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

By M. Drout, A. Soderberg, A. Gal-yam, S. B. Cenko, D. Fox, D. Leonard, D. J. Sand, D. Moon, I. Arcavi, Yoav Green. 2010

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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 2004–2007. 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 Δt ≈ 10 days after V-band maximum is tightly distributed, 〈(V − R)V10〉 = 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 〈MR〉 = −17.9 ± 0.9 mag and 〈MR〉 = −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, 〈MR〉 = −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 56Ni masses of MNi ≈ 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 Mej ≈ 2 M☉ and EK ≈ 1051 erg for SNe Ibc, while for SNe Ic-BL we find higher values, Mej ≈ 5 M☉ and EK ≈ 1052 erg. We discuss the implications for the progenitors of SNe Ibc and their relation to those of engine-driven explosions.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9517e586d94ae0dcbbf4612bad636d4c9aded680

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Citations in the corpus

• The Carnegie Supernova Project I: analysis of stripped-envelope supernova light curves (2017, background): “Drout et al. (2011) published the first multi-band (V and R bands) sample of SNe Ib/c, studying 25 SNe; more recently, Bianco et al. (2014), Modjaz et al. (2014), and Liu et al. (2016) have published optical and near-infrared light curves and visual- wavelength spectroscopy of > 60 SE SNe followed…”
• TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE (2014, background): “In keeping with observations, our dust models assume that the CC SN population suffers from significantly more dust extinction than the SN Ia population, at all redshifts (e.g. Smartt et al. 2009; Drout et al. 2011; Kiewe et al. 2012; Mattila et al. 2012).”
• SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL (2013, background): “The grey box is the region where the two slopes are similar to within 25%. the ones derived for radioactivity-powered Type Ib/c ejecta (Ensman & Woosley 1988; Shigeyama et al. 1990; Valenti et al. 2011; Drout et al. 2011; Eldridge et al. 2013).”
• Short-Duration Gamma-Ray Bursts (2013, background): “Moreover, long GRB-SNe are generally more luminous than normal Type Ib/c SNe (Drout et al. 2011), although there is some overlap in the distributions.”
• Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars (2015, background): “The second additional argument for Ibc SNe coming from interacting binaries is that the ejecta masses calculated from lightcurve modelling are typically in the range 1–4 M (see Valenti et al. 2008; Drout et al. 2011, the results of which are summarised in Eldridge et al. 2013).”
• On the nature of supernovae Ib and Ic (2012, background): “In the last decade, the observational diversity of SNe Ib/c has been documented (Richardson, Branch & Baron 2006; Modjaz 2007; Drout et al. 2011).”
• The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, background): “…Nakamura et al. (2001) 2011bm Ic 5–10 7–17 Valenti et al. (2012) Sample average Ib – 2+1.1−0.8 Drout et al. (2011) Sample average Ic – 1.7+1.4−0.9 Drout et al. (2011) Sample average Ic-BL – 4.7+2.3−1.8 Drout et al. (2011) is the obvious way to explain the differences with a similar physical model.”
• On the diversity of superluminous supernovae: ejected mass as the dominant factor (2015, methodology): “Gal-Yam (2012) notes that some broad-lined SNe Ic, such as SN 2007D (Drout et al. 2011) and SN 2010ay (Sanders et al. 2012), reached peak magnitudes close to those of SLSNe, and likely required an additional energy source on top of the inferred ∼1 M of 56Ni.”
• MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE IN THREE DIMENSIONS (2014, background): “However, a small fraction of CCSNe are hyper-energetic (∼ 10B) and involve relativistic outflows (e.g., Soderberg et al. 2006; Drout et al. 2011).”
• The Magnetar Model for Type I Superluminous Supernovae. I. Bayesian Analysis of the Full Multicolor Light-curve Sample with MOSFiT (2017, result): “We compare these to literature values for normal and broad-lined SNe Ic from Drout et al. (2011) and Taddia et al. (2015), which we note have been derived following similarly simplistic assumptions about the ejecta structure.”
• A new method for estimating the bolometric properties of Ibc supernovae (2013, methodology): “…not unusual, however, as other authors have also used average velocities when calculating the bolometric properties of Ibc SNe using an Arnett-like model, e.g. Drout et al. (2011) used a larger value of 10, 000 km s−1, which although is larger than here, lies at the upper end of our distribution.”
• RAPIDLY EVOLVING AND LUMINOUS TRANSIENTS FROM PAN-STARRS1 (2014, methodology): “The limits on the more luminous transients are less constraining in comparison to type Ib/Ic SN. 8.2.”
• 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).”
• OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, methodology): “From a sample of well-observed V and R light curves of SESNe (e.g., Drout et al. 2011 and references therein), it appears (The complete figure set (72 images) is available in the online journal.) that the R-band maximum occurs 1–3 days later than V-band maximum.”