23 GHz VLBI Observations of SN 2008ax

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23 GHz VLBI Observations of SN 2008ax

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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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  • FAS Scholarly Articles [6463]
    Peer reviewed scholarly articles from the Faculty of Arts and Sciences of Harvard University

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