THE HIGHLY ENERGETIC EXPANSION OF SN 2010bh ASSOCIATED WITH GRB 100316D
THE HIGHLY ENERGETIC EXPANSION OF SN 2010bh ASSOCIATED WITH GRB 100316D
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DOI：
10.1088/0004-637x/753/1/67
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发表时间：
2011-11
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通讯作者：
F. Bufano;E. Pian;J. Sollerman;S. Benetti;G. Pignata;S. Valenti;S. Covino;P. D’Avanzo;D. Malesani;E. Cappellaro;M. Della Valle;J. Fynbo;J. Hjorth;P. Mazzali;D. Reichart;R. Starling;M. Turatto;S. Vergani;K. Wiersema;L. Amati;D. Bersier;S. Campana;Z. Cano;A. Castro-Tirado;G. Chincarini;V. D’Elia;A. de Ugarte Postigo;J. Deng;P. Ferrero;A. Filippenko;P. Goldoni;J. Gorosabel;J. Greiner;F. Hammer;P. Jakobsson;L. Kaper;K. Kawabata;S. Klose;A. Levan;K. Maeda;N. Masetti;B. Milvang-Jensen;F. Mirabel;P. Møller;K. Nomoto;E. Palazzi;S. Piranomonte;R. Salvaterra;G. Stratta;G. Tagliaferri;Masaomi Tanaka;N. Tanvir;R. Wijers
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作者：
F. Bufano;E. Pian;J. Sollerman;S. Benetti;G. Pignata;S. Valenti;S. Covino;P. D’Avanzo;D. Malesani;E. Cappellaro;M. Della Valle;J. Fynbo;J. Hjorth;P. Mazzali;D. Reichart;R. Starling;M. Turatto;S. Vergani;K. Wiersema;L. Amati;D. Bersier;S. Campana;Z. Cano;A. Castro-Tirado;G. Chincarini;V. D’Elia;A. de Ugarte Postigo;J. Deng;P. Ferrero;A. Filippenko;P. Goldoni;J. Gorosabel;J. Greiner;F. Hammer;P. Jakobsson;L. Kaper;K. Kawabata;S. Klose;A. Levan;K. Maeda;N. Masetti;B. Milvang-Jensen;F. Mirabel;P. Møller;K. Nomoto;E. Palazzi;S. Piranomonte;R. Salvaterra;G. Stratta;G. Tagliaferri;Masaomi Tanaka;N. Tanvir;R. Wijers
我们给出了附近(z=0.059)光谱确认的IC型超新星SN 2010bh的光谱和光度学演化，该超新星与软的、长时间的伽马射线暴(X射线闪光)GRB100316D有关。在欧洲南方天文台甚大望远镜(VLT)上使用X-Shooter和FORS2仪器对SN 2010bh进行了密集的后续观测。由于详细的时间覆盖和扩展的波长范围(3,000-24800ä)，我们在超新星中获得了前所未有的丰富的光谱序列，使SN 2010bh成为这一SN类别中研究得最好的代表之一。我们发现，与以前观测到的与伽玛暴有关的SN事件相比，SN 2010bh上升到最大亮度的速度更快(8.0±1.0个静止帧天数)，绝对峰值光度(Lbol≈3×10 42erg S−1)更弱。我们估算出的56Ni质量为0.12±0.02M☉。从广谱特征出发，我们测得S−1的膨胀速度可达47,000公里，高于SNE 1998bw(伽马暴980425)和2006aj(伽马暴060218)。光谱中可能存在氦吸收谱线He Iλ5876和He I 1.083μm，它们分别由∼2,000-30,000 kM S−1和∼28,000-38,000 kM S−1蓝移。然而，由于缺乏对He i 2.058μm线的报道，我们无法确认这样的身份。在爆炸后186天在∼拍摄的星云光谱显示，在6340ä处有一个宽广但微弱的[O I]发射。SN 2010bh的光曲线形状和光球膨胀速度表明，我们目睹了一次高能爆炸，抛射质量很小(Ek≈1052erg和Mej≈3M☉)。观察到的SN 2010bh的性质进一步扩展了GRB SNE类的异质性。
We present the spectroscopic and photometric evolution of the nearby (z = 0.059) spectroscopically confirmed Type Ic supernova, SN 2010bh, associated with the soft, long-duration gamma-ray burst (X-ray flash) GRB 100316D. Intensive follow-up observations of SN 2010bh were performed at the ESO Very Large Telescope (VLT) using the X-shooter and FORS2 instruments. Thanks to the detailed temporal coverage and the extended wavelength range (3000–24800 Å), we obtained an unprecedentedly rich spectral sequence among the hypernovae, making SN 2010bh one of the best studied representatives of this SN class. We find that SN 2010bh has a more rapid rise to maximum brightness (8.0 ± 1.0 rest-frame days) and a fainter absolute peak luminosity (Lbol ≈ 3 × 1042 erg s−1) than previously observed SN events associated with GRBs. Our estimate of the ejected 56Ni mass is 0.12 ± 0.02 M☉. From the broad spectral features, we measure expansion velocities up to 47,000 km s−1, higher than those of SNe 1998bw (GRB 980425) and 2006aj (GRB 060218). Helium absorption lines He i λ5876 and He i 1.083 μm, blueshifted by ∼20,000–30,000 km s−1 and ∼28,000–38,000 km s−1, respectively, may be present in the optical spectra. However, the lack of coverage of the He i 2.058 μm line prevents us from confirming such identifications. The nebular spectrum, taken at ∼186 days after the explosion, shows a broad but faint [O i] emission at 6340 Å. The light curve shape and photospheric expansion velocities of SN 2010bh suggest that we witnessed a highly energetic explosion with a small ejected mass (Ek ≈ 1052 erg and Mej ≈ 3 M☉). The observed properties of SN 2010bh further extend the heterogeneity of the class of GRB SNe.