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dc.contributorVirginia Techen
dc.contributor.authorLazio, T. J. W.en
dc.contributor.authorFey, A. L.en
dc.contributor.authorDennison, B.en
dc.contributor.authorMantovani, F.en
dc.contributor.authorSimonetti, John H.en
dc.contributor.authorAlberdi, A.en
dc.contributor.authorFoley, A. R.en
dc.contributor.authorFiedler, R.en
dc.contributor.authorGarrett, M. A.en
dc.contributor.authorHirabayashi, H.en
dc.contributor.authorJauncey, D. L.en
dc.contributor.authorJohnston, K. J.en
dc.contributor.authorMarcaide, J.en
dc.contributor.authorMigenes, V.en
dc.contributor.authorNicolson, G. D.en
dc.contributor.authorVenturi, T.en
dc.date.accessioned2014-03-10T13:18:51Zen
dc.date.available2014-03-10T13:18:51Zen
dc.date.issued2000-05en
dc.identifier.citationT. Joseph W. Lazio et al. 2000 ApJ 534 706 doi:10.1086/308779en
dc.identifier.issn0004-637Xen
dc.identifier.urihttp://hdl.handle.net/10919/25854en
dc.description.abstractWe report multiepoch VLBI observations of the source PKS 1741-038 (OT 068) as it underwent an extreme scattering event (ESE). Observations at four epochs were obtained, and images were produced at three of these. One of these three epochs was when the source was near the minimum flux density of the ESE, the other two were as the flux density of the source was returning to its nominal value. The fourth epoch was at the maximum flux density during the egress from the ESE, but the VLBI observations had too few stations to produce an image. During the event the source consisted of a dominant, compact component, essentially identical to the structure seen outside the event. However, the source's diameter increased slightly at 13 cm, from near 0.6 mas outside the ESE to near 1 mas during the ESE. An increase in the source's diameter is inconsistent with a simple refractive model in which a smooth refractive lens drifted across the line of sight to PKS 1741-038. We also see no evidence for ESE-induced substructure within the source or the formation of multiple images, as would occur in a strongly refractive lens. However, a model in which the decrease in flux density during the ESE occurs solely because of stochastic broadening within the lens requires a larger broadening diameter during the event than is observed. Thus, the ESE toward PKS 1741-038 involved both stochastic broadening and refractive defocusing within the lens. If the structure responsible for the ESE has a size of order I AU, the level of scattering within an ESE lens may be a factor of 10(7) larger than that in the ambient medium. A filamentary structure could reduce the difference between the strength of scattering in the lens and ambient medium, but there is no evidence for a refractively induced elongation of the source. We conclude that, if ESEs arise from filamentary structures, they occur when the filamentary structures are seen lengthwise. We are able to predict the amount of pulse broadening that would result from a comparable lens passing in front of a pulsar. The pulse broadening would be no more than 1.1 mu s, consistent with the lack of pulse broadening detected during ESEs toward the pulsars PSR B1937+21 and PSR J1643-1224. The line of sight toward PKS 1741-038 is consistent with a turbulent origin for the structures responsible for ESEs. The source PKS 1741-038 lies near the radio Loop I and is seen through a local minimum in 100 mu m emission.en
dc.language.isoen_USen
dc.publisherIOP PUBLISHING LTDen
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectism : generalen
dc.subjectquasars : individual (1741-038)en
dc.subjectradio continuum : ismen
dc.subjectscatteringen
dc.subjectreference frame sourcesen
dc.subjectcompact radio-sourcesen
dc.subjectinterstellar-mediumen
dc.subjectplasmaen
dc.subjectscintillationen
dc.subjectspectrumen
dc.subjectdensityen
dc.subjectmhzen
dc.titleThe Extreme Scattering Event toward PKS 1741-038: VLBI Imagesen
dc.typeArticle - Refereeden
dc.contributor.departmentInstitute for Particle, Nuclear and Astronomical Sciences (IPNAS)en
dc.contributor.departmentPhysicsen
dc.identifier.urlhttp://iopscience.iop.org/0004-637X/534/2/706/en
dc.date.accessed2014-02-28en
dc.title.serialAstrophysical Journalen
dc.identifier.doihttps://doi.org/10.1086/308779en


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