The Origin of the Late-time Luminosity of Supernova 2011dh

Maund, Justyn R.

doi:10.3847/1538-4357/ab2386

Cited by 30 publications

(31 citation statements)

References 57 publications

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“…Different groups obtain somewhat different DTDs (e.g., Graur et al 2014;Heringer et al 2017;Maoz, & Graur 2017;Frohmaier et al 2019;Wiseman et al 2021). I use here the same expression as I derived in Soker (2019b) that I based on the DTDs of Friedmann & Maoz (2018) for galaxy clusters and of Heringer, Pritchet, & van Kerkwijk (2019) for field galaxies…”

Section: The Delay Time Distribution (Dtd)mentioning

confidence: 98%

Common envelope to explosion delay time of Type Ia supernovae

Soker

2019

Monthly Notices of the Royal Astronomical Society

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I study the rate of type Ia supernovae (SNe Ia) within about a million years after the assumed common envelope evolution (CEE) that forms the progenitors of these SNe Ia, and find that the population of SNe Ia with short CEE to explosion delay (CEED) time is ≈ few × 0.1 of all SNe Ia. I also claim for an expression for the rate of these SNe Ia that occur at short times after the CEE, t CEED 10 6 yr, that is different from that of the delay time distribution (DTD) billions of years after star formation. This tentatively hints that the physical processes that determine the short CEED times are different (at least to some extend) from those that determine the DTD at billions of years. To reach these conclusions I examine SNe Ia that interact with a circumstellar matter (CSM) within months after explosion, so called SNe Ia-CSM, and the rate of SNe Ia that on a time scale of tens to hundreds of years interact with a CSM that might have been a planetary nebula, so called SNe Ia inside a planetary nebula (SNIPs). I assume that the CSM in these populations results from a CEE, and hence this study is relevant mainly to the core degenerate (CD) scenario, to the double degenerate (DD) scenario, to the double detonation (DDet) scenario with white dwarf companions, and to the CEE-wind channel of the single degenerate (SD) scenario.

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Section: The Delay Time Distribution (Dtd)mentioning

confidence: 98%

Common envelope to explosion delay time of Type Ia supernovae

Soker

2019

Monthly Notices of the Royal Astronomical Society

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“…We follow Ergon et al (2014) in adopting a distance of d = 7.8 +1.1 −0.9 Mpc to the host galaxy of SN 2011dh, the Whirlpool Galaxy, and in taking a total dust reddening of E (B − V) = 0.07 +0.07 −0.04 mag. Maund (2019) used a light echo to isolate the flux contribution of a surviving companion. We take the upper limit in the F435W filter, and treat the brighter bounds reported by Maund (2019) in the F225W and F336W filters as upper limits (Table 3).…”

Section: Sn 2011dh (Iib)mentioning

confidence: 99%

“…Maund (2019) used a light echo to isolate the flux contribution of a surviving companion. We take the upper limit in the F435W filter, and treat the brighter bounds reported by Maund (2019) in the F225W and F336W filters as upper limits (Table 3).…”

Section: Sn 2011dh (Iib)mentioning

confidence: 99%

How much hydrogen is in Type Ib and IIb supernova progenitors?

Gilkis,

Arcavi

2021

Preprint

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Core-collapse supernovae showing little or no hydrogen (denoted Type IIb and Ib, respectively) are the explosions of massive stars that lost some or most of their outer envelopes. How they lose their mass is unclear, but it likely involves binary interaction. So far, seven progenitors of such supernovae have been identified in pre-explosion imaging (five for Type IIb events and two for Type Ib events). Here we evolve detailed binary stellar evolution models in order to better understand the nature of these progenitors. We find that the amount of hydrogen left in the envelope at the time of explosion greatly depends on the post-interaction mass-loss rate. The leftover hydrogen, in turn, strongly affects progenitor properties, such as temperature and photospheric radius, in non-trivial ways. Together with extinction and distance uncertainties in progenitor data, it is difficult to deduce an accurate progenitor hydrogen mass from pre-explosion imaging. We quantify this uncertainty and find that available data is consistent with the proposed Type Ib -IIb hydrogen mass threshold of 0.033 M (Hachinger et al. 2012) but not with the proposed threshold of 0.001 M (Dessart et al. 2011), implying that even Type Ib progenitors are not pure helium stars. These results alleviate the proposed tension between the Type Ib classification of SN 2019yvr and its candidate progenitor properties (Kilpatrick et al. 2021). We also estimate the brightness of a surviving 2019yvr progenitor companion, which might be detected in future observations.

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“…Currently, there are only four corecollapse SNe with a direct companion detection, i.e. the Type IIb SN 1993J (Maund et al 2004;Fox et al 2014), SN 2001ig (Ryder et al 2018) and SN 2011dh (Folatelli et al 2014;Maund et al 2015;Maund 2019), and the Type Ibn SN 2006jc ). The detected companions can place tight constraints on the initial properties and the pre-SN evolution of the SN progenitor systems.…”

Section: Introductionmentioning

confidence: 99%

An environmental analysis of the Type Ib SN 2019yvr and the possible presence of an inflated binary companion

Sun,

Maund,

Crowther

et al. 2021

Preprint

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SN 2019yvr is the second Type Ib supernova (SN) with a direct detection of its progenitor (system); however, the spectral energy distribution (SED) of the pre-explosion source appears much cooler and overluminous than an expected helium-star progenitor. Using Hubble Space Telescope (HST) images and MUSE integral-field-unit (IFU) spectroscopy, we find the SN environment contains three episodes of star formation; the low ejecta mass suggests the SN progenitor is most likely from the oldest population, corresponding to an initial mass of 10.4 +1.5 −1.3 𝑀 . The pre-explosion SED can be reproduced by two components, one for the hot and compact SN progenitor and one for a cool and inflated yellow hypergiant (YHG) companion that dominates the brightness. Thus, SN 2019yvr could possibly be the first Type Ib/c SN for which the progenitor's binary companion is directly detected on pre-explosion images. Both the low progenitor mass and the YHG companion suggest significant binary interaction during their evolution. Similar to SN 2014C, SN 2019yvr exhibits a metamorphosis from Type Ib to Type IIn, showing signatures of interaction with hydrogen-rich circumstellar material (CSM) at >150 days; our result supports enhanced pre-SN mass loss as an important process for hydrogen-poor stars at the low mass end of core-collapse SN progenitors.

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The Origin of the Late-time Luminosity of Supernova 2011dh

Cited by 30 publications

References 57 publications

Common envelope to explosion delay time of Type Ia supernovae

Common envelope to explosion delay time of Type Ia supernovae

How much hydrogen is in Type Ib and IIb supernova progenitors?

An environmental analysis of the Type Ib SN 2019yvr and the possible presence of an inflated binary companion

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