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

Jerkstrand, A.; Ergon, M.; Smartt, S. J.; Fransson, Claes; Sollerman, J.; Taubenberger, S.; Bersten, Melina C.; Spyromilio, J.

doi:10.1051/0004-6361/201423983

Cited by 149 publications

(299 citation statements)

References 123 publications

(165 reference statements)

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“…With the shell displaced to 19,000 km s −1 , the material needed in the atmosphere of SNIb1999dn to reproduce the 6250 Å feature (M H  10 −3 M e ) is less than 0.01M e <M H  0.2M e inferred for SNIIb1993J by Baron et al (1995). This mass estimate does not also conflict with the swept-up 5×10 −2 M e estimated from model comparisons to late-nebular spectra of SNIIb (Jerkstrand et al 2015).…”

Section: Snib1999dnmentioning

confidence: 60%

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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Section: Snib1999dnmentioning

confidence: 60%

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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“…Figure 18 clearly shows that the spectral evolution in the NIR regime is very similar for iPTF13bvn and SN 2008ax. In the analysis by Jerkstrand et al (2015), Si I λ12,000 from explosively synthesized silicon is preferred over He I λ11,970 for the line emerging at 12,000 Å. We also estimate that the He I velocities have decreased from ∼ 20, 000 km s −1 in the early-time spectra to ∼ 15, 000 km s −1 at +79 d, measured from the absorption minimum of the He I λ10,830 line.…”

Section: Near-infrared Spectroscopy Of Iptf13bvnmentioning

confidence: 68%

“…These are likely signatures of emission from He I λ11,970 or Si I λ12,000 and a blend of Mg I λλ15,040, 15,048. These identifications are based on the modeling of the NIR spectra of SN 2008ax at +130 d by Jerkstrand et al (2015). Figure 18 clearly shows that the spectral evolution in the NIR regime is very similar for iPTF13bvn and SN 2008ax.…”

Section: Near-infrared Spectroscopy Of Iptf13bvnmentioning

confidence: 89%

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PTF12os and iPTF13bvn

Fremling

Sollerman

Taddia

et al. 2016

A&A

Self Cite

180

169

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Context. We investigate two stripped-envelope supernovae (SNe) discovered in the nearby galaxy NGC 5806 by the (intermediate) Palomar Transient Factory [(i)PTF]. These SNe, designated PTF12os/SN 2012P and iPTF13bvn, exploded within ∼ 520 days of one another at a similar distance from the host-galaxy center. We classify PTF12os as a Type IIb SN based on our spectral sequence; iPTF13bvn has previously been classified as Type Ib having a likely progenitor with zero age main sequence (ZAMS) mass below ∼ 17 M . Because of the shared and nearby host, we are presented with a unique opportunity to compare these two SNe. Aims. Our main objective is to constrain the explosion parameters of iPTF12os and iPTF13bvn, and to put constraints on the SN progenitors. We also aim to spatially map the metallicity in the host galaxy, and to investigate the presence of hydrogen in early-time spectra of both SNe. Methods. We present comprehensive datasets collected on PTF12os and iPTF13bvn, and introduce a new automatic referencesubtraction photometry pipeline (FPipe) currently in use by the iPTF. We perform a detailed study of the light curves (LCs) and spectral evolution of the SNe. The bolometric LCs are modeled using the hydrodynamical code hyde. We analyze early spectra of both SNe to investigate the presence of hydrogen; for iPTF13bvn we also investigate the regions of the Paschen lines in infrared spectra. We perform spectral line analysis of helium and iron lines to map the ejecta structure of both SNe. We use nebular models and late-time spectroscopy to constrain the ZAMS mass of the progenitors. We also perform image registration of ground-based images of PTF12os to archival HST images of NGC 5806 to identify a potential progenitor candidate. Results. We find that our nebular spectroscopy of iPTF13bvn remains consistent with a low-mass progenitor, likely having a ZAMS mass of ∼ 12 M . Our late-time spectroscopy of PTF12os is consistent with a ZAMS mass of ∼ 15 M . We successfully identify a source in pre-explosion HST images coincident with PTF12os. The colors and absolute magnitude of this object are consistent between pre-explosion and late-time HST images, implying it is a cluster of massive stars. Our hydrodynamical modeling suggests that the progenitor of PTF12os had a compact He core with a mass of 3.25 −0.011 M of strongly mixed 56 Ni. Spectral comparisons to the Type IIb SN 2011dh indicate that the progenitor of PTF12os was surrounded by a thin hydrogen envelope with a mass lower than 0.02 M . We also find tentative evidence that the progenitor of iPTF13bvn could have been surrounded by a small amount of hydrogen prior to the explosion. This result is supported by possible weak signals of hydrogen in both optical and infrared spectra.

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“…Leloudas et al (2010) connected type Ib/c SNe and gamma-ray bursts to WR stars using the relative B-and K-band brightness of their environments. Spectral synthesis model fitting to spectra of SNe at the nebular phase has been used by Mazzali et al (2010) and Jerkstrand et al (2015) to suggest an initially 15 M progenitor for type Ic SN 2007gr and a type IIb progenitor mass range of 12 -16 M , respectively. Tomasella et al (2013) used hydrodynamical modeling to constrain the ejecta mass of a type II-P event, SN 2012A, to 12.5 M .…”

Section: Introductionmentioning

confidence: 99%

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

Kangas

Portinari

Mattila

et al. 2017

A&A

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We study the spatial correlations between the H α emission and different types of massive stars in two local galaxies, the Large Magellanic Cloud (LMC) and Messier 33. We compare these to correlations derived for core-collapse supernovae (CCSNe) in the literature to connect CCSNe of different types with the initial masses of their progenitors and to test the validity of progenitor mass estimates which use the pixel statistics method. We obtain samples of evolved massive stars in both galaxies from catalogues with good spatial coverage and/or completeness, and combine them with coordinates of main-sequence stars in the LMC from the SIMBAD database. We calculate the spatial correlation of stars of different classes and spectral types with H α emission. We also investigate the effects of distance, noise and positional errors on the pixel statistics method. A higher correlation with H α emission is found to correspond to a shorter stellar lifespan, and we conclude that the method can be used as an indicator of the ages, and therefore initial masses, of SN progenitors. We find that the spatial distributions of type II-P SNe and red supergiants of appropriate initial mass ( 9 M ) are consistent with each other. We also find the distributions of type Ic SNe and WN stars with initial masses 20 M consistent, while supergiants with initial masses around 15 M are a better match for type IIb and II-L SNe. The type Ib distribution corresponds to the same stellar types as type II-P, which suggests an origin in interacting binaries. On the other hand, we find that luminous blue variable stars show a much stronger correlation with H α emission than do type IIn SNe.

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

Cited by 149 publications

References 123 publications

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

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

PTF12os and iPTF13bvn

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

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