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In The Quest For Stokes V - Science Cases And Technical Challenges

hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorWIESEMEYER, Helmut
dc.contributor.authorAGUDO, I.
hal.structure.identifierFORMATION STELLAIRE 2017
dc.contributor.authorBAUDRY, Alain
dc.contributor.authorDOWNES, D.
hal.structure.identifierMax Planck Institute for Radio Astronomy
dc.contributor.authorGÜSTEN, R.
hal.structure.identifierFORMATION STELLAIRE 2017
dc.contributor.authorHERPIN, Fabrice
hal.structure.identifierAquatic Contaminant Research Division
dc.contributor.authorHOUDE, M.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorKREYSA, E.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMAURY, A.
dc.contributor.authorMENTEN, K.
hal.structure.identifierRedZinc Services Ltd.[Dublin]
dc.contributor.authorMORRIS, D.
hal.structure.identifierImmunologie des maladies infectieuses allergiques et autoimmunes
dc.contributor.authorNAVARRO, S.
dc.contributor.authorPAUBERT, G.
dc.contributor.authorPILLAI, T.
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorTHUM, C.
hal.structure.identifierDépartement de Physique
dc.contributor.authorWEISS, A.
dc.date.conference2017-10-25
dc.description.abstractEnCircular polarization is produced either in the emission process through the Zeeman effect, or through the transfer of polarized radiation in a magneto-active medium. While the former mechanism provides a direct access to the strength of the magnetic field along the sightline, the conversion of linear to circular polarization reveals particular magnetic field structures or magnetospheric events. In the first part I will present selected science cases. While Stokes V may be strong in OH masers forming in supernova remnants, the Zeeman effect becomes weaker in masers associated with star-forming environments or circumstellar envelopes. As masers probe restricted physical conditions, the Zeeman effect in thermal lines is a valuable analysis tool, but even more difficult to measure. In particular, the instrumental leakage from linear to circular polarization frequently exceeds the intrinsic Stokes V. This statement also holds for the Faraday conversion in AGN. A correction for instrumental polarization across the field of view is thus essential, but hindered by the lack of suitable calibrators. In the second part I will propose calibration schemes for both the image and UV plane.
dc.language.isoen
dc.title.enIn The Quest For Stokes V - Science Cases And Technical Challenges
dc.typeCommunication dans un congrès
dc.identifier.doi10.5281/zenodo.1038109
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
bordeaux.conference.titleSubmm/mm/cm QUESO Workshop 2017 (QUESO2017), Centimetre-Sub-Millimetre Q&U (and V) European Southern Observatory Workshop, held 25-27 October, 2017 at ESO, Garching bei München, Germany.
bordeaux.countryDE
bordeaux.conference.cityGarching bei München
bordeaux.peerReviewedoui
hal.identifierhal-01633769
hal.version1
hal.invitednon
hal.proceedingsnon
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01633769v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.au=WIESEMEYER,%20Helmut&AGUDO,%20I.&BAUDRY,%20Alain&DOWNES,%20D.&G%C3%9CSTEN,%20R.&rft.genre=unknown


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