Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey

By F. Taddia, J. Sollerman, G. Leloudas, M. Stritzinger, S. Valenti, L. Galbany, R. Kessler, D. Schneider, J. C. Wheeler. 2014

140 citations recorded by the source corpus.

Context. Type Ib/c supernovae (SNe Ib/c) have been investigated in several single-object studies. However, there is still a paucity of works concerning larger, homogeneous samples of these hydrogen-poor transients, in particular regarding the pre-maximum phase of their light curves. Aims. In this paper we present and analyse the early-time optical light curves (LCs, ugriz) of 20 SNe Ib/c from the Sloan Digital Sky Survey (SDSS) SN survey II, aiming to study their observational and physical properties as well as to derive their progenitor parameters. Methods. High-cadence, multi-band LCs are fitted with a functional model and the best-fit parameters are compared among the SN types. Bolometric LCs (BLCs) are constructed for the entire sample. We also computed the black-body (BB) temperature (TBB) and photospheric radius (Rph) evolution for each SN via BB fits on the spectral energy distributions. In addition, the bolometric properties are compared to both hydrodynamical and analytical model expectations. Results. Complementing our sample with literature data, we find that SNe Ic and Ic-BL (broad-line) have shorter rise times than those of SNe Ib and IIb. The decline rate parameter, m15, is similar among the different sub-types. SNe Ic appear brighter and bluer than SNe Ib, but this difference vanishes if we consider host galaxy extinction corrections based on colors. Templates for SN Ib/c LCs are presented. Our SNe have typical TBB of 10000 K at peak, and Rph of 10 15 cm. Analysis of the BLCs of SNe Ib and Ic gives typical ejecta masses Mej 3.6 5.7 M , energies EK 1.5 1.7 10 51 erg, and M( 56 Ni) 0.3 M . Higher values for EK and M( 56 Ni) are estimated for SNe Ic-BL (Mej 5.4 M , EK 10.7 10 51 erg, M( 56 Ni) 1.1 M ). For the majority of SNe Ic and Ic-BL we can put strong limits ( 5.9 days plateau seems to be detected. The rising part of the BLCs is reproduced by power laws with index<2. For two events (SN 2005hm and SN 2007qx) we find signatures of a possible shock break-out cooling tail. Conclusions. Based on the limits for the plateau length and on the slow rise of the BLCs, we find that in most of our SNe Ic and Ic-BL the 56 Ni is mixed up to the outer layers, suggesting that SN Ic progenitors are de facto helium poor. The derived progenitor parameters ( 56 Ni, EK , Mej) are consistent with previous works.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/eb3f48e105324df016d2ac5698bc1d9747136354

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In Astronomy and Astrophysics

1. E. Berger
2. S. Smartt
3. Bing Zhang
4. Z. Cano
5. A. Filippenko
6. B. Metzger
7. A. Gal-yam
8. S. Valenti

In Instrumentation

1. S. Smartt
2. Morgan Fraser
3. A. Filippenko
4. A. Gal-yam
5. S. Valenti
6. Z. Cano
7. P. James
8. A. Jerkstrand

Citations in the corpus

• Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, methodology): “6, however the interested reader is directed to Taddia et al. (2015) for a more thorough discussion of rise times.”
• PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 (2016, result): “This is not consistent with the observed ejecta-mass range of 3.6−5.7 M derived for most SNe Ibc by Taddia et al. (2015).”
• The Carnegie Supernova Project I: analysis of stripped-envelope supernova light curves (2017, methodology): “However, recently we have found evidences for significant mixing in the SNe Ic from studying the SDSS-II SE SN sample (Taddia et al. 2015).”
• 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.”
• On the diversity of superluminous supernovae: ejected mass as the dominant factor (2015, methodology): “This contains a compilation of SNe Ibc from the literature that have good photometric data in griz, as well as the homogeneous SDSS II sample of Taddia et al. (2015)”
• 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, background): “Next, [272] showed that for a sample of SNe Ibc, SNe Ib, Ic, and IcBL have faster rising LCs than SNe Ib, implying that the ejecta in these events are probably well mixed.”
• 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).”