NEARBY SUPERNOVA FACTORY OBSERVATIONS OF SN 2007if: FIRST TOTAL MASS MEASUREMENT OF A SUPER-CHANDRASEKHAR-MASS PROGENITOR

Scalzo, R.; Aldering, G.; Antilogus, P.; Aragon, C.; Bailey, S.; Baltay, C.; Bongard, S.; Buton, C.; Childress, M.; Chotard, N.; Copin, Y.; Fakhouri, H. K.; Gal‐Yam, A.; Gangler, É.; Hoyer, S.; Kasliwal, Mansi M.; Loken, S.; Nugent, P.; Pain, R.; Pécontal, É.; Pereira, R.; Perlmutter, S.; Rabinowitz, D.; Rau, A.; Rigaudier, G.; Runge, K.; Smadja, G.; Tao, C.; Thomas, R. C.; Weaver, B. A.; Wu, Chao

doi:10.1088/0004-637x/713/2/1073

Cited by 347 publications

(461 citation statements)

References 76 publications

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“…In addition, the so-called super-Chandrasekhar mass SNe Ia are thought to contain >1.4 M of SN ejecta and thus are likely formed from the DD scenario (e.g., Howell et al 2006;Yamanaka et al 2009;Scalzo et al 2010;Silverman et al 2011;Taubenberger et al 2011). However, there are a few SNe Ia that show strong evidence for the SD channel, possibly with a red giant (RG) companion.…”

Section: Introductionmentioning

confidence: 99%

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Silverman¹,

Nugent

Gal‐Yam

et al. 2015

Proc. IAU

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Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the beststudied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogenrich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by Hα emission (with widths of ∼2000 km s −1 ) and exhibit large Hα/Hβ intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He i emission. They also show possible evidence of dust formation through a decrease in the red wing of Hα 75-100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na i D absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be −21.3 mag M R −19 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date.

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Section: Introductionmentioning

confidence: 99%

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Silverman¹,

Nugent

Gal‐Yam

et al. 2015

Proc. IAU

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“…At least three events are currently known: SN 2003fg (Howell et al 2006), SN 2007if (Scalzo et al 2010;Yuan et al 2010) and SN 2009dc (Yamanaka et al 2009;Tanaka et al 2010;Silverman et al 2011;Taubenberger et al 2011). A fourth event, SN 2006gz (Hicken et al 2007), is usually classed with these three, although its maximum-light luminosity depends on an uncertain extinction correction from dust in its host galaxy.…”

Section: Introductionmentioning

confidence: 99%

Early ultraviolet emission in the Type Ia supernova LSQ12gdj: No evidence for ongoing shock interaction

Scalzo¹,

Childress²,

Tucker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present photospheric-phase observations of LSQ12gdj, a slowly-declining, UV-bright Type Ia supernova. Classified well before maximum light, LSQ12gdj has extinction-corrected absolute magnitude M B = −19.8, and pre-maximum spectroscopic evolution similar to SN 1991T and the super-Chandrasekhar-mass SN 2007if. We use ultraviolet photometry from Swift, ground-based optical photometry, and corrections from a near-infrared photometric template to construct the bolometric (1600-23800 Å) light curve out to 45 days past B-band maximum light. We estimate that LSQ12gdj produced 0.96 ± 0.07 M ⊙ of 56 Ni, with an ejected mass near or slightly above the Chandrasekhar mass. As much as 27% of the flux at the earliest observed phases, and 17% at maximum light, is emitted bluewards of 3300 Å. The absence of excess luminosity at late times, the cutoff of the spectral energy distribution bluewards of 3000 Å, and the absence of narrow line emission and strong Na I D absorption all argue against a significant contribution from ongoing shock interaction. However, ∼ 10% of LSQ12gdj's luminosity near maximum light could be produced by the release of trapped radiation, including kinetic energy thermalized during a brief interaction with a compact, hydrogen-poor envelope (radius < 10 13 cm) shortly after explosion; such an envelope arises generically in double-degenerate merger scenarios.

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“…Recent discoveries of several very bright Type Ia supernovae (SNe Ia) suggest that their progenitor white dwarfs (WDs) might have super-Chandrasekhar masses of up to 2.4-2.8 M (Hicken et al 2007;Howell et al 2006;Scalzo et al 2010;Silverman et al 2011;Taubenberger et al 2011;Yamanaka et al 2009). Super-Chandrasekhar mass of the progenitors of SNe Ia was first reported by Howell et al (2006) for SN 2003fg (∼ 2.1 M C+O WD with 1.29 ± 0.07 M 56 Ni).…”

Section: Introductionmentioning

confidence: 99%

“…More candidates for super-Chandrasekhar mass progenitors were added to the list, i.e., SN 2006gz, SN 2007if, and SN 2009dc. The very bright SN 2007if requires a 2.4 ± 0.2 M progenitor C+O WD with 1.6 ± 0.1 M 56 Ni (Scalzo et al 2010) and SN 2009dc also demands a 2.0 M progenitor C+O WD with 1.4-1.7 M 56 Ni (Silverman et al 2011) or a ∼ 2.8 M C+O WD with ∼ 1.8 M 56 Ni (Taubenberger et al 2011). Such a large WD mass, highly exceeding M Ch (≈ 1.4 M ), could challenge both the double degenerate (DD) and single degenerate (SD) scenarios.…”

Section: Introductionmentioning

confidence: 99%

“…Such a large WD mass, highly exceeding M Ch (≈ 1.4 M ), could challenge both the double degenerate (DD) and single degenerate (SD) scenarios. Some authors favor a DD merger scenario for these super-Chandrasekhar mass SNe Ia (e.g., Scalzo et al 2010;Silverman et al 2011), mainly because the existing SD scenario provides only M W D 1.8 M (e.g., Chen & Li 2009;Liu et al 2010).…”

Section: Introductionmentioning

confidence: 99%

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A Single Degenerate Model for Ultra Super-Chandrasekhar Mass Progenitors of Type Ia Supernovae – Young and Low Metallicity Environments –

et al. 2011

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Abstract. Some Type Ia supernovae (SNe Ia) are suggested to have progenitor white dwarfs (WDs) with mass of up to 2.4-2.8 M , highly exceeding the Chandrasekhar mass limit. We present a new single degenerate (SD) model for SNe Ia progenitors, in which the WD mass can increase by accretion up to 2.3 (2.7) M from the initial value of 1.1 (1.2) M . The results are consistent with high luminosity SNe Ia such as SN 2003fg, SN 2006gz, SN 2007if, and SN 2009dc. There are three characteristic mass ranges of exploding WDs. In an extreme massive case, differentially rotating WDs explode as a SNe Ia soon after the WD mass exceeds 2.4 M because of a secular instability at T /|W | ∼ 0.14. For a mid mass range of MW D = 1.5-2.4 M , which is supported by differential rotation, it takes some spinning-down time until carbon is ignited to induce an SN Ia explosion. For a lower mass range of MW D = 1.38-1.5 M , they can be supported by rigid rotation until the angular momentum is lost. We also suggest the ultra super-Chandrasekhar mass SNe Ia are born in young and low metallicity environments.

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NEARBY SUPERNOVA FACTORY OBSERVATIONS OF SN 2007if: FIRST TOTAL MASS MEASUREMENT OF A SUPER-CHANDRASEKHAR-MASS PROGENITOR

Cited by 347 publications

References 76 publications

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Early ultraviolet emission in the Type Ia supernova LSQ12gdj: No evidence for ongoing shock interaction

A Single Degenerate Model for Ultra Super-Chandrasekhar Mass Progenitors of Type Ia Supernovae – Young and Low Metallicity Environments –

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