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hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBAUDRY, Alain
dc.contributor.authorLACASSE, Richard
dc.contributor.authorESCOFFIER, Ray
dc.contributor.authorWEBBER, John
dc.contributor.authorGREENBERG, Joseph
dc.contributor.authorPLATT, Laurence
dc.contributor.authorTREACY, Robert
dc.contributor.authorSAEZ, Alejandro F.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorCAIS, Ph.
dc.contributor.authorCOMORETTO, Giovanni
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorQUERTIER, Benjamin
dc.contributor.authorOKUMURA, Sachiko K.
dc.contributor.authorKAMAZAKI, Takeshi
dc.contributor.authorCHIKADA, Yoshihiro
dc.contributor.authorWATANABE, Manabu
dc.contributor.authorOKUDA, Takeshi
dc.contributor.authorKURONO, Yasutake
dc.contributor.authorIGUCHI, Satoru
dc.date.issued2012-09
dc.date.conference2012
dc.identifier.issn0164-9655
dc.description.abstractEnTwo large correlators have been constructed to combine the signals captured by the ALMA antennas deployed on the Atacama Desert in Chile at an elevation of 5050 meters. The Baseline correlator was fabricated by a NRAO/European team to process up to 64 antennas for 16 GHz bandwidth in two polarizations and another correlator, the Atacama Compact Array (ACA) correlator, was fabricated by a Japanese team to process up to 16 antennas. Both correlators meet the same specifications except for the number of processed antennas. The main architectural differences between these two large machines will be underlined. Selected features of the Baseline and ACA correlators as well as the main technical challenges met by the designers will be briefly discussed. The Baseline correlator is the largest correlator ever built for radio astronomy. Its digital hybrid architecture provides a wide variety of observing modes including the ability to divide each input baseband into 32 frequency-mobile sub-bands for high spectral resolution and to be operated as a conventional 'lag' correlator for high time resolution. The various observing modes offered by the ALMA correlators to the science community for 'Early Science' are presented, as well as future observing modes. Coherently phasing the array to provide VLBI maps of extremely compact sources is another feature of the ALMA correlators. Finally, the status and availability of these large machines will be presented.
dc.language.isoen
dc.publisherPrism Business Media
dc.source.titleMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI. Proceedings of the SPIE, Volume 8452, id. 845217-845217-14 (2012) Amsterdam 3-6 July, 2012
dc.title.enPerformance highlights of the ALMA correlators
dc.typeCommunication dans un congrès
dc.identifier.doi10.1117/12.925700
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
bordeaux.journalMillimeter
bordeaux.page17
bordeaux.volume8452
bordeaux.countryNL
bordeaux.title.proceedingMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI. Proceedings of the SPIE, Volume 8452, id. 845217-845217-14 (2012) Amsterdam 3-6 July, 2012
bordeaux.conference.cityAmsterdam
bordeaux.peerReviewedoui
hal.identifierhal-00752220
hal.version1
hal.invitednon
hal.proceedingsoui
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00752220v1
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