DISCOVERY OF THE BROAD-LINED TYPE Ic SN 2013cq ASSOCIATED WITH THE VERY ENERGETIC GRB 130427A
DISCOVERY OF THE BROAD-LINED TYPE Ic SN 2013cq ASSOCIATED WITH THE VERY ENERGETIC GRB 130427A
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DOI：
10.1088/0004-637x/776/2/98
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发表时间：
2013-05
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影响因子：
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通讯作者：
D. Xu;A. U. Postigo;G. Leloudas;T. Kruhler;Z. Cano;J. Hjorth;D. Malesani;J. Fynbo;C. Thoene-C.-Thoen
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作者：
D. Xu;A. U. Postigo;G. Leloudas;T. Kruhler;Z. Cano;J. Hjorth;D. Malesani;J. Fynbo;C. Thoene-C.-Thoen
z < 1的长持续时间伽玛射线暴（GRB）在大多数情况下都伴随着明亮的宽线Ic型超新星（SNe Ic-BL）。最高能量的伽玛暴大多位于高红移处，那里的超新星很难被观测到。在这里，我们提出了早期和后期的观测光学对应的非常活跃的GRB 130427 A。尽管有中等的红移，z = 0.3399 ± 0.0002，GRB 130427 A处于GRB能量分布的高端，各向同性等效能量释放为Eiso = 9.6 × 1053 erg，比其他光谱证实SNe的GRB能量高出一个数量级。在我们密集的光度监测中，我们检测到宿主减去r波段光变曲线中的过量通量，与新兴SN的预期一致，比原型SN 1998 bw暗1.02等。在SN峰值（GRB后16.7天）前后获得的光谱显示了SNe Ic-BL典型的宽起伏，证实了SN的存在，命名为SN 2013 cq。光谱形状和早期峰值时间与GRB 100316 D的高膨胀速度SN 2010 bh相似。我们的研究结果表明，高能量，长持续时间的伽玛暴，通常在高红移检测到，也可以与SNe Ic-BL，指向一个共同的祖先机制。
Long-duration gamma-ray bursts (GRBs) at z < 1 are found in most cases to be accompanied by bright, broad-lined Type Ic supernovae (SNe Ic-BL). The highest-energy GRBs are mostly located at higher redshifts, where the associated SNe are hard to detect observationally. Here, we present early and late observations of the optical counterpart of the very energetic GRB 130427A. Despite its moderate redshift, z = 0.3399 ± 0.0002, GRB 130427A is at the high end of the GRB energy distribution, with an isotropic-equivalent energy release of Eiso ∼ 9.6 × 1053 erg, more than an order of magnitude more energetic than other GRBs with spectroscopically confirmed SNe. In our dense photometric monitoring, we detect excess flux in the host-subtracted r-band light curve, consistent with that expected from an emerging SN, ∼0.2 mag fainter than the prototypical SN 1998bw. A spectrum obtained around the time of the SN peak (16.7 days after the GRB) reveals broad undulations typical of SNe Ic-BL, confirming the presence of an SN, designated SN 2013cq. The spectral shape and early peak time are similar to those of the high expansion velocity SN 2010bh associated with GRB 100316D. Our findings demonstrate that high-energy, long-duration GRBs, commonly detected at high redshift, can also be associated with SNe Ic-BL, pointing to a common progenitor mechanism.