The Luminosity of SN 1999by in NGC 2841 and the Nature of “Peculiar” Type Ia Supernovae

Garnavich, P.; Bonanos, A. Z.; Krisciunas, K.; Jha, Saurabh W.; Kirshner, R.; Schlegel, Eric M.; Challis, P.; Macri, Lucas M.; Hatano, K.; Branch, David; Bothun, G. D.; Freedman, Wendy L.

doi:10.1086/422986

Cited by 183 publications

(281 citation statements)

References 56 publications

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“…the absence of a secondary peak in the red passbands, an intrinsically red color and a fast decline rate Δm 15 (B) = 1.76 ± 0.01 (Folatelli et al 2010 reached Δm 15 (B) = 1.90 ± 0.05 (Garnavich et al 2004) and 1.93 ± 0.10 (Taubenberger et al 2008), respectively. SN 2005ke reached a peak magnitude of V = 14.2 (Contreras et al 2010), which coupled to the estimated distance modulus μ = 32.06 ± 0.27 (Wood-Vasey et al 2008) yields an absolute magnitude M V = −17.9 ± 0.3.…”

Section: General Properties Of Sn 2005kementioning

confidence: 94%

“…From the classification spectrum it was clear that SN 2005ke was a subluminous Type Ia event (Patat et al 2005), very similar to SN 1999by Garnavich et al 2004). The characteristic Ti ii feature at about 4200 Å was clearly detected in the pre-maximum spectra.…”

Section: General Properties Of Sn 2005kementioning

confidence: 94%

“…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). Spectroscopically, they show cool spectra, characterized by intermediate-mass elements, particularly strong O i and Ti ii absorptions, and lower expansion velocities.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: General Properties Of Sn 2005kementioning

confidence: 94%

Section: General Properties Of Sn 2005kementioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

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VLT Spectropolarimetry of the Type Ia SN 2005ke

Patat¹,

Hoêflich²,

Baade³

et al. 2012

A&A

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“…Shown for comparison in the same table are the absolute magnitudes of (1) of SN 1999by were calculated from the photometry of Garnavich et al (2004) and the Cepheid distance modulus of Macri et al (2001).…”

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

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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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“…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%

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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The Luminosity of SN 1999by in NGC 2841 and the Nature of “Peculiar” Type Ia Supernovae

Cited by 183 publications

References 56 publications

VLT Spectropolarimetry of the Type Ia SN 2005ke

VLT Spectropolarimetry of the Type Ia SN 2005ke

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

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

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