THAT004 DISTRIBUTED CONTROL SYSTEM FOR THE TEST
Bibliographic record
Abstract
The control system (TICS) for the test interferometer being built to support the development of the Atacama Large Millimeter Array (ALMA)[1] will itself be a prototype for the final ALMA array, providing a test for the distributed control system under development. TICS will be based on the ALMA Common Software (ACS)[2] (developed at the European Southern Observatory), which provides CORBAbased[3] services and a device management framework for the control software. Simple device controllers will run on single board computers, one of which (known as an LCU) is located at each antenna; whereas complex, compound device controllers may run on centrally located computers. In either circumstance, client programs may obtain direct CORBA references to the devices and their properties. Monitor and control requests are sent to devices or properties, which then process and forward the commands to the appropriate hardware devices as required. Timing requirements are met by tagging commands with (future) timestamps synchronized to a timing pulse, which is regulated by a central reference generator, and is distributed to all hardware devices in the array. Monitoring is provided through a publish/subscribe CORBA-based service. 1 ALMA The Atacama Large Millimeter Array, or ALMA, is a radio astronomy millimeter and sub-millimeter array to be built in Chile’s Atacama desert (at an elevation of 5000m above sea level) in the coming years. The project is an international collaboration among partners from Europe, Japan, Canada, Chile, and the USA. Current plans are for an array consisting of sixty-four parabolic antennas of twelve meter diameter, with configurations ranging in size from a compact configuration, with a maximum baseline of 150 m, to an extended configuration, with a maximum baseline of 10 km. Each of the antennas will contain from four to ten cryogenically cooled receivers, operating in the range from 31 GHz to 950 GHz. Science data will be digitized at each antenna, and transmitted via optical fiber to a central location at a rate of 3 GB/s per antenna.
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How this classification was reachedexpand
Full frame machine prediction
Teacher imitationNot calibrated prevalence, not ground truth. Human validation pending. The Gemma side is a direct model label for every work in the frame, read from the title-only record. The Codex side is a classifier learned from the 10,348 direct Codex labels and calibrated to design-weighted sample rates; fields without enough sample support carry no Codex call. Candidate is the union of the two sides; consensus is their intersection. These outputs are machine_predicted_unvalidated and are not human labels.
Distilled classifier scores by category (both heads)
| Category | Codex | Gemma |
|---|---|---|
| Metaresearch | 0.002 | 0.004 |
| Meta-epidemiology (narrow) | 0.001 | 0.000 |
| Meta-epidemiology (broad) | 0.001 | 0.001 |
| Bibliometrics | 0.002 | 0.002 |
| Science and technology studies | 0.001 | 0.001 |
| Scholarly communication | 0.004 | 0.003 |
| Open science | 0.003 | 0.003 |
| Research integrity | 0.002 | 0.002 |
| Insufficient payload (model declined to judge) | 0.073 | 0.048 |
Machine scores (provisional)
The two teacher heads of the student model, read on this work. A score orders the frame for review; it never asserts a category, and the validation status ships verbatim with every row.
Baseline scores from an immature model (maturity gate not passed, 7 training rounds). Scores rank; they never assert a category.
score_only:v0-immature-baseline · verbatim from the scoring run: score_only means the number may rank works, and no category label ships from itClassification
machine, unvalidatedMachine predicted; a candidate call from one source (direct Gemma or distilled Codex), not a consensus.
How this classification was reached, model by model and score by score, is at the end of the page under "How this classification was reached".