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23 GHz VLBI observations of SN 2008ax (Research Note)
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Martí Vidal, Iván; Marcaide Osoro, Juan María; Alberdi, A.; Guirado Puerta, Jose Carlos; Pérez Torres, Miguel Ángel; Ros Ibarra, Eduardo; Shapiro, I.I.; Beswick, R.J.; Muxlow, T.W.B.; Pedlar, A.; Argo, M.K.; Immler, S.; Panagia, N.; Stockdale, C.J.; Sramek, R.A.; Van Dyk, S. D.; Weiler, K.W.
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This document is a artículoDate2009
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Este documento está disponible también en :
http://www.aanda.org/index.php?option=article&access=doi&doi=10.1051/0004-6361/200912034
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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 0.48 ± 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 ± 0.30) × 105 km s−1 (case of a double source) and (5.2 ± 1.3) × 104 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.
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