Spectral evolution of the peculiar Ic Supernova 1998bw
Identifieur interne : 000520 ( Main/Exploration ); précédent : 000519; suivant : 000521Spectral evolution of the peculiar Ic Supernova 1998bw
Auteurs : R. A. Stathakis [Australie] ; B. J. Boyle [Australie] ; D. H. Jones [Australie] ; M. S. Bessell [Australie] ; T. J. Galama [États-Unis] ; Lisa M. Germany [Australie] ; M. Hartley [Australie] ; D. M. James [Australie] ; C. Kouveliotou [États-Unis] ; I. J. Lewis [Australie] ; Q. A. Parker ; K. S. Russell [Australie] ; E. M. Sadler [Australie] ; C. G. Tinney [Australie] ; J. Van Paradijs [Pays-Bas, États-Unis] ; P. M. Vreeswijk [Pays-Bas]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2000-06.
English descriptors
- KwdEn :
Abstract
Supernova 1998bw holds the record for the most energetic Type Ic explosion, one of the brightest radio supernovae and probably the first supernova associated with a γ‐ray burst. In this paper we present spectral observations of SN 1998bw observed in a cooperative monitoring campaign using the Anglo‐Australian Telescope, the UK Schmidt Telescope and the Siding Springs Observatories 2.3‐m telescope. We investigate the evolution of the spectrum between 7 and 94 d after V‐band maximum in comparison with well‐studied examples of Type Ic SNe in order to quantify the unusual properties of this supernova event. Though the early spectra differ greatly from observations of classical Ic supernovae (SNe), we find that the evolution from the photospheric to nebular phases is slow but otherwise typical. The spectra differ predominantly in the extensive line blending and blanketing which has been attributed to the high velocity of the ejecta. We find that by day 19, the absorption line minima blueshifts are 10–50 per cent higher than other SNe and on day 94 emission lines are 45 per cent broader, as expected if the progenitor had a massive envelope. However, it is difficult to explain the extent of line blanketing entirely by line broadening, and we argue that an additional contribution from other species is present, indicating unusual relative abundances or physical conditions in the envelope.
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DOI: 10.1046/j.1365-8711.2000.03373.x
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Kouveliotou</name><affiliation></affiliation><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>NASA Marshall Space Flight Center, ES‐84, Huntsville, AL 35812</wicri:regionArea><wicri:noRegion>AL 35812</wicri:noRegion></affiliation></author><author><name sortKey="Lewis, I J" sort="Lewis, I J" uniqKey="Lewis I" first="I. J." last="Lewis">I. J. Lewis</name><affiliation wicri:level="1"><country xml:lang="fr">Australie</country><wicri:regionArea>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710</wicri:regionArea><wicri:noRegion>NSW 1710</wicri:noRegion></affiliation></author><author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><affiliation><wicri:noCountry code="subField">3HJ</wicri:noCountry></affiliation></author><author><name sortKey="Russell, K S" sort="Russell, K S" uniqKey="Russell K" first="K. S." last="Russell">K. S. 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In this paper we present spectral observations of SN 1998bw observed in a cooperative monitoring campaign using the Anglo‐Australian Telescope, the UK Schmidt Telescope and the Siding Springs Observatories 2.3‐m telescope. We investigate the evolution of the spectrum between 7 and 94 d after V‐band maximum in comparison with well‐studied examples of Type Ic SNe in order to quantify the unusual properties of this supernova event. Though the early spectra differ greatly from observations of classical Ic supernovae (SNe), we find that the evolution from the photospheric to nebular phases is slow but otherwise typical. The spectra differ predominantly in the extensive line blending and blanketing which has been attributed to the high velocity of the ejecta. We find that by day 19, the absorption line minima blueshifts are 10–50 per cent higher than other SNe and on day 94 emission lines are 45 per cent broader, as expected if the progenitor had a massive envelope. However, it is difficult to explain the extent of line blanketing entirely by line broadening, and we argue that an additional contribution from other species is present, indicating unusual relative abundances or physical conditions in the envelope.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Pays-Bas</li><li>États-Unis</li></country><region><li>Hollande-Septentrionale</li></region><settlement><li>Amsterdam</li></settlement><orgName><li>Université d'Amsterdam</li></orgName></list><tree><noCountry><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name></noCountry><country name="Australie"><noRegion><name sortKey="Stathakis, R A" sort="Stathakis, R A" uniqKey="Stathakis R" first="R. A." last="Stathakis">R. A. Stathakis</name></noRegion><name sortKey="Bessell, M S" sort="Bessell, M S" uniqKey="Bessell M" first="M. S." last="Bessell">M. S. Bessell</name><name sortKey="Boyle, B J" sort="Boyle, B J" uniqKey="Boyle B" first="B. J." last="Boyle">B. J. Boyle</name><name sortKey="Germany, Lisa M" sort="Germany, Lisa M" uniqKey="Germany L" first="Lisa M." last="Germany">Lisa M. Germany</name><name sortKey="Hartley, M" sort="Hartley, M" uniqKey="Hartley M" first="M." last="Hartley">M. Hartley</name><name sortKey="James, D M" sort="James, D M" uniqKey="James D" first="D. M." last="James">D. M. James</name><name sortKey="Jones, D H" sort="Jones, D H" uniqKey="Jones D" first="D. H." last="Jones">D. H. Jones</name><name sortKey="Lewis, I J" sort="Lewis, I J" uniqKey="Lewis I" first="I. J." last="Lewis">I. J. Lewis</name><name sortKey="Russell, K S" sort="Russell, K S" uniqKey="Russell K" first="K. S." last="Russell">K. S. Russell</name><name sortKey="Sadler, E M" sort="Sadler, E M" uniqKey="Sadler E" first="E. M." last="Sadler">E. M. Sadler</name><name sortKey="Tinney, C G" sort="Tinney, C G" uniqKey="Tinney C" first="C. G." last="Tinney">C. G. Tinney</name></country><country name="États-Unis"><noRegion><name sortKey="Galama, T J" sort="Galama, T J" uniqKey="Galama T" first="T. J." last="Galama">T. J. Galama</name></noRegion><name sortKey="Kouveliotou, C" sort="Kouveliotou, C" uniqKey="Kouveliotou C" first="C." last="Kouveliotou">C. Kouveliotou</name><name sortKey="Van Paradijs, J" sort="Van Paradijs, J" uniqKey="Van Paradijs J" first="J." last="Van Paradijs">J. Van Paradijs</name></country><country name="Pays-Bas"><region name="Hollande-Septentrionale"><name sortKey="Van Paradijs, J" sort="Van Paradijs, J" uniqKey="Van Paradijs J" first="J." last="Van Paradijs">J. Van Paradijs</name></region><name sortKey="Vreeswijk, P M" sort="Vreeswijk, P M" uniqKey="Vreeswijk P" first="P. M." last="Vreeswijk">P. M. Vreeswijk</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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