Evidence for a High-Velocity Carbon-rich Layer in the Type I[CLC]a[/CLC] SN 1990N

Fisher, Adam; Branch, David; Nugent, P.; Baron, Edward

doi:10.1086/310660

Cited by 87 publications

(104 citation statements)

References 36 publications

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“…Evidence has been presented for the strongest optical C ii line, l6580, in SN 1998aq (Branch et al 2003), SN 1990N (Jeffery et al 1992;Mazzali 2001), SN 1999ac (Garavini et al 2005), and SN 1994D and SN 1996X (Branch et al 2003 and Paper I). Thomas et al (2007) presented the most convincing evidence in SN 2006D.…”

Section: Discussionmentioning

confidence: 97%

“…For SN 1994D, we fit it in the conventional way, with a simple PV Si ii component (a fit is shown in Paper I). For SN 2003du, the feature appears to consist of two marginally resolved components (Stanishev et al 2007), so we use The unusual, nearly flat-bottomed 6100 Å absorption of the early spectrum of SN 1990N has been discussed by several authors (Jeffery et al 1992;Fisher et al 1997;Mazzali 2001). Mattila et al (2005) showed that the 1 week premax spectrum of SN 2001el resembled the early spectrum of SN 1990N (see their Fig.…”

Section: Core-normal Sne Iamentioning

confidence: 99%

“…Therefore, exactly how the group boundaries were drawn was not important. (Gerardy et al 2004), and SN 2004S (Krisciunas et al 2007); the broad-line SN 1983G (McCall et al 1984 and SN 2002er (Kotak et al 2006); and the shallow-silicon SN 1999aa , SN 1999ac (Garavini et al 2005), SN 2000E (Valentini et al 2003), SN 2005cg (Quimby et al 2006), and SN 2003fg (the proposed super-Chandrasekhar SN Ia, also known as SNLS-03D3bb; Howell et al 2006;Jeffery et al 2007a; but see also Hillebrandt et al 2007). SN 1999ac is a borderline case: in Figure 1, it falls between two core-normals, but on the basis of the shape, depth, and width of the 6100 Å absorption, we include it with the shallow-silicons.…”

Section: Introductionmentioning

confidence: 99%

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Comparative Direct Analysis of Type Ia Supernova Spectra. III. Premaximum

Branch¹,

Troxel²,

Jeffery³

et al. 2007

PUBL ASTRON SOC PAC

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ABSTRACT.A comparative study of spectra of 21 Type Ia supernovae (SNe Ia) obtained about 1 week before maximum light, and 8 spectra obtained 11 or more days before maximum, is presented. To a large extent, the premaximum spectra exhibit the defining characteristics of the four groups defined in Paper II (core normal, broad line, cool, and shallow silicon). Comparisons with SYNOW synthetic spectra show that all strong features and most weak ones can be accounted for in a plausible way. The issues of detached high-velocity features, the possible ubiquity of carbon clumps, the maximum detectable ejecta velocities, and the possibility of blueshifted emission-line peaks are discussed.

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Section: Discussionmentioning

confidence: 97%

Section: Core-normal Sne Iamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Comparative Direct Analysis of Type Ia Supernova Spectra. III. Premaximum

Branch¹,

Troxel²,

Jeffery³

et al. 2007

PUBL ASTRON SOC PAC

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“…The identification of IMEs is confirmed by fitting the spectrum with the SN spectrum-synthesis code SYNOW (Fisher et al 1997). Although SYNOW has a simple, parametric approach to creating synthetic spectra, it is a powerful tool to aid line identifications (see Paper I for details).…”

Section: Maximum-light Spectrummentioning

confidence: 99%

EARLY- AND LATE-TIME OBSERVATIONS OF SN 2008ha: ADDITIONAL CONSTRAINTS FOR THE PROGENITOR AND EXPLOSION

Foley

Brown

Rest

et al. 2009

ApJ

143

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We present a new maximum-light optical spectrum of the extremely low luminosity and exceptionally low-energy Type Ia supernova (SN Ia) 2008ha, obtained one week before the earliest published spectrum. Previous observations of SN 2008ha were unable to distinguish between a massive star and white dwarf (WD) origin for the SN. The new maximum-light spectrum, obtained one week before the earliest previously published spectrum, unambiguously shows features corresponding to intermediate mass elements, including silicon, sulfur, and carbon. Although strong silicon features are seen in some core-collapse SNe, sulfur features, which are a signature of carbon/ oxygen burning, have always been observed to be weak in such events. It is therefore likely that SN 2008ha was the result of a thermonuclear explosion of a carbon-oxygen WD. Carbon features at maximum light show that unburned material is present to significant depths in the SN ejecta, strengthening the case that SN 2008ha was a failed deflagration. We also present late-time imaging and spectroscopy that are consistent with this scenario.

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“…Signatures of carbon might also be detected as C III λ4649 in so-called "Shallow Silicon" SN Ia that display spectral signatures of overall higher ionization species, e.g., SN 1991T and 1997br (Hatano et al 2002;Garavini et al 2004;Parrent et al 2011;Zheng et al 2013;Scalzo et al 2014b). Seemingly smaller amounts of unburned material of the C+O progenitor, or burned material of the He+C+O progenitor, are frequently detected for so-called "Core Normal" SN Ia (Jeffery et al 1992;Fisher et al 1997;Branch et al 2005; Thomas et al 2007), while signatures of C I λ10691 are detected for several events, and possibly all SN Ia (Höflich et al 2002;Marion et al 2015;Hsiao et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

Parrent¹,

Howell²,

Fesen³

et al. 2016

Mon. Not. R. Astron. Soc.

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SN 2012dn is a super-Chandrasekhar mass candidate in a purportedly normal spiral (SAcd) galaxy, and poses a challenge for theories of type Ia supernova diversity. Here we utilize the fast and highly parameterized spectrum synthesis tool, SYNAPPS, to estimate relative expansion velocities of species inferred from optical spectra obtained with six facilities. As with previous studies of normal SN Ia, we find that both unburned carbon and intermediate mass elements are spatially coincident within the ejecta near and below 14,000 km s −1 . Although the upper limit on SN 2012dn's peak luminosity is comparable to some of the most luminous normal SN Ia, we find a progenitor mass exceeding ∼ 1.6 M is not strongly favored by leading merger models since these models do not accurately predict spectroscopic observations of SN 2012dn and more normal events. In addition, a comparison of light curves and host-galaxy masses for a sample of literature and Palomar Transient Factory SN Ia reveals a diverse distribution of SN Ia subtypes where carbon-rich material remains unburned in some instances. Such events include SN 1991T, 1997br, and 1999aa where trace signatures of C III at optical wavelengths are presumably detected.

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Evidence for a High-Velocity Carbon-rich Layer in the Type I[CLC]a[/CLC] SN 1990N

Cited by 87 publications

References 36 publications

Comparative Direct Analysis of Type Ia Supernova Spectra. III. Premaximum

Comparative Direct Analysis of Type Ia Supernova Spectra. III. Premaximum

EARLY- AND LATE-TIME OBSERVATIONS OF SN 2008ha: ADDITIONAL CONSTRAINTS FOR THE PROGENITOR AND EXPLOSION

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

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