of Multiple Region Modes (Band 6):

- 1 quadrant observes (in USB) uses mode 47, 125 GHz BW, 1 quadrant observes (in USB) uses mode 47, 125 GHz BW, 1024 spectral points at 0.16 km s1024 spectral points at 0.16 km s-1-1 SR, 2 polzns, 4-bit, Nyq.: SR, 2 polzns, 4-bit, Nyq.: 1/4 for 1/4 for CO 2-1 at 230.5 GHzCO 2-1 at 230.5 GHz,, 1/4 for 1/4 for NN22D+ 3-2 at 231.3 GHzD+ 3-2 at 231.3 GHz,,

1/4 for 1/4 for CHCH33OH 8OH 8-1-1-7-700 E at 229.8 GHz E at 229.8 GHz,,

1/4 for 1/4 for SOSO22 11(5,7) - 12(4,8) at 229.3 GHz 11(5,7) - 12(4,8) at 229.3 GHz, ,

for 4 windows each with 256 spectral points (BW: 164 km sfor 4 windows each with 256 spectral points (BW: 164 km s -1-1))

- 1 quadrant observes (in LSB) 1 quadrant observes (in LSB) CC1818O 2-1, O 2-1, 1313CO 2-1, SO 5CO 2-1, SO 566-4-455 and and

CHCH33OH 8OH 800-7-711 E E also in mode 47, as above also in mode 47, as above

- 2 quadrants: LSB/USB 2 quadrants: LSB/USB continuumcontinuum in time division mode (69) in time division mode (69)

ALMA

This is all very challenging, but it is This is all very challenging, but it is important to figure it all out before important to figure it all out before

proposals are written!proposals are written!

““I think anyone who does not take full advantage of the correlator deserves to I think anyone who does not take full advantage of the correlator deserves to be publicly ridiculed.”be publicly ridiculed.” - Anonymous- Anonymous

ALMAALMA 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)

ALMANA 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

ALMANAASC 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

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.

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!

ALMASplatalogue: CO example

ALMASplatalogue: frequency search

ALMA

JPL

Splatalogue

CDMSLovas/NIST

SLAIM

Recomb ToyaMA

WWW

JPL+ CDMS+

WWW WWW WWW WWW

Currently Available Public Molecular Spectral Line Currently Available Public Molecular Spectral Line Databases & InterfacesDatabases & Interfaces

ToyaMA+NRAO Rec Freq

Other Apps

API

Softwareapplications

ALMA Archive

SLA

P p

roto

col

ALMA OTAstronomers

ALMASplatalogue in the ALMA OTSplatalogue in the ALMA OT

ALMA

JPL

Splatalogue

CDMS

Lovas/NIST

SLAIM

Recomb ToyaMA

WWW

NRAO Rec Freq

Other Apps

JPL+ CDMS+

WWW WWW WWW

Molecular Spectral Line Databases & Interfaces in the Molecular Spectral Line Databases & Interfaces in the VO Era (A model)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/HerschelGenerated Databases

AstronomersSoftware

applicationsALMA Archive ALMA OT

ALMA/HerschelGenerated DatabasesALMA/Herschel

Generated Databases

ALMAAdvanced Tools for Lab Spectroscopy

Advanced Tools for Astronomy

LabSpectroscopy

SpectralLine

Database(s)

CollisionalCross

Sections

RadiativeTransfer

Molecular Theory

Source Editor

(geometry, structure)

VO Queries (Users or applications)

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 – [email protected]

Andrew Markwick – [email protected]

ALMAALMA is nearly here!Are we Ready?

D. Barkats

64th International Symposium on Molecular Spectroscopy June 22 - 26, 2009 – Columbus, Ohio...

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