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

Kangas, T.; Portinari, L.; Mattila, S.; Fraser, M.; Kankare, E.; Izzard, Robert G.; James, P. A.; González-Fernández, C.; Maund, Justyn R.; Thompson, A.

doi:10.1051/0004-6361/201628705

Cited by 27 publications

(25 citation statements)

References 129 publications

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“…In comparison with other SN types it has also been shown that SNe IIn exhibit the least association with ongoing star formation compared to the other CCSNe (Habergham et al 2014). Kangas et al (2017) showed that the SN IIn population does not share a similar spatial distribution in host galaxy Hα light with LBV stars. They are instead best matched with the RSG stars, whose distribution suggests relatively lower mass compared to LBV stars.…”

Section: Discussionmentioning

confidence: 99%

Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy

Kuncarayakti

Anderson

Galbany

et al. 2018

A&A

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Context. Observationally, supernovae are divided into subclasses pertaining to their distinct characteristics. This diversity naturally reflects the diversity in the progenitor stars. It is not entirely clear however, how different evolutionary paths leading massive stars to become a supernova are governed by fundamental parameters such as progenitor initial mass and metallicity. Aims. This paper places constraints on progenitor initial mass and metallicity in distinct core-collapse supernova subclasses, through a study of the parent stellar populations at the explosion sites. Methods. Integral field spectroscopy (IFS) of 83 nearby supernova explosion sites with a median distance of 18 Mpc has been collected and analysed, enabling detection and spectral extraction of the parent stellar population of supernova progenitors. From the parent stellar population spectrum, the initial mass and metallicity of the coeval progenitor are derived by means of comparison to simple stellar population models and strong-line methods. Additionally, near-infrared IFS was employed to characterise the star formation history at the explosion sites. Results. No significant metallicity differences are observed among distinct supernova types. The typical progenitor mass is found to be highest for supernova type Ic, followed by type Ib, then types IIb and II. Type IIn is the least associated with young stellar populations and thus massive progenitors. However, statistically significant differences in progenitor initial mass are observed only when comparing supernovae IIn with other subclasses. Stripped-envelope SN progenitors with initial mass estimate lower than 25 M are found; these are thought to be the result of binary progenitors. Confirming previous studies, these results support the notion that core-collapse supernova progenitors cannot arise from single-star channel only, and both single and binary channels are at play in the production of core-collapse supernovae. Near-infrared IFS suggests that multiple stellar populations with different ages may be present in some of the supernova sites. As a consequence, there could be a non-negligible amount of contamination from old populations, and therefore the individual age estimates are effectively lower limits.

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Section: Discussionmentioning

confidence: 99%

Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy

Kuncarayakti

Anderson

Galbany

et al. 2018

A&A

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“…There is evidence to show that SN type Ib originate from binary systems (Leloudas et al 2011;Eldridge et al 2013;Kuncarayakti et al 2013a;Folatelli et al 2016;Galbany et al 2016;Lyman et al 2016;Kangas et al 2017;Kuncarayakti et al 2018;Taddia et al 2018;Prentice et al 2019), whereby the SN progenitor loses its hydrogen envelope through mass transfer to its companion star rather than through stellar winds. It is also thought that at least some SNe Ic are the result of binary star interactions, although single star progenitor channels may also exist.…”

Section: Converting Stellar Age To Mmentioning

confidence: 99%

The 50–100 pc scale parent stellar populations of Type II supernovae and limitations of single star evolution models

Schady

Eldridge

Anderson

et al. 2019

Monthly Notices of the Royal Astronomical Society

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There is observational evidence of a dearth in core-collapse supernova (ccSN) explosions from stars with zero age main sequence (ZAMS) mass M 0 ≈ 17 − 30M , referred to as the 'red supergiant problem'. However, simulations now predict that above 20 M , we should indeed only expect stars within certain pockets of M 0 to produce a visible SN explosion. Validating these predictions requires large numbers of ccSNe of different types with measured M 0 which is challenging. In this paper we explore the reliability of using host galaxy emission lines and the Hα equivalent width to constrain the age, and thus the M 0 of ccSNe progenitors. We use the Binary Population and Spectral Synthesis models to infer a stellar population age from MUSE observations of the ionised gas properties and Hα EW at the location of eleven ccSNe with reliable M 0 measurements. Comparing our results to published M 0 values, we find that models that do not consider binary systems yield stellar ages that are systematically too young (thus M 0 too small), whereas accounting for binary system interactions typically overpredict the stellar age (thus underpredict M 0 ). Taking into account the effects of photon leakage bring our M 0 estimates in much closer agreement with expectations. These results highlight the need for careful modelling of diffuse environments, such as are present in the vicinity of type II SNe, before ionised emission line spectra can be used as reliable tracers of progenitor stellar age.

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“…A key benefit of this analysis is that it provides a basic comparative measure of the location properties of different types of sources, such as SNe and the types of stars that are their likely progenitors (see e.g. Leloudas et al 2010;Kangas et al 2017); however, its main disadvantage is that it only probes the bulk properties of the environment, but not the specific physical processes associated with the evolution of populations of massive stars or their influence on the environments (Crowther 2013).…”

Section: Normalised Pixel Statisticsmentioning

confidence: 99%

The very young resolved stellar populations around stripped-envelope supernovae

Maund

2018

Monthly Notices of the Royal Astronomical Society

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The massive star origins for Type IIP supernovae (SNe) have been established through direct detection of their red supergiants progenitors in pre-explosion observations; however, there has been limited success in the detection of the progenitors of H-deficient SNe. The final fate of more massive stars, capable of undergoing a Wolf-Rayet phase, and the origins of Type Ibc SNe remains debated, including the relative importance of single massive star progenitors or lower mass stars stripped in binaries. We present an analysis of the ages and spatial distributions of massive stars around the sites of 23 stripped-envelope SNe, as observed with the Hubble Space Telescope, to probe the possible origins of the progenitors of these events. Using a Bayesian stellar populations analysis scheme, we find characteristic ages for the populations observed within 150 pc of the target Type IIb, Ib and Ic SNe to be log(t) = 7.20, 7.05 and 6.57, respectively. The Type Ic SNe in the sample are nearly all observed within 100 pc of young, dense stellar populations. The environment around SN 2002ap is an important exception both in terms of age and spatial properties. These findings may support the hypothesis that stars with M init > 30M produce a relatively large proportion of Type Ibc SNe, and that these SN subtypes arise from progressively more massive progenitors. Significantly higher extinctions are derived towards the populations hosting these SNe than previously used in analysis of constraints from pre-explosion observations. The large initial masses inferred for the progenitors are in stark contrast with the low ejecta masses estimated from SN light curves.

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

Cited by 27 publications

References 129 publications

Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy

Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy

The 50–100 pc scale parent stellar populations of Type II supernovae and limitations of single star evolution models

The very young resolved stellar populations around stripped-envelope supernovae

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