DISCOVERY OF THE BROAD-LINED TYPE Ic SN 2013cq ASSOCIATED WITH THE VERY ENERGETIC GRB 130427A

Xu, D.; Postigo, A. de Ugarte; Leloudas, G.; Krühler, T.; Cano, Z.; Hjorth, J.; Malesani, D.; Fynbo, J. P. U.; Thöne, C. C.; Sánchez-Ramírez, R.; Schulze, S.; Jakobsson, P.; Kaper, L.; Sollerman, J.; Watson, Derrick G.; Cabrera-Lavers, A.; Cao, Chen; Covino, S.; Flores, H.; Geier, S.; Gorosabel, J.; Hu, Shaoming; Milvang-Jensen, B.; Sparre, Martin; Xin, L. P.; Zhang, T. M.; Zheng, W.; Zou, Yuan‐Chuan

doi:10.1088/0004-637x/776/2/98

Cited by 122 publications

(112 citation statements)

References 47 publications

Supporting

Mentioning

102

Contrasting

Order By: Relevance

“…In SN 2013cq this feature appears to be broader and blueshifted relative to SN 1998bw, as observed by Xu et al (2013). Our comparison suggests that this peak may fit better with the slightly higher velocity SN 2003dh (Hjorth et al 2003;Mazzali et al 2003), the only one of the comparison SNe to arise from a luminous cosmological GRB.…”

Section: Supernova Propertiessupporting

confidence: 62%

“…A full description of the afterglow is given in Perley et al (2014) and Maselli et al (2014). Deep photometric and spectroscopic observations over the first 10 days post burst revealed a rebrightening, consistent with the presence of an SNe Ic, SN 2013cq Xu et al 2013). …”

Section: Observationssupporting

confidence: 56%

“…Alternatively, this could be suggestive of a much higher velocity SN such as SN 2010bh (Bufano et al 2012;Cano et al 2011) as favored by Xu et al (2013), who infer v ph = 32,000 km s −1 from the Fe ii (5169 Å) at an epoch of 12.5 restframe days. This does provide a good match to the location and width of the feature; however, the overall spectral shape and luminosity of SN 2010bh are also very different from SN 2013cq.…”

Section: Supernova Propertiesmentioning

confidence: 93%

“…In particular, the proximate, bright star-forming region considerably contaminates the SNe (>20% at the red end of our spectrum beyond 9000 Å). This region is also likely to be the dominant host contaminant in ground-based spectroscopy (since the host galaxy is resolved), and has quite different colors from the global host, implying potentially significant systematic errors when the broadband Sloan Digital Sky Survey (SDSS) colors of the host are used to attempt a subtraction (e.g., Xu et al 2013;Melandri et al 2014). Here, we can directly remove this contribution via the subtraction of the deep second epoch.…”

Section: Isolating the Supernovamentioning

confidence: 99%

“…The isotropic energy release of E iso ∼ 10 54 erg, places it in the most luminous 5% of GRBs observed to date by Swift, and a factor of 100 brighter than GRB 030329 (Hjorth et al 2003), which was the most luminous GRB with a well-studied SN. At a redshift of z = 0.340 (Levan et al 2013;Xu et al 2013;Perley et al 2014), the burst is close enough that any SN is open to spectroscopic study, and indeed the presence of an SN, SN 2013cq, has been established Xu et al 2013). Here, we use the resolution of the Hubble Space Telescope (HST) to resolve and dramatically reduce the galaxy contribution and its UV capability to track the afterglow, hence enabling a view of the SN as free as possible from the host, afterglow, and atmospheric hinderance.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

HUBBLE SPACE TELESCOPEOBSERVATIONS OF THE AFTERGLOW, SUPERNOVA, AND HOST GALAXY ASSOCIATED WITH THE EXTREMELY BRIGHT GRB 130427A

Levan¹,

Tanvir²,

Fruchter³

et al. 2014

ApJ

Self Cite

View full text Add to dashboard Cite

We present Hubble Space Telescope (HST) observations of the exceptionally bright and luminous Swift gamma-ray burst (GRB), GRB 130427A. At z = 0.34, this burst affords an excellent opportunity to study the supernova (SN) and host galaxy associated with an intrinsically extremely luminous burst (E iso > 10 54 erg): more luminous than any previous GRB with a spectroscopically associated SN. We use the combination of the image quality, UV capability, and invariant point-spread function of HST to provide the best possible separation of the afterglow, host, and SN contributions to the observed light ∼17 rest-frame days after the burst, utilizing a host subtraction spectrum obtained one year later. Advanced Camera for Surveys grism observations show that the associated SN, SN 2013cq, has an overall spectral shape and luminosity similar to SN 1998bw (with a photospheric velocity, v ph ∼ 15,000 km s −1 ). The positions of the bluer features are better matched by the higher velocity SN 2010bh (v ph ∼ 30,000 km s −1 ), but this SN is significantly fainter and fails to reproduce the overall spectral shape, perhaps indicative of velocity structure in the ejecta. We find that the burst originated ∼4 kpc from the nucleus of a moderately star forming (1 M yr −1 ), possibly interacting disk galaxy. The absolute magnitude, physical size, and morphology of this galaxy, as well as the location of the GRB within it, are also strikingly similar to those of GRB 980425/SN 1998bw. The similarity of the SNe and environment from both the most luminous and least luminous GRBs suggests that broadly similar progenitor stars can create GRBs across six orders of magnitude in isotropic energy.

show abstract

Section: Supernova Propertiessupporting

confidence: 62%

Section: Observationssupporting

confidence: 56%

Section: Supernova Propertiesmentioning

confidence: 93%

Section: Isolating the Supernovamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

HUBBLE SPACE TELESCOPEOBSERVATIONS OF THE AFTERGLOW, SUPERNOVA, AND HOST GALAXY ASSOCIATED WITH THE EXTREMELY BRIGHT GRB 130427A

Levan¹,

Tanvir²,

Fruchter³

et al. 2014

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

Gamma-Ray Burst Progenitors

Levan¹,

Crowther²,

Grijs³

et al. 2016

Gamma-Ray Bursts

View full text Add to dashboard Cite

We review our current understanding of the progenitors of both long and short duration gamma-ray bursts (GRBs). Constraints can be derived from multiple directions, and we use three distinct strands; (i) direct observations of GRBs and their host galaxies, (ii) parameters derived from modelling, both via population synthesis and direct numerical simulation and (iii) our understanding of plausible analog progenitor systems observed in the local Universe. From these joint constraints, we describe the likely routes that can drive massive stars to the creation of long GRBs, and our best estimates of the scenarios that can create compact object binaries which will ultimately form short GRBs, as well as the associated rates of both long and short GRBs. We further discuss how different the progenitors may be in the case of black hole engine or millisecond-magnetar models for the production of GRBs, and how central engines may provide a unifying theme between many classes of extremely luminous transient, from luminous and super-luminous supernovae to long and short GRBs.

show abstract

Gamma-Ray Bursts

Wang

Zhang

2022

Handbook of X-Ray and Gamma-Ray Astrophysics

View full text Add to dashboard Cite

DISCOVERY OF THE BROAD-LINED TYPE Ic SN 2013cq ASSOCIATED WITH THE VERY ENERGETIC GRB 130427A

Cited by 122 publications

References 47 publications

HUBBLE SPACE TELESCOPEOBSERVATIONS OF THE AFTERGLOW, SUPERNOVA, AND HOST GALAXY ASSOCIATED WITH THE EXTREMELY BRIGHT GRB 130427A

HUBBLE SPACE TELESCOPEOBSERVATIONS OF THE AFTERGLOW, SUPERNOVA, AND HOST GALAXY ASSOCIATED WITH THE EXTREMELY BRIGHT GRB 130427A

Gamma-Ray Burst Progenitors

Gamma-Ray Bursts

Contact Info

Product

Resources

About