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dc.contributor.author	Marti-Vidal, I.
dc.contributor.author	Alberdi, A.
dc.contributor.author	Ros, E.
dc.contributor.author	Shapiro, Irwin Ira
dc.contributor.author	Beswick, R.J.
dc.contributor.author	Pedlar, A.
dc.contributor.author	Immler, S.
dc.contributor.author	Panagia, N.
dc.contributor.author	Van Dyk, S.
dc.contributor.author	Marcaide, J. M.
dc.contributor.author	Guirado, J. C.
dc.contributor.author	Perrez-Torres, M. A.
dc.contributor.author	Muxlow, T. W. B.
dc.contributor.author	Argo, M. K.
dc.contributor.author	Stockdale, C. J.
dc.contributor.author	Sramek, R. A.
dc.contributor.author	Weiler, K. W.
dc.date.accessioned	2012-06-25T14:40:47Z
dc.date.issued	2009
dc.identifier.citation	Marti-Vidal, I., J. M. Marcaide, A. Alberdi, J. C. Guirado, M. A. Pérez-Torres, E. Ros, Irwin Ira Shapiro, et al. 2009. 23 GHz VLBI Observations of SN 2008ax. Astronomy & Astrophysics 499(3): 649-652.	en_US
dc.identifier.issn	0004-6361	en_US
dc.identifier.uri	http://nrs.harvard.edu/urn-3:HUL.InstRepos:8919559
dc.description.abstract	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 recoveredfrom our VLBI image is \(0.8 \pm 0.3 mJy\) (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 \(0.48 \pm 0.12 mJy\), 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 \((1.90 \pm 0.30) \times 10^{5} km\) \(s^{-1}\) (case of a double source) and \((5.2 \pm 1.3) \times 10^{4} km\) \(s^{-1}\) (taking the 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.	en_US
dc.description.sponsorship	Astronomy	en_US
dc.language.iso	en_US	en_US
dc.publisher	EDP Sciences	en_US
dc.relation.isversionof	doi:10.1051/0004-6361/200912034	en_US
dc.relation.hasversion	http://arxiv.org/pdf/0904.0337v1.pdf	en_US
dash.license	OAP
dc.subject	NGC 4490	en_US
dc.subject	galaxies	en_US
dc.subject	radio continuum	en_US
dc.subject	stars	en_US
dc.subject	supernovae	en_US
dc.subject	SN 2008ax	en_US
dc.title	23 GHz VLBI Observations of SN 2008ax	en_US
dc.type	Journal Article	en_US
dc.description.version	Accepted Manuscript	en_US
dc.relation.journal	Astronomy & Astrophysics	en_US
dash.depositing.author	Shapiro, Irwin Ira
dc.date.available	2012-06-25T14:40:47Z

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