Optical and Infrared Photometry of the Unusual Type Ia Supernova 2000cx

Candia, P.; Krisciunas, K.; Suntzeff, Nicholas B.; González, David; Espinoza, J.; Leiton, R.; Rest, A.; Smith, R. C.; Cuadra, Jorge; Tavenner, T.; Logan, Chelsea; Snider, Keely; Thomas, M.; West, Andrew A.; González, Guillermo; González, S.; Phillips, M. M.; Hastings, N. C.; McMillan, R.

doi:10.1086/368229

Cited by 70 publications

(54 citation statements)

References 39 publications

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“…Very sub-luminous objects may completely lack a secondary maximum. Similar trends appear in the J, H, and K-band LC (Krisciunas et al 2004b), although interesting exceptions have been sought out (e.g., SN 2000cx Candia et al 2003). Despite the theoretical insights (e.g., Hoflich et al 1995;Wheeler et al 1998;Pinto & Eastman 2000a,b;Kasen 2006), the origin of the NIR secondary maximum and its dependence on the SN ejecta properties remain unclear.…”

Section: Introductionmentioning

confidence: 81%

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The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Biscardi

Brocato

Arkharov

et al. 2012

A&A

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Aims. We present optical and near-infrared (NIR) photometry of supernova (SN) 2008fv and a brief investigation of SN type Ia to search for possible correlations between the properties of NIR light curves and the optical decline rate. Methods. We analyse our BVRI and JHK observations to derive light curves (LCs), colour curves, and the bolometric behaviour of SN 2008fv. Data range from about five days before to two months after maximum. We also collect a database of the main characteristics of NIR LCs of SNe Ia available in literature. Results. We find close similarities between the observed LCs of the SN event studied here and SN 2000E. SN 2008fv is a slow-declining SNe Ia with a post-maximum decline of Δm 15,B = 0.96 ± 0.08 mag and a B-band maximum luminosity of M B,0 = −19.40 ± 0.1 mag, close to the value of normal SNe Ia. The optical and NIR data allow us to constrain the host galaxy reddening of NGC 3147, E(B−V) = 0.22 ± 0.05 mag and its distance μ = 33.2 ± 0.1 mag. Furthermore, we derive a synthesized 56 Ni mass of about 0.7 M , by using the well-known relation between the maximum luminosity of the uvoir bolometric light curve and the initial content of 56 Ni. We investigate the correlation between the NIR characteristics of LCs and optical properties by collecting data of a sample of 40 SNe. We derive quantitative relationships involving the epoch of the secondary maximum in the JHK bands and the decline rate Δm 15 (B). Further, we find no correlations between Δm 15 measured in the JHK bands and the optical Δm 15 (B). In contrast, quite evident correlations with the Δm 15 (B) and Δm 40 (J)/Δm 15 (H).

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Section: Introductionmentioning

confidence: 81%

“…All data are corrected for the total Galactic+host reddening), by assuming the proper value for R V (see text). The NIR loci predicted by Candia et al (2003) and Krisciunas et al (2004c) are also plotted as dashed and dot -short dashed lines. Table 11.…”

Section: Optical and Near-ir Colour Curvesmentioning

confidence: 99%

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Biscardi

Brocato

Arkharov

et al. 2012

A&A

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“…Light-curve fitters fail to produce decent fits for SN 2000cx (Li et al, 2001b), and absolute magnitudes estimated by them cannot be trusted. Unfortunately, the distance to NGC 524, the host galaxy of SN 2000cx, is not well constrained, and it has therefore been debated whether SN 2000cx was overluminous, normal or even subluminous (Li et al, 2001b;Candia et al, 2003). The most recent calibrations actually suggest that the peak luminosity of SN 2000cx was similar to that of normal SNe Ia (Silverman et al, 2013).…”

Section: Cx-like Sne: Rare Weirdosmentioning

confidence: 99%

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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“…For the smoothed spectrum of SN 2000cx shown in Fig. 5 we use a reddening E B−V = 0.08 (Schlegel et al 1998) and a distance of 33 Mpc (Candia et al 2003). SN 2000cx was a rather peculiar SN Ia around maximum light, peculiarities including an unusual light-curve and an unusual color evolution (Li et al 2001).…”

Section: Spectrummentioning

confidence: 99%

Three-dimensional modeling of type Ia supernovae – The power of late time spectra

Kozma¹,

Fransson²,

Hillebrandt

et al. 2005

A&A

111

118

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Abstract. Late time synthetic spectra of type Ia supernovae, based on three-dimensional deflagration models, are presented. We mainly focus on one model, "c3_3d_256_10s", for which the hydrodynamics (Röpke 2005, A&A, 432, 969) and nucleosynthesis (Travaglio et al. 2004(Travaglio et al. , A&A, 425, 1029 was calculated up to the homologous phase of the explosion. Other models with different ignition conditions and different resolution are also briefly discussed. The synthetic spectra are compared to observed late time spectra. We find that while the model spectra after 300 to 500 days show a good agreement with the observed Fe II-III features, they also show too strong O I and C I lines compared to the observed late time spectra. The oxygen and carbon emission originates from the low-velocity unburned material in the central regions of these models. To get agreement between the models and observations we find that only a small mass of unburned material may be left in the center after the explosion. This may be a problem for pure deflagration models, although improved initial conditions, as well as higher resolution decrease the discrepancy. The relative intensity from the different ionization stages of iron is sensitive to the density of the emitting iron-rich material. We find that clumping, with the presence of low density regions, is needed to reproduce the observed iron emission, especially in the range between 4000 and 6000 Å. Both temperature and ionization depend sensitively on density, abundances and radioactive content. This work therefore illustrates the importance of including the inhomogeneous nature of realistic three-dimensional explosion models. We briefly discuss the implications of the spectral modeling for the nature of the explosion.

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Optical and Infrared Photometry of the Unusual Type Ia Supernova 2000cx

Cited by 70 publications

References 39 publications

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

The Extremes of Thermonuclear Supernovae

Three-dimensional modeling of type Ia supernovae – The power of late time spectra

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