On the Light Curve and Spectrum of SN 2003dh Separated from the Optical Afterglow of GRB 030329
On the Light Curve and Spectrum of SN 2003dh Separated from the Optical Afterglow of GRB 030329
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DOI：
10.1086/429284
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发表时间：
2005-01
期刊：
影响因子：
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通讯作者：
J. Deng;J. Deng;N. Tominaga;P. Mazzali;K. Maeda;K. Nomoto
中科院分区：
文献类型：
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作者：
J. Deng;J. Deng;N. Tominaga;P. Mazzali;K. Maeda;K. Nomoto
根据GRB 030329的光谱资料，计算了超新星2003 dh的净光变曲线和光谱，时间跨度从超新星极大前约6天到极大后约60天。使用早期余辉模板从观测到的光谱中减去U波段通量的大部分，因为在富含金属的快速移动的SN大气中，强线覆盖极大地抑制了UV和U波段SN通量。用与超新星SN 1998 bw相连的伽马射线暴（GRB）的蓝端光谱来确定扣除量。宿主星系模板的减少影响了后期的结果。SN 2003 dh的光变曲线比SN 1998 bw窄，在达到最大值之前上升得一样快，达到一个可能较暗的最大值，然后下降得快1.2-1.4倍。然后建立UVOIR辐射热SN光变曲线。考虑到不确定性，可以用Mej ~ 7 ± 3 M，EK ~ 3.5 ± 1.5 × 1052尔格，EK/Mej ~ 5符合以前的谱模型，M（56 Ni）~ 0.4 M的球形喷出物模型来再现。这表明其前身主序质量约为25-40 M，低于SN 1998 bw，但明显高于正常的Ic型超新星SN e和与GRB无关的超新星SN 2002 ap。
The net optical light curves and spectra of the supernova (SN) 2003dh are obtained from the published spectra of GRB 030329, covering about 6 days before SN maximum to about 60 days after. The bulk of the U-band flux is subtracted from the observed spectra using early-time afterglow templates, because strong line blanketing greatly depresses the UV and U-band SN flux in a metal-rich, fast-moving SN atmosphere. The blue-end spectra of the gamma-ray burst (GRB) connected hypernova SN 1998bw is used to determine the amount of subtraction. The subtraction of a host galaxy template affects the late-time results. The derived SN 2003dh light curves are narrower than those of SN 1998bw, rising as fast before maximum, reaching a possibly fainter maximum, and then declining ~ 1.2-1.4 times faster. We then build UVOIR bolometric SN light curve. Allowing for uncertainties, it can be reproduced with a spherical ejecta model of Mej ~ 7 ± 3 M☉, EK ~ 3.5 ± 1.5 × 1052 ergs, with EK/Mej ~ 5 following previous spectrum modeling, and M(56Ni) ~ 0.4 M☉. This suggests a progenitor main-sequence mass of ~25-40 M☉, lower than SN 1998bw but significantly higher than normal Type Ic SNe and the GRB-unrelated hypernova SN 2002ap.