Revealing the binary origin of Type Ic superluminous supernovae through nebular hydrogen emission

Moriya, Takashi J.; Liu, Zheng-Wei; Mackey, Jonathan; Chen, Ting-Wan; Langer, N.

doi:10.1051/0004-6361/201527515

Cited by 27 publications

(23 citation statements)

References 58 publications

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“…This may be in tension with the massive binary model because it predicted that we should see both redshifted and blueshifted Hα emission lines relative to the host galaxies (Moriya et al 2015). Interestingly, the velocity offsets between the broad Hα and the host galaxies change from positive to negative with time for two of the events.…”

Section: Discussionmentioning

confidence: 87%

See 1 more Smart Citation

Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Yan

Lunnan

Perley

et al. 2017

ApJ

121

134

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We present observations of two new hydrogen-poor superluminous supernovae (SLSN-I), iPTF15esb and iPTF16bad, showing late-time Hα emission with line luminosities of 1 3 10 41 ( -) erg s −1 and velocity widths of (4000-6000) km s −1 . Including the previously published iPTF13ehe, this makes up a total of three such events to date. iPTF13ehe is one of the most luminous and the slowest evolving SLSNe-I, whereas the other two are less luminous and fast decliners. We interpret this as a result of the ejecta running into a neutral H-shell located at a radius of ∼10 16 cm. This implies that violent mass loss must have occurred several decades before the supernova explosion. Such a short time interval suggests that eruptive mass loss could be common shortly before core collapse, and more importantly helium is unlikely to be completely stripped off the progenitor and could be present in the ejecta. It is a mystery why helium features are not detected, even though nonthermal energy sources, capable of ionizing He, may exist as suggested by the O II absorption series in the early-time spectra. Our late-time spectra (+240 days) appear to have intrinsically lower [O I] 6300 Å luminosities than that of SN2015bn and SN2007bi, which is possibly an indication of less oxygen (<10 M e ). The blueshifted Hα emission relative to the hosts for all three events may be in tension with the binary model proposed for iPTF13ehe. Finally, iPTF15esb has a peculiar light curve (LC) with three peaks separated from one another by ∼22 days. The LC undulation is stronger in bluer bands. One possible explanation is ejecta-circumstellar medium interaction.

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Section: Discussionmentioning

confidence: 87%

“…The third possibility is proposed by Moriya et al (2015), where the progenitor is in a binary system with a massive, H-rich companion star ( M 20 >  ). The explosive ejecta strip off a small amount of H from the companion star, which is then mixed in the inner regions of the ejecta.…”

Section: Nature Of the Hα Emission And Implication For Helium In The mentioning

confidence: 99%

Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Yan

Lunnan

Perley

et al. 2017

ApJ

121

134

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“…The existence of hydrogen-free dense CSM in Type I SLSNe has been speculated in many studies (Chevalier & Irwin 2011; Moriya & Maeda 2012;Ginzburg & Balberg 2012;Chatzopoulos et al 2013a;Sorokina et al 2016;Chen et al 2016;Tolstov et al 2017a,b). The existence of a CSM shell is also identified in the Type Ic SLSN iPTF16eh (Lunnan et al 2018a), as well as in three Type Ic SLSNe with late-phase hydrogen emission (Yan et al 2015(Yan et al , 2017, but see also Moriya et al 2015). In our energetic core-collapse SN models, the dense CSM may have been formed shortly before the explosion by the pulsational pair-instability (Woosley et al 2007;Woosley 2017) because the carbon-oxygen core of our progenitor is massive enough to initiate the instability.…”

Section: Discussionmentioning

confidence: 91%

Synthetic spectra of energetic core-collapse supernovae and the early spectra of SN 2007bi and SN 1999as

Moriya

Mazzali

Tanaka

2019

Monthly Notices of the Royal Astronomical Society

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SN 2007bi and SN 1999as are among the first superluminous supernovae discovered. SN 2007bi was suggested to be powered by the radioactive decay of a large amount (5 − 10 M ⊙ ) of 56 Ni. SN 1999as has a similar spectrum to SN 2007bi. One suggested way to synthesize such a large amount of 56 Ni is through energetic core-collapse supernovae from very massive progenitors. Although the synthetic light curves of extremely energetic core-collapse supernovae have been shown to be consistent with SN 2007bi, no synthetic spectra have been reported. Here, we present synthetic spectra of extremely energetic core-collapse supernovae during the photospheric phases. We find that the ejecta density structure above 13, 000 − 16, 000 km s −1 needs to be cut in order to explain the co-existing broad and narrow line absorptions in SN 2007bi and SN 1999as. The density cut is likely caused by the interaction between the supernova ejecta and a dense circumstellar medium. Our results indicate that about 3 M ⊙ of hydrogen-free dense circumstellar media might exist near the progenitors of SN 2007bi and SN 1999as. These massive circumstellar media would significantly affect the lightcurve and spectral properties of the supernovae. The precursors that are sometimes observed in superluminous supernovae might be related to the collision of the ejecta with such dense circumstellar media. We also confirm results of previous studies that synthetic spectra from pair-instability supernova models do not match the early spectra of SN 2007bi and SN 1999as.

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“…Finally, recent observations of the SNIb2014C reveal evidence for interaction with a hydrogen-rich circumstellar medium (CSM) that was expelled in the years prior to the explosion (Milisavljevic et al 2015; see also Chugai & Chevalier 2006;Moriya et al 2015;Yan et al 2015). Should we then expect trace amounts of hydrogen to remain within the outermost layers of the progenitor for some of these typeI core-collapse events?…”

Section: Introductionmentioning

confidence: 99%

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Parrent

Milisavljević

Söderberg

et al. 2016

ApJ

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Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000-6400 Å in typeI spectra are due to more than Si IIλ6355. However, while an interpretation of conspicuous Si IIλ6355 can approximate 6150 Å absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 Å features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with highquality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 Å; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si IIλ6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000-6400 Å features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in Hα, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II.

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Revealing the binary origin of Type Ic superluminous supernovae through nebular hydrogen emission

Cited by 27 publications

References 58 publications

Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory

Synthetic spectra of energetic core-collapse supernovae and the early spectra of SN 2007bi and SN 1999as

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

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