{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360004233289579648.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2011rs004694"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2011RS004694"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2011RS004694"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"A newly developed UHF radiotelescope for interplanetary scintillation observations: Solar Wind Imaging Facility"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>A large‐aperture radiotelescope called the Solar Wind Imaging Facility (SWIFT) has been developed at the Toyokawa Observatory of the Solar‐Terrestrial Environment Laboratory (STEL), Nagoya University. The SWIFT is dedicated to interplanetary scintillation (IPS) observations of the solar wind at 327 MHz, the same frequency as that of the existing STEL IPS system. The aim of this instrument is to improve the spatial and temporal resolutions of tomographic reconstructions from STEL IPS observations by increasing the number of usable lines of sight within a given time period. The SWIFT consists of a pair of asymmetric cylindrical parabolic reflector antennas with an aperture size of 108 m (N‐S) by 19 m (E‐W), and a 192‐element phased array receiver system which forms a single beam steerable between 60°S and 30°N with respect to the zenith. Since the antenna beam is fixed in the local meridian, IPS observations are taken around the time of meridian transit for each source. The performance of the SWIFT has been tested using preliminary observations for strong discrete sources and diffuse galactic background.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004233289579526","@type":"Researcher","foaf:name":[{"@value":"M. Tokumaru"}],"jpcoar:affiliationName":[{"@value":"Solar‐Terrestrial Environment Laboratory Nagoya University  Nagoya Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004233289579655","@type":"Researcher","foaf:name":[{"@value":"M. Kojima"}],"jpcoar:affiliationName":[{"@value":"Solar‐Terrestrial Environment Laboratory Nagoya University  Nagoya Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004233289579392","@type":"Researcher","foaf:name":[{"@value":"K. Fujiki"}],"jpcoar:affiliationName":[{"@value":"Solar‐Terrestrial Environment Laboratory Nagoya University  Nagoya Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004233289579652","@type":"Researcher","foaf:name":[{"@value":"K. Maruyama"}],"jpcoar:affiliationName":[{"@value":"Solar‐Terrestrial Environment Laboratory Nagoya University  Nagoya Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004233289579654","@type":"Researcher","foaf:name":[{"@value":"Y. Maruyama"}],"jpcoar:affiliationName":[{"@value":"Solar‐Terrestrial Environment Laboratory Nagoya University  Nagoya Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004233289579648","@type":"Researcher","foaf:name":[{"@value":"H. Ito"}],"jpcoar:affiliationName":[{"@value":"Solar‐Terrestrial Environment Laboratory Nagoya University  Nagoya Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004233289579650","@type":"Researcher","foaf:name":[{"@value":"T. Iju"}],"jpcoar:affiliationName":[{"@value":"Solar‐Terrestrial Environment Laboratory Nagoya University  Nagoya Japan"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00486604"},{"@type":"EISSN","@value":"1944799X"}],"prism:publicationName":[{"@value":"Radio Science"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2011-08-25","prism:volume":"46","prism:number":"5","prism:startingPage":"RS0F02"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2011RS004694"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2011RS004694"}],"createdAt":"2011-08-05","modifiedAt":"2023-10-31","project":[{"@id":"https://cir.nii.ac.jp/crid/1040282257046928000","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"21340140"},{"@type":"JGN","@value":"JP21340140"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-21340140/"}],"notation":[{"@language":"ja","@value":"第24太陽活動極小期における特異太陽風構造の解明"},{"@language":"en","@value":"STUDY OF PECULIAR SOLAR WIND STRUCTURE AT CYCLE 24 SOLAR MINIMUM"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050001338805701632","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Plasma distribution of Comet ISON (C/2012 S1) observed using the radio scintillation method"}]},{"@id":"https://cir.nii.ac.jp/crid/1050295336679601280","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Interplanetary Scintillation Observations of Solar-Wind Disturbances During Cycles 23 and 24"}]},{"@id":"https://cir.nii.ac.jp/crid/1050564288758236928","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"North-south asymmetry in global distribution of the solar wind speed during 1985–2013"},{"@value":"North‐south asymmetry in global distribution of the solar wind speed during 1985–2013"}]},{"@id":"https://cir.nii.ac.jp/crid/1050845763733650304","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs"}]},{"@id":"https://cir.nii.ac.jp/crid/1360008373646758784","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Design of an asymmetric parabolic cylinder antenna with high aperture efficiency"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011143708599808","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Heliospheric tomography using interplanetary scintillation observations: 3. 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