SN 1983V in NGC 1365 and the Nature of Stripped Envelope Core‐Collapse Supernovae

Clocchiatti, A.; Wheeler, J. C.; Phillips, M. M.; Suntzeff, Nicholas B.; Cristiani, S.; Phillips, Andrew C.; Harkness, Robert; Dopita, Michael A.; Beuermann, K.; Rosa, M. R.; Grosbøl, P.; Lindblad, P. O.; Filippenko, A. V.

doi:10.1086/304268

Cited by 58 publications

(54 citation statements)

References 65 publications

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“…The most detailed discussions of line identiÐcations in SN 1994I, and SNe Ic in general, have been by Clocchiatti et al (1996Clocchiatti et al ( , 1997. The major contributors to some of the spectral features in Figure 1 are clear.…”

Section: Introductionmentioning

confidence: 94%

Direct Analysis of Spectra of the Type Ic Supernova SN 1994I

Millard

Branch

Baron

et al. 1999

ApJ

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Synthetic spectra generated with the parameterized supernova synthetic-spectrum code SYNOW are compared to observed photospheric-phase spectra of the Type Ic supernova SN 1994I. The observed optical spectra can be well matched by synthetic spectra that are based on the assumption of spherical symmetry. We consider the identiÐcation of the infrared absorption feature observed near 10250 A , which previously has been attributed to He I j10830 and regarded as strong evidence that SN 1994I ejected some helium. We have difficulty accounting for the infrared absorption with He I alone. It could be a blend of He I and C I lines. Alternatively, we Ðnd that it can be Ðtted by Si I lines without compromising the Ðt in the optical region. In synthetic spectra that match the observed spectra, from 4 days before to 26 days after the time of maximum brightness, the adopted velocity at the photosphere decreases from 17,500 to 7000 km s~1. Simple estimates of the kinetic energy carried by the ejected mass give values that are near the canonical supernova energy of 1051 ergs. The velocities and kinetic energies that we Ðnd for SN 1994I in this way are much lower than those that we Ðnd elsewhere for the peculiar Type Ic SNe 1997ef and 1998bw, which therefore appear to have been hyperenergetic.

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Section: Introductionmentioning

confidence: 94%

Direct Analysis of Spectra of the Type Ic Supernova SN 1994I

Millard

Branch

Baron

et al. 1999

ApJ

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“…In SN 1987M the feature is resolved into three minima which match well with Fe ii λλ4923, 5018, 5169 (multiplet 42). In SN 1983V and SN 1994I only two minima are resolved, identified as 5018Å and 5169Å (Clocchiatti et al 1997;Iwamoto et al 1998;Iwamoto et al 2000). However, we find that the identifi- cation of the bluer line as 4923Å results in better agreement with other features.…”

Section: Days 7-19mentioning

confidence: 48%

“…In SN 1987M the band extends blueward compared to the other SNe. The absorption band is attributed to Fe ii blends, centred at rest wavelengths of 4274Å and 4555Å (Clocchiatti et al 1997). An alternative identification for the second minimum is Mg ii λ4481 (Filippenko 1997), which gives velocities which are more in agreement with other features for all but SN 1987M.…”

Section: Days 7-19mentioning

confidence: 99%

“…In this paper we present preliminary results by looking at the most notable features of the spectrum in comparison to classic Ic SNe SN 1983V (Clocchiatti et al 1997), SN 1987M (Filippenko, Porter & Sargent 1990) and SN 1994I (Clocchiatti et al 1996;Filippenko et al 1995), and to SN 1997ef which has unusually broad lines and bears the closest resemblance to SN 1998bw (Iwamoto et al 2000). …”

Section: Spectral Evolutionmentioning

confidence: 99%

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Spectral evolution of the peculiar Ic Supernova 1998bw

Stathakis

Boyle

Jones

et al. 2000

Monthly Notices of the Royal Astronomical Society

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SN 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 AAT, UKST and the SSO 2.3-m telescope. We investigate the evolution of the spectrum between 7 and 94 days after V-band maximum in comparison to 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 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% higher then other SNe and on day 94 emission lines are 45% 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 additional contribution from other species is present, indicating unusual relative abundances or physical conditions in the envelope.

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“…To a first approximation, the light curves of SNe I are all broadly similar [2]. SNe Ib usually have slower decline rates than SNe Ic; however, SNe Ic may come in "slow" and "fast" varieties [3,4]. The light curves of SNe II exhibit much dispersion [5], though it is useful to subdivide the majority of them into two relatively distinct subclasses [6,7].…”

Section: Introductionmentioning

confidence: 99%

Optical Observations of Core-Collapse Supernovae

Filippenko

2005

Nuclear Physics A

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SN 1983V in NGC 1365 and the Nature of Stripped Envelope Core‐Collapse Supernovae

Cited by 58 publications

References 65 publications

Direct Analysis of Spectra of the Type Ic Supernova SN 1994I

Direct Analysis of Spectra of the Type Ic Supernova SN 1994I

Spectral evolution of the peculiar Ic Supernova 1998bw

Optical Observations of Core-Collapse Supernovae

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