The subluminous, spectroscopically peculiar type IA supernova 1991bg in the elliptical galaxy NGC 4374

Filippenko, A. V.; Richmond, M.; Branch, David; Gaskell, C. Martin; Herbst, W.; Ford, Charles; Treffers, R. R.; Matheson, T.; Ho, Luis C.; Dey, Arjun; Sargent, W. L. W.; Small, Todd; Breugel, W. J. M. van

doi:10.1086/116339

Cited by 458 publications

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“…We tested our method on SN 2014J, a heavily reddened SN Ia in the nearby galaxy M 82, and find good agreement between the estimates from the γ-ray observations (Churazov et al 2014;Diehl et al 2015, see Table 4). Faint, 91bg-like SNe Ia, which show typically lower luminosities (Filippenko et al 1992;Leibundgut et al 1993), do not display a second maximum in their NIR light curves and are not in our sample. Therefore, the true dispersion in peak luminosity and M56 Ni for SN Ia will likely be larger than what is derived here.…”

Section: Discussionmentioning

confidence: 75%

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

Dhawan

Leibundgut

Spyromilio

et al. 2016

A&A

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The increase in the number of Type Ia supernovae (SNe Ia) has demonstrated that the population shows greater diversity than has been assumed in the past. The reasons (e.g. parent population, explosion mechanism) for this diversity remain largely unknown. We investigated a sample of SNe Ia near-infrared light curves and correlated the phase of the second maximum with the bolometric peak luminosity. The peak bolometric luminosity is related to the time of the second maximum (relative to the B light curve maximum) as follows: L max (10 43 erg s −1 ) = (0.039 ± 0.004) × t 2 (J)(days) + (0.013 ± 0.106). 56 Ni masses can be derived from the peak luminosity based on Arnett's rule, which states that the luminosity at maximum is equal to the instantaneous energy generated by the nickel decay. We checked this assumption against recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models and find this assumption is valid to within 10% in recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models. The L max vs. t 2 relation is applied to a sample of 40 additional SNe Ia with significant reddening (E(B − V) > 0.1 mag), and a reddening-free bolometric luminosity function of SNe Ia is established. The method is tested with the 56 Ni mass measurement from the direct observation of γ-rays in the heavily absorbed SN 2014J and found to be fully consistent. Super-Chandrasekhar-mass explosions, in particular SN 2007if, do not follow the relations between peak luminosity and second IR maximum. This may point to an additional energy source contributing at maximum light. The luminosity function of SNe Ia is constructed and is shown to be asymmetric with a tail of low-luminosity objects and a rather sharp high-luminosity cutoff, although it might be influenced by selection effects.

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Section: Discussionmentioning

confidence: 75%

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

Dhawan

Leibundgut

Spyromilio

et al. 2016

A&A

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“…The crucial year was 1991, when the bright, slowly declining SN1991T [74,105], and the faint, intrinsically red and fast declining SN1991bg [50,71,119] were discovered. Other under-and over-luminous objects have been found since then [66].…”

Section: Type Ia Supernovaementioning

confidence: 99%

Classification of Supernovae

Turatto

2003

Supernovae and Gamma-Ray Bursters

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Abstract. The current classification scheme for supernovae is presented. The main observational features of the supernova types are described and the physical implications briefly addressed. Differences between the homogeneous thermonuclear type Ia and similarities among the heterogeneous core collapse type Ib, Ic and II are highlighted. Transforming type IIb, narrow line type IIn, supernovae associated with GRBs and few peculiar objects are also discussed.

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“…These objects, commonly dubbed "91bg-like" after the prototypical event SN 1991bg (Filippenko et al 1992;Leibundgut et al 1993), deviate quite significantly from the behavior defined by core-normal events (Branch et al 2006). Photometrically, they are about 2 mag fainter, display rapidly declining light curves with narrower peaks, lack a secondary maximum in the near-infrared (NIR) bands, have redder colors at maximum light, and obey a different relation between maximum luminosity and light curve shape (Garnavich et al 2004).…”

Section: Introductionmentioning

confidence: 99%

VLT Spectropolarimetry of the Type Ia SN 2005ke

Patat¹,

Hoêflich²,

Baade³

et al. 2012

A&A

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Aims. In this study we try to answer the question whether or not subluminous Type Ia supernovae have additional distinctive properties when examined from the point of view of the explosion geometry. Methods. We have performed optical spectropolarimetric observations of the Type Ia SN 2005ke at 3 epochs (days −8, −7, and +76). The explosion properties are derived by comparing the data to explosion and radiation transfer models. Results. The supernova shows polarimetric properties that are very similar to the only other subluminous event for which spectropolarimetry is available, i.e. SN 1999by. The data present a very marked dominant axis, which is shared by both the continuum and lines such as Si ii λ6355, suggesting that the relatively large, global asymmetry is common to the photosphere and the line-forming region. The maximum polarization degree observed in the Si ii λ6355 absorption reaches 0.39 ± 0.08%. At variance with what is seen in core-normal Type Ia, SN 2005ke displays significant continuum polarization, which grows from the blue to the red and peaks at about 7000 Å, reaching ∼0.7%. The properties of the polarization and flux spectra can be understood within the framework of a subluminous delayed-detonation (DD), or pulsating DD scenario, or white dwarf (WD) mergers. The difference in appearance with respect to core-normal SNe Ia is caused by low photospheric temperatures in combination with layers of unburned C, and more massive layers of the products of explosive C and O burning. The comparatively high level of continuum polarization is explained in terms of a significant global asymmetry (∼15%), which is well reproduced by an oblate ellipsoidal geometry within the general context of a DD explosion. Conclusions. Our results suggest that SN 2005ke arose either from a single-degenerate system in which the WD is especially rapidly rotating, close to the break-up velocity, or from a double-degenerate merger. Based on the current polarization data, we cannot distinguish between these two possibilities. Possible tests are discussed.

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The subluminous, spectroscopically peculiar type IA supernova 1991bg in the elliptical galaxy NGC 4374

Cited by 458 publications

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A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

Classification of Supernovae

VLT Spectropolarimetry of the Type Ia SN 2005ke

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The subluminous, spectroscopically peculiar type IA supernova 1991bg in the elliptical galaxy NGC 4374

Cited by 458 publications

References 0 publications

A reddening-free method to estimate the56Ni mass of Type Ia supernovae

A reddening-free method to estimate the56Ni mass of Type Ia supernovae

Classification of Supernovae

VLT Spectropolarimetry of the Type Ia SN 2005ke

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A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae