SN 2003du: 480 days in the life of a normal type Ia supernova

Stanishev, V.; Goobar, A.; Benetti, S.; Kotak, R.; Pignata, G.; Navasardyan, H.; Mazzali, P. A.; Amanullah, R.; Garavini, G.; Nobili, S.; Qiu, Y.; Elias‐Rosa, N.; Ruiz‐Lapuente, P.; Méndez, J.; Meikle, P.; Patat, F.; Pastorello, A.; Altavilla, G.; Gustafsson, M.; Harutyunyan, A.; Iijima, Takashi; Jakobsson, P.; Kichizhieva, M. V.; Lundqvist, Peter; Mattila, S.; Melinder, Jens; Павленко, Е. П.; Pavlyuk, N. N.; Sollerman, J.; Tsvetkov, D. Yu.; Turatto, M.; Hillebrandt, W.

doi:10.1051/0004-6361:20066020

Cited by 162 publications

(167 citation statements)

References 118 publications

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“…SN 2005hk is in our 1 week premax sample of shallow-silicons (with fitting parameters in Table 6 also used in Chornock et al 2006), and SN 2002cx was in our maximum-light sample of shallow-silicons. But as discussed in Paper II and elsewhere (Li et al 2003;Branch et al 2004b;Jha et al 2006;Chornock et al 2006;Stanishev et al 2007;Phillips et al 2007), in spite of certain spectroscopic similarities to SN 1991T-like SNe, the SN 2002cx-like SNe appear to be physically distinct from other SNe Ia.…”

Section: Cool Sne Iamentioning

confidence: 75%

“…Following the discovery of HV Ca ii and HV Fe ii in SN 1994D (Hatano et al 1999b), HV Ca ii has been recognized by many authors: see Li et al (2001), Thomas et al (2004), and Branch et al (2004aWang et al (2003), Kasen et al (2003), and Mattila et al (2005) on SN 2001el; Mazzali et al (2005aGerardy et al (2004) and Stanishev et al (2007Quimby et al (2006and Garavini et al (2007) on SN 2005cf. In premaximum spectra of SNe Ia, HV Ca ii is ubiquitous (Mazzali et al 2005b;and this paper), and in Paper II, we regularly invoked HV Ca ii, even at maximum light.…”

Section: Discussionmentioning

confidence: 99%

“…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%

“…As with the 1 week premax spectrum of SN 2001el and the early spectrum of SN 1990N, the 6100 Å absorption of SN 1999ee can be fitted with a single broad PV component or an unresolved combination of a PV and an HV feature. For the same reasoning given in the discussion of SN 1990N and SN 2001el and the results of Garavini et al (2007) and Stanishev et al (2007), we use the two components. Figure 14 shows the spectra of the core-normal SN 2003du and the three shallow-silicons of the early sample.…”

Section: Shallow-silicon Sne Iamentioning

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: Cool Sne Iamentioning

confidence: 75%

Section: Discussionmentioning

confidence: 99%

Section: Core-normal Sne Iamentioning

confidence: 99%

Section: Shallow-silicon Sne Iamentioning

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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“…Note that the velocity of O I λ7774 measured in the spectra of SN 2007bi can only be treated as a lower-limit, as a consequence of contamination in the blue-wing by the [Ca II] feature. (Phillips et al 1999;Mazzali et al 1995), 2003du with E(B − V) = 0.01 (Anupama et al 2005;Stanishev et al 2007) and 1994D with E(B−V) = 0.042 (Meikle et al 1996;Turatto et al 1996). …”

Section: Photospheric Velocitiesmentioning

confidence: 99%

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

Young¹,

Smartt²,

Valenti³

et al. 2010

A&A

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137

132

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Aims. The aim of this paper is to discuss the nature of two type Ic supernovae SN 2007bg and SN 2007bi and their host galaxies. Both supernovae were discovered in wide-field, non-targeted surveys and are found to be associated with sub-luminous blue dwarf galaxies identified in SDSS images. Methods. We present BVRI photometry and optical spectroscopy of SN 2007bg and SN 2007bi and their host galaxies. Their lightcurves and spectra are compared to those of other type Ic SNe and analysis of these data provides estimates of the energetics, total ejected masses and synthesised mass of 56 Ni. Detection of the host galaxy emission lines allows for metallicity measurements. Results. Neither SNe 2007bg nor 2007bi were found in association with an observed GRB, but from estimates of the metallicities of their host-galaxies they are found to inhabit similar low-metallicity environments as GRB associated supernovae. The radio-bright SN 2007bg is hosted by an extremely sub-luminous galaxy of magnitude M B = −12.4 ± 0.6 mag and an estimated oxygen abundance of 12 + log(O/H) = 8.18 ± 0.17 (on the Pettini & Pagel 2004 scale). The early lightcurve evolution of SN 2007bg matches the fastpace decline of SN 1994I giving it one of the fastest post-maximum decline rates of all broad-lined type Ic supernovae known to date and, when combined with its high expansion velocities, a high kinetic energy to ejected mass ratio (E K /M ej ∼ 2.7). We also show that SN 2007bi is possibly the most luminous type Ic known, reaching a peak magnitude of M R ∼ −21.3 mag and displays a remarkably slow decline, following the radioactive decay rate of 56 Co to 56 Fe throughout the course of its observed lifetime. SN 2007bi also displays an extreme longevity in its spectral evolution and is still not fully nebular at approximately one year post-maximum brightness. From a simple model of the bolometric light curve of SN 2007bi we estimate a total ejected 56 Ni mass of M Ni = 3.5−4.5 M , the largest 56 Ni mass measured in the ejecta of a supernova to date. There are two models that could explain the high luminosity and large ejected 56 Ni mass. One is a pair-instability supernova (PISN) which has been predicted to occur for massive stars at low metallicities. We measure the host galaxy metallicity of SN 2007bi to be 12 + log(O/H) = 8.15 ± 0.15 (on the McGaugh 1991 scale) which is somewhat high to be consistent with the PISN model. An alternative is the core-collapse of a C+O star of 20−40 M which is the core of a star of originally 50−100 M .

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The Extremes of Thermonuclear Supernovae

Taubenberger¹

2016

Handbook of Supernovae

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The majority of thermonuclear explosions in the Universe seem to proceed in a rather standardised way, as explosions of carbon-oxygen (CO) white dwarfs in binary systems, leading to 'normal' Type Ia supernovae (SNe Ia). However, over the years a number of objects have been found which deviate from normal SNe Ia in their observational properties, and which require different and not seldom more extreme progenitor systems. While the 'traditional' classes of peculiar SNe Ia -luminous '91T-like' and faint '91bg-like' objects -have been known since the early 1990s, other classes of even more unusual transients have only been established 20 years later, fostered by the advent of new wide-field SN surveys such as the Palomar Transient Factory. These include the faint but slowly declining '02es-like' SNe, 'Ca-rich' transients residing in the luminosity gap between classical novae and supernovae, extremely short-lived, fast-declining transients, and the very luminous so-called 'super-Chandrasekhar' SNe Ia. Not all of them are necessarily thermonuclear explosions, but there are good arguments in favour of a thermonuclear origin for most of them. The aim of this chapter is to provide an overview of the zoo of potentially thermonuclear transients, reviewing their observational characteristics and discussing possible explosion scenarios.

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SN 2003du: 480 days in the life of a normal type Ia supernova

Cited by 162 publications

References 118 publications

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

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

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

The Extremes of Thermonuclear Supernovae

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