THE FIRST SYSTEMATIC STUDY OF TYPE Ibc SUPERNOVA MULTI-BAND LIGHT CURVES

Abstract

We present detailed optical photometry for 25 Type Ibc supernovae (SNe Ibc) within d ≈ 150 Mpc obtained with the robotic Palomar 60-inch telescope in [2004][2005][2006][2007]. This study represents the first uniform, systematic, and statistical sample of multi-band SNe Ibc light curves available to date. We correct the light curves for host galaxy extinction using a new technique based on the photometric color evolution, namely, we show that the (V − R) color of extinction-corrected SNe Ibc at ∆t ≈ 10 d after V −band maximum is tightly distributed, (V − R) V 10 = 0.26 ± 0.06 mag. Using this technique, we find that SNe Ibc typically suffer from significant host galaxy extinction, E(B −V ) ≈ 0.4 mag. A comparison of the extinction-corrected light curves for helium-rich (Type Ib) and helium-poor (Type Ic) SNe reveals that they are statistically indistinguishable, both in luminosity and decline rate. We report peak absolute magnitudes of M R = −17.9 ± 0.9 mag and M R = −18.3 ± 0.6 mag for SNe Ib and Ic, respectively. Focusing on the broad-lined (BL) SNe Ic, we find that they are more luminous than the normal SNe Ibc sample, M R = −19.0 ± 1.1 mag, with a probability of only 1.6% that they are drawn from the same population of explosions. By comparing the peak absolute magnitudes of SNe Ic-BL with those inferred for local engine-driven explosions (GRB-SN 1998bw, XRF-SN 2006aj, and SN 2009bb) we find a 25% probability that relativistic SNe are drawn from the overall SNe Ic-BL population. Finally, we fit analytic models to the light curves to derive typical 56 Ni masses of M Ni ≈ 0.2 and 0.5 M ⊙ for SNe Ibc and SNe Ic-BL, respectively. With reasonable assumptions for the photospheric velocities, we further extract kinetic energy and ejecta mass values of M ej ≈ 2 M ⊙ and E K ≈ 10 51 erg for SNe Ibc, while for SNe Ic-BL we find higher values, M ej ≈ 5 M ⊙ and E K ≈ 10 52 erg. We discuss the implications for the progenitors of SNe Ibc and their relation to those of engine-driven explosions.

Towards a better understanding of the evolution of Wolf–Rayet stars and Type Ib/Ic supernova progenitors

“…Massive progenitors of M f > 8 M ⊙ would result in too broad light curves compared to those of ordinary SNe Ic (e.g., Dessart et al 2017). Studies on SN light curves and spectra indicate that ordinary SNe Ic have ejecta masses less than about 5-6 M ⊙ (e.g., Drout et al 2011;Cano 2013;Taddia et al 2015;Lyman et al 2016), except for some extreme cases like iPTF15dtg (M ejecta ≈ 10 M ⊙ ; Taddia et al 2016). In this regard, our result with f WR = 1.58, which predicts M f 5 M ⊙ for SN Ic progenitors, is in better agreement with observations than those with the NL prescription.…”

The supernova–gamma-ray burst–jet connection

“…type Ic supernovae, with no hydrogen or helium in their spectra? Using the well-defined sample of normal Ic supernovae from Drout et al [30] and a more heterogeneous sample of BL Ic supernovae from a variety of sources, we plot cumulative histograms of their peak magnitudes in figure 4. Type Ic supernovae seem to be fainter than supernovae related to gamma-ray bursts, whereas the situation is less clear-cut for Ic-BL supernovae with no gamma-ray bursts.…”

“…[3]. The normal Ic supernovae are from Drout et al [30]. The Ic-BL distribution comes from a variety of sources and as such represents a more ill-defined sample.…”

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

“…In particular, the lack of hydrogen-rich layers in progenitors of stripped-envelope core-collapse SNe (i.e., Type IIb/Ib/Ic SNe), is often suggested to be caused by binary interaction (e.g., Wheeler & Levreault 1985;Ensman & Woosley 1988;Podsiadlowski, Joss, & Hsu 1992;Nomoto et al 1994;Shigeyama et al 1994;Woosley et al 1994;Bersten et al 2012Bersten et al , 2014Fremling et al 2014;Ergon et al 2015;Eldridge et al 2015;Lyman et al 2016a). The small typical ejecta mass estimated from light curves (LCs) of stripped-envelope SNe (≃ 1 − 5 M⊙, e.g., Sauer et al 2006;Drout et al 2011;Taddia et al 2015;Lyman et al 2016a), and nucleosynthetic signatures estimated from their spectral modeling (e.g., Jerkstrand et al 2015), support progenitors with relatively small zero-age main-sequence (ZAMS) masses. The less massive ZAMS mass stars need to remove their hydrogen-rich envelopes with mass loss caused by binary interactions because of their inefficient radiationdriven wind (e.g., Podsiadlowski, Joss, & Hsu 1992;Nomoto, Iwamoto, & Suzuki 1995;Podsiadlowski et al 2004b;Izzard, Ramirez-Ruiz, & Tout 2004;Yoon, Woosley, & Langer 2010;Eldridge, Langer, & Tout 2011;Benvenuto, Bersten, & Nomoto 2013;Lyman et al 2016a;Eldridge & Maund 2016).…”

“…While typical Type Ib/Ic SNe reach their peak luminosity in ∼ 20 days (e.g., Drout et al 2011;Prentice et al 2016), rapidly-evolving SN LCs rise in less than ∼ 10 days and decline quickly on a similar timescale (e.g., Poznanski et al 2010;Perets et al 2010;Kawabata et al 2010;Kasliwal et al 2010;Ofek et al 2010;Kasliwal et al 2012;Drout et al 2013Drout et al , 2014Inserra et al 2015). The simplest way to interpret the rapid LC evolution of some Type Ib/Ic SNe is that their ejecta mass is much smaller than in the more slowly evolving SNe (see also, e.g., Kleiser & Kasen 2014;Drout et al 2014;Tanaka et al 2016).…”