A COMPACT DEGENERATE PRIMARY-STAR PROGENITOR OF SN 2011fe

Bloom, J.; Kasen, Daniel; Shen, Ken J.; Nugent, P.; Butler, Nathaniel R.; Graham, M. L.; Howell, D. A.; Kolb, U.; Holmes, S.; Haswell, C. A.; Burwitz, V.; Rodríguez, J.; Sullivan, M.

doi:10.1088/2041-8205/744/2/l17

Cited by 296 publications

(360 citation statements)

References 54 publications

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“…The diffusion of radiation from the shock-heated ejecta in the explosion is thought to be a contributor to the excess luminosity of SNe in addition to the luminosity generated by nickel heating. This shock breakout model has been used to put considerable constraints on the radius of the progenitor star by detecting the early shock luminosity (Nugent et al 2011;Bloom et al 2012). …”

Section: Cooling Of the Shock-heated Wdmentioning

confidence: 99%

“…5, we compare the early-time observations of SN 2012cg in the uvm2-band to the predicted early-time light curves from the analytical model of RLW12 to examine the possibility that the early excess luminosity detected in SN 2012cg was produced from cooling of the shock-heated WD. Here, we assume an explosion energy of 10 51 erg, an ejecta mass of 1.4 M ⊙ , a form factor of 0.05, and an electron scattering opacity 0.2 cm 2 g −1 (Bloom et al 2012). As shown in Fig.…”

Section: Cooling Of the Shock-heated Wdmentioning

confidence: 99%

“…This has been suggested to be evidence that supports the SD scenario because such CSM is generally expected to exist around SN Ia progenitor as the result of mass transfer from the companion star, as well as from WD winds. On the other hand, there is some evidence in favour of the DD scenario, e.g., the nondetection of pre-explosion companion stars in normal SNe Ia (Li et al 2011;Bloom et al 2012), the absence of H/He features in the nebular spectra of SNe Ia (Leonard 2007;Lundqvist et al 2013Lundqvist et al , 2015Shappee, Kochanek & Stanek 2013;Maguire et al 2016), the lack of radio and X-ray emission around peak brightness (Bloom et al 2012;Brown et al 2012;Chomiuk et al 2012;Horesh et al 2012;Margutti et al 2014), and the absence of a sur-viving companion star in SN Ia remnants (Kerzendorf et al 2009;Schaefer & Pagnotta 2012).…”

Section: Introductionmentioning

confidence: 99%

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Constraining the progenitor of the Type Ia Supernova SN 2012cg

Liu

Stancliffe

2016

Mon. Not. R. Astron. Soc.

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The nature of the progenitors of Type Ia supernovae (SNe Ia) is not yet fully understood. In the single-degenerate (SD) scenario, the collision of the SN ejecta with its companion star is expected to produce detectable ultraviolet (UV) emission in the first few days after the SN explosion within certain viewing angles. It was recently found that the B − V colour of the nearby SN Ia SN 2012cg at about sixteen days before the maximum B-band brightness was about 0.2 mag bluer than those of other normal SNe Ia, which was reported as the first evidence for excess blue light from the interaction of normal SN Ia ejecta with its companion star. In this work, we compare current observations for SN 2012cg from its pre-explosion phase to the late-time nebular phase with theoretical predictions from binary evolution and population synthesis calculations for a variety of popular progenitor scenarios. We find that a main-sequence donor or a carbon-oxygen white dwarf donor binary system is more likely to be the progenitor of SN 2012cg. However, both scenarios also predict properties which are in contradiction to the observed features of this system. Taking both theoretical and observational uncertainties into account, we suggest that it might be too early to conclude that SN 2012cg was produced from an explosion of a Chandrasekhar-mass white dwarf in the SD scenario. Future observations and improved detailed theoretical modelling are still required to place a more stringent constraint on the progenitor of SN 2012cg.

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Section: Cooling Of the Shock-heated Wdmentioning

confidence: 99%

Section: Cooling Of the Shock-heated Wdmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Constraining the progenitor of the Type Ia Supernova SN 2012cg

Liu

Stancliffe

2016

Mon. Not. R. Astron. Soc.

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“…Extremely nearby SNe Ia which were discovered soon after explosion have recently led to tight constraints on the size and luminosity of the companion star, thus ruling out many plausible SD scenarios for these objects (e.g., Nugent et al 2011;Ganeshalingam et al 2011;Brown et al 2012;Foley et al 2012a;Bloom et al 2012;Silverman et al 2012b). 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).…”

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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“…The closeness of SN2011fe has made it possible to obtain the tightest constraints on the supernova and its progenitor system to date in a variety of observational windows. Red giant and helium star companions, symbiotic systems, systems at the origin of optically thick winds or containing recurrent novae are excluded for SN2011fe (Li et al 2011a;Bloom et al 2012;Brown et al 2012;Chomiuk et al 2012), leaving only either DD or a few cases of SD as possible progenitor systems of this supernova.…”

Section: Introductionmentioning

confidence: 99%

Observation of SN2011fe with INTEGRAL

Isern¹,

Jean²,

Bravo³

et al. 2013

A&A

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Context. SN2011fe was detected by the Palomar Transient Factory in M101 on August 24, 2011, a few hours after the explosion. From the early optical spectra it was immediately realized that it was a Type Ia supernova, thus making this event the brightest one discovered in the past twenty years. Aims. The distance of the event offered the rare opportunity of performing a detailed observation with the instruments onboard INTEGRAL to detect the γ-ray emission expected from the decay chains of 56 Ni. The observations were performed in two runs, one before and around the optical maximum, aimed to detect the early emission from the decay of 56 Ni, and another after this maximum aimed to detect the emission of 56 Co. Methods. The observations performed with the instruments onboard INTEGRAL (SPI, IBIS/ISGRI, JEMX, and OMC) were analyzed and compared with the existing models of γ-ray emission from this kind of supernova. In this paper, the analysis of the γ-ray emission has been restricted to the first epoch. Results. SPI and IBIS/ISGRI only provide upper limits to the expected emission due to the decay of 56 Ni. These upper limits on the gamma-ray flux are 7.1 × 10 −5 ph/s/cm 2 for the 158 keV line and 2.3 × 10 −4 ph/s/cm 2 for the 812 keV line. These bounds allow rejecting at the 2σ level explosions involving a massive white dwarf, ∼1 M in the sub-Chandrasekhar scenario and specifically all models that would have substantial amounts of radioactive 56 Ni in the outer layers of the exploding star responsible for the SN2011fe event. The optical light curve obtained with the OMC camera also suggests that SN2011fe was the outcome of the explosion of a CO white dwarf, possibly through the delayed detonation mode, although other ones are possible, of a CO that synthesized ∼0.55 M of 56 Ni. For this specific model, INTEGRAL would have only been able to detect this early γ-ray emission if the supernova had occurred at a distance < ∼ 2 Mpc. Conclusions. The detection of the early γ-ray emission of 56 Ni is difficult, and it can only be achieved with INTEGRAL if the distance of the event is close enough. The exact distance depends on the specific SNIa subtype. The broadness and rapid rise of the lines are probably at the origin of this difficulty.

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A COMPACT DEGENERATE PRIMARY-STAR PROGENITOR OF SN 2011fe

Cited by 296 publications

References 54 publications

Constraining the progenitor of the Type Ia Supernova SN 2012cg

Constraining the progenitor of the Type Ia Supernova SN 2012cg

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Observation of SN2011fe with INTEGRAL

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