The Broad-lined Type Ic SN 2003jd

By S. Valenti, S. Benetti, E. Cappellaro, Ferdinando Patat, P. Mazzali, Massimo Turatto, K. Hurley, K. Maeda, A. Gal-yam, R. Foley and 21 more. 2007

171 citations recorded by the source corpus.

The results of a world-wide coordinated observational campaign on the broad-lined Type Ic SN 2003jd are presented. In total, 74 photometric data points and 26 spectra were collected using 11 different telescopes. SN 2003jd is one of the most luminous SN Ic ever observed. A comparison with other Type Ic supernovae (SNe Ic) confirms that SN 2003jd represents an intermediate case between broad-line events (2002ap, 2006aj), and highly energetic SNe (1997ef, 1998bw, 2003dh, 2003lw), with an ejected mass of M_{ej} = 3.0 +/- 1 Mo and a kinetic energy of E_{k}(tot) = 7_{-2}^{+3} 10^{51} erg. SN 2003jd is similar to SN 1998bw in terms of overall luminosity, but it is closer to SNe 2006aj and 2002ap in terms of light-curve shape and spectral evolution. The comparison with other SNe Ic, suggests that the V-band light curves of SNe Ic can be partially homogenized by introducing a time stretch factor. Finally, due to the similarity of SN 2003jd to the SN 2006aj/XRF 060218 event, we discuss the possible connection of SN 2003jd with a GRB.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5782b08cc7d226e8ea0b9babfb97a070767b6947

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Citations in the corpus

The diversity of Type II supernova versus the similarity in their progenitors (2016, methodology): “All magnitudes were converted to fluxes and integrated using Simpson’s Rule (see Valenti et al. 2008, for more details on this method).”
On the diversity of superluminous supernovae: ejected mass as the dominant factor (2015, methodology): “Since the input time-scale is known for 56Ni-powered SNe, the light-curve width is typically a measurement of the diffusion time (e.g. Arnett 1982; Valenti et al. 2008a; Drout et al. 2011).”
The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, background): “…et al. (2010), Hunter et al. (2009) 2006aj Ic 1.3 2 Mazzali et al. (2006), Maeda et al. (2007) 2002ap Ic 1.2 2.5 Mazzali et al. (2007) 2003jd Ic – 3 Valenti et al. (2008a) 2008D Ib 1.1 3.6 Dessart et al. (2012) 2004aw Ic – 5 Valenti et al. (2008a) 2009jf Ib – 5–7 Valenti et al. (2011) 1997ef…”
Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey (2014, background): “…single-object papers (e.g., SN 2004aw, Taubenberger et al. 2006; SN 2007Y, Stritzinger et al. 2009; SN 1999ex Stritzinger et al. 2002; SN 2003jd Valenti et al. 2008; SN 2007gr Hunter et al. 2009; SN 2009bb Pignata et al. 2011; SN 2003dh Lipkin et al. 2004; SN 2010bh Cano et al. 2011), but not…”
Nebular emission-line profiles of Type Ib/c supernovae - Probing the ejecta asphericity (2009, methodology): “Another 4 spectra of the Asiago archive were shown by Turatto (2003) and Valenti et al. (2008) before.”
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).”
Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae (2009, methodology): “…curve and 56Ni Mass The bolometric light curve of SN 2004et was computed by correcting the observed magnitudes for reddening and convertig to flux values before integrating the combined flux from theUBVRIJHK bands excluding the overlapping regions of the filters (see also Valenti et al. 2008).”
A new method for estimating the bolometric properties of Ibc supernovae (2013, methodology): “Instead other means of ascertaining the properties of the progenitor stars has arisen mostly via modelling of spectroscopy and photometry of the SNe themselves (e.g. Iwamoto et al. 1998; Mazzali et al. 2002; Valenti et al. 2008).”
Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, methodology): “…per cent uncertainty in our choice of κopt = 0.06 cm2 g−1; previous studies have assumed values of 0.05 (Drout et al. 2011), 0.06 (Maeda et al. 2003; Valenti et al. 2008), 0.07 (Cano 2013; Taddia et al. 2015) and 0.08 cm2 g−1 (Pignata et al. 2011), largely driven by the values of κopt near peak…”