A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?

Zhang, Jujia; Sasdelli, Michele; Zhang, Tianmeng; Liu, Zheng-Wei; Mazzali, P. A.; Meng, Xiangcun; Maeda, Keiichi; Chen, Jun-Cheng; Huang, Fang; Zhao, Xulin; Zhang, Kaicheng; Zhai, Qingfeng; Pian, E.; Wang, Bo; Chang, Liang; Yi, Weimin; Wang, Chuanjun; Wang, Xueli; Xin, Yuxin; Wang, Jianguo; Lun, Bao-Li; Zheng, Xingming; Zhang, Xiliang; Fan, Yufeng; Bai, Jinming

doi:10.3847/0004-637x/817/2/114

Cited by 25 publications

(19 citation statements)

References 96 publications

(95 reference statements)

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“…While luminous SN 1991T-like SNe (Filippenko et al 1992a;Phillips et al 1992) may just be a "more efficient" extension of normal SNe Ia (Mazzali et al 1995;Sasdelli et al 2014;Zhang et al 2016), at the low end of the SN Ia luminosity distribution different mechanisms may be operating. SN 1991bg (Filippenko et al 1992b;Leibundgut et al 1993), the prototypical "fast decliner", and the class which takes its name, which is characterised by spectra showing lines of low-excitation ions (Mazzali et al 1997), have been suggested to be the product of a merger of two WDs below the Chandrasekhar mass (Mazzali & Hachinger 2012;Pakmor et al 2011).…”

Section: Introductionmentioning

confidence: 99%

The nebular spectra of the transitional Type Ia Supernovae 2007on and 2011iv: broad, multiple components indicate aspherical explosion cores

Mazzali

Ashall

Pian

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The nebular-epoch spectrum of the rapidly declining, "transitional" type Ia supernova (SN) 2007on showed double emission peaks, which have been interpreted as indicating that the SN was the result of the direct collision of two white dwarfs. The spectrum can be reproduced using two distinct emission components, one red-shifted and one blue-shifted. These components are similar in mass but have slightly different degrees of ionization. They recede from one another at a line-of-sight speed larger than the sum of the combined expansion velocities of their emitting cores, thereby acting as two independent nebulae. While this configuration appears to be consistent with the scenario of two white dwarfs colliding, it may also indicate an off-centre delayed detonation explosion of a near Chandrasekhar-mass white dwarf. In either case, broad emission line widths and a rapidly evolving light curve can be expected for the bolometric luminosity of the SN. This is the case for both SNe 2007on and 2011iv, also a transitional SN Ia which exploded in the same elliptical galaxy, NGC 1404. Although SN 2011iv does not show double-peaked emission line profiles, the width of its emission lines is such that a two-component model yields somewhat better results than a single-component model. Most of the mass ejected is in one component, however, which suggests that SN 2011iv was the result of the off-centre ignition of a Chandrasekhar-mass white dwarf.

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Section: Introductionmentioning

confidence: 99%

The nebular spectra of the transitional Type Ia Supernovae 2007on and 2011iv: broad, multiple components indicate aspherical explosion cores

Mazzali

Ashall

Pian

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…It has been accepted that SNe Ia arise from thermonuclear runaway explosions of carbon-oxygen white dwarfs (CO WDs) in binaries, although their progenitor systems and explosion mechanisms are still under debate (see, e.g. Podsiadlowski et al 2008;Hillebrandt et al 2013;Höflich et al 2013;Wang et al 2013;Zhang et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The core-degenerate scenario for the progenitors of Type Ia supernovae

Wang¹,

Zhou²,

Zuo³

et al. 2016

Mon. Not. R. Astron. Soc.

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The origin of the progenitors of type Ia supernovae (SNe Ia) is still uncertain. The core-degenerate (CD) scenario has been proposed as an alternative way for the production of SNe Ia. In this scenario, SNe Ia are formed at the final stage of common-envelope evolution from a merger of a carbon-oxygen white dwarf (CO WD) with the CO core of an asymptotic giant branch companion. However, the birthrates of SNe Ia from this scenario are still not well determined. In this work, we performed a detailed investigation on the CD scenario based on a binary population synthesis approach. The SN Ia delay times from this scenario are basically in the range of 90 Myr−2500 Myr, mainly contributing to the observed SNe Ia with short and intermediate delay times although this scenario can also produce some old SNe Ia. Meanwhile, our work indicates that the Galactic birthrates of SNe Ia from this scenario are no more than 20% of total SNe Ia due to more careful treatment of mass transfer. Although the SN Ia birthrates in the present work are lower than those in Ilkov & Soker, the CD scenario cannot be ruled out as a viable mechanism for the formation of SNe Ia. Especially, SNe Ia with circumstellar material from this scenario contribute to 0.7−10% of total SNe Ia, which means that the CD scenario can reproduce the observed birthrates of SNe Ia like PTF 11kx. We also found that SNe Ia happen systemically earlier for a high value of metallicity and their birthrates increase with metallicity.

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“…The spectroscopic criteria eliminate the peculiar SN 2006bt, as it contains Ti ii features. Note that using spectra alone can lead to misleading results, such as those of SN 2011hr (Zhang et al 2016) and LSQ12gdj (Scalzo et al 2014). Note that CSS140126 is a border-line case between a 1991T-like and a 2003fg-like SNe, it has only one low S/N optical spectrum which is featureless, a primary i-band maximum which peaks after that of B band, but displays a secondary i-band maximum.…”

Section: Sample Characteristicsmentioning

confidence: 99%

Carnegie Supernova Project: The First Homogeneous Sample of "Super-Chandrasekhar Mass"/2003fg-like Type Ia Supernova

Ashall,

Lu,

Hsiao

et al. 2021

Preprint

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We present a multi-wavelength photometric and spectroscopic analysis of thirteen "Super-Chandrasekhar Mass"/2003fg-like type Ia Supernova (SNe Ia). Nine of these objects were observed by the Carnegie Supernova Project. 2003fg-like SNe have slowly declining light curves (∆m 15 (B) <1.3 mag), and peak absolute B-band magnitudes between −19 < M B < −21 mag. Many 2003fg-like SNe are located in the same part of the luminosity width relation as normal SNe Ia. In the optical B and V bands, 2003fg-like SNe look like normal SNe Ia, but at redder wavelengths they diverge from normal objects. Unlike other luminous SNe Ia, 2003fg-like SNe generally have only one i-band maximum which peaks after the epoch of B-band maximum, while their NIR light curve rise times can be 40 days longer than those of normal SNe Ia. They are also at least one magnitude brighter in the NIR bands than normal SNe Ia, peaking above M H < −19 mag, and generally have negative Hubble residuals. Spectroscopically, 2003fg-like SNe exhibit peculiarities such as unburnt carbon well past maximum light, a large spread (8000-12000 km s −1 ) in Si ii λ6355 velocities at maximum light with no rapid early velocity decline, no clear H-band break at +10 d, and low ionization lines in the nebular phase. We find that SNe with a larger pseudo equivalent width of C ii at maximum light have lower Si ii λ6355 velocities and slower declining light curves. There are also multiple factors that contribute to the peak luminosity of 2003fg-like SNe. The explosion of a C-O degenerate core inside a carbon-rich envelope is consistent with these observations. Such a configuration may come from the core degenerate scenario.

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A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?

Cited by 25 publications

References 96 publications

The nebular spectra of the transitional Type Ia Supernovae 2007on and 2011iv: broad, multiple components indicate aspherical explosion cores

The nebular spectra of the transitional Type Ia Supernovae 2007on and 2011iv: broad, multiple components indicate aspherical explosion cores

The core-degenerate scenario for the progenitors of Type Ia supernovae

Carnegie Supernova Project: The First Homogeneous Sample of "Super-Chandrasekhar Mass"/2003fg-like Type Ia Supernova

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