{"@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/1360002217423152000.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1088/0004-6256/149/2/60"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/1538-3881/149/i=2/a=60/pdf"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/1538-3881/149/i=2/a=60?key=crossref.5ea97678d2b2099cf2db91f30cb06e42"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1409.4151"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"COMPARISON OF ALGORITHMS FOR DETERMINATION OF ROTATION MEASURE AND FARADAY STRUCTURE. I. 1100–1400 MHZ"}],"description":[{"notation":[{"@value":"(abridged) We run a Faraday structure determination data challenge to benchmark the currently available algorithms including Faraday synthesis (previously called RM synthesis in the literature), wavelet, compressive sampling and $QU$-fitting. The frequency set is similar to POSSUM/GALFACTS with a 300 MHz bandwidth from 1.1 to 1.4 GHz. We define three figures of merit motivated by the underlying science: a) an average RM weighted by polarized intensity, RMwtd, b) the separation $����$ of two Faraday components and c) the reduced chi-squared. Based on the current test data of signal to noise ratio of about 32, we find that: (1) When only one Faraday thin component is present, most methods perform as expected, with occasional failures where two components are incorrectly found; (2) For two Faraday thin components, QU-fitting routines perform the best, with errors close to the theoretical ones for RMwtd, but with significantly higher errors for $����$. All other methods including standard Faraday synthesis frequently identify only one component when $����$ is below or near the width of the Faraday point spread function; (3) No methods, as currently implemented, work well for Faraday thick components due to the narrow bandwidth; (4) There exist combinations of two Faraday components which produce a large range of acceptable fits and hence large uncertainties in the derived single RMs; in these cases, different RMs lead to the same Q, U behavior, so no method can recover a unique input model."}]},{"notation":[{"@value":"15 pages, 8 figures, 5 tables, accepted by AJ. Some figures have been degraded, for a full resolution version, see http://physics.usyd.edu.au/~xhsun/datachallengeI.pdf"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380002217423152002","@type":"Researcher","foaf:name":[{"@value":"X. H. Sun"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855555","@type":"Researcher","foaf:name":[{"@value":"L. Rudnick"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855426","@type":"Researcher","foaf:name":[{"@value":"Takuya Akahori"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855557","@type":"Researcher","foaf:name":[{"@value":"C. S. Anderson"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855425","@type":"Researcher","foaf:name":[{"@value":"M. R. Bell"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855553","@type":"Researcher","foaf:name":[{"@value":"J. D. Bray"}]},{"@id":"https://cir.nii.ac.jp/crid/1380002217423152003","@type":"Researcher","foaf:name":[{"@value":"J. S. Farnes"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855559","@type":"Researcher","foaf:name":[{"@value":"S. Ideguchi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855558","@type":"Researcher","foaf:name":[{"@value":"K. Kumazaki"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855554","@type":"Researcher","foaf:name":[{"@value":"T. O’Brien"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855424","@type":"Researcher","foaf:name":[{"@value":"S. P. O’Sullivan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380002217423152001","@type":"Researcher","foaf:name":[{"@value":"A. M. M. Scaife"}]},{"@id":"https://cir.nii.ac.jp/crid/1380002217423152004","@type":"Researcher","foaf:name":[{"@value":"R. Stepanov"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855556","@type":"Researcher","foaf:name":[{"@value":"J. Stil"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855552","@type":"Researcher","foaf:name":[{"@value":"K. Takahashi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380002217423152000","@type":"Researcher","foaf:name":[{"@value":"R. J. van Weeren"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284920604855427","@type":"Researcher","foaf:name":[{"@value":"M. Wolleben"}]}],"publication":{"publicationIdentifier":[{"@type":"EISSN","@value":"15383881"}],"prism:publicationName":[{"@value":"The Astronomical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2015-01-19","prism:volume":"149","prism:number":"2","prism:startingPage":"60"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","dc:rights":["http://iopscience.iop.org/info/page/text-and-data-mining","http://iopscience.iop.org/page/copyright"],"url":[{"@id":"http://stacks.iop.org/1538-3881/149/i=2/a=60/pdf"},{"@id":"http://stacks.iop.org/1538-3881/149/i=2/a=60?key=crossref.5ea97678d2b2099cf2db91f30cb06e42"}],"createdAt":"2015-01-19","modifiedAt":"2020-11-06","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=polarization","dc:title":"polarization"},{"@id":"https://cir.nii.ac.jp/all?q=Cosmology%20and%20Nongalactic%20Astrophysics%20(astro-ph.CO)","dc:title":"Cosmology and Nongalactic Astrophysics (astro-ph.CO)"},{"@id":"https://cir.nii.ac.jp/all?q=radio%20continuum:%20general","dc:title":"radio continuum: general"},{"@id":"https://cir.nii.ac.jp/all?q=FOS:%20Physical%20sciences","dc:title":"FOS: Physical sciences"},{"@id":"https://cir.nii.ac.jp/all?q=magnetic%20fields","dc:title":"magnetic fields"},{"@id":"https://cir.nii.ac.jp/all?q=techniques:%20polarimetric","dc:title":"techniques: polarimetric"},{"@id":"https://cir.nii.ac.jp/all?q=ISM:%20magnetic%20fields","dc:title":"ISM: magnetic fields"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Instrumentation%20and%20Methods%20for%20Astrophysics","dc:title":"Astrophysics - Instrumentation and Methods for Astrophysics"},{"@id":"https://cir.nii.ac.jp/all?q=Instrumentation%20and%20Methods%20for%20Astrophysics%20(astro-ph.IM)","dc:title":"Instrumentation and Methods for Astrophysics (astro-ph.IM)"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Cosmology%20and%20Nongalactic%20Astrophysics","dc:title":"Astrophysics - Cosmology and Nongalactic Astrophysics"}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040282257402539008","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"12J05235"},{"@type":"JGN","@value":"JP12J05235"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-12J05235/"}],"notation":[{"@language":"ja","@value":"宇宙大規模構造を用いた初期宇宙の探査"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360002217600468096","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Interacting large-scale magnetic fields and ionized gas in the W50/SS433 system"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002217650995968","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Cosmic magnetism in centimeter- and meter-wavelength radio astronomy"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004234734783872","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Performance test of RM CLEAN and its evaluation with chi-square value"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004239486619008","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Strategy to Explore Magnetized Cosmic Web with Forthcoming Large Surveys of Rotation Measure"}]},{"@id":"https://cir.nii.ac.jp/crid/1360009142782097920","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"An iterative reconstruction algorithm for Faraday tomography"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011145306311936","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Recognizing magnetic structures by present and future radio telescopes with Faraday rotation measure synthesis"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011145488805632","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Detection Thresholds and Bias Correction in Polarized Intensity"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285709639009152","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Performance test of QU-fitting in cosmic magnetism study"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567189440042240","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Faraday Tomography Tutorial"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567189627279616","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Study of the Vertical Magnetic Field in Face-on Galaxies Using Faraday Tomography"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574094017058432","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"MAGNETIC FIELD STRUCTURE OF THE LARGE MAGELLANIC CLOUD FROM FARADAY ROTATION MEASURES OF DIFFUSE POLARIZED EMISSION"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848659664259712","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Properties of intrinsic polarization angle ambiguities in Faraday tomography"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848664416752768","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Faraday Tomography of the SS433 Jet Termination Region"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855568519916032","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Complex Faraday depth structure of active galactic nuclei as revealed by broad-band radio polarimetry"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855570782899072","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"MultiNest: an efficient and robust Bayesian inference tool for cosmology and particle physics"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855570796304000","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Observation of Turbulent Fluctuations in the Interstellar Plasma Density and Magnetic Field on Spatial Scales of 0.01 to 100 Parsecs"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855571090037760","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"SIMULATED FARADAY ROTATION MEASURES TOWARD HIGH GALACTIC LATITUDES"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855571324540800","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"WSRT Faraday tomography of the Galactic ISM at <i>λ</i> ~ 0.86 m"}]},{"@id":"https://cir.nii.ac.jp/crid/1361131644206744960","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Performance Test of QU-Fitting"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137043549888768","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FARADAY ROTATION MEASURE DUE TO THE INTERGALACTIC MAGNETIC FIELD. II. THE COSMOLOGICAL CONTRIBUTION"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137044190529408","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Faraday rotation measure synthesis for magnetic fields of galaxies"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137044350933504","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The origin and evolution of cosmic magnetism"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137044562869760","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A NEW MODEL OF THE GALACTIC MAGNETIC FIELD"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137045388601088","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"ANTISYMMETRY IN THE FARADAY ROTATION SKY CAUSED BY A NEARBY MAGNETIZED BUBBLE"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137045554349824","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"New<i>λ</i>6 cm and<i>λ</i>11 cm observations of the supernova remnant CTA 1"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137045846414464","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Polarized synchrotron radiation from the Andromeda galaxy M 31 and background sources at 350 MHz"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418519127229696","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"THERMAL PLASMA IN THE GIANT LOBES OF THE RADIO GALAXY CENTAURUS A"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418519608182784","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FARADAY ROTATION MEASURE DUE TO THE INTERGALACTIC MAGNETIC FIELD"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418520173694464","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FARADAY SIGNATURE OF MAGNETIC HELICITY FROM REDUCED DEPOLARIZATION"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418520466045568","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The NRAO VLA Sky Survey"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418520493177472","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The latitude dependence of the rotation measures of NVSS sources"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418520990706816","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Magnetic field tomography, helical magnetic fields and Faraday depolarization"}]},{"@id":"https://cir.nii.ac.jp/crid/1361699993569971712","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Faraday synthesis"}]},{"@id":"https://cir.nii.ac.jp/crid/1361699994517716864","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"ROTATION MEASURE SYNTHESIS OF GALACTIC POLARIZED EMISSION WITH THE DRAO 26-m TELESCOPE"}]},{"@id":"https://cir.nii.ac.jp/crid/1361699994521883904","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Simulated square kilometre array maps from Galactic  3D-emission models"}]},{"@id":"https://cir.nii.ac.jp/crid/1361699994957284096","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Multi-frequency polarimetry of the Galactic radio  background\n around 350 MHz"}]},{"@id":"https://cir.nii.ac.jp/crid/1361699995440273280","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Wavelet-based Faraday rotation measure synthesis"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981468657633152","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"MODELING THE MAGNETIC FIELD IN THE GALACTIC DISK USING NEW ROTATION MEASURE OBSERVATIONS FROM THE VERY LARGE ARRAY"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981469063589120","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"INTEGRATED POLARIZATION OF SOURCES AT λ ∼ 1 m AND NEW ROTATION MEASURE AMBIGUITIES"}]},{"@id":"https://cir.nii.ac.jp/crid/1362262943358493568","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Magnetic fields and spiral arms in the galaxy M51"}]},{"@id":"https://cir.nii.ac.jp/crid/1362544419320890752","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FARADAY ROTATION OF THE SUPERNOVA REMNANT G296.5+10.0: EVIDENCE FOR A MAGNETIZED PROGENITOR WIND"}]},{"@id":"https://cir.nii.ac.jp/crid/1362544420318083584","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A BROADBAND POLARIZATION CATALOG OF EXTRAGALACTIC RADIO SOURCES"}]},{"@id":"https://cir.nii.ac.jp/crid/1362825893800649728","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Improved CLEAN reconstructions for rotation measure synthesis with maximum likelihood estimation"}]},{"@id":"https://cir.nii.ac.jp/crid/1363107369680019840","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"SPARSE FARADAY ROTATION MEASURE SYNTHESIS"}]},{"@id":"https://cir.nii.ac.jp/crid/1363107370803577600","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Measurements and simulation of Faraday rotation across the Coma radio relic"}]},{"@id":"https://cir.nii.ac.jp/crid/1363388844418886400","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"THE EXTENT OF MAGNETIC FIELDS AROUND GALAXIES OUT TO\n                    <i>z</i>\n                    ∼ 1"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670318704155520","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A broad-band flux scale for low-frequency radio telescopes"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670318724296576","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"On the Depolarization of Discrete Radio Sources by Faraday Dispersion"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670318773696768","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"DERIVING THE GLOBAL STRUCTURE OF THE GALACTIC MAGNETIC FIELD FROM FARADAY ROTATION MEASURES OF EXTRAGALACTIC SOURCES"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670319070844544","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Depolarization and Faraday effects in galaxies"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670319818662400","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"MAGNETIC FIELDS IN LARGE-DIAMETER H II REGIONS REVEALED BY THE FARADAY ROTATION OF COMPACT EXTRAGALACTIC RADIO SOURCES"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670320046963072","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"THE DISTRIBUTION OF POLARIZED RADIO SOURCES >15 μJy IN GOODS-N"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670320261290112","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A ROTATION MEASURE IMAGE OF THE SKY"}]},{"@id":"https://cir.nii.ac.jp/crid/1363951794020562944","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Faraday rotation measure synthesis"}]},{"@id":"https://cir.nii.ac.jp/crid/1363951794207951616","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Multimodal nested sampling: an efficient and robust alternative to Markov Chain Monte Carlo methods for astronomical data analyses"}]},{"@id":"https://cir.nii.ac.jp/crid/1363951795716390016","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The application of compressive sampling to radio astronomy"}]},{"@id":"https://cir.nii.ac.jp/crid/1364233268211386112","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Westerbork SINGS survey"}]},{"@id":"https://cir.nii.ac.jp/crid/1364233268582588288","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A SURVEY OF EXTRAGALACTIC FARADAY ROTATION AT HIGH GALACTIC LATITUDE: THE VERTICAL MAGNETIC FIELD OF THE MILKY WAY TOWARD THE GALACTIC POLES"}]},{"@id":"https://cir.nii.ac.jp/crid/1364233268698212608","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"SPECTROPOLARIMETRY WITH THE ALLEN TELESCOPE ARRAY: FARADAY ROTATION TOWARD BRIGHT POLARIZED RADIO GALAXIES"}]},{"@id":"https://cir.nii.ac.jp/crid/1364233270971505280","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"MAGNETIZED GAS IN THE SMITH HIGH VELOCITY CLOUD"}]},{"@id":"https://cir.nii.ac.jp/crid/1370002217423152026","@type":"Product","relationType":["references"]},{"@id":"https://cir.nii.ac.jp/crid/1520854805141936384","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Exploring the intergalactic magnetic field by means of Faraday tomography"}]},{"@id":"https://cir.nii.ac.jp/crid/1523669555306504960","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Fisher analysis on wide-band polarimetry for probing the intergalactic magnetic field"}]},{"@id":"https://cir.nii.ac.jp/crid/1883679867987515264","@type":"Dataset","relationType":["isSupplementedBy"],"jpcoar:relatedTitle":[{"@value":"Modeling Faraday structures. I. 1100-1400 MHz"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1088/0004-6256/149/2/60"},{"@type":"KAKEN","@value":"PRODUCT-9408623"},{"@type":"OPENAIRE","@value":"doi_dedup___::6a618252c759320857a7cbd4b663afa9"},{"@type":"CROSSREF","@value":"10.1093/mnras/stx338_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.1093/pasj/psx123_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.1093/pasj/psw039_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.3390/galaxies6040118_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.1093/mnras/staa3580_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.1093/mnras/sty2862_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.3390/galaxies6040140_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.3847/1538-4357/aa79a1_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.3390/galaxies6040137_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"},{"@type":"CROSSREF","@value":"10.3390/galaxies7030069_references_DOI_Hw6ZV9cgEvOPmKeJalo9w0hAVEQ"}]}