A new method for estimating the bolometric properties of Ibc supernovae

By Z. Cano. 2013

134 citations recorded by the source corpus.

The bolometric properties (nickel mass, ejecta mass and kinetic energies) of 61 Ibc supernovae (SNe), including 20 gamma-ray burst and X-rayflash (GRB/XRF), 19 Ib, 13 Ic and nine Ic-BL (broad-lined) SNe are presented. All of the available BVRI photometry in the literature have been collected and used in a new method that utilizes a template supernova (SN 1998bw) and an analytical model to accurately estimate the bolometric properties of each SN. A statistical analysis of the bolometric properties is then performed, where it is found that GRB/XRF SNe are the most energetic, and eject more mass (including nickel content) than Ib, Ic and Ic-BL SNe. The results are then compared to the existing progenitor models of Ibc SNe, where it is concluded that it is highly likely that at least two progenitor channels exist for producing a Ibc SN: most Ibc SNe arise via binary interactions, where the mass of the stellar progenitor is less than what is attributed to a Wolf‐Rayet star. Conversely, the progenitors of Ic-BL and GRB/XRF are more massive than those of Ib and Ic SNe, and a key difference between GRB/XRF SNe and Ic-BL SNe is progenitor metallicity, where it is observed that the latter arise from more metal-rich progenitors. As mass loss in massive stars is influenced by metal content, theprogenitors ofIc-BLSNelosemoremass,and thereforemoreangular momentum, before exploding. It is expected that the explosion mechanism in Ic-BL and GRB/XRF SNe is ‘engine-driven’(i.e.anaccretingblackhole,oramillisecondmagnetar),buttheincreasedmass loss of Ic-BL SNe means the central engine is less powerful than in GRB/XRF SNe. Finally, it is found that the SNe that accompany GRBs and XRFs are statistically indistinguishable, and some mechanism other than metallicity is needed to explain the differences in the high-energy components in these events.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/91f5685a02ffbdcb3e0bb01ded712e8bb4b5a265

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In Astronomy and Astrophysics

1. S. Smartt
2. N. Smith
3. A. Filippenko
4. S. Valenti
5. D. Schneider
6. Z. Cano
7. A. Gal-yam
8. E. Berger

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).”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, methodology): “g s 1); ULGRBs: GRB-SNe associated with ultra-long-duration GRBs (see Section3). Excluding SN 2011kl. yunits: 1051 erg zunits: 1043 erg s 1 NB: Average bolometric properties of SNe Ib and Ic are from [17]. When SN 2011kl is included in the sample, L p = 1:2 1043 erg s 1, with ˙ Lp = 0:7 10 43 erg s ”
• 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).”
• Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, methodology): “This numerical factor difference is likely partly responsible for the somewhat smaller (albeit consistent) EK values for the subtype averages we find compared to Cano (2013), as discussed later.”
• Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death (2013, background): “The modeling of SN Ibc lightcurves also provides strong constraints to the amount of ejecta mass (e.g. Drout et al. 2011; Dessart et al. 2011; Cano 2013), with an average value of 4.6 M (Cano 2013).”
• The Carnegie Supernova Project I: analysis of stripped-envelope supernova light curves (2017, methodology): “As compared to SNe IIb, Ib and Ic, SNe IcBL are generally characterized by higher EK and larger 56Ni masses (see, e.g., Cano 2013; Taddia et al. 2015; Lyman et al. 2016).”
• Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey (2014, methodology): “These results were also found by (Drout et al. 2011) and Cano (2013).”