Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae

By J. Lyman, D. Bersier, P. James, P. Mazzali, J. Eldridge, Morgan Fraser, E. Pian. 2014

250 citations recorded by the source corpus.

Literature data are collated for 38 stripped-envelope core-collapse supernovae (SE SNe; i.e. SNe IIb, Ib, Ic and Ic-BL) that have good light curve coverage in more than one optical band. Using bolometric corrections derived in previous work, the bolometric light curve of each SN is recovered and template bolometric light curves provided. Peak light distributions and decay rates are investigated; SNe subtypes are not cleanly distinguished in this parameter space, although some grouping of types does occur and there is a suggestion of a Phillips-like relation for most SNe Ic-BL. The bolometric light curves are modelled with a simple analytical prescription and compared to results from more detailed modelling. Distributions of the explosion parameters shows the extreme nature of SNe Ic-BL in terms of their 56Ni mass and the kinetic energy, however ejected masses are similar to other subtypes. SNe Ib and Ic have very similar distributions of explosion parameters, indicating a similarity in progenitors. SNe~IIb are the most homogeneous subtype and have the lowest average values for 56Ni mass, ejected mass, and kinetic energy. Ejecta masses for each subtype and SE SNe as a whole are inconsistent with those expected from very massive stars. The majority of the ejecta mass distribution is well described by more moderately massive progenitors in binaries, indicating these are the dominant progenitor channel for SE SNe.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6634f8498631e63275e00b9e85032f6790a34547

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. S. Smartt
2. M. Limongi
3. A. Chieffi
4. S. Valenti
5. A. Filippenko
6. A. Gal-yam
7. Z. Cano
8. J. Sollerman

In Nuclear and High Energy Physics

1. A. Chieffi
2. M. Limongi
3. S. Smartt
4. A. Gal-yam
5. Z. Cano
6. Xuefeng Wu
7. Z. Dai
8. Shan-Qin Wang

Citations in the corpus

• The Zwicky Transient Facility: Science Objectives (2019, background): “…supernovae (SE SNe) samples currently available in the literature are mainly targeted (i.e., 34 SE SNe in Taddia et al. 2018b, CSP), and non-homogenous (i.e. collections by Cano 2013, Lyman et al. 2016, and Prentice et al. 2016), or rather small (i.e., 20 SNe in Taddia et al. 2015, SDSS II).”
• Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range −3 ≤ [Fe/H] ≤ 0 (2018, methodology): “…ejected masses of 3–4Me estimated from the SNIb light curve fitting (Wheeler & Levreault 1985; Ensman & Woosley 1988; Dessart et al. 2011, 2015, 2016; Lyman et al. 2016); and (d) a limiting mass between SNIIP and SNIb corresponding to MIIP∼17Me implies a fraction of SNIb of ∼26% of all…”
• PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 (2016, background): “Similar low values for ejecta masses of SNe Ib/c were also deduced by Cano (2013) and Lyman et al. (2016).”
• Observational and Physical Classification of Supernovae (2016, unknown): “This finding is confirmed by Taddia et al. (2015) and Lyman et al. (2016), in particular regarding the pre-peak, rising part of the light curve, and applies even for unusually luminous events such as SN 2010ay (Sanders et al. 2012).”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, methodology): “een determine by sophisticated numerical simulations (hydrodynamical models coupled with radiative transfer codes) [3,7,36,47,48,108,111,112,113,114,115,116,117,118,119,120], and analytical modelling [17,25,31,32,40,41,43,107,121,122,123]. A summary of the derived bolometric properties for individua”
• The Carnegie Supernova Project I: analysis of stripped-envelope supernova light curves (2017, methodology): “Following the approach by Lyman et al. (2016), we consider that single progenitor star models with initial masses above 20 M⊙, computed by the binary population and spectral synthesis (BPASS) code (Eldridge et al. 2008; Eldridge & Stanway 2009), cannot produce ejecta masses below a value of about…”