Abstract
Long-duration gamma-ray bursts (GRBs) have been found to be associated with broad-lined type-Ic supernovae (SNe), but only a handful of cases have been studied in detail. Prompted by the discovery of the exceptionally bright, nearby GRB130427A (redshift z=0.3399), we aim at characterising the properties of its associated SN2013cq. This is the first opportunity to test directly the progenitors of high-luminosity GRBs. We monitored the field of the Swift long duration GRB130427A using the 3.6-m TNG and the 8.2-m VLT during the time interval between 3.6 and 51.6 days after the burst. Photometric and spectroscopic observations revealed the presence of the type Ic SN2013cq. Spectroscopic analysis suggests that SN2013cq resembles two previous GRB-SNe, SN1998bw and SN2010bh associated with GRB980425 and XRF100316D, respectively. The bolometric light curve of SN2013cq, which is significantly affected by the host galaxy contribution, is systematically more luminous than that of SN2010bh ($\sim$ 2 mag at peak), but is consistent with SN1998bw. The comparison with the light curve model of another GRB-connected SN2003dh, indicates that SN2013cq is consistent with the model when brightened by 20%. This suggests a synthesised radioactive $^{56}$Ni mass of $\sim 0.4 M_\odot$. GRB130427A/SN2013cq is the first case of low-z GRB-SN connection where the GRB energetics are extreme ($E_{\rm \gamma, iso} \sim 10^{54}$ erg). We show that the maximum luminosities attained by SNe associated with GRBs span a very narrow range, but those associated with XRFs are significantly less luminous. On the other hand the isotropic energies of the accompanying GRBs span 6 orders of magnitude (10$^{48}$ erg $< E_{\rm \gamma, iso} <$ 10$^{54}$ erg), although this range is reduced when corrected for jet collimation. The GRB total radiated energy is in fact a small fraction of the SN energy budget.
Highlights
The majority of nearby under-energetic long duration gammaray bursts and X-ray flashes (GRBs and XRFs1 with total isotropic energy Eiso < 1051 erg) are associated with with highly energetic supernovae (SNe; Mazzali et al 2006a,b)
We show that the maximum luminosities attained by SNe associated with gamma-ray bursts (GRBs) span a very narrow range, but those associated with XRFs are significantly less luminous
GRB 130427A follows the well known Amati (Epeak−Eiso, Amati et al 2002) and Yonetoku (Epeak−Liso, Yonetoku et al 2004) correlations (Maselli et al 2014). This made the study of the properties and evolution of SN 2013cq interesting, since no very energetic GRB has ever been detected at relatively low redshift, so that this is the first occurrence of a connection between a SN and a GRB that has all the characteristics of a cosmological event
Summary
The majority of nearby under-energetic long duration gammaray bursts and X-ray flashes (GRBs and XRFs1 with total isotropic energy Eiso < 1051 erg) are associated with with highly energetic supernovae (SNe; Mazzali et al 2006a,b). GRB 130427A follows the well known Amati (Epeak−Eiso, Amati et al 2002) and Yonetoku (Epeak−Liso, Yonetoku et al 2004) correlations (Maselli et al 2014) This made the study of the properties and evolution of SN 2013cq interesting, since no very energetic GRB has ever been detected at relatively low redshift, so that this is the first occurrence of a connection between a SN and a GRB that has all the characteristics of a cosmological event. The extraordinarily high observed energetics of GRB 130427A and its closeness motivated our optical multi-band search and the intensive follow-up of its associated SN
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
