Signatures of a Companion Star in Type Ia Supernovae

Maeda, Keiichi; Kutsuna, Masamichi; Shigeyama, Toshikazu

doi:10.1088/0004-637x/794/1/37

Cited by 59 publications

(63 citation statements)

References 71 publications

(123 reference statements)

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“…A true norm could also originate from multiple binary configurations and explosive conditions Blondin et al 2012;Dessart et al 2014). Similarly, select subclasses may either represent bimodal characteristics of one or two dominant channels (Maeda et al 2010;Maund et al 2010;Röpke et al 2012;Liu et al 2015), or a predominant family where continuous differences such as progenitor metallicities (among other parameters) yield the observed diversity (Nugent et al 1995;Lentz et al 2000;Höflich et al 2002;Scalzo et al 2014a;Maeda et al 2014). A dominant one (or two) progenitor system + explosion mechanism might then manifest properties about the norm that reach out into the same observational parameter space inhabited by the most peculiar subgroups (Baron 2014).…”

Section: Discussionmentioning

confidence: 99%

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

Parrent¹,

Howell²,

Fesen³

et al. 2016

Mon. Not. R. Astron. Soc.

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SN 2012dn is a super-Chandrasekhar mass candidate in a purportedly normal spiral (SAcd) galaxy, and poses a challenge for theories of type Ia supernova diversity. Here we utilize the fast and highly parameterized spectrum synthesis tool, SYNAPPS, to estimate relative expansion velocities of species inferred from optical spectra obtained with six facilities. As with previous studies of normal SN Ia, we find that both unburned carbon and intermediate mass elements are spatially coincident within the ejecta near and below 14,000 km s −1 . Although the upper limit on SN 2012dn's peak luminosity is comparable to some of the most luminous normal SN Ia, we find a progenitor mass exceeding ∼ 1.6 M is not strongly favored by leading merger models since these models do not accurately predict spectroscopic observations of SN 2012dn and more normal events. In addition, a comparison of light curves and host-galaxy masses for a sample of literature and Palomar Transient Factory SN Ia reveals a diverse distribution of SN Ia subtypes where carbon-rich material remains unburned in some instances. Such events include SN 1991T, 1997br, and 1999aa where trace signatures of C III at optical wavelengths are presumably detected.

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Section: Discussionmentioning

confidence: 99%

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

Parrent¹,

Howell²,

Fesen³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…This could either be done by searching for absorption or emission lines from a circumstellar medium (CSM) around normal SNe Ia (e.g., Mattila et al 2005;Patat et al 2007b;A&A 577, A39 (2015) Simon et al 2009;Dilday et al 2012;Lundqvist et al 2013;Sternberg et al 2014) or by identifying material blasted off or evaporated from the non-compact companion owing to the impact of the SN ejecta (e.g., Mattila et al 2005;Leonard 2007;Shappee et al 2013;Lundqvist et al 2013;Maeda et al 2014). Of these, absorption lines from a CSM may be the least conclusive, since such lines may also exist in DD scenarios (Shen et al 2013) or in alternative scenarios for SNe Ia (e.g., .…”

Section: Introductionmentioning

confidence: 99%

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

121

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Aims. This study aims at constraining the origin of the nearby Type Ia supernovae (SNe), 2011fe and 2014J. The two most favoured scenarios for triggering the explosion of the white dwarf supernova progenitor is either mass loss from a non-degenerate companion or merger with another white dwarf. In the former, there could be a significant amount of leftover material from the companion at the centre of the supernova. Detecting such material would therefore favour the single-degenerate scenario. Methods. The left-over material from a possible non-degenerate companion can reveal itself after about one year, and in this study such material was searched for in the spectra of SN 2011fe (at 294 days after the explosion) using the Large Binocular Telescope and for SN 2014J using the Nordic Optical Telescope (315 days past explosion). The observations were interpreted using numerical models simulating the expected line emission from ablated material from the companion star. λλ7291, 7324 could be traced for in any of the two supernovae. When systematic uncertainties are included, the limits on hydrogen-rich ablated gas are 0.003 M in SN 2011fe and 0.0085 M in SN 2014J, where the limit for SN 2014J is the second lowest ever, and the limit for SN 2011fe is a revision of a previous limit. Limits are also put on heliumrich ablated gas, and here limits from [O I] λ6300 provide the upper mass limits 0.002 M and 0.005 M for SNe 2011fe and 2014J, respectively. These numbers are used in conjunction with other data to argue that these supernovae can stem from double-degenerate systems or from single-degenerate systems with a spun-up/spun-down super-Chandrasekhar white dwarf. For SN 2011fe, other types of hydrogen-rich donors can very likely be ruled out, whereas a main-sequence donor system with large intrinsic separation is still possible for SN 2014J. Helium-rich donor systems cannot be ruled out for any of the two supernovae, but the expected short delay time for such progenitors makes this possibility less likely, especially for SN 2011fe. Published data for SNe 1998bu, 2000cx, 2001el, 2005am, and 2005cf are used to constrain their origin. We emphasise that the results of this study depend on the sought-after lines emerging unattenuated from the central regions of the nebula. Detailed radiative transfer calculations with longer line lists than are presently used are needed to confirm that this is, in fact, true. Finally, the broad lines of SNe 2011fe and 2014J are discussed, and it is found that the [Ni II] λ7378 emission is redshifted by ∼+1300 km s −1 , as opposed to the known blueshift of ∼−1100 km s −1 for SN 2011fe. [Fe II] λ7155 is also redshifted in SN 2014J. SN 2014J belongs to a minority of SNe Ia that both have a nebular redshift of [Fe II] λ7155 and [Ni II] λ7378, and a slow decline of the Si II λ6355 absorption trough just after B-band maximum.

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“…In the nebular phase when the inner layers are transparent, emission from the contaminated inner layers becomes observable. It has been argued that nebular Hα emission from the stripped matter should be detectable in Type Ia SNe that originate in single-degenerate progenitor systems, although this has not yet been observed (Mattila et al 2005;Leonard 2007;Shappee et al 2013;Lundqvist et al 2013Lundqvist et al , 2015Maeda et al 2014). The stripped mass in Type Ia SNe is estimated to be less than ∼10 −3 M .…”

Section: Introductionmentioning

confidence: 98%

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

Moriya

Liu

Mackey

et al. 2015

A&A

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We propose that nebular Hα emission, as detected in the Type Ic superluminous supernova iPTF13ehe, stems from matter that is stripped from a companion star when the supernova ejecta collide with it. The temporal evolution, the line broadening, and the overall blueshift of the emission are consistent with this interpretation. We scale the nebular Hα luminosity predicted for Type Ia supernovae in single-degenerate systems to derive the stripped mass required to explain the Hα luminosity of iPTF13ehe. We find a stripped mass of 0.1−0.9 solar masses, assuming that the supernova luminosity is powered by radioactivity or magnetar spin down. Because a central heating source is required to excite the Hα emission, an interaction-powered model is not favored for iPTF13ehe if the Hα emission is from stripped matter. We derive a companion mass of more than 20 solar masses and a binary separation of less than about 20 companion radii based on the stripping efficiency during the collision, indicating that the supernova progenitor and the companion formed a massive close binary system. If Type Ic superluminous supernovae generally occur in massive close binary systems, the early brightening observed previously in several Type Ic superluminous supernovae may also be due to the collision with a close companion. Observations of nebular hydrogen emission in future Type Ic superluminous supernovae will enable us to test this interpretation.

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Signatures of a Companion Star in Type Ia Supernovae

Cited by 59 publications

References 71 publications

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

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

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