The Rise Time of Type Ia Supernovae from the Supernova Legacy Survey

Conley, A.; Howell, D. A.; Howes, A.; Sullivan, M.; Astier, P.; Balam, D.; Basa, S.; Carlberg, R. G.; Fouchez, D.; Guy, J.; Hook, I. M.; Neill, James D.; Pain, R.; Perrett, K.; Pritchet, C. J.; Regnault, Nicolas; Rich, J.; Taillet, R.; Aubourg, É.; Bronder, J.; Ellis, Richard S.; Fabbro, S.; Filiol, M.; Borgne, D. Le; Palanque-Delabrouille, N.; Perlmutter, S.; Ripoche, P.

doi:10.1086/507788

Cited by 101 publications

(107 citation statements)

References 39 publications

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“…The slow evolution of brightness in SN 2009dc around the maximum suggests that the rising time of the bolometric luminosity is comparable to or slightly longer than those of SN 2006gz (∼18.5 days; Hicken et al 2007) or typical SNe Ia (∼19 days; e.g., Conley et al 2006). Assuming t r = 20 days for SN 2009dc, we derive the 56 Ni mass of 1.2 ± 0.3 M for the no host extinction case.…”

Section: Bolometric Light Curve and 56 Ni Massmentioning

confidence: 78%

EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

Yamanaka

Kawabata

Kinugasa

et al. 2009

ApJ

160

146

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Section: Bolometric Light Curve and 56 Ni Massmentioning

confidence: 78%

EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

Yamanaka

Kawabata

Kinugasa

et al. 2009

ApJ

160

146

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“…The light curves evolve very slowly. For SN 2009dc, Silverman et al (2011 reported a first detection on an image taken 21 d before B-band maximum, and estimated a rise time of 23 ± 2 d, significantly longer than in normal SNe Ia (17-20 d; Conley et al 2006;Hayden et al 2010). Also the decline rates after peak are among the slowest ever observed for SNe Ia, with ∆ m 15 (B) between 0.7 and 0.9.…”

Section: Early-time Light Curves and Peak Luminositymentioning

confidence: 98%

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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“…As discussed in § 4.2, we have assumed for SN 2005hk that the explosion occurred 15 days before B maximum. For SN 2001el and SN 1999by, we have taken this number to be 18.1 and 11.0 days before B maximum, respectively, which we derived from the average B light-curve rise time given by Conley et al (2006) after application of stretch values appropriate for both SNe. Figure 15 emphasizes the subluminous nature of SN 2005hk, but also shows that these events are not as extreme as the SN 1991bg-like SNe Ia.…”

Section: Absolute Magnitudes and Uvoir Bolometric Light Curvementioning

confidence: 99%

The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations?

Phillips¹,

Li²,

Frieman³

et al. 2007

PUBL ASTRON SOC PAC

206

112

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ABSTRACT. We present extensive photometry and optical spectroscopy of the Type Ia u g r i BVRIYJHK s supernova (SN) 2005hk. These data reveal that SN 2005hk was nearly identical in its observed properties to SN 2002cx, which has been called "the most peculiar known Type Ia supernova." Both supernovae exhibited highionization SN 1991T-like premaximum spectra, yet low peak luminosities like that of SN 1991bg. The spectra reveal that SN 2005hk, like SN 2002cx, exhibited expansion velocities that were roughly half those of typical Type Ia supernovae. The R and I light curves of both supernovae were also peculiar in not displaying the secondary maximum observed for normal Type Ia supernovae. Our YJH photometry of SN 2005hk reveals the same peculiarity in the near-infrared. By combining our optical and near-infrared photometry of SN 2005hk with published ultraviolet light curves obtained with the Swift satellite, we are able to construct a bolometric light curve from ∼15 days before to ∼60 days after B maximum. The shape and unusually low peak luminosity of this light curve, plus the low expansion velocities and absence of a secondary maximum at red and near-infrared wavelengths, are all in reasonable agreement with model calculations of a three-dimensional deflagration that produces ∼0.2 M , of 56 Ni.

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The Rise Time of Type Ia Supernovae from the Supernova Legacy Survey

Cited by 101 publications

References 39 publications

EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

The Extremes of Thermonuclear Supernovae

The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations?

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