Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Hunter, David J.; Valenti, S.; Kotak, R.; Meikle, W. P. S.; Taubenberger, S.; Pastorello, A.; Benetti, S.; Stanishev, V.; Smartt, S. J.; Trundle, C.; Arkharov, A. A.; Bufano, F.; Cappellaro, E.; Carlo, E. Di; Dolci, M.; Elias‐Rosa, N.; Frandsen, S.; Fynbo, J. P. U.; Hopp, U.; Larionov, V. M.; Laursen, Peter; Mazzali, P. A.; Navasardyan, H.; Ries, C.; Riffeser, A.; Rizzi, L.; Tsvetkov, D. Yu.; Turatto, M.; Wilke, S.

doi:10.1051/0004-6361/200912896

Cited by 124 publications

(112 citation statements)

References 107 publications

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“…However, the constraints obtained are not necessarily inconsistent, and at least in the O/C zone, a small amount of molecular (CO) cooling at day ∼100, increasing to an intermediate amount after day ∼250, seems reasonable. Carbon-monoxide emission has been reported for the Type Ic SNe 2002ew (Gerardy et al 2002) and 2007gr (Hunter et al 2009), but for Type Ib and IIb SNe we have found no reports of CO emission in the literature. However, there is a feature near 23 000 Å in the NIR spectra of SN 1993J (Matthews et al 2002) that could be interpreted as a modest amount of CO first-overtone emission.…”

Section: Dust Molecules and The Mir Evolutioncontrasting

confidence: 54%

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

Ergon

Jerkstrand

Sollerman

et al. 2015

A&A

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We present optical and near-infrared (NIR) photometry and spectroscopy as well as modelling of the lightcurves of the Type IIb supernova (SN) 2011dh. Our extensive dataset, for which we present the observations obtained after day 100, spans two years, and complemented with Spitzer mid-infrared (MIR) data, we use it to build an optical-to-MIR bolometric lightcurve between days 3 and 732. To model the bolometric lightcurve before day 400 we use a grid of hydrodynamical SN models, which allows us to determine the errors in the derived quantities, and a bolometric correction determined with steady-state non-local thermodynamic equilibrium (NLTE) modelling. Using this method we find a helium core mass of 3.1 +0.7 −0.4 M for SN 2011dh, consistent within error bars with previous results obtained using the bolometric lightcurve before day 80. We compute bolometric and broad-band lightcurves between days 100 and 500 from spectral steady-state NLTE models, presented and discussed in a companion paper. The preferred 12 M (initial mass) model, previously found to agree well with the observed spectra, shows a good overall agreement with the observed lightcurves, although some discrepancies exist. Time-dependent NLTE modelling shows that after day ∼600 a steadystate assumption is no longer valid. The radioactive energy deposition in this phase is likely dominated by the positrons emitted in the decay of 56 Co, but seems insufficient to reproduce the lightcurves, and what energy source is dominating the emitted flux is unclear. We find an excess in the K and the MIR bands developing between days 100 and 250, during which an increase in the optical decline rate is also observed. A local origin of the excess is suggested by the depth of the He  20 581 Å absorption. Steady-state NLTE models with a modest dust opacity in the core (τ = 0.44), turned on during this period, reproduce the observed behaviour, but an additional excess in the Spitzer 4.5 µm band remains. Carbon-monoxide (CO) first-overtone band emission is detected at day 206, and possibly at day 89, and assuming the additional excess to be dominated by CO fundamental band emission, we find fundamental to first-overtone band ratios considerably higher than observed in SN 1987A. The profiles of the [O ] 6300 Å and Mg ] 4571 Å lines show a remarkable similarity, suggesting that these lines originate from a common nuclear burning zone (O/Ne/Mg), and using small scale fluctuations in the line profiles we estimate a filling factor of 0.07 for the emitting material. This paper concludes our extensive observational and modelling work on SN 2011dh. The results from hydrodynamical modelling, steady-state NLTE modelling, and stellar evolutionary progenitor analysis are all consistent, and suggest an initial mass of ∼12 M for the progenitor.

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Section: Dust Molecules and The Mir Evolutioncontrasting

confidence: 54%

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

Ergon

Jerkstrand

Sollerman

et al. 2015

A&A

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“…That molecules can form in stripped-envelope SNe was evidenced by the detection of the CO first overtone in the Type Ic SN 2000ew at ∼100 days (Gerardy et al 2002). A second detection was reported for the Type Ic SN 2007gr (Hunter et al 2009), where high observational cadence showed the onset of CO overtone emission between 50−70 days. The CO first overtone detection in SN 2011dh (E14b) provides the first unambigous detection of CO in a Type Ib or IIb SN.…”

Section: Moleculesmentioning

confidence: 89%

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 classical Type Ic SN 1994I, which had an ejecta mass of only 1 M⊙(e.g., Iwamoto et al 1994;Sauer et al 2006) may be an example of a SN Ic located between typical stripped-envelope SNe and ultra-stripped SNe. Also, the low-mass Type Ic SN 2007gr (Hunter et al 2009;Mazzali et al 2010) may be an even more extreme case.…”

Section: Diversitymentioning

confidence: 99%

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We investigate light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are the explosions of heavily stripped massive stars which lost their envelopes via binary interactions with a compact companion star. They eject only ∼ 0.1 M ⊙ and may be the main way to form double neutronstar systems which eventually merge emitting strong gravitational waves. We follow the evolution of an ultra-stripped supernova progenitor until iron core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae using the nucleosynthesis results and present their expected properties. Ultra-stripped supernovae synthesize ∼ 0.01 M ⊙ of radioactive 56 Ni, and their typical peak luminosity is around 10 42 erg s −1 or −16 mag. Their typical rise time is 5 − 10 days. Comparing synthesized and observed spectra, we find that SN 2005ek, some of the so-called calcium-rich gap transients, and SN 2010X may be related to ultra-stripped supernovae. If these supernovae are actually ultra-stripped supernovae, their event rate is expected to be about 1 per cent of core-collapse supernovae. Comparing the double neutron-star merger rate obtained by future gravitational-wave observations and the ultra-stripped supernova rate obtained by optical transient surveys identified with our synthesized light-curve and spectral models, we will be able to judge whether ultra-stripped supernovae are actually a major contributor to the binary neutron star population and provide constraints on binary stellar evolution.

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Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Cited by 124 publications

References 107 publications

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

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

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

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