The<sup>44</sup>Ti-powered spectrum of SN 1987A

Jerkstrand, A.; Fransson, Claes; Kozma, Cecilia

doi:10.1051/0004-6361/201015937

Cited by 172 publications

(272 citation statements)

References 110 publications

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“…In the case of the [O I] doublet we note that the Hα from the reverse shock overlaps with the Å 6364 component and that there may also be blending with emission from FeIl6300 (Fransson & Kozma 2002). It is also possible that there is a contribution from HeIl5876 blended with the NaI doublet, although Jerkstrand et al (2011) find that NaI dominates. The identification of the MgII lines is discussed in Jerkstrand et al (2011) and Fransson et al (2013).…”

Section: Spatial Alignment Of Data Setsmentioning

confidence: 75%

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Larsson

Fransson

Spyromilio³

et al. 2016

ApJ

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Due to its proximity, SN1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN1987A obtained ∼10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of Hα to date, the first 3D maps for 44 Ti. The time evolution of Hα shows that it is predominantly powered by X-rays from the ring, in agreement with previous findings. All lines that have sufficient signal show a similar large-scale 3D structure, with a north-south asymmetry that resembles a broken dipole. This structure correlates with early observations of asymmetries, showing that there is a global asymmetry that extends from the inner core to the outer envelope. On smaller scales, the two brightest lines, Hα and [Si I]+[Fe II] 1.644 μm, show substructures at the level of ∼200-1000 km s -1 and clear differences in their 3D geometries. We discuss these results in the context of explosion models and the properties of dust in the ejecta.

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Section: Spatial Alignment Of Data Setsmentioning

confidence: 75%

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Larsson

Fransson

Spyromilio³

et al. 2016

ApJ

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“…Each zone in the core is distributed over N cl = 10 4 identical clumps (see Jerkstrand et al (2011) for details on how this is 1 A more detailed investigation of the line profiles in SN 2011dh is given in E14b.…”

Section: The Corementioning

confidence: 99%

Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh

Jerkstrand

Ergon

Smartt

et al. 2014

A&A

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We investigate line formation processes in Type IIb supernovae (SNe) from 100 to 500 days post-explosion using spectral synthesis calculations. The modelling identifies the nuclear burning layers and physical mechanisms that produce the major emission lines, and the diagnostic potential of these. We compare the model calculations with data on the three best observed Type IIb SNe to-date − SN 1993J, SN 2008ax, and SN 2011dh. Oxygen nucleosynthesis depends sensitively on the main-sequence mass of the star and modelling of the [O I] λλ6300, 6364 lines constrains the progenitors of these three SNe to the M ZAMS = 12−16 M range (ejected oxygen masses 0.3−0.9 M ), with SN 2011dh towards the lower end and SN 1993J towards the upper end of the range. The high ejecta masses from M ZAMS 17 M progenitors give rise to brighter nebular phase emission lines than observed. Nucleosynthesis analysis thus supports a scenario of low-to-moderate mass progenitors for Type IIb SNe, and by implication an origin in binary systems. We demonstrate how oxygen and magnesium recombination lines may be combined to diagnose the magnesium mass in the SN ejecta. For SN 2011dh, a magnesium mass of 0.02−0.14 M is derived, which gives a Mg/O production ratio consistent with the solar value. Nitrogen left in the He envelope from CNO burning gives strong [N II] λλ6548, 6583 emission lines that dominate over Hα emission in our models. The hydrogen envelopes of Type IIb SNe are too small and dilute to produce any noticeable Hα emission or absorption after ∼150 days, and nebular phase emission seen around 6550 Å is in many cases likely caused by [N II] λλ6548, 6583. Finally, the influence of radiative transport on the emergent line profiles is investigated. Significant line blocking in the metal core remains for several hundred days, which affects the emergent spectrum. These radiative transfer effects lead to early-time blueshifts of the emission line peaks, which gradually disappear as the optical depths decrease with time. The modelled evolution of this effect matches the observed evolution in SN 2011dh.

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“…This could lead us to underestimate line scattering and fluorescence. As noted in Pérez- Torres et al (2014), more recent models (e.g., Jerkstrand et al 2011) with more extensive line lists and more complete sets of ions and atomic levels, albeit not yet time-dependent, should be used to estimate these effects.…”

Section: Uncertaintiesmentioning

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

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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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The⁴⁴Ti-powered spectrum of SN 1987A

Cited by 172 publications

References 110 publications

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh

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

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The44Ti-powered spectrum of SN 1987A

Cited by 172 publications

References 110 publications

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Three-Dimensional Distribution of Ejecta in Supernova 1987a at 10,000 Days

Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh

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

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The⁴⁴Ti-powered spectrum of SN 1987A