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dc.contributor.authorMarti-Vidal, I.
dc.contributor.authorMarcaide, J.
dc.contributor.authorAlberdi, A.
dc.contributor.authorGuirado, J.
dc.contributor.authorPrez-Torres, M.
dc.contributor.authorRos, E.
dc.contributor.authorShapiro, I.
dc.contributor.authorBeswick, R.
dc.contributor.authorMuxlow, T.
dc.contributor.authorPedlar, A.
dc.contributor.authorArgo, Megan
dc.identifier.citationMarti-Vidal, I and Marcaide, J and Alberdi, A and Guirado, J and Prez-Torres, M and Ros, E and Shapiro, I and Beswick, R and Muxlow, T and Pedlar, A and Argo, M and Immler, S and Panagia, N and Stockdale, C and Sramek, R and Van Dyk, S and Weiler K. 23 GHz VLBI observations of SN 2008ax. Astronomy and Astrophysics. 499 (3): pp. 649-652.

We report on phase-referenced 23 GHz Very-Long-Baseline-Interferometry (VLBI) observations of the type IIb supernova SN 2008ax,made with the Very Long Baseline Array (VLBA) on 2 April 2008 (33 days after explosion). These observations resulted in a marginal detection of the supernova. The total flux density recovered from our VLBI image is 0.8 0.3 mJy (one standard deviation). As it appears, the structure may be interpreted as either a core-jet or a double source. However, the supernova structure could be somewhat confused with a possible close by noise peak. In such a case, the recovered flux density would decrease to 0.480.12 mJy, compatible with the flux densities measured with the VLA at epochs close in time to our VLBI observations. The lowest average expansion velocities derived from our observations are (1.90±0.30) 105 km s-1 (case of a double source) and (5.2±1.3) 104 km s-1 (takingthe weaker source component as a spurious, close by, noise peak, which is the more likely interpretation). These velocities are 7.3 and 2 times higher, respectively, than the maximum ejecta velocity inferred from optical-line observations.

dc.publisherEDP Sciences
dc.subjectradio continuum
dc.subjectNGC 4490
dc.subjectSN 2008ax
dc.title23 GHz VLBI observations of SN 2008ax
dc.typeJournal Article
dcterms.source.titleAstronomy and Astrophysics

© ESO 2009 Article published by EDP Sciences

curtin.accessStatusOpen access
curtin.facultyFaculty of Science and Engineering
curtin.facultyCurtin Institute of Radio Astronomy

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