The Type IIb SN 2008ax: spectral and light curve evolution

Pastorello, A.; Kasliwal, M. M.; Crockett, R. M.; Valenti, S.; Arbour, R.; Itagaki, K.; Kaspi, S.; Gal‐Yam, A.; Smartt, S. J.; Griffith, R. L.; Maguire, K.; Ofek, E. O.; Seymour, N.; Stern, Daniel; Wiethoff, W.

doi:10.1111/j.1365-2966.2008.13618.x

Cited by 117 publications

(139 citation statements)

References 72 publications

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“…This is more than the few ×10 −1 M expected for type IIb SNe (e.g. SN 2008ax, see Pastorello et al 2008b, and references therein), but surely less than the several solar masses estimated for a normal type IIP SN (e.g. Nadyozhin 2003).…”

Section: Discussionmentioning

confidence: 91%

SN 1999ga: a low-luminosity linear type II supernova?

Pastorello

Crockett

Martin

et al. 2009

A&A

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Context. Type II-linear supernovae are thought to arise from progenitors that have lost most of their H envelope by the time of the explosion, and they are poorly understood because they are only occasionally discovered. It is possible that they are intrinsically rare, but selection effects due to their rapid luminosity evolution may also play an important role in limiting the number of detections. In this context, the discovery of a subluminous type II-linear event is even more interesting. Aims. We investigate the physical properties and characterise the explosion site of the type II SN 1999ga, which exploded in the nearby spiral galaxy NGC 2442. Methods. Spectroscopic and photometric observations of SN 1999ga allow us to constrain the energetics of the explosion and to estimate the mass of the ejected material, shedding light on the nature of the progenitor star in the final stages of its life. The study of the environment in the vicinity of the explosion site provides information on a possible relation between these unusual supernovae and the properties of the galaxies hosting them. Results. Despite the lack of early-time observations, we provide reasonable evidence that SN 1999ga was probably a type II-linear supernova that ejected a few solar masses of material, with a very small amount of radioactive elements of the order of 0.01 M .

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Section: Discussionmentioning

confidence: 91%

SN 1999ga: a low-luminosity linear type II supernova?

Pastorello

Crockett

Martin

et al. 2009

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“…Some SNe IIb show a distinct primary peak, but most do not (e.g. SN 2008ax, Pastorello et al 2008;Tsvetkov et al 2009Ergon et al 2014). As LSQ13cuw was discovered early, it is unlikely that a primary peak was missed.…”

Section: Photometrymentioning

confidence: 99%

“…Table B.1 lists the local sequence stars from the SDSS DR9 catalogue that were used to calibrate the LT and LCOGT g r i -band Ripero et al (1993); g) Corwin et al (1993); h) Centurion et al (1993); i) Hanzl et al (1993); j) Tweedy et al (1993); k) Dumont et al (1993); l) Pressberger et al (1993); m) Lewis et al (1994); n) Barbon et al (1995); o) Pastorello et al (2008); p) Tsvetkov et al (2009); q) Ergon et al (2014).…”

Section: A31 Radiusmentioning

confidence: 99%

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

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We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P.

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“…Both sets of spectra were, up to 360 days, flux calibrated to the photometry in T11. We adopt a distance of 9.6 Mpc (Pastorello et al 2008;T11) an extinction E B−V = 0.40 mag (T11), a recession velocity 565 km s −1 (M10), a 56 Ni mass of 0.10 M (T11), and an explosion of March 3, 2008 (T11).…”

Section: Sn 2008axmentioning

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

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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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The Type IIb SN 2008ax: spectral and light curve evolution

Cited by 117 publications

References 72 publications

SN 1999ga: a low-luminosity linear type II supernova?

SN 1999ga: a low-luminosity linear type II supernova?

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

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

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